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RESULTS 

op 

ASTRONOMICAL  OBSERVATIONS 

MADE  DURING-  THE  YEARS  1834,  5,  6,  7,  8, 

AT  THE  CAPE  OF  GOOD  HOPE. 


RESULTS 

OF 

ASTRONOMICAL  OBSERVATIONS 

MADE   DURING  THE  YEARS    1834,  5,  6,  7,  8, 

AT  THE  CAPE  OF  GOOD  HOPE; 

BEING  THE  COMPLETION   OF  A  TELESCOPIC  SURVEY  OF  THE 
WHOLE  SURFACE  OF  THE  VISIBLE  HEAVENS. 

COMMENCED  IN  1825, 


BY 

Sir   JOHN   F.   W.    HERSCHEL,   Bart,,   K.  H. 

M.A. ;  D.C.L.;  F.R.S.  L.  &  E.  ;  Hon.  M.R.I.A.  ;  P.R.A.S. ;  F.G.S.  ;  M.C.U.P.S.; 

CORRESPONDENT  OR  HONORARY   MEMBER  OF   THE    IMPERIAL,    ROYAL,   AND   NATIONAL    ACADEMIES    OF  SCIENCES  OF 
BERLIN,  BRUSSELS,   COPENHAGEN,    GOTTINGEN,  HAARLEM,  MASSACHUSETTS    (u.  S.),  MODENA, 
NAPLES,   PARIS,   PETERSBURG,   STOCKHOLM,   TURIN,   AND   WASHINGTON   (u.  S.)  ; 
THE   ITALIAN   AND    HELVETIC    SOCIETIES  ; 
THE    ACADEMIES,    INSTITUTES,    ETC.    OF   ALBANY  (u.  S.),    BOLOGNA,  CATANIA   (GIOENIAN),  DIJON,  LAUSANNE. 
NANTES,    PADUA,    PALERMO,    ROME    (DEI    LINCEl),   VENICE    (ATHENAEUM),     AND    WILNA  ; 
THE   PHILOM ATHIC   SOCIETY  OF   PARIS  ;    ASIATIC   SOCIETY    OF   BENGAL  ; 
SOUTH    AFRICAN   LITERARY   AND   PHILOSOPHICAL   SOCIETY  (c.  G.  H.)  ;   LITERARY  AND   HISTORICAL   SOCIETY   OF  QUEBEC  : 

HISTORICAL  SOCIETY  OF   NEW  YORK  (u.  S.)  ; 
ROYAL  MEDICO-CHIRURGICAL  SOCIEY,  AND   INSTITUTION    OF    CIVIL   ENGINEERS,   LONDON  ; 
GEOGRAPHICAL   SOCIETY   OF   BERLIN;   ASTRONOMICAL   AND    METEOROLOGICAL   SOCIETY  OF   BRITISH  GUIANA: 

ETC.   ETC.  ETC. 


LONDON: 

PUBLISHED  BY  SMITH,  ELDEK  AND  CO.,  CORNHILL. 

1847. 


I  I  0  551 


HSZ 


London : 

Printed  by  Stewart  &  Murray, 
Old  Bailey. 


TO 

%\)t  JWemorp  of 

THE   LATE  ^ 

\ 

HUGH,   DUKE  OF  NORTHUMBERLAND, 

CHANCELLOR  OF  THE  UNIVERSITY  OF  CAMBRIDGE, 

THE  ENLIGHTENED  FRIEND 
AND   MUNIFICENT  PATRON   OF  SCIENCE, 

€f)t$  WlOVk 

IS    GRATEFULLY  INSCRIBED 

BY 

THE  AUTHOR. 


CONTENTS. 


Page 

Introduction       .......  v 


CHAPTER  I. 

Of  the  Nebulae  of  the  Southern  Hemisphere      ...  1 

CHAPTER  II. 

Of  the  Double  Stars  of  the  Southern  Hemisphere  .  165 


CHAPTER  III. 

Of  Astrometry,  or  the  Numerical  Expression  of  the  Apparent  Magnitudes  of 

the  Stars        .  .  .  .  .  .  .304 


CHAPTER  IV. 

Of  the  Distribution  of  Stars,  and  of  the  Constitution  of  the  Galaxy  in  the 

Southern  Hemisphere     ......  373 

CHAPTER  V. 

Observations  of  Halley's  Comet,  with  Remarks  on   its   Physical  Condition, 

and  that  of  Comets  in  General    .....  393 

CHAPTER  VI. 

Observations  of  the  Satellites  of  Saturn  ....  414 

CHAPTER  VII. 

Observations  of  the  Solar  Spots  .  .  .  .  .431 

Appendix  ......  438 


INTRODUCTION. 


(i.)  The  work  which  is  now  presented  to  the  astronomical  public,  completes  a 
review  of  the  sidereal  heavens,  which  I  commenced  about  the  year  1825,  proposing 
to  myself,  at  that  time,  no  further  object  than  a  re-examination  of  the  nebulae 
and  clusters  of  stars  discovered  by  my  Father  in  his  "  Sweeps  of  the  Heavens," 
and  described  by  him  in  three  catalogues  presented  to  the  Royal  Society,  and 
published  by  that  illustrious  body  in  their  Transactions  for  the  years  1786,  1789, 
and  1802.  This  re-examination  occupied  about  eight  years,  and  its  results  were 
presented  to  the  Royal  Society  in  the  year  1833,  in  the  form  of  a  catalogue, 
arranged  in  order  of  Right  Ascension,  and  published  in  their  Transactions  for 
the  same  year.  In  this  work  are  recorded  observations  of  2306  nebulae  and  clusters, 
of  which  1781  are  identical  with  objects  occurring,  either  in  my  Father's  catalogues, 
in  the  small  but  interesting  collection  published  by  Messier  in  the  Memoires  de 
VAcademie  des  Sciences  for  1771,  and  the  Connaissance  des  Terns  for  1783,  1784; 
and  in  M.  Struve's  catalogue  of  double  stars  :  the  remaining-  525  are  new.  Besides 
these  more  especial  objects  of  pursuit,  however,  a  great  number  of  double  stars, 
of  all  classes  and  orders,  were  noticed  and  described,  and  their  places  taken,  to 
the  amount,  altogether,  of  between  three  and  four  thousand,  the  observations 
of  which,  being  reduced  and  arranged  in  order  of  Right  Ascension,  have  been, 
from  time  to  time,  published  by  the  Royal  Astronomical  Society  of  London,  in 
six  catalogues,  which  will  be  found  in  the  2nd,  3rd,  4th,  6th,  and  9th  volumes 
of  their  Transactions. 

(ii.)  Having  so  far  succeeded  to  my  wish  (the  places  of  the  objects  thus 
determined  proving,  on    the  whole,  satisfactory),  and  having  by  this  practice 

a 


vi  INTRODUCTION". 

acquired  sufficient  mastery  of  the  instrument  employed  (a  reflecting*  telescope  of 
18i  inches  clear  aperture,  and  20-feet  focus,  on  my  Father's  construction),  and 
of  the  delicate  process  of  polishing'  the  specula ;  being-,  moreover,  strongly  invited 
by  the  peculiar  interest  of  the  subject,  and  the  wonderful  nature  of  the  objects 
which  presented  themselves  in  the  course  of  its  prosecution,  I  resolved  to  attempt 
the  completion  of  a  survey  of  the  whole  surface  of  the  heavens,  and  for  this 
purpose  to  transport  into  the  other  hemisphere  the  same  instrument  which  had 
been  employed  in  this,  so  as  to  g'ive  a  unity  to  the  results  of  both  portions  of 
the  survey,  and  to  render  them  comparable  with  each  other. 

(iii.)  Accordingly,  having-  placed  the  instrument  in  question,  as  well  as  an 
equatorially  mounted  achromatic  telescope  of  five  inches  aperture,  and  seven  feet 
focal  leng-th,  by  Tulley,  which  had  served  me  for  the  measurement  of  double  stars 
in  England;  together  with  such  other  astronomical  apparatus  as  I  possessed,  in  a 
fitting  condition  for  the  work,  and  taken  every  precaution,  by  secure  packing,  to 
insure  their  safe  arrival  in  an  effective  state,  at  their  destination,  they  were  con- 
veyed (principally  by  water  carriage)  to  London,  and  there  shipped  on  board 

the  Mount  Stewart  Elpliinstone,  an  East  India  Company's  ship,   Richardson, 

Esq.  Commander,  in  which,  having  taken  passage  for  myself  and  family  for  the 
Cape  of  Good  Hope,' we  joined  company  at  Portsmouth,  and  sailing  thence  on  the 
13th  November,  1833,  arrived,  by  the  blessing  of  Providence,  safely  in  Table  Bay, 
on  the  15th  January,  1834,  and  landed  the  next  morning,  after  a  pleasant  voyage, 
diversified  by  few  nautical  incidents,  and  without  seeing  land  in  the  interim.  It 
was  most  fortunate  that,  availing  himself  of  a  very  brief  opportunity  afforded  by  a 
favourable  change  of  wind,  our  captain  put  to  sea  when  he  did,  as  we  subsequently 
heard  that,  immediately  after  our  leaving  Portsmouth,  and  getting  out  to  sea,  an 
awful  hurricane  had  occurred  from  the  S.  W.  (of  which  we  experienced  nothing), 
followed  by  a  series  of  south-west  gales,  which  prevented  any  vessel  sailing  for  six 
weeks.  In  effect,  the  first  arrival  from  England,  after  our  own,  was  that  of 
the  Claudine,  on  the  4th  of  April,  with  letters  dated  January  1st. 

(iv.)  Having  disembarked  the  instruments  without  accident,  and  placed  them, 
temporarily,  in  one  of  the  Government  storehouses  (being  permitted  to  do  so  through 
the  obliging  kindness  of  W.  Petrie,  Esq.  Deputy  Commissary  General  of  the 
Colony),  my  next  care  was  to  look  out  for  a  comfortable  residence  in  a  locality 
suitable  for  their   erection.     This  I  was  fortunate  enough  speedily  to  find  at 


INTRODUCTION.  vil 

the  mansion  of  a  Dutch  proprietor,  W.  A.  Schonnberg',  Esq.,  bearing-  the  name 
of  Feldhuysen,  or  Feldhausen,  about  six  miles  from  Cape  Town,  in  the  direction 
of  Wynberg-,  a  spot  charmingly  situated  on  the  last  gentle  slope  at  the  base  of 
the  Table  Mountain,  on  its  eastern  side,  Avell  sheltered  from  dust,  and,  as  far  as 
possible  from  wind,  by  an  exuberant  growth  of  oak  and  fir  timber;  far  enough 
removed  from  the  mountain  to  be,  for  the  most  part,  out  of  the  reach  of  annoyance 
from  the  clouds  which  form  so  copiously  over  and  around  its  summit,  yet  not 
so  far  as  to  lose  the  advantage  of  the  reaction  of  its  mural  precipices  against 
the  south-east  winds  which  prevail  with  great  violence  during-  the  finer  and  clearer 
months,  but  which  seldom  blow  home  to  the  rock  on  this  side,  being,  as  it  were, 
gradually  heaved  up  by  a  mass  of  comparatively  quiescent  air  imprisoned  at  the 
root  of  the  precipice,  and  so  gliding  up  an  inclined  plane  to  the  summit  on 
the  windward  side,  while  they  rush  perpendicularly  down  on  the  leeward  with 
tremendous  violence  like  a  cataract,  sweeping  the  face  of  the  cliffs  towards  Cape 
Town,  which  they  fill  (as  well  as  the  valley  in  which  it  stands)  with  dust  and  uproar, 
chiefly  during  the  nig'ht.  This  residence  needing  some  repairs,  and  being-,  in  fact, 
not  then  actually  vacant,  a  temporary  residence  was  secured,  at  a  convenient  dis- 
tance, in  a  tenement  belonging*  to    Borcherds,  Esq.,  of  Cape  Town,  called 

Welterfrieden,  whence  I  could  superintend  the  erection  of  the  instruments,  which 
was  forthwith  commenced,  and  pushed  forward  with  such  effect,  that  on  the 
22nd  of  February  I  was  enabled  to  gratify  my  curiosity  by  a  view  of  a  Crucis, 
the  nebula  about  r?  Argus,  and  some  other  remarkable  objects,  in  the  20-feet 
reflector  5  and,  on  the  night  of  the  5th  of  March,  to  commence  a  regular  course  of 
sweeping. 

(v.)  Shortly  after,  the  erection  of  a  building  was  commenced  to  receive  the 
equatorial  instrument,  which,  so  soon  as  the  walls  were  settled,  and  the  pier,  which 
was  of  brick,  laid  in  Roman  cement,  consolidated,  was  placed  on  its  supports,  and 
being  surmounted  by  a  revolving  roof  of  a  peculiar  construction  (See  Art.  158), 
contrived  by  myself,  and  constructed  in  England  for  the  purpose,  was  brought  into 
approximate  adjustment ;  and  on  the  2nd  of  May,  a  series  of  micrometrical  measures 
of  southern  double  stars  was  commenced  by  the  measurement  of  a  Centauri,  the 
chief  among  them.  I  ought  to  observe  that,  on  unpacking  this  and  the  other 
instruments  and  apparatus,  not  a  sing-le  article  was  found  to  have  sustained  injury. 

(vi.)  The  Frontispiece  to  this  volume  exhibits  the  Reflector,  and  the  building 


viii  INTRODUCTION. 

containing"  the  Equatorial,  in  their  enclosure,  a  kind  of  orchard,  surrounded  on 
all  sides  by  trees,  but  commanding-  a  tolerably  near  approach  to  both  the  southern, 
eastern,  and  northern  horizon.  To  the  west,  the  nearer  vicinity  of  the  trees, 
though  cutting-  off  much  of  the  sky,  yet  afforded  a  valuable  protection  from 
the  fury  of  the  north-west  gales  which  prevail  in  the  winter  months.  Nor  was 
it  without  some  regret  on  this  account,  that  the  removal  of  a  portion  of  this  friendly 
shelter  was  resolved  on  to  afford  a  view  of  the  comets  of  Encke  and  Halley,  when 
so  situated  as  to  require  it.  The  exact  geographical  site  of  Feldhausen  was  found 
by  trigonometrical  measurement  (See  Appendix  E),  to  be  2'  53".  55  south,  and 
0m  4M1  west  of  that  of  the  Royal  Observatory  of  the  Cape,  that  is  to  say,  in  Lat. 
33°  58'  56".55,  Long.  22h  4Cra  9M1  from  Greenwich.  Its  altitude  above  the  site 
of  that  building  was  ascertained  by  barometrical  observation  to  be  112.23  feet, 
or  about  142  feet  above  the  mean  sea-level  of  Table  Bay  (See  Appendix  B). 

(vii.)  As  I  have  mentioned  the  Royal  Observatory  of  the  Cape,  I  must  take 
this  distinct  and  early  opportunity  to  acknowledge  my  many  and  great  obli- 
gations to  my  excellent  friend,  Thomas  Maclear,  Esq.,  its  director,  whose  ardent 
love  for  the  science  to  which  he  has  devoted  himself,  seconded  by  talent  of  no 
common  order,  by  resource  which  no  difficulties  exhaust,  and  by  activity  which 
no  exertion  wearies,  has  secured,  and  continues  to  secure,  for  the  noble  esta- 
blishment under  his  direction,  a  reputation  of  the  highest  rank,  and  for  himself, 
the  best  titles  to  the  gratitude  of  his  country,  and  the  approbation  of  the  govern- 
ment he  serves.  To  his  kindness  I  am  indebted  for  much  and  most  valuable 
aid  in  fixing-,  with  all  the  precision  which  the  fine  instruments  under  his  command 
could  afford,  the  Right  Ascensions  of  a  great  many  stars  of  which  a  knowledge  was 
indispensable  in  the  reduction  of  my  sweeps,  and  which  I  neither  could  obtain 
with  sufficient  exactness  from  the  existing  catalogues,  nor  had  any  means  of 
ascertaining-  for  myself,  unless  by  entering  upon  an  express  course  of  observation 
for  that  very  purpose,  such  as  formed  no  part  of  my  original  design,  and  for  which 
a  much  superior  transit  to  that  I  had  brought  out  with  me  would  have  been 
requisite.  Previous  to  leaving-  Eng-land,  I  had  procured  a  MS.  list  of  the 
stars  of  the  Brisbane  Catalogue,  then  preparing  for  publication,  containing-  the 
places  of  between  seven  and  eight  thousand  southern  stars,  and  on  this 
Catalogue,  when  it  should  appear,  I  had  confidently  reckoned  for  as  many  well 
determined  zero  stars  as  I  could  possibly  need,  the  s}*stem  of  observing  I  pro- 


INTRODUCTION.  ix 

posed  to  follow  being-  entirely  differential.  With  the  Polar  distances  of 
that  catalogue,  I  seldom  had  much  occasion  to  find  mult;  but  as  respects  the 
Right  Ascensions;  I  experienced  less  satisfaction  in  its  use.  On  mentioning 
this  circumstance  to  Mr.  Maclear,  he,  with  ready  alacrity,  at  once  offered 
to  determine  this  important  element,  by  direct  observation,  for  as  many  zero 
stars  as  I  might  require,  thus  rescuing-  me  from  a  very  serious  difficult}^.  I  need 
hardly  add  that  I  g'ladly  availed  myself  of,  and  drew  largely  on  his  kindness  ; 
and  the  results  of  his  observations  in  the  cases  of  about  070  stars,  fixed  by  two  or 
three  observations  of  each,  have  proved  a  most  material  assistance  to  me  in  the 
reduction  of  my  sweeps.  Nor  was  this  the  only  instance  of  useful  and  effective 
aid  rendered  me  from  the  same  quarter. 

(viii.)  Previous  to  quitting-  England,  I  had  eng-ag-ed  the  services  of  an 
attendant  for  the  purpose  of  working-  the  sweeping-,  and  other  mechanical  move- 
ments, of  the  Reflector  during-  the  observations,  and  executing-  any  necessary 
repairs.  John  Stone,  the  person  so  eng-ag-ed,  to  the  useful,  and,  indeed,  indis- 
pensable qualifications  of  a  ready  mechanic,  whether  in  wood  or  iron  work,  joined 
that  of  experience  in  this  particular  employment,  having-  performed  that  office  for 
me  during-  a  considerable  portion  of  my  review  of  the  northern  heavens,  Avith 
undeviating-  steadiness  and  reg-ularity,  as  he  continued  to  do  during-  the  whole 
of  that  of  the  southern,  without  once  absenting-  himself  from  his  duty.  This 
indispensable  manual  aid  excepted,  it  is  rig-ht  to  mention  that  the  whole  of  the 
observations,  as  well  as  the  entire  work  of  reducing-,  arranging-,  and  preparing-  them 
for  the  press,  has  been  executed  by  myself.  The  repolishing-  of  the  reflectors, 
it  will  of  course  be  understood,  could  be  delegated  to  no  other  person. 

(ix.)  Of  these  I  was  provided  with  three,  viz.,  one  made  by  my  Father,  and 
used  by  him  in  his  20-feet  sweeps,  and  other  observations ;  one  made  by  myself, 
under  his  inspection  and  instructions ;  and  one  which  I  ground  and  figured  sub- 
sequently, but  which  was  cast  at  the  same  time,  and  from  the  same  metal  as  that  last 
mentioned.  They  are  each  18j  inches  of  clear  diameter  of  polished  surface,  and  all, 
so  far  as  I  am  able  to  judge,  equally  reflective  when  freshly  polished,  and  in  even- 
respect  similar  in  their  performance.  One  of  them  (the  first  completed,  of  the  two 
newer  ones  above  mentioned)  is  about  two  inches  longer  in  focus  than  the  others, 
a  difference  which,  the  figure  being  otherwise  good,  it  has  not  been  thoug-ht  worth 
while  to  correct. 

b 


X  INTRODUCTION. 

(x.)  The  operation  of  repolishing  was  performed  whenever  needed,  the  whole 
of  the  requisite  apparatus  being*  brought  for  the  purpose.  It  was  very  much  more 
frequently  required  than  in  England;  and  it  may  be  regarded  as  fortunate  that 
I  did  not,  as  at  first  proposed  (relying  on  the  possession  of  three  perfect  metals), 
leave  the  apparatus  in  question  behind.  Being  apprehensive  that  in  a  climate  so 
much  warmer,  difficulties  would  arise  in  hitting  the  proper  temper  of  the  polishing 
material,  slight  imperfections  of  surface,  induced  by  exposure,  were  for  a  while 
tolerated ;  but,  confidence  in  this  respect  once  restored,  and  practice  continually 
improving,  I  soon  became  fastidious,  and  on  detection  of  the  slightest  dimness 
on  any  part  of  the  surface,  the  metal  was  at  once  remanded  to  the  polisher. 

(xi.)  And  here,  perhaps,  I  may  be  allowed  a  digression  on  a  point  of  the 
utmost  importance  in  the  use  of  reflecting  specula,  viz.,  the  mode  of  supporting 
the  metal  in  its  case.  This,  in  my  own  practice,  is  provided  for  as  follows : — 
between  the  back  of  the  case  and  the  mirror  are  interposed  six  or  eight  thicknesses 
of  coarse  woollen  baize,  or  blanketing,  of  even  texture,  and  quite  free  from  knots, 
stitched  together  at  the  edges  to  prevent  any  hard  substance  from  getting  between 
them.  On  this  bed  the  metal  is  laid  flat,  and  being  shaken  into  a  concentric 
situation,  as  respects  the  rim  of  the  case,  two  supports  formed  of  strips  of  similar 
woollen  stuff,  many  times  doubled,  occupying  about  30°  each  of  the  circumference 
of  the  case,  are  introduced,  so  as  to  leave  an  arc  of  about  40°  unoccupied,  opposite 
the  point  which  is  intended  to  be  placed  lowermost  in  the  tube.  The  case  being 
then  raised  into  an  inclined  position  by  the  other  handle,  and  slightly  shaken, 
the  mirror  takes  its  own  free  bearing-  on  these  supports,  which  by  their  elasticity 
obviate  the  possibility  of  any  lateral  compression  which  might  g'o  to  the  extent 
of  seriously  disfiguring  the  metallic  surface,  were  the  whole  vertical  pressure  of  the 
mirror  confined  to  a  hard  point  near  the  bottom,  or  even  distributed  over  two  or 
three  metallic  bearings  in  the  circumference. 

(xii.)  Simple,  and  indeed  homely  as  this  mode  of  bedding  the  speculum  may 
appear,  it  is,  I  am  satisfied,  as  effectual  (it  certainly  is  quite  as  little  costly 
and  cumbersome)  as  any  which  can  be  contrived.  The  uniform  support  of  a 
reflector  over  its  whole  extent,  is  a  point  of  the  last  importance  to  its  optical 
performance.  A  distortion  of  figure  by  flexure,  which  in  the  object-glass  of  a 
refracting  telescope  would  produce  no  appreciably  injurious  effect,  would  be  utterly 
fatal  to  distinct  vision  in  a  ref  ecting  one.    This  will  be  made  apparent  if  we  con- 


INTRODUCTION.  xi 

aider  the  different  modes  in  which  the  convergence  of  the  rays  is  effected  by  reflexion 
at  a  curved  metallic  surface,  and  by  refraction  through  one  or  more  glass  lenses. 
In  the  former  case,  the  whole  deviation  of  the  ray  from  its  original  direction 
is  effected  at  one  surface,  and,  in  amount,  is  equal  to  twice  the  inclination  of  that 
surface  to  a  perpendicular  on  the  original  direction.  Any  alteration,  therefore, 
which  flexure  may  produce  on  the  inclination  of  the  surface  (supposed  originally 
parabolic)  of  a  speculum  to  its  axis,  at  a  given  point,  will  produce  an  angular 
deviation  of  the  reflected  ray  from  its  proper  course  to  a  double  amount.  And 
the  lateral  aberration  produced  by  such  deviation  will  be  expressed  by  that  double 
amount  of  angular  flexure,  multiplied  by  the  focal  distance,  and  is,  therefore, 
the  more  injurious  the  greater  is  the  focal  length.  On  the  other  hand,  in  the 
case  of  a  refracting  telescope,  the  deviation  of  a  ray  is  effected  by  the  prismaticity 
of  the  medium,  or  media,  of  which  the  object-giass  consists,  at  the  points  where 
the  ray  penetrates  them,  and  is  independent  of  the  absolute  inclination  of  either 
separate  surface  to  the  axis.  In  consequence,  however,  this  inclination  may  change 
by  flexure  in  any  one  of  the  lenses  of  which  the  object-giass  consists,  yet,  so  long- 
as  both  surfaces  of  the  lens  bend  alike,  which  they  cannot  but  do  in  any  con- 
ceivable case  of  flexure  short  of  fracture,  the  effective  prismatic  angle  at  that 
point,  and  consequently,  also,  the  inclination  of  the  transmitted  ray  to  the  axis 
remains  absolutely  unaltered,  and  the  whole  amount  of  lateral  aberration  produced 
is  that  which  arises  from  the  bodily  displacement  of  the  transmitting  portion  of 
the  lens  in  a  direction  to  or  from  the  focus  by  the  effect  of  the  flexure,  a  dis- 
placement which,  in  itself  utterly  inappreciable,  is  still  farther  reduced  in  its 
effect  to  produce  lateral  aberration,  that  it  comes  to  be  multiplied  by  a  fraction 
whose  numerator  at  the  maximum  is  the  semi-aperture  of  the  object-giass,  and 
whose  denominator  is  the  focal  length  of  it. 

(xiii.)  This  inequality  of  proportion  between  the  two  cases  is  still  farther 
augmented  by  the  lightness  of  glass  compared  with  metal,  which  (surface  for 
surface,  and  rigidity  for  rigidity)  makes  the  absolute  flexure  of  a  given  thickness 
of  glass  much  less  than  of  an  equal  thickness  of  metal.  And  it  is  very  fortunate 
that  all  these  conditions  hold  good ;  for  since  there  is  no  possibility  of  supporting 
a  transparent  substance  against  flexure,  without  stopping*  the  light,  this  cause 
alone  (had  it  acted  to  the  extent  it  does  in  reflectors)  would  long"  since  have 
banished  large   object-glasses  from  practical  use.     A  speculum  (I  speak  from 


xii  INTRODUCTION. 

experience)  of  the  dimensions  and  thickness  used  in  my  sweeps,  is  totally  sported 
by  supporting*  it  on  three  metallic  points  at  the  circumference,  when  directed  to  the 
zenith.  The  image  of  every  considerable  star  becomes  triangular,  throwing  out 
long-  flaring  caustics  at  the  angles.  On  one  occasion,  I  supported  a  mirror  simply 
against  a  flat  board,  at  about  45°  elevation  from  the  horizon.  In  this  state  its 
performance  was  tolerably  good ;  but  on  stretching-  a  thin  packthread  vertically 
down  the  middle  of  the  board,  so  as  to  bring1  the  weight  to  rest  on  this  as  on  one 
axis,  the  images  of  stars  were  elongated,  in  a  horizontal  direction,  to  a  preposterous 
extent,  and  all  distinct  vision  utterly  destroyed  by  the  division  of  the  mirror  into 
two  lobes,  each  retaining*  something-  of  its  parabolic  figure,  separated  by  a  vertical 
band,  in  a  state  of  distortion,  and  of  no  figure  at  all. 

(xiv.)  Springs  are  sometimes  used  by  opticians  at  the  back  of  a  small  mirror, 
for  the  purpose  of  keeping  it  home  to  the  rim  of  its  case.  They  are  usually 
three  in  number,  and  so  far  as  mere  support  of  the  mirror  is  concerned,  they 
act  as  three  non-elastic  supports  would  do,  i.  e.  disadvantageous^.  More 
numerous  and  weaker  springs  distributed  over  the  whole  of  the  back  of  the  case 
would  seem  to  be  preferable,  but  they  ought  to  be  so  weak  that  all  should  be  much 
compressed  and  brought  into  full  action  by  the  pressure.  And  even  then,  if  the 
metal  be  confined  in  its  case  by  a  rim  in  front,  a  spring-pressure  upward,  which  in 
a  horizontal  position  of  the  surface  would  barely  sustain  it  in  contact  with  the  rim. 
will  urge  it,  when  placed  vertically  against  the  rim,  with  a  force  equal  to  the 
whole  weight  of  the  metal  applied  over  its  surface  in  a  direction  perpendicular 
thereto,  and  will  tend  therefore  to  distort  it  in  that  position,  to  the  very  same 
amount,  but  in  an  opposite  direction,  that  it  would  have  been  distorted  by  gravity 
in  the  other  position,  had  the  springs  been  absent,  and  the  support  been  given  by  a 
metallic  ring-  at  the  circumference  of  the  back. 

(xv.)  Nothing,  therefore,  is  gained,  so  far  as  obviating  flexure  is  concerned, 
by  a  distribution  of  elastic  support,  so  Jong  as  the  mirror  is  pressed  against  a  rim 
in  front.  To  make  such  a  mode  of  support  effective,  the  metal  must  be  free  to 
rise  and  fall,  and  the  friction  on  the  lower  circumference  must  be  counteracted, 
either  by  resting  it  in  a  circular  iron  chair,  provided  with  exterior  rollers,  or 
otherwise  equably  supporting  the  lower  portion  of  its  edge,  so  as  to  allow  of  its 
shifting  forwards  or  backwards  without  sensible  friction ;  as,  for  instance,  bv 
suspending  the  metal  from  the  upper  side  of  its  case,  in  a  jointed  frame,  composed 


INTRODUCTION.  xiii 

of  two  semicircles  of  steel  loosely  riveted  at  the  extremities  of  their  common, 
horizontal  diameter,  to  admit  of  free  play  at  the  joint,  the  lower  semicircle  being- 
thin,  and  lined  with  velvet  or  flannel  to  ensure  equal  pressure  against  the  lower 
edge  of  the  metal ;  the  upper  stronger,  and  increasing"  gradually  in  stiffness 
towards  the  top,  by  which  the  whole  should  be  suspended  on  a  hinge-pin.* 

(xvi.)  As  an  experiment,  I  constructed  a  case,  having*  the  back  of  stout  wood 
set  over  with  ninety  steel  springs,  of  such  strength  as  to  be  all  of  them  pressed 
nearly  into  contact  with  the  wood  by  the  weight  of  the  mirror  laid  horizontally 
on  them,  and  distributed  with  as  much  uniformity  as  possible  in  their  points  of 
bearing  over  the  whole  surface  of  the  back,  the  face  being  left  entirely  unconfined. 
So  supported,  the  performance  of  the  mirror  was  good  at  all  altitudes,  but  by  no 
means  better  than  when  bedded  on  woollen  cloths,  as  above  described,  nor,  indeed, 
equal  to  it ;  and,  in  fact,  when  we  consider  that  each  fibre  of  wool  is  a  delicate 
coiled  spring  of  almost  perfect  elasticity,  it  is  clear  that  no  artificial  arrangement 
of  metallic  spring's  we  can  make,  can  attain  the  perfection  of  such  a  natural 
one  (if  we  may  so  apply  the  term),  either  in  uniformity  of  distribution,  or  in 
delicacy  of  application.  This  consideration  led  me  to  abandon  the  use  of  a  spring- 
case,  after  making  a  very  few  sweeps  with  it,  and  re-adopt,  in  its  stead,  the 
woollen  bedding  which  had  been  laid  aside  to  make  way  for  what  proved  to  be, 
in  effect,  no  substantial  improvement  on  it.  It  is  essential,  however,  that  a 
great  many  thicknesses  of  the  baize  or  blanket  employed,  should  be  used,  by  which 
only  the  effect  of  flexure  in  the  wooden  bach  itself  of  the  case  can  be  eliminated. 
And  to  keep  up  the  elasticity  of  the  fibre,  it  should  be  occasionally  taken  out 
and  beaten. j" 

(xvii.)  A  serious,  indeed  a  fatal  objection,  would  appear  to  lie  against  the 
use  of  flexible,  elastic,  or  any  kind  of  moveable  support  for  the  mirror;  in  the 
fluctuations  liable  to  be  caused  by  it  in  the  line  of  collimation  when  the  inclination 

*  This  was  written  while  ignorant  of  the  very  ingenious  contrivance  by  which  Lord  Rosse  affords 
an  equable,  or  nearly  equable  support  to  his  large  reflector.  Comparative  trial  of  the  several  methods  can 
alone  decide,  in  any  proposed  case,  which  is  the  most  effectual. 

f  The  following  memorandum  occurs  in  sweep  687  : — 

"  The  mirror,  though  a  capital  one,  has,  for  the  last  three  nights,  given  distorted  images  with 
its  full  aperture,  which  appear  horned  and  tailed.  To-night,  before  the  sweep,  I  took  it  out,  and 
carefully  smoothed,  shook  up,  and  remade  its  bed.  Now,  nothing  can  be  finer.  It  lies  at  its  ease, 
and  equally  supported  all  over,  and  all  the  appendages  are  clean  gone." 

c 


Xiv  INTRODUCTION. 

of  the  mirror  to  the  horizon  is  varied,  and  which  must  inevitably  take  place 
it'  there  be  either  the  least  friction  of  the  lower  edge  on  its  support,  or  anything 
short  of  mathematical  exactness  in  the  distribution  of  the  pressure.  But  this 
objection  is  completely  obviated  in  my  mode  of  observation,  by  the  use  of  an 
interior  collimating'  telescope,  as  described  in  Phil.  Trans.  1833,  p.  488.  The 
collimator  used  in  the  greater  part  of  these  observations  differed  only  from  that  there 
described,  1st,  in  being-  a  more  powerful  telescope  (viz.,  an  achromatic  of  four  feet 
focal  length,  with  a  good  object-glass,  2|  in.  aperture),  and,  2nd,  in.  having-  the 
plane  speculum  placed,  not  as  there  described,  between  the  object-glass  and  its  focus, 
but  beyond  the  focus  (in  Avhich  the  collimating-  cross  is  fixed),  so  as  to  illuminate 
that  cross  by  the  light  of  a  lamp  external  to  the  tube  of  the  large  reflector, 
collected  by  a  lens  upon  the  cross,  both  great  improvements  in  practice. 

(xviii.)  Sweeping  (for  so  I  shall  continue  to  denominate  the  system  of  obser- 
vation in  zones  of  3°  breadth  in  Polar  distance  in  search  of  new  objects),  was 
prosecuted,  in  the  absence  of  the  moon,  on  all  occasions  when  wreather  permitted, 
and  the  definition  of  the  etars  was  such  as  to  render  it  worth  while  to  do  so. 
And  this  leads  me  to  speak  of  the  climate  of  the  Cape  as  regards  its  favourableness 
or  unfavourableness  for  astronomical  observation.  In  the  hot  season  (from  October 
to  March),  and  especially  during  the  hotter  months  of  that  season,  the  nights  are 
for  the  most  part,  superb,  at  least  in  all  the  flat  region  at  a  few  miles  distance 
from  the  mountains;  but  in  their  immediate  vicinity,  the  south-east  wind  (then 
generally  prevalent)  frequently  brings  with  it  a  belt  of  cloud  extending  many 
miles  from  the  hills,  and  cutting  off  the  view  of  the  sky.  This  (which  is  some- 
times called  a  black  south-easter)  comes  on  often  at  night,  and  lasts  several  nights 
in  succession.  Very  often,  too,  when  no  such  impediment  exists,  the  excessive 
heat  and  dryness  of  the  sandy  plains  gives  rise  to  a  disturbance  of  the  optical 
tranquillity  of  the  air,  so  as  to  destroy,  or  much  impair,  distinct  vision,  and 
that  frequently  in  a  very  singular  manner.  In  some  cases,  the  images  of  the 
stars  are  violently  dilated,  and  converted  into  ill-defined  nebulous  balls,  or  puffs, 
of  10  or  15"  or  more  in  diameter.*    In  others,  they  form  soft,  quiet,  round  pellets 

*  During-  the  conjunction  of  Saturn  and  y  Virginia,  at  the  end  of  March,  1834,  hoth  were 
seen  in  the  same  field  of  the  20-feet  reflector,  in  such  a  state  of  indefinition,  that  hut  for  the  greater 
quantity  and  different  colour  of  the  light  of  Saturn,  it  could  not  have  been  told  which  was  the  planet, 
and  which  the  star.    Yet,  to  all  appearance,  the  night  would  have  been  judged  a  fine  one. 


INTRODUCTION.  XV 

of  3  or  4"  diameter,  very  unlike  the  "spurious  discs"  which  they  present  when 
best  defined,  and  rather  resembling"  planetary  nebulae.  In  other  cases,  again, 
the  structure,  as  it  were,  of  these  pellets  is  disclosed,  and  they  are  seen  to  arise 
from  an  infinitely  rapid  vibratory  movement  of  the  central  point,  in  all  possible 
directions,  while,  on  a  few  occasions,  the  appearances  have  been  exceedingly  per- 
plexing- and  singular,  and  such  as  there  is  difficulty  in  accounting-  for  on  any  optical 
principle  whatever.* 

(xix.)  Even  in  the  hottest  season,  however,  nights  of  admirable  definition 
occur,  especially  looking-  southwards.  But,  what  is  not  a  little  remarkable,  in 
the  very  hottest  days,  looking  northwards  over  the  burning  tract  intervening 
between  Feldhausen  and  Table,  or  Saldanha  Bay,  the  most  admirable  and  tranquil 
definition  of  the  solar  spots,  and  other  phenomena  of  the  sun's  disc,  is  by  no  means 
unfrequent.  In  such  cases,  I  presume  the  strongly  heated  stratum  of  air  incum- 
bent on  the  surface  of  the  soil,  is  swept  off  by  the  south-east  wind  blowing  from 
False  to  Table  Bay,  before  it  ascends  high  enough  to  interfere  with  the  visual 
ray.  To  how  high  a  temperature  the  soil  is  occasionally  heated,  will  be  seen  in 
Appendix  (C). 

(xx.)  During  the  autumnal  months  of  May,  June,  and  July,  when  the  weather 
is  generally  cool,  and  the  nights  cold,  hot  winds  frequently  set  in  from  the  north, 
usually  in  the  night ;  at  first  moderate,  and  alternating  with  cold  gusts  from 
the  opposite  quarter,  but  rapidly  gaining  the  prevalence,  till,  in  a  few  hours,  they 
attain  the  violence  of  a  hard  gale  and  glowing  oven-like  heat.f     Thus  they  con- 


*  The  discs  ill  defined  and  agitated  points,  surrounded  with  distant  halos.  Where  thrown  out 
of  focus  inwards,  the  images,  instead  of  circular  discs,  would  present  large  central  vacuities,  absolutely 
void  of  light,  round  which  a  turban-fashioned  phenomenon,  in  a  constant  state  of  vorticose  motion,  was 
seen.  Occasionally,  the  image  so  thrown  out  of  focus  takes  the  form  of  a  narrow  circular  arc,  with 
a  terminal  concentration  ;  when  thrown  out  of  focus  outrvards,  a  vivid  central  point,  surrounded  with 
an  extensive  circular  area  of  light.  The  phenomena  have  manifestly  a  reference  to  the  state  of  the 
air  in  the  tube  of  the  telescope,  and  at  its  aperture,  and  would  seem  to  indicate  the  existence  of  a  cone 
of  heated  air  projecting  beyond  the  aperture  of  the  tube.  The  tube  of  a  reflector  being  necessarily  open 
at  the  mouth,  ascending  and  descending  currents  of  hot  and  cold  air  (usually  rotating  spirally)  become 
established,  and  are  very  prejudicial  to  distinct  vision.  The  remedy  is  obvious ;  viz.,  to  dispense  with 
a  tube  altogether,  substituting  for  it  a  light,  strong,  inflexible  framework  of  cast  or  wrought  iron.  In 
refracting  telescopes,  in  which  the  air  is  completely  enclosed,  its  circulation  is  not  nearly  so  offensive. 

f  I  annex  the  readings  of  a  thermometer  on  the  night  of  July,  1834,  on  the  desk,  in  the  open  air, 
in  the  gallery  of  the  20-feet  reflector.    Minimum  before  midnight  40°.4.    At  midnight,  the  hot  wind 


Xvi  INTRODUCTION. 

tinue  to  blow,  frequently  for  thirty-six  or  forty-eig-ht  hours,  becoming-  at  length 
cool,  and  finally  settling-  into  rain.  Now  it  is  not  a  little  remarkable,  that  however 
unfavourable  to  vision  this  conflict  of  hot  and  cold  currents  is  at  the  coming,'  on 
of  such  a  g'ale,  no  sooner  does  it  become  established  than  the  imag-es  become 
concentrated,  and  settle  down  not  unfrequently  into  excellent  definition. 

(xxi.)  It  is,  however,  in  the  cooler  months,  from  May  to  October  inclusive, 
and  more  especially  in  June  and  July,  that  the  finest  opportunities  occur.  The 
state  of  the  air  in  these  months,  as  reg-ards  definition,  is  habitually  g"ood,  and  im- 
perfect vision  is  rather  the  exception  than  the  rule.  The  best  nig-hts  occur  after 
the  heavy  rains  which  fall  at  this  season  have  ceased  for  a  day  or  two;  and  on 
these  occasions,  the  tranquillity  of  the  images,  and  sharpness  of  vision  is  such,  that 
hardly  any  limit  is  set  to  magnifying-  power  but  what  the  aberrations  of  the  specula 
necessitate.* 


set  in,  after  a  brief  conflict,  of  the  nature  described  in  the  text ;  the  thermometer  instantly  rose 
to  50°.  At 

hm  ohm  o  hm  o 

1  39  a. m.  it  stood  at  64.0  2    3  a.  m.  it  stood  at  69.0  2  38  a.  m.  it  stood  at  69.4 

1  53   „         „       68.7  2  10   „         „       70.4  2  47    „         „  71.0 

1  59    „  „       65.0  2  18   „  „       70.0  3  18   „         „  68.0 

2  1    „         „       68.1  2  22    „         „  71.0 

Minimum  before  sunrise  next  morning,  60.0 
*  On  such  occasions,  optical  phenomena,  of  extraordinary  splendour,  are  produced  by  intercepting 
the  light  of  a  bright  star,  by  diaphragms  pierced  in  regular  patterns,  and  extending  over  the  whole 
aperture  of  the  telescope,  such,  for  example,  as  large  sheets  of  card-board  or  zinc,  pierced  by  machinery 
(which  gives  perfect  regularity),  either  with  circular  holes,  uniformly  disposed,  or  with  any  regular  and 
not  too  complicated  pattern.  The  appearances  so  produced  (which  strike  every  one  who  witnesses  them 
with  surprise  and  delight),  though  they  may  be  seen  whenever  the  air  is  in  a  moderately  good  state, 
are  infinitely  enhanced  in  their  beauty  by  the  perfect  tranquillity  which  prevails  on  such  occasions 
as  these.  They  depend  on  the  optical  law  of  interferences ;  and  many  beautiful  examples  of  their 
explanation  on  that  principle,  fully  worked  out  in  detail,  will  be  found  in  M.  Schwerd's  treatise,  "  Die 
Beugungserscheinungen  aus  den  Fundamentalgesetzen  der  Undulations — theorie  analytisch  entwickelt.'* 
&c.  (Manheim,  1835). 

The  "triangular  aperture,"  or  diaphragm  which  admits  the  light  through  an  opening  concentm- 
with  the  speculum  in  the  form  of  an  ecpiilateral  triangle,  to  whose  use  as  a  means  of  separating  close 
double  stars  continual  reference  will  be  found  in  the  following  pages,  affords  an  elegant  example 
of  this  theory,  in  the  sharpness  of  the  central  disc  which  it  produces,  and  the  absence  of  all  appendages 
other  than  six  perfectly  straight  delicate  rays  running  oft*  at  angles  of  60°  from  the  disc.  In  a  letter 
addressed,  Dec.  24,  1834,  to  the  late  Captain  B.  Hall,  of  which  I  retain  a  copy,  I  find  an  observation  of 
Canopus,  with  such  an  aperture,  and  a  magnifying  power  of  1200,  thus  described: — "The  disc  is 


INTRODUCTION. 


xvii 


(xxii.)  Among*  the  irregular  and  accidental  optical  effects  of  peculiar  atmo- 
spheric conditions  incident  to  the  climate,  there  are  one  or  two  which  seem  deserving- 
of  especial  notice.  The  first  is  that  phenomenon  which,  when  it  occurs,  I  have 
designated  by  the  epithet,  the  "nebulous  haze."  Its  effect  is  to  convert  every 
star  of  the  9th  magnitude  and  upwards,  into  a  "  nebulous  star,"  meaning  thereby 
a  well-defined  star,  with  a  faint,  nebulous  photosphere  of  greater  or  less  extent, 
according  to  the  brightness  of  the  star,  surrounding  it.  This  phenomenon  occurs  in 
a  perfectly  clear  sky,  free  from  the  slightest  suspicion  of  cloud.  It  comes  on  very 
suddenly  and  unexpectedly,  and  goes  off  as  suddenly,  lasting  sometimes  only  a 
few  minutes ;  at  others,  longer.  Thus,  in  sweep  500,  Oct.  5,  1834,  it  commenced 
at  22h  4m  st,  when  a  star  7  m  was  observed  to  be  surrounded  with  it,  having  come 
on  quite  suddenly,  and  continued  to  affect  all  the  brighter  stars  until  22h  54m,  when 
it  was  quite  gone,  being  described  as  extraordinary  in  intensity,  and  very  trouble- 
some during  its  continuance.  From  this  time  till  0h  27m,  all  was  clear,  when  it 
suddenly  came  on  again,  ct  in  an  instant.  A  star  7  m  was  quite  free,  but  on  drawing- 
it  back"  (after  it  had  left  the  field  for  re-examination),  "it  was  found  to  be  com- 
pletely involved,"  the  sky  continuing-  all  the  while  pure,  so  far  as  the  naked  eye 
could  discern.  Again,  in  sweep  598,  June  18,  1835,  we  have  "  15h  37m  ST.  A 
nebulous  haze  came  on  in  an  instant,  extending*  to  stars  9  m ;  yet  the  sky  is  as  clear 
as  ever,  and  the  calm  unbroken. — "  15h  44m — (a  star  6  m  in  the  field).  The  nebu- 
lous haze  is  gone;  it  did  not  last  two  minutes." — "  16h  23m.  The  nebulous  haze 
came  on  again  in  a  moment."  Such  remarks  might  lead  to  a  suspicion  of  dew  upon 
the  eye-piece,  or  the  breath  of  the  observer  settling  on  the  glass;  but  repeated 
examination  (the  phenomenon  being  very  common)  has  satisfied  me  that  such  is  not 
the  cause,  but  that  it  is  really  of  atmospheric  origin.  Similar  nebulous  affections 
occur  in  our  English  climate ;  but  it  is  their  much  g-reater  frequency,  and  the 
suddenness  of  their  appearance  and  disappearance,  which  forms  so  remarkable  a 
feature  at  the  Cape. 


an  exact  circle,  and  the  six  rays  which  such  an  aperture  always  gives,  are  perfectly  straight,  delicate, 
brilliant  lines,  like  brig'htly  illuminated  threads,  running-  far  out  beyond  the  field  of  view,  and  (what  is 
singular)  capable  of  being-  followed,  like  real  appendages  to  the  star,  long-  after  the  star  itself  had  left  the 
field.  In  examining  stars  to  see  if  they  are  close  double,  I  always  apply  the  triangular  aperture.  It 
reduces  the  discs  to  hardly  more  than  a  third  of  their  size,  and  gives  them  a  clearness  and  perfection 
incredible  without  trial." 

d 


xviii 


INTRODUCTION. 


(xxiii.)  Another  peculiarity  which  lias  frequently  given  rise  to  remark,  is  the 
opacity  of  cloud,  as  compared  with  what  prevails  in  England.  My  Sweeping 
Registers,  at  Slough,  are  full  of  instances  of  double  stars  with  small  companions, 
clusters,  &c.  seen  through  cloud  of  considerable  apparent  density  to  the  unassisted 
eye.  Of  this  I  have  elsewhere  stated  remarkable  instances.  It  was  my  usual 
practice  there  to  continue  sweeping*  during-  moderately-clouded  intervals,  for  the  sake 
of  securing-  at  least  such  new  double  stars  as  mig-ht  occur,  or  obtaining-  micrometric 
measures  of  known  ones  placed  on  the  working*  list.  Such  advantag-e  could  seldom 
be  taken  of  clouded  intervals  at  Feldhausen,  and  from  the  whole  tenor  of  my 
experience  of  that  locality,  the  impression  remains  of  a  very  decided  difference,  in 
this  respect,  between  the  two  stations. 

(xxiv.)  Meteorological  observations  of  the  barometer,  thermometers,  wet 
and  dry,  the  actinometer,  &c,  with  the  usual  record  of  weather,  were  made  on 
the  appointed  term-days,  or  days  of  equinox  and  solstice ;  at  first  during-  thirty-six 
hours,  subsequently,  during-  twenty-four  only,  from  hour  to  hour.  These,  however, 
are  only  valuable  when  taken  in  conjunction  with  others  of  the  same  kind ;  and 
having-  already  been  published  in  the  pages  of  the  Athcnmnn,  and  elsewhere, 
and  received  as  much  discussion  as  they  have  appeared  to  need,  in  a  report 
which  I  had  the  honour  to  communicate  to  the  British  Association,  for  the  advance- 
ment of  science,  and  which  has  been  published  by  that  body,  it  has  been  thought 
unnecessary  to  reprint  them. 

(xxv.)  It  was,  however,  my  intention  to  have  placed  on  record,  in  this  volume, 
the  results  of  a  great  mass  of  Actinometric  observation  made  since  the  year  1824 
(at  Avhich  epoch  my  attention  was  first  directed  to  that  method  of  ascertaining- 
the  intensity  of  solar  radiation,  which  may  not  inaptly  be  termed  dynamical,  in 
contradistinction  to  the  usual  statical  method  by  the  observation  of  blackened 
thermometers,  photometers,  &c.)  In  addition  to  these,  between  five  and  six 
hundred  sets  of  such  observations  obtained  at  the  Cape,  would,  I  supposed,  have 
afforded  valuable  climatological  data,  and  led  to  conclusions  otherwise  important. 
Unfortunately,  the  necessity  of  a  correction  by  a  variable  factor  depending  on 
the  temperature  attained  by  the  liquid  enclosed  in  the  cylinder  of  the  instrument, 
had  not  been  foreseen  and  provided  for  in  any  of  these  observations,  and  only 
became  apparent  when  the  omission  was  beyond  remedy,  viz.,  when  the  results 
were  drawn  out,  and  ready  for  press.    They  are,  therefore,  suppressed  for  the 


INTRODUCTION. 


xix 


present,  leaving*  it  to  future  examination  to  determine  whether  among1  them 
there  may  not  he  a  portion,  made  under  such  circumstances,  or  registered  in 
such  a  manner  as  to  admit  of  the  temperature  and,  therefore,  the  correction 
in  question  heing'  ascertained  and  applied,  and  providing*  against  a  similar  evil  in 
future  by  a  simple  and  easily  applied  addition  to  the  instrument  itself. 

(xxvi.)  The  principles  upon  which  the  reduction  of  the  observations  made  with 
the  reflector  is  executed,  are  explained  at  large  in  the  Appendix  to  my  Catalogue 
of  northern  nebulas,  Phil.  Trans.  1833,  p.  482,  et  seq.,  and  need  not  here  be 
repeated.  Only  as  respects  the  precession  in  Right  Ascension,  a  slight  change  is 
introduced.  That  correction  depending*  both  on  the  Rigiit  Ascension  and  Polar 
distance  of  the  object,  would  introduce,  if  attempted  to  be  included  in  the  general 
system  of  interpolation  there  adopted,  a  term  of  double  entry  which,  however, 
since  the  zone  SAvept  is  of  small  breadth,  not  exceeding*  3°,  may  be  resolved  into 
two ;  the  one  a  term  of  singie  entry,  depending*  only  on  the  time  and  expressing* 
the  precession  for  a  constant  polar  distance,  that  of  the  middle  of  the  zone ;  the  other 
a  correction  of  this  for  objects  occurring*  out  of  the  middle  of  the  zone.  This 
latter  portion  is  a  term  of  double  entry ;  but  it  is  necessarily  of  very  small 
magnitude,  seldom  exceeding*  a  few  tenths  of  a  second  of  time.  In  the  system  of 
reduction  adopted  in  my  former  catalogue,  this  term  is  simply  negiected ;  or  the 
precession  is  reg-arded  as  the  same  throughout  the  breadth  of  the  zone.  Thus  it 
becomes  a  mere  function  of  the  time  of  observation,  and  merg*es  in  the  general 
correction  for  the  time,  to  be  interpolated  as  there  explained.  In  the  reduction 
of  the  present  series  of  observations,  this  did  not  appear  admissible,  and  it  became 
necessary,  therefore,  to  proceed  somewhat  differently,  making  a  special  exception 
of  the  precession  in  Eight  Ascension.  This  was  done  as  follows :  all  the  Right 
Ascensions  of  the  zero  stars  were  brought  up  to  the  beginning  of  the  year  nearest 
to  the  date  of  the  observation,  and  the  process,  in  its  original  form,  followed  out, 
as  if  to  reduce  the  observations  of  the  sweep  to  that  epoch.  The  reduction  (R) 
in  this  case,  consists  of  two  terms  (A)  and  (B),  of  singie  entry,  the  former  a 
function  of  the  time,  the  latter  of  the  polar  distance.  To  bring  these  to  the 
common  epoch  (1830)  adopted  throughout,  the  precession  is  thrown  into  the  form 
P  +  p,  where  P  is  the  precession  for  the  middle  of  the  zone,  and  p  is  the 
small  correction  to  be  applied  to  P  to  obtain  the  precession  for  any  other  point 


XX 


INTRODUCTION. 


out  of  the  middle.  Of  these,  P,  being*  a  function  of  the  time,  merges  in  A,  and 
is  added  to,  and  so  included  in  it;  and  p  is  calculated  by  a  small  table,  of 
double  entry,  and  applied  to  each  star  according-  to  its  proper  amount  and  sign. 

(xxvii.)  Great  and  unavoidable  delay  having  occurred  in  the  publication  of  these 
pages,  an  opportunity  has  been  afforded  for  a  careful  revision  of  the  Catalogues  sub- 
sequent to  their  printing"  off.  In  the  course  of  this  a  considerable  list  of  corrigenda 
has  been  accumulated,  partly  arising  from  error  of  the  press,  partly  of  copying,  and 
partly  of  calculation.  A  few  nebula?  and  double  stars  also,  which  are  not  included 
in  the  Catalogues,  having*  escaped  the  process  of  arrangement  by  which  they  were 
constructed,  have  been  discovered  in  the  sweeping- journals,  as  well  as  some  additional 
observations  of  others  which  are  so  included.  These  are  appended  accordingly  to 
the  list  of  corrig-enda.  Some  errors  which  vitiate  the  letter-press  are  also  noticed. 
They  are  few,  and  for  the  most  part  trivial,  Avith  the  exception  of  two  very  obnoxious 
ones  which  the  reader  is  requested  to  bear  in  mind,  or  correct  for  himself.  In  page 
299,  the  major  semiaxis  of  the  orbit  of  y  Virginia  is  stated  at  9".C9,  whereas  it 
oug-ht  to  be  3".58 ;  and  in  pag*e  308,  equation  (A),  the  numerical  coefficient  in  the 
value  of  fx,  instead  of  3.1514,  should  be  2744.7. 

(xxviii.)  It  remains  to  say  something"  as  to  the  mode  of  introducing*  this  work 
into  the  world.  To  the  munificent  destination  of  his  Grace  the  late  Duke  of 
Northumberland,  of  a  large  sum,  in  aid  of  its  publication,  it  owes  its  appearance 
as  a  sing*le  and  separate  work,  instead  of  a  series  of  unconnected  memoirs,  scattered 
over  the  volumes  of  academical  bodies.  The  lamented  decease  of  that  illustrious 
nobleman  prevented  his  witnessing*  its  final  completion.  His  liberal  intentions, 
however,  have  been  fully  carried  out  by  the  worthy  successor  to  his  titles  and  his 
spirit ;  whose  kind  and  gracious  interest  in  it,  I  should  be  wanting*  in  all  proper 
feeling*,  were  I  to  omit  this  opportunity  of  acknowledging. 


CHAPTER  I. 
OF  THE  NEBULiE  OF  THE  SOUTHERN  HEMISPHERE. 


OBSERVATIONS  OP  NEBULiE  AND  CLUSTERS  OF  STARS  TAKEN  IN  THE  COURSE 
OF  SWEEPING  WITH  THE  TWENTY-PEET  REFLECTOR. 

I.— INTRODUCTION  TO  THE  CATALOGUE  OF  NEBULAE. 

(1)  The  Catalogue  of  Southern  Nebulae,  which  forms  the  subject  of  this  chapter,  is  similar,  in 
every  particular  of  its  arrangement  and  construction,  to  my  Catalogue  of  Northern  Nebulae 
and  Clusters,  published  in  the  Transactions  of  the  Royal  Society,  for  1833,  and  is  reduced  to  the 
same  epoch  (1830-0),  for  the  purpose  of  facilitating  the  union  of  the  two  catalogues  into  one 
general  one.  Like  that  Catalogue,  it  presents,  assembled  in  one  view,  the  reduced  results  of 
all  the  observations  of  each  object  which  have  occurred  in  the  regular  course  of  sweeping,  in 
which  either  its  place  has  been  taken  (however  roughly),  or  in  which  any  particular  in  its 
appearance  or  physical  character  has  been  noted  ;  without  any  selection  of  good,  or  suppression  of 
discprdant  observations  whatever.  To  that  work  I  shall,  therefore,  refer  for  the  explanation, 
should  any  appear  to  be  needed,  of  its  arrangement,  and  of  the  purport  of  the  several  columns 
of  which  it  consists.  In  effect,  however,  these  sufficiently  explain  themselves,  with  exception 
of  the  abbreviations  employed  in  the  descriptions  and  columns  of  Synonyms,  which  it  is 
necessary  to  repeat  for  the  convenience  of  the  reader,  to  whom  they  would  otherwise  be 
unintelligible  without  perpetual  reference  to  another  volume,  which  he  might  not  have  at 
hand.  The  dates  of  the  several  sweeps  referred  to  in  this  and  my  former  catalogues,  will  be 
found  synoptically  arranged  in  the  table  immediately  appended  to  the  catalogue  now  in 
question. 

(2)  North  Polar  distances  are  preferred  to  south,  though  most  of  the  objects  in  the  Cata- 
logue are  situated  in  the  southern  hemisphere,  for  the  sake  of  uniformity,  and  for  the  main- 
tenance of  a  general  rule  in  applying  precession ;  and  for  a  similar  reason  Polar  distance  is 
preferred  to  declination,  not  merely  because  by  so  doing  the  signs  +  and  —  (fertile  sources  of 
mistake)  are  avoided,  but  also  because  all  doubt  or  hesitation  as  to  the  sense  in  which  the 
above-mentioned  element  is  to  be  applied  is  thereby  totally  precluded,  considerations  of  such 
moment  as  ought,  I  think,  to  lead  to  the  universal  disuse  of  declinations,  and  the  adoption  of 
North  polar  distances  in  their  stead,  in  all  astronomical  catalogues  henceforward  to  be  pub- 
lished.   It  ought  also  to  be  mentioned  that  the  "  sweeps  "  referred  to  in  the  last  column,  as 


2 


OBSERVATIONS  OF 


those  in  which  the  observations  occur,  are  numbered  forward  in  continuation  of  my  series  of 
northern  sweeps  made  at  Slough ;  so  that  the  Cape  series  (consisting  of  382  sweeps) 
commences  with  sweep  429,  and  terminates  with  sweep  810.  The  general  reference  num- 
bers in  the  first  column  are,  in  like  manner,  continued  onward  from  No.  2307,  the 
"  omitted"  nebula  added  after  the  2306  regularly  entered  in  order  of  R.  A.,  in  the  Northern 
Catalogue. 

The  following  is  the  system  of  abbreviations  adopted  : — 

1.  In  the  column  of  Synonyms — 
The  roman  and  arabic  numerals  (as  1.45)  occurring  together,  refer  to  the  classes  and 
numbers  of  nebulse  and  clusters  discovered  by  my  Father,  and  published  in  his 
catalogues : 

The  letter  B,  followed  by  a  number,  refers  to  the  "  Brisbane  Catalogue  "  of  Stars,  by 

the  general  number  of  that  catalogue  : 
M,  so  followed,  to  Messier's  Catalogue  of  Nebulse  : 

A,         „  to  Mr.  Dunlop's  do.  do.,  published  in  the  Transactions  of  the  Royal 

Society,  for  1828  : 
h,  followed  by  a  number,  to  my  Northern  Catalogue. 

(2.)  In  the  column  of  Descriptions  and  Remarks — 


denotes 


B 
b 
br 


CI  or  el  


comp 
D 
d 
E 

e 
ee 
F 
f 

fig 
g 

i  or  irr 
L 


Bright. 

brighter. 

broad. 

considerably. 

cluster. 

compressed. 

double  star. 

diameter,  distance. 

extended,  elongated,  or  elliptic. 

extremely. 

excessively. 

Faint. 

following. 

figure. 

gradually. 

irregular. 

large. 


1 

M 

m 

N 

neb 

n 

P 

pos 

R 

r 

S 
s 

St 

sc 

V 

vv 


denotes 


long,  or  a  little, 
in  the  middle, 
much, 
nebula. 

nebulous ;  nebulosity, 
north. 

pretty  (not  very) ;  preceding. 

angle  of  position. 

round. 

resolvable. 

small. 

south,  suddenly, 
stars, 
scattered, 
very. 

very  very  (exceedingly). 


*  Star. 

®  Globular  cluster. 

O  Planetary  nebula. 

c  Moon  above  the  horizon. 

c  c  Moon  very  troublesome. 


(3)  In  order  to  fix  in  the  reader's  mind  the  appearances  represented  by  such  combinations, 
occurring  in  the  description  of  a  nebula,  as  gbM  (gradually  brighter  in  the  middle),  pslbM 
(pretty  suddenly  a  little  brighter  in  the  middle),  &c. ;  it  will  suffice  to  refer  to  the  explanatory 
plate  (PI.  IX.  Phil.  Trans,  vol.  for  1833),  and  to  the  accompanying  table  of  explanations, 


NEBULAE  AND  CLUSTERS  OF  STARS. 


3 


p.  494,  of  the  same  volume,  in  which,  however,  an  important  erratum  exists  (viz.,  in  the  expla- 
nations of  figures  16,  17,  and  18,  in  which  the  abbreviations  pmbM,  mbM,  and  vmbM,  are,  by 
mistake,  printed  instead  of  the  correct  ones  descriptive  of  those  figures  which  are  psbM,  sbM, 
and  vsbM,  respectively). 

(4)  As  an  example  of  the  use  of  these  abbreviations  in  the  description  of  a  nebula,  the 
following  is  taken  from  the  preface  to  the  Northern  Catalogue  above  referred  to. 

"  vB  ;  vL ;  IE  ;  vgpmbM ;  50'7  1 ;  45"  br ;  pos  29°'3  by  microm.  a  *  9m.  45°  np,  dist.  80"," 
which  expanded  runs  thus  :  —  "  Very  bright ;  very  large  ;  a  little  extended  ;  very  gradually 
pretty  much  brighter  in  the  middle ;  50"  long  ;  45"  broad  ;  angle  of  position  (reckoned  from 
the  north  and  from  a  meridian  in  the  direction  north,  following,  south,  preceding)  measured 
290-3  by  the  micrometer.  A  star  of  the  ninth  magnitude  is  situated  45°  north  preceding  the 
centre  of  the  nebula  and  at  a  distance  from  it  of  80"  (both  by  estimation)."  Measured  angles 
are  always  marked  as  above  in  degrees  and  decimals.    Estimated  ones  without  decimals. 

(5)  It  will  of  course  be  readily  understood  that  very  great  differences  will  occur  in  the 
descriptions  of  one  and  the  same  nebula  taken  on  different  nights,  and  under  different  atmo- 
spheric circumstances,  as  well  as  in  different  states  of  the  mirror  and  the  eye :  nor  will  it  at  all 
startle  one  accustomed  to  the  observation  of  nebulae  to  see  such  an  object  described  at  one  time 
as  F  ;  S  ;  R  (faint,  small,  round),  and  at  another  as  B  ;  pL ;  pmE  ;  r ;  (bright ;  pretty  large  ; 
pretty  much  extended  ;  resolvable),  &c.  It  is  from  a  collection  of  all  these  descriptions  that 
the  true  or  final  description  has  to  be  made  out,  in  doing  which  it  is  to  be  recollected  that  the 
higher  observed  degrees  of  brightness,  size,  and  extension  are  to  be  preferred  in  general  to  the 
lower  ones,  since  atmospheric  and  other  deteriorating  causes  always  act  in  derogation  of  these 
qualities.  For  it  appears  to  be  a  general  law  in  the  constitution  of  "  extended"  nebulae,  that 
their  interior  or  brighter  strata  are  more  nearly  spherical  than  their  exterior  or  fainter ;  their 
ellipticity  diminishing  as  we  proceed  from  without  inwards,  a  character,  so  far,  in  favour  of  a 
rotation  on  an  axis,  in  the  manner  of  a  body  whose  component  parts  have  such  an  amount  of 
mutual  connexion  as  to  admit  of  such  a  mode  of  rotation,  and  of  the  exertion  of  some  degree  of 
pressure  one  on  another.  It  by  no  means,  however,  follows,  that  such  a  mode  of  rotation  can 
be  regarded  as  demonstrated  by  the  general  phenomenon  in  question,  since  a  system  of  internal 
movements  among  an  assemblage  of  bodies  perfectly  disconnected,  and  acting  on  each  other 
solely  by  attractive  forces  exerted  at  a  distance,  is  at  least  conceivable,  by  which  the  same 
appearances  to  a  remote  spectator  would  be  produced. 

(6)  The  number  of  nebulae  and  clusters  comprised  in  the  catalogue  here  presented,  is  1708. 
Of  these  eighty-nine  are  identical  with  objects  previously  observed  by  myself  at  Slough,  and 
which  occur,  in  consequence,  in  my  Northern  Catalogue.  In  these  cases  it  has  been  preferred 
to  number  them  onwards,  regularly  in  succession,  as  if  now  for  the  first  time  observed,  rather 
than  interrupt  the  succession  by  breaks  or  by  the  re-insertion  of  earlier  numbers.  The  letter  h, 
with  its  accompanying  number  in  the  column  of  synonyms,  will  point  out  the  places  in  the 
former  catalogue  of  such  of  these  as  occur  there  for  the  first  time ;  and  a  reference  to  that 
catalogue  being  made  will  readily  identify  such  others  as  have  previously  been  described  by 
my  Father,  or  by  Messier. 

(7)  Of  the  objects  remaining,  135  are  nebulae  and  clusters  of  my  Father's  catalogues,  now, 
for  the  first  time,  reobserved ;  9  are  Messier's,  5  of  which  are  identical  with  objects  catalogued 


4 


OBSERVATIONS  OF 


by  Mr.  Dunlop  ;  and  206  others  have  also  been  identified,  with  more  or  less  certainty  (indicated 
by  the  absence  or  presence  of  the  sign  ?),  with  objects  observed  by  Mr.  Dunlop,  and  described 
iu  his  Catalogue  of  Nebulae.  The  rest  of  the  629  objects,  comprised  in  that  catalogue,  have 
escaped  my  observation  ;  and  as  I  am  not  conscious  of  any  such  negligence  in  the  act  of 
sweeping  as  could  give  rise  to  so  large  a  defalcation,  but,  on  the  contrary,  by  entering  them 
on  my  working  lists  (at  least,  until  the  general  inutility  of  doing  so,  and  loss  of  valuable  time 
in  fruitless  search,  thereby  caused  it  to  become  apparent),  took  the  usual  precautions  to  ensure 
their  rediscovery  ;  and  as  I  am,  moreover,  of  opinion  that  my  examination  of  the  southern 
circumpolar  region  will  be  found,  on  the  whole,  to  have  been  an  effective  one,  I  cannot  help  con- 
cluding that,  at  least  in  the  majority  of  those  cases,  a  want  of  sufficient  light  or  defining  power 
in  the  instrument*  used  by  Mr.  Dunlop,  has  been  the  cause  of  his  setting  down  objects 
as  nebulae  where  none  really  exist.  That  this  is  the  case,  in  many  instances,  I  have  con- 
vinced myself  by  careful  and  persevering  search  over  and  around  the  places  indicated  in  his 
catalogue. 


II.— REMARKS  ON  THE  CATALOGUE. 

Of  the  degree  of  precision  attributable  to  the  places  of  the  objects  it  comprises. 

(8)  A  great  number  of  the  objects  described  in  the  following  catalogue  rely  on  single 
observations  for  the  determination  of  their  places.  On  this  point  a  remark  applies  similar  to 
that  made  on  the  same  subject  in  my  Northern  Catalogue.  To  have  secured  two  or  more 
observations  of  each  recorded  nebula,  would  have  required  the  whole  surface  of  the  heavens 
to  have  been  swept  at  least  four  times  over,  on  the  system  of  observation  pursued,  viz.,  twice 
for  discovery,  and  twice  for  verification  and  precise  determination.  In  going  a  second  time 
over  the  same  ground,  or  even  a  third,  in  the  richer  regions  of  the  heavens,  it  would  have  been 
very  unadvisable  to  have  arrested  the  sweeping  process  at  each  nebula  detected  in  the  first 
course  of  sweeps  for  the  purpose  of  reobserving  it ;  since,  by  so  doing,  the  escape  of  every 
other  object  of  interest  (whether  nebula,  cluster,  or  double  star),  situated  in  the  same  zone,  and 
within  two  or  three  minutes  in  right  ascension,  or  even  more,  if  the  object  reobserved  were  in 
anyway  interesting,  would  have  been  infallibly  insured.  With  such  an  instrument  as  that  which 
I  employed,  the  place  of  an  object  cannot  be  determined  with  precision  otherwise  than  by 
including  it  in  a  zone  with  sufficient  zero  stars  to  form  a  connected  series:  and  to  have  carried 
out  this  process  with  that  especial  view  (however  desirable  a  thing  in  itself)  would  have 
required  at  least  two,  and  probably  three  years  of  additional  observation.  As  it  was,  it  proved 
difficult,  and,  in  fact,  was  not  entirely  accomplished,  to  go  clearly  twice  over  every  part  of  the 
surface  of  the  hemisphere;  and,  in  consequence,  anything  approaching  to  such  a  systematic 


*  A  9-inch  Newtonian  reflector,  of  9  feet  focal  length,  which,  in  point  of  light,  would  correspond  to  ahout 
one-seventh  of  that  used  in  my  sweeps.  That  such  was  its  construction,  I  conclude  from  the  mention  of  the  largt 
mirror  in  Philosophical  Transactions,  1828,  p.  113. 


NEBULuE  AND  CLUSTERS  OF  STARS.  ■> 

revision  and  reobservation  of  individuals  was  quite  out  of  the  question,  unless  in  the  case  of  objects 
of  peculiar  interest,  which  it  would  have  been  wrong  not  to  have  reobserved ;  or  in  those  cases 
where,  in  crowded  regions,  it  became  absolutely  necessary  to  multiply  observations  to  avoid 
confounding  together  different  individuals.  Indeed,  in  the  case  of  the  two  nubecula?,  and 
especially  in  that  of  the  Nubecula  Major,  it  was  found  necessary  (such  is  their  richness)  to 
abandon  the  system  of  observing  in  zones  of  3°  in  breadth,  and  to  break  them  up  into  single 
degrees,  so  as  to  afford  longer  intervals  between  the  transits ;  by  which  alone  the  observation 
of  all  their  component  nebulse  could  be  satisfactorily  secured.  However  where,  owing  to 
the  occurrence  of  important  objects  in  a  zone,  it  was  thought  advisable  to  go  over  it  more 
than  twice  the  opportunity  of  reobservation  was  of  course  seized,  if  tolerably  certain  that  by 
so  doing  there  were  no  risk  of  missing  a  nebula  previously  unobserved. 

(9)  Under  these  circumstances  it  is  of  course  interesting  to  have  some  means  of 
satisfying  ourselves  what  confidence  is  due  to  a  single  observation  of  place.  And  this  is 
afforded  by  the  arrangement  of  the  catalogue  itself,  in  which  the  results  of  all  the  individual 
observations  of  each  object,  reduced  independently  and  in  almost  every  case  (of  necessity)  by 
a  different  series  of  zero  stars  are  confronted  together.  Without  going  into  calculations  on 
the  theory  of  probabilities,  it  will  be  tolerably  evident  to  any  one  who  may  cast  his  eyes 
over  the  columns  of  R  A,  and  NPD,  that,  if  we  put  aside  loose  objects  such  as  large  clusters 
of  stars  without  any  remarkable  star  centrally  situated  as  a  point  of  reference ;  or  large  ill- 
defined  or  irregularly  shaped  nebulae ;  as  well  as  observations  marked  as  imperfect  (by  the 
sign  +  ) ;  cases  are  comparatively  rare  in  which  two  observations  of  the  same  object  differ 
by  a  whole  minute  in  N  P  D,  or  by  a  quantity  in  R  A,  which,  when  converted  into  space 
according  to  the  rule  for  convergence  of  meridians  will  give  the  same  amount  of  discordance 
in  the  direction  of  the  parallel.  For  the  great  majority  of  objects,  therefore,  the  line  of 
collimation  of  a  telescope,  pointed  according  to  the  mean  of  the  observations  recorded  (when 
more  than  one),  will  strike  upon  a  point  of  the  heavens  within  the  visible  area  of  the  nebula 
observed,  even  though  its  angular  diameter  should  not  exceed  a  single  minute  of  a  degree. 

(10)  In  the  cases  of  single  observations,  mistakes  of  reading  and  of  reduction  are  the 
most  dangerous,  and  to  these  the  results  of  such  observations  are  of  course  always  more  or 
less  liable.  I  have  every  reason  to  hope  that  such  mistakes  have  been  very  unfrequent. 
Whenever  the  smallest  ground  for  suspicion  has  occurred,  the  reductions  have  been  carefully 
re-examined.  It  was  my  intention  to  have  gone  over  the  whole  of  the  reductions  twice,  and 
the  work  has  been  partly  done,  but  I  found  myself  unequal  to  the  task  of  completing  it. 
However,  in  order  to  form  a  notion  on  some  better  ground  than  mere  general  impression  of 
the  probable  frequency  of  such  mistakes,  after  drawing  out  in  order  of  R  A  the  fair  copy  of 
the  reduced  catalogue,  I  proceeded  to  compare  the  places  of  such  nebula?  and  other  well- 
defined  objects  common  to  both  the  Northern  and  Southern  Catalogues  as  have  their  places 
determined  only  by  one  observation  in  the  latter.  This  afforded  sixty-five  comparisons  in  R  A, 
and  sixty-eight  in  N  P  D,  in  the  course  of  which  the  errors  detected  in  reading  and  reduction 
were  as  follows  : — 

.     fin  the  Southern  Catalogue        ......  0 

Errors  of  reduction)  T         -v  ^  .  i 

I  In  the  JN  orthern  Catalogue  1 


c 


6 


OBSERVATIONS  OF 


Errors  of  reaclin 


flm 

8"{p 


lm  of  Chronometer  in  R  A  1 

inNPD   .2 

Mistakes  of  wire  in  observations  of  R  A     .       .       .       .       .       .       •  .0 

The  error  of  reduction  thus  detected  affects  the  R  A  of  the  nebula  h.  1540  of  the  Northern 
Catalogue  which,  in  place  of  13h  0m  30s  *4,  should  be  13h  0m  50s  4. — The  chronometer  readings 
are  liable  to  an  occasional  error  of  lm  when  the  second  hand  stands  between  50s  and  60 ;  and 
the  minute  so  erroneously  read  is  almost  certain  to  be  in  excess.  It  is  therefore  a  useful 
precaution,  in  looking  out  for  a  nebula  or  other  object,  whose  place  is  settled  only  by  a  single 
observation,  to  presume  the  possibility  of  such  an  error,  and  to  have  the  eye  at  the  eye- piece 


a  full  minute  before  the  registered  time. 


The  effect  of  an  erroneous  degree  in  Polar  distance 


is  much  worse ;  as  it  necessarily  causes  the  loss  of  the  observation ;  but  in  all  the  above 
compared  cases  the  instrument  having  been  set  to  the  places  of  the  nebulae  by  the  working 
lists  previously  prepared,  the  degree  has  probably  been  read  and  registered  more  negligently 
than  in  the  case  of  an  unknown  object,  the  attention  having  been  concentred  on  the  minutes 
and  seconds.  I  may  further  observe  that,  in  the  very  great  number  of  cases  where  the  same 
unknown  nebula  has  been  swept  over  several  times,  instances  of  misreading  such  as  those  above 
considered  appear  to  have  been  very  rare.  In  such  cases  they  detect  themselves,  and  though 
of  course  in  registering  them,  in  the  catalogue  form  adopted,  they  have  always  been  corrected 
when  discovered,  yet  the  fact  of  such  correction  being  made  is,  in  every  instance,  expressly 
noticed  in  the  column  of  Remarks.  Much  care  also  has  been  taken  to  examine  the  catalogue 
for  cases  where  two  nebulae  occurring  in  different  sweeps,  and  otherwise  agreeing  both  in 
description  and  place,  differ  by  a  single  minute  of  time  in  R  A,  or  by  a  single  degree  in  N  P  D 
(for  in  the  system  of  observing  adopted,  a  misreading  of  2°  is  hardly  jwssible).  In  such  cases 
there  necessarily  arises  a  suspicion  of  identity  which,  when  it  occurs,  is  also  noticed  in  the 
remarks  annexed. 

(11)  Correcting  these  mistakes  of  reading,  the  actual  discordances  found  to  subsist 
between  the  two  Catalogues  run  as  follows  :  — 


Discordances  in  R  A. 

Discordances 

in  N  P  D. 

s 

s 

Above  0" 

but  not  exceeding 

20"  — 

34 

Above  0-0 

but  not 

exceeding 

1-0  — 

32 

„  20" 

>> 

40"  — 

20 

„  1-0 

») 

j) 

20  — 

14 

„  40" 

ii 

it 

60"  — 

5 

„  2-0 

)» 

>» 

3-0  — 

11 

„  60' 

>> 

>i 

80"  — 

5 

„  3-0 

)» 

>> 

4-0  — 

8 

„  80' 

?i 

»» 

90"  — 

4 

„  4-0 

j» 

u 

0 

„  90" 

>» 

0 

65 

68 

(12)  Although  the  number  of  observations  thus  compared  is  not  large,  yet  it  suffices  to 
afford  a  reasonable  presumption  (taking  the  error  at  half  the  discordance)  that  the  place  of  a 
well-defined  nebula,  determined  by  a  single  observation,  will  seldom  be  found  in  error  to  the 
extent  of  30''  of  space  in  the  direction  of  the  parallel,  or  of  45"  in  that  of  the  meridian.  The 
entry  of  a  known  and  expected  nebula  to  which  the  telescope  has  been  set  into  the  field  of  view 
bisected  by  the  horizontal  wire  is  a  thing  of  no  uncommon  occurrence. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


7 


Explanation  of  the  figures  referred  to  in  the  Catalogue  of  Southern  Nebula:  and  clusters,  with 
more  detailed  descriptions  and  monographs  of  some  of  the  most  remarkable  nebula;  of  the 
Southern  Hemisphere. 

(13)  Fig.  1,  Plate  II.;  M.  17  =  h.  2008;  RA  18h  Um  N  P  D.  106°  15'.  This  very 
remarkable  object  is  figured  in  my  Northern  Catalogue  (fig.  35),  but  owing  to  the  deficiency 
of  Micrometrical  measures  for  laying  clown  the  stars,  its  form  is  far  from  accurately  expressed 
in  that  representation.  In  particular  the  large  horse-shoe-shaped  arc  which  forms  so  striking 
and  conspicuous  an  appendage  to  the  bright  oblique  streak  observed  by  Messier  at  its  preceding 
termination,  is  there  represented  too  much  elongated  in  a  vertical  direction  and  as  bearing 
altogether  too  large  a  proportion  to  that  streak,  and  to  the  total  magnitude  of  the  object. 
The  nebulous  diffusion  too,  at  the  preceding  end  of  that  arc,  forming  the  preceding  angle  and 
base  line  of  the  capital  Greek  omega  (12)  to  which  the  general  figure  of  the  nebula  has  been 
likened,  is  now  so  little  conspicuous  as  to  induce  a  suspicion  that  some  real  change  may  have 
taken  place  in  the  relative  brightness  of  this  portion  compared  with  the  rest  of  the  nebula ; 
seeing  that  a  figure  of  it  made  on  the  25th  of  June,  1837  (on  which  occasion  other  details 
presently  to  be  noticed  were  well  seen,  and  for  the  first  time  distinctly  delineated),  expresses  no 
such  diffusion,  but  represents  the  arc  as  breaking  off  before  it  even  attains  fully  to  the  group 
of  small  stars  at  the  preceding  angle  of  the  Omega.  Neither  is  the  smaller  of  the  two  nebulous 
knots  at  its  following  angle  close  adjoining  to  the  small  star  there  situated  so  conspicuous  as  to 
have  attracted  particular  notice  either  on  that  occasion,  or  on  the  13th  August,  1835,  when  a 
pretty  elaborate  drawing  was  made  of  all  the  then  known  parts  of  the  nebula,  and  a  number  of 
measures  taken  with  the  twenty-feet  position  micrometer  with  a  view  to  the  construction  of  a 
correct  monograph  of  it. 

(14)  Under  these  circumstances  the  argument  for  a  real  change  in  the  nebula  might  seem 
to  have  considerable  weight.  Nevertheless  they  are  weakened  or  destroyed  by  a  contrary 
testimony  entitled  to  much  reliance.  Mr.  Mason,  a  young  and  ardent  astronomer,  a  native 
of  the  United  States  of  America,  whose  premature  death  is  the  more  to  be  regretted,  as  he 
was  (so  far  as  I  am  aware)  the  only  other  recent  observer  who  has  given  himself,  with  the 
assiduity  which  the  subject  requires,  to  the  exact  delineation  of  nebulae,  and  whose  figures  I 
find  at  all  satisfactory,  expressly  states  (Mem.  American  Phil.  Soc.  vol.  vii.  Art.  xiii.  p.  177) 
that  both  the  nebulous  knots  were  well  seen  by  himself  and  his  coadjutor  Mr.  Smith,  on  the 
1st  August,  1839,  i.  e.  two  years  subsequent  to  the  date  of  my  last  drawing.  Mr.  Mason  also 
declares  the  upper  and  larger  knot  to  be  irresolvable  by  his  telescope  (a  reflector  of  12 
inches  aperture  and  14  feet  focal  length  constructed  by  himself).  In  this  particular  my 
observations  of  1835  and  1837,  so  far  agree  that  its  resolvability  is  not  mentioned  in  words 
or  indicated  in  the  diagrams  made  on  those  occasions.  And,  with  respect  to  the  diffusion  of 
the  nebula  among  the  group  of  stars  at  the  preceding  angle  and  along  the  base-line  of  the 
Omega,  it  is  represented  as  tolerably  conspicuous  in  his  figure — for  which  reason,  and  because 
it  was  decidedly  noticed  as  a  feature  in  my  earlier  observations,  I  have  retained  both  it  and 
the  lesser  knot  in  my  present  figure,  considering  the  negative  evidence  of  their  having  escaped 
delineation  on  those  two  nights  as  outweighed  by  the  positive  testimony  in  favour  of  their 


s 


OBSERVATIONS  OF 


existence  both  at  an  earlier  and  a  later  epoch.  Neither  Mr.  Mason  however,  nor  any  other 
observer,*  appears  to  have  had  the  least  suspicion  of  the  existence  of  the  fainter  horse-shoe 
arc  attached  to  the  follotving  extremity  of  Messier's  streak.  It  was  seen  on  both  the  nights 
in  question,  but  only  delineated  in  its  true  form  and  magnitude  on  the  latter.  It  merits, 
however,  a  more  particular  attention  than  I  was  then  able  to  bestow  on  it,  as  it  is  possible  that 
yet  other  convolutions  may  exist.  I  should  observe  that  the  three  stars  which  mark  its 
extremity  are  not  micrometrically  laid  down. 

(15)  The  stars  visible  in  this  nebula  are  for  the  most  part  too  small  to  admit  of  their 
differences  of  R  A  and  NPD  being  taken  with  the  equatorial  micrometer  conveniently. 
Accordingly  only  three  or  four  have  been  so  laid  down.  The  more  conspicuous  of  the 
remaining  ones  down  to  the  12th,  and  one  or  two  of  smaller  magnitudes  have  been  determined 
by  triangulation  from  these  by  angles  of  position  taken  with  the  20  feet  position  micrometer. 
Several  of  these  angles  were  measured  in  England,  the  rest  at  the  Cape,  on  the  13th  August, 
1835.  No  reason  existing  for  preference,  the  means  of  all  the  observed  positions  belonging  to 
the  same  pairs  of  stars  were  adopted,  and  the  whole  system  of  angles  projected  on  a  chart 


*  Dr.  Lamont,  in  his  Academical  Thesis  on  Nebulae,  read  before  the  Bavarian  Academy,  Aug.  25,  1837,  has 
given  a  figure  of  this  nebula,  accompanied  with  a  description.  In  this  figure  the  nebulous  effusion  at  the 
preceding  angle,  and  along  the  preceding  base  line  of  the  Omega,  is  represented  as  very  conspicuous ;  indeed 
much  more  so  than  I  can  persuade  myself  it  was  his  intention  it  should  appear — the  engraver  having  probably 
overdone  it.  However,  it  justifies  my  retaining  it.  He  has  not  given  any  indication  of  the  additional  loop  at 
the  following  end  of  Messier's  branch.  He  also  remarks,  as  Mr.  Mason  has  done,  on  the  irresolvability  of  the 
insulated  knot ;  and,  as  observed  in  the  text,  I  am  not  disposed  to  insist  on  its  being  resolvable.  He  accounts, 
however,  for  my  having  considered  it  as  such,  by  the  existence  of  two  very  minute  stars  in  it.  These  have 
escaped  my  notice.  I  ought  here  to  observe,  that  Dr.  Lamont  appears  to  have  misconceived  my  meaning  in 
that  part  of  the  description  of  this  nebula,  appended  to  my  Northern  Catalogue,  where  it  is  said  that,  "  With 
a  view  to  a  more  exact  representation  of  this  curious  nebula"  {more  exact,  that  is  to  say,  than  the  figure  there 
given),  "  I  have  at  different  times  taken  micrometrical  measures  of  the  relative  places  of  the  stars  in  and  near 
it,  by  which,  when  laid  down  as  in  a  chart,  its  limits  may  be  traced  and  identified,  as  I  hope  soon  to  have  a  better 
opportunity  to  do,"  &c.  Dr.  L.  interprets  this  passage  to  mean,  that  the  figure  in  that  catalogue  was  based 
upon  a  series  of  micrometrical  measures,  whereas  he  finds  material  discordances  between  that  figure  and  his 
own  (no  doubt  accurate)  measurements.  But  this  is  neither  the  purport  of  the  passage  cited,  nor  its  plain 
grammatical  sense.  A  few,  but  very  rude  and  imperfect  micrometric  measures,  no  doubt  were  used  in  con- 
structing that  figure  ;  but  for  the  most  part  it  is  a  mere  eye  draft,  and,  as  now  appears,  considerably  distorted. 
Though  not  relevant  to  the  immediate  subject,  I  will  take  this  opportunity  (as  another  may  not  occur)  to  notice 
a  point  of  some  interest,  which  has  arisen  on  a  comparison  of  Dr.  Lamont's  figure  and  description  of  the 
Planetary  Nebula  h.  2037,  with  my  own  observations.  According  to  Dr.  L.,  that  nebula  has  two  small  stars 
nf,  one  upon  the  very  edge,  the  other  removed  from  it  by  f  of  the  diameter  of  the  nebula.  The  former  is 
the  star  observed  and  described  by  me  in  my  catalogue,  but  it  is  there  called  11  m,  whereas,  on  referring 
to  the  original  observation,  I  find  the  figures  to  be  15,  the  five  being  obscurely  written  over  a  1  as  a  correction. 
No  engraving  was  made  of  this  nebula,  but  in  both  the  sweeps  where  it  was  observed  diagrams  were  made, 
which  agree  in  representing  this  star,  not,  as  in  Dr.  Lamont's  figure,  precisely  on  the  edge,  but  at  a  distance 
from  it  about  \,  or  |  at  most,  of  the  diameter.  The  other  star  was  not  marked  on  either  occasion.  Being 
considerably  more  distant,  it  was  passed  over  among  the  "  many  other  stars  in  the  field."  My  reason  for 
drawing  attention  to  this  point  is  that,  from  all  the  circumstances  of  the  case,  there  can  be  very  little 
doubt  of  a  relative  motion  of  the  objects  inter  se ;  and  it  will  be  therefore  interesting  to  re-observe  them, 
which  I  trust  Dr.  L.  will  do. 


NEBULA  AND  CLUSTERS  OF  STARS. 


9 


by  means  of  a  protractor.  Thus,  from  the  equatorial ly  determined  stars  adopted  as  a  basis 
of  projection  others  were  derived  by  the  intersection  of  their  directions,  and  from  these  again 
others,  and  so  on ;  using  always  the  best  trigonometrical  combinations  the  respective  cases 
would  admit,  and  adjusting  cases  of  discordant  intersections  as  they  arose,  on  an  impartial 
consideration  of  their  merits.*  From  the  stars  so  laid  down  by  triangulation,  others  depending 
only  on  eye-drafts  were  then  inserted  on  the  chart  according  to  their  configurations.  Finally, 
the  differences  of  R  A  and  NPDof  the  stars  of  these  two  latter  classes  were  read  off  from  the 
chart  by  the  aid  of  diagonal  scales,  and  the  whole  entered  in  a  catalogue ;  which  done,  the 
nebula  was  then  Avorked  in  upon  the  chart  as  carefully  as  possible  according  to  the  united 
evidence  of  all  the  drawings  and  diagrams  at  any  time  procured  of  it  or  of  any  of  its  parts. 

(16)  The  following  is  the  Catalogue  in  question,  in  which  the  first  column  contains  the 
number  for  future  reference — the  second,  letters  for  more  convenient  citation,  the  third  the 
magnitude  assigned  to  the  star  on  a  comparison  of  all  the  observations  neglecting  half 
magnitudes  below  the  8th.  The  fourth  column  contains  the  difference  of  right  ascension  in 
seconds  of  time,  and  the  fifth  that  of  North  Polar  distance  in  parts  of  the  equatorial  wire 
micrometer,  (1000  parts  =  4'  0".4.)  from  the  chief  or  Zero  star,  which  in  this  case  is  the 
conspicuous  star  a  little  preceding  the  summit  of  the  brighter  horse-shoe.  Lastly,  the  sixth 
column  contains  the  classes  to  which  the  determinations  of  the  stars  belong  in  respect  of 
probable  precision ;  class  1,  containing  stars  determined  by  differences  directly  observed  with 
the  equatorial ;  2,  stars  projected  by  triangulation  as  above  described,  and  3,  stars  inserted  from 
eye-drafts.    Dots  attached  ( : )  denote  want  of  precision. 

CATALOGUE  OF  THE  STARS  LAID  DOWN  IN  THE  DRAWINGS  OF  M  17  =  h.  2008. 


No. 

Letter. 

a 

X 

ARA 
from  a. 
Sec.  Dec. 

y 

ANPD 
from  a. 
Parts. 

tn 
a 

3 

No. 

Letter. 

3 

X 

ARA 
from  a. 
Sec.  Dec. 

y 

ANPD 
from  a. 
Parts. 

en 

03 

a 

3 

i 

p 

14 

-  7-i 

—  720 

2 

23 

1 

IO 

+  !5-9 

-1530 

2.3 

2 

1 

K 

IT, 

-  6.1 

—  840 

3 

24 

e 

12 

+  16.1 

-1755 

3 

3 

17 

-  5-3 

—  910 

3 

25 

s 

9 

+  17.2 

— 1640 

2 

4 

X 

14 

-  4.1 

-  34° 

2 

26 

e 

8 

+  !9-3 

+  1450 

2 

5 

T 

-  4.0 

-  745 

3 

27 

n 

!3 

+21.0 

— 1710 

3 

6 

7 

1 1 

-  3-6 

-  970 

1 

28 

V 

'5 

+22.0 

—  1 10 

3  : 

7 

c 

IO 

-  1.8 

+  1215 

2 

29 

w 

!5 

+  22.7 

—  220 

3  = 

8 

0 

13 

—  1.2 

—  960 

2 

30 

s 

r3 

+27.1 

—  1 180 

3  ••• 

9 

7T 

15 

—  1.0 

—  825 

3 

31 

b 

II 

+28.2 

+  560 

2 

IO 

Z 

1 1 

-  0.9 

+  480 

1,2 

32 

d 

H 

+28.3 

+  80 

3  • 

ii 

a 

9 

.  0.0 

0 

1 

33 

<T 

12 

+29.0 

-  880 

3  " 

12 

S 

16 

.  0.0 

-  33° 

3 

34 

1 

1 1 

+  33-9 

—  1450 

3  :: 

r3 

V 

13 

+  0.5 

-  510 

2 

35 

a 

13 

+  35-2 

—  360 

2 

14 

f 

9 

+  4-4 

+  1805 

2 

36 

V 

12 

+  37-2 

-1750 

3  : 

15 

f 

13 

+  4-9 

-  660 

2 

37 

k 

10 

+  39.8 

— 1700 

2 

16 

K 

12 

+  6.4 

+  205 

2 

38 

t 

14 

+40.5 

-1330 

3  " 

17 

X 

1.3 

+  7-3 

-  840 

2 

39 

m 

1 1 

+41.4 

— 1300 

3  :: 

18 

£ 

1 1 

+  7-3 

-  47° 

2 

40 

u 

+44-9 

— 1000 

3  :: 

'9 

0) 

15 

+  7.5 

—  630 

2 

41 

h 

1 1 

+45.0 

—  640 

3  " 

20 

10 

+  8.2 

-  275 

1 

42 

P 

9 

+  59.0 

+  325 

3  - 

21 

12 

+  8.6 

+  560 

2 

43 

q 

10 

+63.6 

+  415 

3  :: 

22 

16 

+  12.9 

+  13° 

3 

44 

r 

1 1 

+67.8 

+  650 

3  :: 

*  When  a  star  is  determined,  in  this  mode  of  proceeding,  by  three  or  more  intersecting  lines  which  do  not 
meet  in  a  single  point,  bad  trigonometrical  combinations  must  be  disregarded,  and  the  centre  of  gravity  of  the 
intersections  afforded  by  the  good  ones  only  taken. 

D 


10 


OBSERVATIONS  OF 


Fig.  2,  Plate  II.  H.  IV.  41  =V.  10,  11,  12=h.  1991.    R  A.  17h  52m ;  NPD1130!'. 

(17)  I  have  been  rather  unfortunate  in  my  figures  of  this  nebula.  That  given  in  my 
Northern  Catalogue  (fig.  80)  is  not  to  be  taken  as  more  than  an  attempt,  and  that  a  most  rude 
and  imperfect  one  to  show  the  situation  of  the  fine  triple  star  in  its  centre  with  respect  to  the 
nearer  portions  of  the  three  principal  surrounding  nebulous  masses.  It  is  stated  in  the 
observations  recorded  in  that  Catalogue,  that  a  careful  drawing  made  of  the  nebula  was  lost, 
and  that  the  figure  there  given  was  constructed  from  much  less  elaborate  sketches  (in  fact 
the  rudest  imaginable)  aided  by  memory.  The  drawing  from  which  my  present  figure  is 
constructed,  was  the  work  of  a  single  night  only  (about  the  beginning  of  August  1835,  for  it 
bears  no  date,  though  the  time  can  be  ascertained  nearly  from  other  circumstances).  No 
previous  micrometrical  measurements  however  having  been  procured  of  the  stars  involved  and 
adjacent,  wherewith  to  prepare  a  "  working  skeleton"  for  laying  down  the  nebula,  both 
nebula  and  stars  were  worked  in  by  the  unassisted  eye,  and  although  a  series  of  angles  of 
position  among  the  principal  stars  was  taken  after  the  completion  of  the  drawing  (all  single 
measures),  their  results  when  subsequently  projected,  exhibited  some  material  disagreements 
from  the  eye-draft  in  respect  of  the  situations  of  several  of  them  inter  se,  and  in  one  instance 
(that  of  the  star  marked  k  in  the  Catalogue  annexed)  the  situation  so  projected  proved  quite 
irreconcileable  with  the  eye-draft,  a  discordance  which  however  disappeared  on  supposing  an 
error  of  5°  to  have  been  committed  in  one  of  the  angles  of  position  (from  /3)  by  which  it  had 
been  determined.  However  as  (allowing  such  an  error  to  have  been  committed)  the  angles  in 
question  sufficed  to  fix  the  relative  places  of  the  six  chief  stars  a  13  e  77  9  k  by  direct 
intersections,  and  of  £  t  A  p  v  <p  x>  each  by  a  measured  position  from  /3  combined  with 
undoubted  allineations  among  the  other  stars,  on  the  whole  in  a  tolerably  satisfactory  manner, 
there  was  little  difficulty  in  inserting  the  other  stars  of  the  eye-draft  so  as  to  preserve  their 
configurations,  and  thence  to  lay  down  the  nebula  upon  them  without  doing  violence  either 
to  its  general  aspect,  or  to  any  important  feature.  Had  the  discordance  in  question  been 
detected  before  the  final  removal  of  the  telescope  it  would  have  been  easily  rectified,  but  the 
original  drawing  having  been  considered  at  the  time  satisfactory,  it  was  put  aside  and  not 
subsequently  re-examined  and  compared  with  the  nebula  itself,  a  circumstance  the  more  to  be 
regretted  as  this  wonderful  object,  independent  of  its  intrinsic  interest,  has  also  been  made  a 
subject  of  especial  and  elaborate  examination  by  Mason  in  his  paper  already  cited,  illustrated 
with  a  well-executed  figure  constructed  from  observations  in  the  year  1839. 

(18)  On  comparing  our  figures,  they  will  be  found  to  agree  in  every  essential  particular 
allowing  for  the  difference  of  light  between  reflectors  of  12  and  18  inches  aperture,  with  one 
rather  remarkable  exception,  viz.,  in  the  form  of  the  southern  mass  of  the  trifid  nebula  and  the 
character  of  the  curvature  of  the  three  paths  or  avenues  which  lead  up  to  the  triple  star. 
Mason  represents  these  avenues  as  free  from  any  abrupt  change  of  direction,  the  northern 
and  the  preceding  of  them  branching  out  with  an  easy  and  graceful  bifurcation  from  the 
southern  :  whereas  my  figure  whose  correctness  in  this  respect  I  cannot  doubt,  gives  to  the 
preceding  avenue  a  remarkably  sudden  and  uncouth  flexure,  like  a  gnarled  branch  of  an  oak, 
just  at  its  divergence  from  the  other  two.  The  southern  nebulous  mass,  in  my  figure,  has  a 
considerably  wider  extension  towards  the  preceding  side  than  in  Mason's  which  represents  it  as 


NEBULAE  AND  CLUSTERS  OF  STARS. 


11 


nearly  round ;  but  as  this  portion  is  very  faint  there  was  probably  not  light  enough  in  his 
telescope  to  render  the  whole  visible.*  On  comparing  his  stars  with  mine  as  laid  down  from 
the  following  catalogue,  some  will  be  found  to  which  I  have  none  corresponding  (and  vice 
versa),  and  it  is  not  unlikely  that  many  more  may  have  escaped  my  notice,  not  for  want  of 
power  in  the  telescope  to  show  them,  but  for  want  of  a  sufficiently  prolonged  and  methodical 
scrutiny  specially  directed  to  this  point.  Such  objects  in  fact  cannot  be  adequately  described 
and  figured  in  a  single  night.  They  require  repeated  examination  and  breaking  up  into 
triangles  to  be  explored  in  detail,  and  the  near  proximity  of  this  in  particular  to  another 
extensive  and  complex  nebula  (Messier's  8th),  from  which  it  is  distant  hardly  more  than  a 
degree,  renders  a  fuller  examination  of  it  desirable,  with  a  view  to  the  possibility  of  tracing  a 
nebulous  connexion  between  them. 

CATALOGUE  OF  THE  STARS  LAID  DOWN  IN  THE  FIGURE  OF  H.  IV.  41  =  h.  1991. 


No. 

Letter. 

Mag. 

X 

ARA 
from  a  in 
time. 
Sec.  Dec. 

y 

ANPD 
from  a  in 
Mic.  Pts. 

Parts. 

Class. 

No. 

Letter. 

Mag. 

X 

ARA 
from  a  in 
time. 

Sec.  Dec. 

y 

ANPD 
from  a  in 
Mic.  Pts. 
Parts. 

5 

i 

£ 

12 

-  8.0 

"  875 

2 

iS 

e 

11 

+  7-i 

—  290 

2 

2 

C 

IS 

-  6.9 

-  39° 

3 

16 

1 

13 

+  7.2 

—  2980 

2.3 

3 

P 

n 

-  6.4 

—  2230 

2.3 

17 

K 

12 

+  7-6 

4-  280 

2.3 

4 

X 

H 

-  4-i 

—  2460 

2.3 

18 

I 

1 1 

+  7-6 

— 1000 

2.3 

5 

a 

15 

-  4-i 

4-  300 

2.3 

19 

0 

13 

+  7-6 

-1490 

3 

6 

r 

g 

-  0.4 

+  5° 

3 

20 

P 

6.7 

4-  8.8 

-1845 

2 

7 

b 

IS 

-  0.3 

—  830 

3 

21 

7T 

13 

+  9-° 

-1430 

3 

8 

a 

6.7 

0.0 

0 

22 

<T 

13 

+  9.0 

—  3180 

3 

9 

$ 

!3 

+  0.1 

-  25 

3 

23 

T 

13 

4- 1 1.7 

-3340 

3 

IO 

V 

13 

+  1.8 

—  360 

3 

24 

V 

11 

4- 1 1.9 

-  45o 

£ 

ii 

13 

+  2-9 

-  535 

3 

25 

\ 

12 

4-14.4 

+  54° 

2.3 

12 

13 

+  4-3 

— 1510 

3 

26 

V 

!3 

4-21.5 

— 2400 

2-3 

13 

r3 

+  6.6 

-  "5 

3 

27 

<P 

13 

+22.8 

—2970 

2.3 

H 

14 

4-  7-° 

4-1230 

3 

Fig.  3,  PI.  II.  V.  30 ;  C  Orionis ;  R  A  5h  27m  ;NPD  94°  57'. 

(19)  Although  I  have  not  succeeded  in  tracing  any  nebulous  connexion  between  this  nebula 
and  the  great  one  about  6  Orionis,  yet  as  their  distance  is  not  much  more  than  half  a  degree,  it 
not  improbably  forms  part  of  one  great  nebulous  system  extending  southwards  through  and 
beyond  that  nebula  as  far  as  t  Orionis  up  to  which  star  a  pretty  conspicuous  branch  of  the  great 
nebula  runs.  More  powerful  telescopes  than  mine  must  decide  this  point.  Meanwhile,  as  this 
nebula  has  never  before  been  figured,  and  offers  much  that  is  remarkable  in  its  form  and  relation 
to  the  involved  stars,  I  have  bestowed  some  care  in  getting  at  least  a  tolerably  correct  repre- 
sentation of  it.  My  figure  is  constructed  from  two  drawings  made  on  the  5th  of  November, 
1834,  and  the  29th  January,  1835,  and  from  a  series  of  equatorial  differences  of  R  A  and 
N  P  D  of  the  principal  stars  involved  in  it  (those  of  Class  1,  in  the  accompanying  Catalogue) 


*  A  mistake  of  importance,  as  it  enlarges  the  apparent  scale  of  his  figure  in  the  direction  of  the  meridian,  has 
been  committed  by  Mr.  Mason's  engraver.  The  parallels  of  declination  in  both  the  figures  of  this  nebula  which 
are  marked  22°  45',  ought  to  have  been  marked  22°  50'.  The  places  of  his  stars  being  determined  by  numerous 
and  elaborate  micrometrical  measures,  are  no  doubt  more  correct  than  mine. 


L2 


OBSERVATIONS  OF 


obtained  on  the  7th  and  9tli  January,  1835,  which,  though  less  numerous  than  might  have 
been  desired,  have  afforded  a  sufficient  basis  of  reference  for  laying  down  the  others  from  the 
means  of  readings  taken  on  both  the  eye-drafts  which  agree  sufficiently  well  with  each  other 
to  claim  for  the  stars  marked  as  of  class  2,  a  degree  of  exactness  not  inferior  to  what  would 
have  been  afforded  by  direct  measures  with  the  position  micrometer. 


CATALOGUE  OF  THE  STARS  LAID  DOWN  IN  THE  DRAWING  OF  V.  30. 


No. 

Letter. 

Mag. 

X 

ARA 
from  a. 

Sec.  Dec. 

y 

ANPD 
from  a. 

Parts. 

Class. 

No. 

Letter. 

Mag. 

X 

ARA 
from  a. 

Sec.  Dec. 

y 

ANPD 
from  a. 
Parts. 

Class. 

i 

i 

IO 

-28.8 

-io5S 

2 

14 

12 

—  0.2 

+  725 

2 

? 

13 

-19.5 

-  842 

2 

15 

a 

6 

0.0 

0 

3 

P 

14 

-19-3 

-  238 

16 

0 

J3 

+  1.9 

-  75* 

2 

4 

y 

8 

-18.8 

— 1560 

1 

17 

T 

»+ 

+  2.8 

-  818 

2 

5 

X 

12 

— 17.6 

-1735 

2 

18 

V 

H 

+  4-6 

—  1308 

2 

6 

9 

10 

-  9.8 

+  359 

1 

r9 

V 

12 

+  6.0 

4-1305 

2 

7 

K 

1 1 

-  9.0 

—  1265 

2 

20 

f 

10 

+  8.4 

+  969 

1 

8 

n 

IO 

-  7-7 

—2198 

2 

21 

\ 

15 

+  8.6 

—  1702 

2 

9 

I 

IO 

-  7-2 

-2295 

2 

22 

s 

9 

+  10.5 

-  65 

1,2 

IO 

a 

16 

-  6.3 

—  1050 

2 

23 

7 

+  16.8 

+  244 

1 

1 1 

b 

16 

-  5-i 

— 1210 

2 

24 

X 

'5 

+  19.0 

—2140 

2 

12 

7T 

13 

-  i-5 

+  i55 

2 

25 

<P 

H 

+  28.8 

+  28 

2 

'3 

(T 

14 

—  1.0 

-1595 

2 

26 

a) 

+40.0 

+  45 

2 

The  stars  7/  and  £  form  the  double  star  2.  746 ;  a  is  identical  with  c1  Orionis  =  A  S  C 
680;  and  /3  with  c2  Orionis  =  V.  154.  Piazzi.  Just  beyond  the  limit  of  the  figure  occurs 
the  star  V.  144  Piazzi,  whose  differences  in  R  A  and  N  P  D  from  a  are  —  59s.  5  and  —  436  Pts. 

Fig.  4,  PI.  II.  30  (Bode)  Doradus,=Lac  449.  Neb.=  J3.  1038=A.  142=h.  2941. 

RA  5k  40m :  N  P  D  159°  IP 

(20)  This  is  one  of  the  most  singular  and  extraordinary  objects  which  the  heavens  present, 
and  derives  no  small  addition  to  its  intrinsic  interest  from  its  situation,  which  is  among  the 
thickest  of  the  nebulae  and  clustering  groups  of  the  greater  Nubecula,  of  whose  total  area  it 
occupies  about  one  five-hundredth  part.  For  these  reasons,  as  well  as  because  ifs  real  nature  has 
been  completely  misunderstood,  and  its  magnified  appearance  so  strangely  misrepresented  in  the 
only  figure  which  I  am  aware  to  have  been  made  of  it  as  to  convey  an  entirely  erroneous  impression 
both  of  its  form  and  structure ;  I  have  taken  great  pains  to  give  as  nearly  as  possible  a  perfect 
representation  of  it  as  it  appeared  in  the  twenty  feet  reflector  on  a  great  many  occasions,  but  more 
especially  on  the  29th  November,  1834,  when  a  "  very  careful  drawing"  was  made  of  it  by  the 
eye  alone,  unaided  by  any  micrometrical  measures;  and  on  the  21st  and  22nd  December,  1835, 
when  the  nebula  was  worked  in  from  the  telescope  on  a  "  skeleton"  previously  prepared  by  an 
approximate  reduction  of  the  micrometrical  measures  of  its  principal  stars,  forming  a  chart,  with  a 
system  of  triangles,  for  its  reception  and  for  that  of  minute  stars  not  susceptible  of  micrometric 
measurement,  or  not  considered  as  of  sufficient  importance  to  be  so  measured.  This  is  the 
only  mode  in  which  correct  monographs  can  be  executed  of  nebulae  of  this  kind  which  consist 
of  complicated  windings  and  ill-defined  members  obliterated  by  the  smallest  illumination  of 


NEBULAE  AND  CLUSTERS  OF  STARS. 


the  field  of  view ;  and  in  which  the  small  stars,  when  very  numerous,  can  be  mapped  down 
with  tolerable  precision. 

(21)  The  following  catalogue  contains  all  the  stars  which  I  have  been  able  distinctly 
to  perceive  within  the  area  occupied  by  the  nebula  and  nearly  adjacent  to  it.    Owing  to  the 

CATALOGUE  OF  THE  STARS  LAID   DOWN  IN  THE  MONOGRAPH   OF  THE  NEBULA 

h.  2941  =  30  (BODE)  DORADUS,  &c. 


No. 

T.ptter 

Mag. 

Co  *rd 

1 1  UIll    ti  111 

pQT3.ll. 

Sec.  Dec. 

y 

1  1  1  •  11 1  ([  1X1 

Sec.  Dec. 

Class. 

No. 

inciter. 

Mag. 

Co-ord. 

fr(im    «  ir» 
11  lllll   (f  Ill 

parall. 
Sgc.  Dec. 

y 

Co-ord. 

Trmvi  ft  ill 

1 1  Dill   11  111 

&CC.  Dec. 

Class. 

I 

'3 

 582.0 

260  0 

2 

54 

12 

19.3 

39  5- 1 

2 

2 

J4 

—  -767  0 

— 209.0 

3 

C  c 

J3 

—  16.0 

-4-  1 1 1  c 

1 

j 

— 161. c 

3 

c6 

14 

—   I  I.J. 

■ — 284..  A. 

2 

A. 

—  i.<;8.0- 

—  I85.O: 

3 

C7 

17 

—  IO.  1 

j 

  l86.2 

3 

c 

j 

15 

—  "3  C  C  C 

-4-  \ii  1 
— 1  JJ-i 

3 

c8 

13 

—  08 

—     6  Q 

2 

6 

14 

—  -3  C  7.0 
j)  j 

-4-  61.7 

3 

CO 

14 

y-+ 

—  266.7 

3 

7 

14 

—  -3AC.O 

-4- 101.2 

1 

i). , 

7 
s 

10. 11 

—  6.7 

—    C2. 1 

1 

8 

it 

T 

— 148 .0: 

3 

61 

12 

4.-6 

—  68.9 

2 

o 

x4 

—  •!  ■?  T.O 

+  264.0 

3 

62 

14 

—  2.8 

—  1 1 0  6 

2.3 

JO 

14 

—  326.8 

3 

16 

—  6.0 

2 

1 1 

325*°: 

3 

61 
°4 

15 

0.7 

+  '3-5 

2 

12 

V 
A 

12 

—  298. 1 

+  284.O 

2 

6c 

13 

—    0  c 

—  22.0 

2 

I  "2 

I 

11 

  92.8 

1 

66 

a 

9 

0.0 

0.0 

1 

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14 


OBSERVATIONS  OF 


convergence  of  the  meridians  so  near  the  pole,  they  are  laid  down  in  the  figure,  and  entered 
in  the  catalogue,  not  according  to  differences  of  R  A  and  polar  distance  expressed  as  usual  in 
time  and  in  parts  of  the  equatorial  micrometer  —  but  according  to  the  values  x  and  y  of 
rectangular  co-ordinates  measured  on  the  parallel  and  meridian  passing  through  the  central 
star,  and  both  expressed  in  seconds  of  absolute  angular  measure. 

(22)  The  first  class  of  stars  in  this  catalogue  comprises  those  which  have  been 
determined  by  the  combination  of  direct  measures  of  differences  of  R  A  and  N  P  D  taken 
with  the  equatorial  with  angular  measures  of  position  taken  with  the  20  feet  micrometer,  or 
by  such  only  of  the  latter  description  of  measures  as  I  consider  on  the  whole,  from  their 
number  and  satisfactory  coincidence  of  their  results,  equal  in  weight  to  such  direct  deter- 
minations. The  second  class  contains  stars  determined  by  the  projection  of  angles  of  position 
only  but  less  numerous  and  accurate  than  those  of  class  1,  or  in  which  angles  of  position 
not  alone  sufficient  for  determining  the  co-ordinates  have  been  combined  either  with  observed 
differences  of  II  A,  or  with  distances  obtained  from  configurations  with  stars  of  class  1, 
capable  of  affording  a  considerable  degree  of  exactness.  Class  3,  contains  stars  inserted  on 
the  "  skeleton"  by  the  eye,  and  whose  co-ordinates  therefore  will  be  more  or  less  exact 
according  to  their  situation,  whether  favourable  or  unfavourable  for  good  configurations. 
Some  of  these  which,  owing  either  to  the  employment  of  a  measured  angle  or  to  some  other 
favourable  circumstance,  appear  to  claim  a  higher  degree  of  confidence,  are  indicated  by  2.3 
in  the  column  of  classes. 

(23)  The  stars  thus  scattered  over  the  area  occupied  by  this  nebula  may  or  may  not  be 
systematically  connected  with  it,  either  as  an  individual  object,  or  as  part  of  the  vast  and 
complex  system  which  constitutes  the  Nubecula.  In  respect  of  their  arrangement  there  is 
nothing  to  distinguish  them  from  those  which  occupy  the  rest  of  the  area  covered  by  the 
nubecula,  in  which  every  variety  of  condensation  and  mode  of  distribution  is  to  be  met  with. 
The  nebula  itself  (as  seen  in  the  20  feet  reflector)  is  of  the  milky  or  irresolvable  kind — quite 
as  free  from  any  mottling  or  incipient  stellar  appearance  as  any  other  nebula  which  I  can 
remember  to  have  examined  with  that  instrument.  Its  situation  in  the  Nubecula  is 
immediately  adjacent  to  two  large  and  rich  clusters  (h.  2922.  and  h.  2931.).  Mr.  Dunlop 
remarks  that  "  the  30  Doradus  is  surrounded  by  a  number  of  nebulse  of  considerable 
magnitudes,  9  or  10  in  number,  with  the  30  Doradus  in  the  centre,"  of  which  nebula?  he  gives 
a  figured  representation.  For  what  objects  these  can  be  intended  I  am  quite  at  a  loss  to 
conjecture,  unless  they  be  the  brighter  portions  of  the  nebulous  convolutions  seen  without 
their  connecting  embranchments.  But  with  this  supposition  their  relative  situations,  inten- 
sities, and  magnitudes  in  the  figure  alluded  to,  so  far  as  I  am  able  to  judge,  appear 
irreconcilable. 

Fig.  1,  Plate  I.  Messier.  8  =  h.  3722 ;  It  A.  17h  53m  27s ;  N  P  D.  114°  21'  16". 

(24)  This  fine  and  complicated  nebula  is,  as  already  remarked,  a  near  neighbour  of 
H.  IV.  41,  and  is  also  closely  adjacent  to,  and  partly  intermixed  with,  the  cluster  h.  3725,  which 
follows  the  chief  star  in  the  nebula  (9  Sagittarii)  about  lm  in  R  A,  nearly  on  the  same  parallel. 
It  is  also  preceded  about  4m  of  time  by  a  large  and  loose,  but  very  rich  cluster  (h.  3717)  about 


NEBULAE  AND  CLUSTERS  OF  STARS. 


15 


a  quarter  of  a  degree  to  the  south ;  so  that  its  neighbourhood  is  in  a  high  degree  rich  and 
interesting.  Its  brighter  portion  may  be  described  as  consisting  of  three  pretty  distinct  streaks, 
or  masses  of  nebula  of  a  milky  or  irresolvable  character,  arched  together  at  their  northern 
extremities  so  as  to  form  some  resemblance  to  the  arches  of  an  italic  letter  m  very  obliquely 
written,  and  this  is  the  aspect  under  which  it  strikes  the  eye  on  a  cursory  view.  On  closer 
attention  these  streaks  are  seen  to  be  connected  and  run  into  each  other  below  (or  to  the  south) 
by  branches  and  projections  of  fainter  light,  and  to  form  three  distinct  basins,  insulating  oval 
spaces,  one  entirely,  the  others  comparatively  dark.  Northwards,  a  great  effusion  of  faint 
nebula  runs  out,  insulating  a  larger  and  more  ill-defined  basin  of  great  extent  and  irregular 
form  which  in  some  measure  communicates  with  the  best-defined  and  darker  of  the  three  oval 
spaces  already  spoken  of.  The  preceding  and  brighter  of  the  three  streaks  is  very  remarkably 
distinguished  by  a  vivid  and  abrupt  concentration  of  its  light  to  a  kind  of  elongated  nucleus? 
just  following  a  star  {n,  No.  36  of  the  accompanying  catalogue)  and  so  near  it  that  on  a  careless 
view  it  might  be  regarded  as  having  that  star  for  its  centre  of  condensation.  But  with 
moderate  attention  this  is  seen  not  to  be  the  case.  The  proper  nucleus  is  decidedly  not 
stellar,  and  resembles  much  more  that  of  the  nebula  in  Andromeda  than  any  other  I  can  call  to 
mind  as  a  term  of  comparison.  The  whole  area  occupied  by  this  nebula,  taking  in  all  the 
convolutions  I  have  been  able  to  trace,  is  about  one-fifth  of  a  square  degree. 

(25)  In  delineating  this  object  every  attention  has  been  paid  to  exactness.  As  the  stars 
in  it  are  numerous  and  many  of  them  conspicuous  in  the  equatorial,  the  relative  places  of  these 
were  in  the  first  instance  ascertained  by  between  400  and  500  differential  observations  of  R  A. 
and  NPD  taken  with  that  instrument  on  the  6th,  11th,  12th,  and  15th  of  September  1836, 
and  the  13th  and  26th  of  July  1837.  From  these  measures  skeleton  charts  were  then 
constructed,  and  being  divided  into  convenient  triangles,  the  nebula  was  worked  in  upon  them 
and  the  smaller  stars  inserted  within  the  triangles  on  the  nights  of  September  4th  and  5th,  and 
October  3rd,  1837,  and  on  one  previous  occasion,  about  the  same  time,  but  of  which  the  date  is 
not  specially  recorded.  On  the  6th  September  1836,  also,  a  series  of  angles  of  position  among 
the  principal  stars  were  also  taken  with  the  20  feet  micrometer.  From  the  whole  evidence 
thus  afforded,  and  by  the  collation  of  a  diagram  (not  of  much  value)  made  in  sweep  474,  the 
figure  of  the  nebula  now  presented  to  the  public,  and  the  subjoined  catalogue  of  stars  observed 
in  it  have  been  constructed.  In  all  these  figures  of  nebulae  I  have  held  it  unadvisable  to 
disfigure  the  engraving  with  letters  or  numbers  pointing  out  the  stars.  It  is  easy  for  any  one 
who  may  wish  to  go  into  any  minute  comparison  of  them  with  the  actual  objects  to  take  up 
the  places  of  the  stars  on  tracing  paper,  and  then  by  affixing  to  them  their  proper  references 
by  the  catalogue  to  form  a  skeleton  chart  adapted  for  his  purpose.  I  should  observe  that  in 
this  catalogue  and  figure  only  such  portion  of  the  cluster  VI.  13,  as  is  intermingled  with 
the  nebula  is  included:  neither  has  attention  been  paid  to  the  mapping  down  of  stars  out 
of  the  area  occupied  by  it  or  closely  adjacent. 

The  stars  A,  D,  and  X  of  the  catalogue  are  identified  respectively  with  A  S  C.  2074 
(9  Sagittarii),  A  S  C.  2078,  and  A  S  C.  2067  (7  Sagittarii). 


16 


OBSERVATIONS  OF 


CATALOGUE  OF  THE  STARS  TO  ACCOMPANY  THE  MONOGRAPH  OF  THE  NEBULA  M.  8  =  h.  3722 
RA  OF  THE  STAR  A  (=  9  SAGITTARII)  17'  53    27  .2  NPD  114°  21'  16". 


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I  O  1 

V 

+  51.12 

707 

38 

p 

12 

—  8.76 

-I-  Ifi77 

j 

100 

'3 

+  23.O 

— 1660 

3 

l62 

/* 

1 1 

J_ri  9 
-f-51.0. 

2040 

3 

39 

16 

—  8.1 

—  810 

■> 

10 1 

14 

+  23.6 

—  1245 

3 

163 

J3 

+  52.3. 

4-1390 

3 

40 

r 

12 

-  7-39 

4-  107 

I 

102 

t 

8 

+  23.61 

—2646 

1 

164 

J5 

+  5+7- 

+  1200 

3 

41 

X 

12 

—  6.2. 

+  15 

3 

103 

16 

+  23.8 

+  1980 

3 

l65 

V 

1 1 

+  54-78 

+  I723 

1 

42 

13 

-  5-7- 

4-  300 

3 

104 

14 

+  24.2 

+  2210 

3 

166 

12 

+  56.2 

-I59O 

3 

43 

y 

1 1 

-  5.07 

— 1178 

1 

105 

q 

12 

+  25.2 

— 1030 

3 

I67 

12 

+  56.5. 

—  830 

3 

44 

15 

-  5.0. 

4-2560 

3 

106 

i5 

+  25.8. 

— 2160 

3 

168 

P 

12 

+57.6. 

+  IOIO 

3 

45 

J5 

-  1.6. 

4-2695 

3 

107 

13 

+  26.O5 

+  2098 

2 

I69 

11 

+  61.0 

—  891 

2 

46 

14 

—  1.2. 

4-2520 

3 

108 

16 

+  26.2. 

+ 1900 

3 

I70 

*S 

+61.4 

+  1215 

3 

47 
48 

16 

—  1.1. 

4-2750 

3 

109 

14 

+  835 

3 

171 

12 

+61.8 

+  670 

3 

13 

-  0.9. 

-  130 

3 

no 

+28.0. 

-1765 

3 

172 

w 

12 

+  61.9 

-  459 

1 

49 

A 

13 

-  0.9. 

-  90 

3 

in 

M 

+28.87 

-  53 

1 

173 

J5 

+62.4 

+  1217 

3 

5° 

6 

0 

0 

1 

1 12 

S 

12 

+29.0. 

— 1921 

2 

174 

w' 

J3 

+62.5 

-  439 

3 

5i 

14 

+  0.1. 

+2525 

3 

113 

16 

+29.4. 

+  1715 

3 

*75 

•4 

+63-3- 

+  715 

3 

52 

16 

+  1.1. 

—  1050 

3 

114 

E 

10 

+29-55 

+  1183 

1 

176 

14 

4-65-3- 

-  125 

3 

53 

16 

+  1.4. 

+  1360 

3 

"5 

+  29.6 

+  45° 

3 

177 

U 

1 1 

+66.13 
+69.4 

+  1485 

1 

54 

!5 

+  1.5. 

+  1100 

3 

116 

b 

+  29.9. 

+  J57 

2 

178 

12 

—  73° 

3 

55 
56 

J3 

4-  2.0. 

+  345 

3 

117 

+  30.0. 

— 1600 

3 

179 

13 

4-7°-8 

+  870 

3 

15 

4-  2.1. 

+  59° 

3 

118 

a 

+  3*44 

-  15 

1 

180 

11 

+71.05 

—  1082 

2 

57 

B 

H 

+  3.1. 

+  1280 

3 

119 

d 

+  31.64 

-  135 

2 

181 

15 

+7I-3 

+  160 

3 

58 

7 

+  4-78 

—  722 

1 

120 

V 

+  31.66 

+  !557 

1 

182 

14 

+72.3 

+  5°5 

3 

59 
60 
61 
62 

!3 

+  5.0. 

+  1010 

3 

121 

+  31.8. 

-J335 

3 

183 

14 

+77-1 

+  760 

3 

X 

12 

+  6.0. 

+  46° 

3 

122 

+32.1. 

— 1690 

3 

184 

1 1 

+77-2 

-1315 

3 

15 

4-  6.0. 

—  1050 

3 

123 

+  32.3. 

+  280 

3 

185 

D 

6 

+  77-75 

4-  638 

1 

!3 

+  6.4. 

+  1895 

3 

124 

15 

+  32.4. 

— 1400 

3 

186 

"3 

+81.0 

+  265 

3 

NEBUUE  AND  CLUSTERS  OF  STARS. 


17 


Fig.  2,  PL  I.  h.  3435=  k  Crucis.    R  A,  12h  43m  36%  N  P  D  149°  25'  31"  =  Lac.  1110  (Neb.) 

=  A  301  =  B  4225. 

(26)  Though  set  down  by  Lacaille  as  nebulous,  and  on  that  authority  entered  as  a 
nebula  in  Bode's  Catalogue,  no  nebula  is  perceptible  in  any  part  of  the  extent  of  this  cluster, 
which  though  neither  a  large  nor  a  rich  one,  is  yet  an  extremely  brilliant  and  beautiful  object 
when  viewed  through  an  instrument  of  sufficient  aperture  to  show  distinctly  the  very  different 
colours  of  its  constituent  stars,  which  give  it  the  effect  of  a  superb  piece  of  fancy  jewellery. 
Tbe  area  occupied  by  it  is  about  one-forty-eighth  part  of  a  square  degree,  within  which  area  I 
have  laid  down,  partly  from  micrometric  measurements  (as  regards  the  large  stars)  and  partly 
from  intertriangulation  by  the  eye  (as  respects  the  small  ones),  the  stars  (110  in  number)  of  the 
following  catalogue. 


CATALOGUE   OF  THE   STARS   LAID   DOWN   IN  THE  CLUSTER  h.  3435   ABOUT  k  CRUCIS. 


No. 

Letter. 

Mag. 

X 

ARA 
from  a  in 
time. 

Sec.  Dec. 

y 

ANPD 
from  a  in 
Mic.  Pts. 
Parts. 

Class. 

No. 

Letter. 

X 

ARA 
from  a  in 
time. 
Sec.  Dec. 

y 

ANPD 
from  a  in 
Mic.  Pts. 
Parts. 

Class. 

No. 

Letter. 

CS 

X 

ARA 
from  a  in 
time. 
Sec.  Dec. 

y 

ANPD 
from  a  in 
Mic.  Pts. 
Parts. 

Class. 

i 

7T 

10 

-27.5 

-  695: 

2: 

38 

1 1 

4-  7-6 

—  421 

3 

75 

V2 

1 1 

4-24.4 

-  653 

2 

2 

12 

-19.1 

—  840 

3 

39 

14 

4-  8.6 

-  643 

3 

76 

1 

10 

+  24.7 

4-  282 

1 

3 

14 

—  14.2 

-  595 

3 

40 

14 

4-  9.2 

-  646 

3 

77 

I 

9 

+  24.8 

-  56 

1 

4 

12 

-14. 1 

-  468 

3 

41 

13 

+  9-6 

-  734 

3 

78 

12 

4-25.1 

-  558 

3 

5 

15 

— 13.2 

-  35i 

3 

42 

14 

4-10.6 

-  735 

3 

79 

14 

4-25-7 

—  800 

3 

6 

IS 

—  12.3 

— 1002 

3 

43 

11 

+  11.0 

— 1211 

3 

80 

f3 

7 

4-26.3 

-  718 

1 

7 

12 

—  12. 1 

-  695 

3 

44 

14 

4- 1 1.2 

-1168 

3 

81 

14 

4-26.5 

—  283 

3 

8 

13 

-  8.6 

— 1130 

3 

45 

16 

4-12.2 

-  327 

3 

82 

0 

10 

4-26.7 

-  874 

2 

9 

15 

-  8.5 

-  958 

3 

46 

a 

11 

4-12.3 

-  334 

2 

83 

'4 

4-26.8 

-  797 

3 

10 

14 

-  6-3 

—  73o 

3 

47 

H 

4-12.5 

-  384 

3 

84 

13 

+  27.0 

— 1060 

3 

ii 

K 

10 

-  6.0 

—  1468 

2: 

48 

11 

4-13.2 

— 1014 

1 

85 

13 

+  27.6 

-  357 

3 

12 

13 

—  47 

—  1 100 

3 

49 

15 

+  13-4 

-  463 

3 

86 

16 

4-27.8 

+  i°4 

3 

r3 

15 

-  4.0 

—  265 

3 

5° 

15 

+  J3-9 

-  493 

3 

87 

14 

4-27.8 

—  1073 

3 

14 

14 

-  4° 

—  910 

3 

5i 

14 

+  14.2 

-  237 

3 

88 

13 

4-27.9 

+  78 

3 

15 

-  3.2 

—  260 

3 

52 

8 

8 

+  15.2 

-  43° 

1 

89 

15 

4-28.0 

-  431 

3 

16 

13 

-  2.3 

—  620 

3 

53 

!3 

+  15-4 

-  85 

3 

90 

12 

4-28.6 

—  949 

3 

17 

11 

-  1-5 

-  879 

1 

54 

14 

+  I5-9 

-  7% 

3 

91 

J4 

+  28.6 

—  416 

3 

18 

13 

—  1.1 

-  490 

3 

55 

14 

+  16.0 

-  49° 

3 

92 

12 

4-29.0 

-  575 

3 

*9 

15 

—  0.2 

-1043 

3 

56 

<t> 

10 

+  16.3 

-  374 

1 

93 

1 1 

+  29.4 

-  656 

3 

20 

a 

7 

0 

0 

1 

57 

!3 

4-16.3 

+  5 

3 

94 

11 

4-29.6 

-  452 

3 

21 

!3 

+  0.4 

4-  211 

3 

58 

12 

4-16.7 

—  7i7 

3 

95 

1 1 

4-30.2 

—  726 

3 

22 

*5 

4-  0.6 

-  854 

3 

59 

0 

1 1 

4-16.7 

—  1003 

2 

96 

14 

+  30.4 

—  926 

3 

23 

13 

+  0.8 

—  IOIO 

3 

60 

14 

+  17.8 

-  942 

3 

97 

13 

4-32.9 

-  484 

3 

24 

12 

4-  2.6 

4-  105 

3 

61 

13 

4-17-9 

-  724 

3 

98 

13 

+  33-7 

—  426 

3 

25 

1 1 

+  2.7 

-  448 

3 

62 

15 

4-18.0 

-  458 

3 

99 

15 

+  34-5 

—  726 

3 

26 

1 1 

+  2.8 

—  662 

3 

63 

£ 

9 

+  18.9 

-  3»3 

1 

100 

P 

10 

4-34-7 

-1313 

1 

27 

V 

I  I 

+  3-° 

-  813 

1 

64 

a 

*3 

+  19.0 

-  39° 

3 

101 

X 

12 

+  35-9 

—  925 

2 

28 

14 

+  3-i 

— 1300 

3 

65 

r3 

+  19-5 

—  74° 

3 

102 

1 

7.8 

4-36.9 

—  106 

1 

29 

13 

+  3-3 

—  208 

3 

66 

13 

4-20.5 

—  284 

3 

103 

16 

+  37-3 

—  720 

3 

30 

15 

+  3-6 

—  610 

3 

67 

15 

4-21.2 

-1037 

3 

104 

16 

4-38-7 

-1 143 

3 

31 

12 

+  3-7 

4-  140 

3 

68 

14 

4-21.4 

-1093 

3 

105 

15 

4-40.1 

—  1 121 

3 

32 

I  I 

+  3-8 

-  566 

3 

69 

13 

+21.4 

-  325 

3 

106 

15 

4-42.0 

—  1 165 

3 

33 

12 

+  3-9 

—  276 

3 

70 

1 1 

4-21.7 

-  675 

3 

107 

a 

12 

4-43-8 

-  9°3 

2 

34 

14 

+  4-° 

—  79° 

3 

7i 

15 

4-22.7 

-  366 

3 

108 

12 

4-46.0 

-  583 

3 

35 

15 

+  4-4 

— 1200 

3 

72 

*i 

9 

4-23.8 

—  1 121 

1 

109 

14 

+47-3 

-  648 

3 

36 

14 

+  4-7 

-  712 

3 

73 

vl 

1 1 

4-24.0 

-  644 

2 

1 10 

T 

1 1 

+  5J-5 

-  585 

2 

37 

14 

4-  4-8 

-  366 

3 

74 

12 

4-24.4 

—  22 

3 

F 


IS 


OBSERVATIONS  OF 


(27)  Colour  is  conspicuous  in  the  following  stars  of  the  above  catalogue: — 

a  Greenish-white.  o  Green.  Blue-green. 

/3  Greenish-white.  e  Bed.  a  Ruddy. 

y  Greenish-white.  (  Green. 

The  stars  of  Class  1,  have  been  determined  by  equatorial  differences  of  E  A  and  NPD. 
Those  of  Class  2,  by  angular  measures  or  good  allineations  combined  with  an  observed 
difference  of  R  A  and  those  of  Class  3,  on  a  simple  reading  off  of  the  places  as  inserted  by  the 
eye  within  the  triangle  of  a  prepared  skeleton.  The  A  N  P  D  of  the  star  IT.  (No.  1) 
may  be  8  or  10"  in  error,  owing  to  a  probable  mistake  in  reading,  in  one  of  the  equatorial 
measures  of  position. 

Plate  III.  figs.  1,  2,  3,  4,  5,  6. 

(28)  The  six  figures  on  this  plate  are  all  delineated  on  a  uniform  scale,  the  area 
included  in  each  being  9' 30"  in  the  vertical  direction  or  that  of  the  meridian,  and  11'  in 
that  of  the  parallel,  or  about  one-fiftieth  of  a  square  degree.  The  first  of  them  (fig.  1,) 
represents  Lacaille's  nebula  47  Toucani  of  Bode's  Catalogue,  or  No.  2322  in  mine,  resolved 
into  stars  as  described  in  the  observations  above  recorded,  and  as  seen  on  a  great  many 
other  occasions.  The  contrast  between  the  rose-coloured  light  of  the  interior  and  the  white 
of  the  exterior  portions  cannot,  of  course,  be  represented  in  an  engraving,  but  of  the  pheno- 
menon itself,  I  have  no  doubt.  The  double  star  on  the  south  preceding  edge  of  the  more 
condensed  portion  has  jn'obably  no  connexion  with  the  cluster. 

(29)  The  law  of  condensation  of  this  cluster  is 
remarkable.  Three  distinct  stages  or  steps  of  degra- 
dation are  noticeable ;  the  density  at  any  point  of  the 
diameter  being  proportional  to  the  ordinate  of  a 
curve  whose  form  is  that  of  the  annexed  figure,  in 
which  the  diameter  of  the  central  elevated  portion 
corresponds  to  13s.5  of  right  ascension.  Its  figure  is 
round,  and  not  elliptic, — (at  least  not  so  elliptic)  as  described  and  figured  by  Mr.  Dunlop. 
I  will  not  take  upon  myself  to  say  that  the  extreme  outlying  stars  which  extend  to  10'  or 
12'  on  all  sides  from  the  centre  may  not  show  some  tendency  to  elongation  in  one  direction 
rather  than  another ;  but  as  regards  all  its  interior  portion,  on  the  very  frequent  occasions 
on  which  I  have  viewed  it  myself  and  shown  it  to  others,  I  have  always  considered  its 
appropriate  designation  to  be  a  (/lobular  cluster,  nor  has  any  remark  to  the  contrary  made 
by  those  who  have  examined  it  in  my  presence  led  me  to  regard  this  character  as  doubtful. 
I  am  more  particular  than  I  otherwise  should  be  in  noticing  this  discrepancy,  because  all 
my  experience  has  led  me  to  conclude  that  the  globular  form  is  much  more  generally 
accompanied  with  perfect  resolution  into  stars  than  the  elliptical.  Indeed  I  can  hardly 
call  to  mind  an  instance  of  an  elliptical  nebula  of  any  considerable  size  and  brightness* 


*  The  oval  nebula  M.  1  =  h.  357,  near  I  Tauri,  is  barely  resolvable  in  the  twenty  feet  reflector ;  and 
if  I  am  correctly  informed,  the  three  feet  speculum  of  Lord  Rosse  suffices  for  its  complete  resolution.  The 
great  nebula  of  Andromeda,  however,  as  also  the  first  of  my  Father's  5th  class  (h.  61),  discovered  by  Miss 


NEBULAE  AND  CLUSTERS  OF  STARS. 


19 


which  the  power  of  the  20  feet  reflector  suffices  so  to  resolve ;  while  examples  on  the  other 
side,  of  globular  clusters  perfectly  resolved,  without  any  remaining  suspicion  of  unresolved 
nebulosity  are  innumerable.  Between  these  two  characters  then,  (ellipticity  of  form  and  diffi- 
culty of  resolution)  there  undoubtedly  exists  some  physical  connexion.  Possibly  the  conditions 
of  dynamical  equilibrium  in  a  sphere  may  be  compatible  with  larger  intervals  and  greater 
separate  magnitudes  than  in  an  ellipsoid — a  subject  on  which  more  hereafter.  It  deserves 
also  to  be  noticed  that  in  very  elliptic  nebulse  which  have  a  spherical  centre,  (as  in  M.  65  = 
h.  854)  a  "  resolvable"  or  mottled  character  often  distinguishes  the  central  portion,  while  the 
branches  exhibit  nothing  of  the  kind. 

(30)  The  remaining  five  figures  of  this  plate  represent  fields  of  view  (or  at  least  so 
much  of  the  circular  field  of  15'  in  diameter  as  can  be  included  in  the  rectangular  area 
of  each  figure)  in  the  Nubecula  Major.  They  are  for  the  most  part  eye-drafts  assisted  as 
to  the  proportions  of  the  parts  in  copying  for  the  engraver  by  a  few  measured  angles.  The 
original  drafts  were  made  with  much  care,  not  in  the  course  of  sweeping,  but  in  observations 
devoted  especially  to  that  purpose,  on  the  full  scale,  or  very  nearly  so,  on  which  they  are 
engraved,  in  order  to  illustrate  the  strange  and  anomalous  variety  of  structure  which  subsists 
in  that  system.  In  addition  to  the  descriptions  appended  in  the  catalogue  to  the  observed 
places  of  the  several  nebulse  of  which  these  respective  groups  consist,  there  are  some  other 
particulars  which  require  notice,  as  follow. 

(31)  Fig.  4,  Plate  III. — The  single  observation  of  /  523,  No.  50,  would  appear  to  have 
been  somewhat  hurried  owing  to  the  quick  succession  of  objects,  and  the  stars  referred  to 
as  mixed  with  the  group  may  be  either  the  two  stellar  nuclei  of  the  brighter  nebulas  in  the 
upper  group  taken  for  stars,  or  may  refer  to  the  stars  intermingled  with  those  in  the  lower 
and  the  intermediate  ones.  The  nebulous  mass  which  this  figure  is  principally  intended  to 
represent,  consists  of  at  least  8  nebular  nuclei,  four  of  which  are  much  more  conspicuous 
than  the  others,  and  in  hazy  weather,  or  with  an  inferior  telescopic  power,  appear  as  four 
distinct  nebulas  forming  a  trapezium,  for  which  reason  their  places  as  derived  from  the 
drawing  by  measurement  on  a  scale  have  been  inserted  in  this  catalogue. 

(32)  Fig.  5,  Plate  III. — The  two  brighter  portions  of  the  principal  nebula  (the  "  triple 
nebula"  of  the  descriptions)  have  somewhat  of  a  mottled  or  resolvable  character  which  is 
not  alluded  to  in  the  sweeps — probably  for  want  of  time  for  the  eye  to  grow  accustomed  to 
the  object. 

(33)  Fig.  6,  Plate  III. — The  "  Binuclear  nebula,"  as  it  is  called  in  the  descriptions, 
"  at  the  southern  end  of  an  arc-formed  cluster,"  consists  in  reality  of  four  nuclei,  (one  of 
them  very  faint)  feebly  united  by  very  faint  nebula.  The  fourth  is,  however,  almost 
detached.  The  long  attention  bestowed  on  this  nebula  has  also  led  to  the  detection  of 
another  very  faint  nebula,  (that  which  follows  the  double  star  in  the  lower  part  of  the 
figure)  h.  2810  which  had  been  overlooked  in  all  the  sweeps,  and  is  entered  in  the 
catalogue  on  the  evidence  of  this  figure. 

(34)  Besides  these  more  elaborately   delineated  groups,   three   other  groups  in  the 


C.  Herschel,  by  far  the  most  conspicuous  among  elliptic  nebula?,  have  hitherto,  so  far  as  I  am  aware,  resisted 
every  power  which  has  been  applied  to  them. 


20 


OBSERVATIONS  OF 


Nubecula  Major,  are  also  represented  in  Plate  IV.  Figs.  7,  9,  and  Plate  VI.  Fig.  20, 
from  diagrams  made  in  the  course  of  sweeping  and  without  the  same  pretensions  to 
exactness  which  the  foregoing  possess,  though  tending  to  give  a  very  good  idea  of  the 
objects  they  represent,  as  well  as  further  to  elucidate  the  peculiar  character  of  the 
Nubecula. 

(35)  Plate  IV.  Fig.  1,  h.  2552. — This  curious  object  belongs  to  the  class  of  Annular 
nebula  with  centres,  a  class  consisting  so  far  as  we  at  present  know  of  only  three  individuals, 
viz.  this  and  the  two  extraordinary  objects  M.  51,  and  M.  64,  represented  in  figures  25  and 
27,  of  my  Northern  Catalogue,  between  which  the  nebula  now  under  consideration  holds  a 
kind  of  middle  place.  Although  the  nebulous  ellipse  into  which  the  annulus  is  obliquely 
projected  is  incomplete  at  the  extremities  of  its  longer  axis,  yet  its  general  form  cannot  be 
mistaken.  Tbe  central  mass  is  much  more  concentrated  than  that  of  M.  51,  and 
resembles  more  nearly  that  of  M.  64,  which  latter,  it  is  further  to  be  remarked,  has  for 
its  nucleus  either  a  double  star  or  some  resolvable  group  putting  on  that  appearance, 
while  our  present  object  is  expressly  stated  to  have  a  resolvable  nucleus. 

(36)  Plate  IV.  Fig.  2,  h.  3501  is  a  very  problematic  object,  and  must  be  regarded  at 
present  as  forming  a  genus  apart,  since  it  evidently  differs  from  mere  "  double  nebulae," 
not  only  in  the  singular  relation  of  its  two  halves  to  each  other,  (having  each  a  well  and 
an  ill-defined  side,  their  sharply  terminated  edges  being  turned  towards  each  other  and 
exactly  parallel)  but  also  by  the  intervention  of  the  delicate  nebulous  streak  intermediate 
between  them  and  lying  in  exactly  the  same  general  direction.  It  may  perhaps  be  considered 
that  the  nebulae  V.  24  and  I.  43,  (figs.  37  and  50,  of  my  Northern  Catalogue)  offer  some  analogy 
of  structure  to  this;  but  if  so  it  is  a  very  remote  one,  the  nebulae  constituting  these  objects 
being  in  both  instances  very  unequal  in  size  and  brightness,  and  being  individually  merely 
elongated  nebulae  of  the  ordinary  type,  which  these  are  not.  On  the  other  hand  we  have,  in 
the  completely  resolved  cluster,  Plate  V.  Fig.  5,  an  object  which,  removed  to  such  a  distance 
as  to  appear  nebulous,  would  present  a  considerable  approach  to  it  in  point  of  general 
aspect. 

(37)  Plate  IV.  Figs.  3  and  6,  h.  3239  and  2370,  are  objects  evidently  analogous,  and 
may  be  termed  "  falcated  nebulae,"  the  falcated  form,  however,  being  inueh  less  marked 
in  the  latter  than  the  former,  the  train  forming  a  less  conspicuous  appendage.  Each  has 
a  double  star  (or  a  resolvable  nucleus  putting  on  that  appearance)  in  its  head  or  more 
condensed  part.  It  should  be  observed  that  the  stars  in  fig.  3,  are  put  in  without  any 
attempt  at  individual  delineation.  This  fine  nebula  occurs  in  a  very  rich  part  of  the 
milky  way,  in  that  wonderfully  superb  region  which  ushers  in  the  great  nebula  about  n 
Argus. 

(38)  Plate  IV.  Fig.  4 ;  h.  3075  is  an  object  altogether  unique.  The  resemblance  to  a 
"  bust  or  silhouette  profile,"  though  really  obvious,  is  perhaps  somewhat  exaggerated  (as  all 
such  fancied  resemblances  are  sure  to  be)  though  involuntarily,  in  the  drawing.  It  is 
described  by  my  Father,  as  "  a  broad  extended  nebulosity  forming  a  parallelogram  with  a 
ray  southwards."    He  does  not  make  any  mention  of  the  stars  in  it  (see  his  Catalogue,  V.  21.). 

(39)  Plate  IV.  Fig.  5,  h.  3523.— This  is  Bode's  185  Centauri,  observed  by  Lacaille, 
and  remarked  by  him  as  nebulous.     The  reader  will  not  fail  to  compare  it  with  V.  43, 


NEBULA  AND  CLUSTERS  OF  STARS. 


21 


figured  in  my  Northern  Catalogue  (fig.  55),  to  which  it  bears  a  perfect  analogy.  They  are 
the  two  finest  specimens  of  their  class — that  of  large,  faint,  oval  nebula  with  small,  bright, 
exceedingly  condensed,  oval  nuclei.  And  it  will  not  escape  notice,  on  comparison  of  the  figures, 
that  in  both  cases  the  nucleus  appears  to  contain  within  it  a  still  smaller  round  kernel. 
The  minute  scrutiny  of  these  objects  with  instruments  of  larger  aperture  and  high  magnifying 
powers,  would  be  in  the  highest  degree  interesting  and  instructive.  The  situation  of  185 
Centauri,  is  however  too  low  for  very  satisfactory  observation  in  these  latitudes. 

(40)  Plate  IV.  fig.  7  =  h.  2859,  &c,  fig.  8  =  h.  2315,  and  Plate  V.  fig.  10  =  h.  2359  — 
represent  nebulae  of  irregular  forms  having  a  tendency  to  several  centres  of  condensation; 
in  the  case  of  fig.  7  but  little  conspicuous — in  that  of  fig.  8  (otherwise  remarkable  for  its 
extravagant  length  and  crooked  shape)  much  more  so,  while  in  PI.  V.  fig.  10,  the  formation 
of  separate  nuclei  is  decided,  the  intermediate  faint  nebula  barely  sufficing  to  mark  them  as 
forming  a  connected  system.  We  may  conjecture,  though  to  us  and  probably  to  a  remote 
posterity,  it  can  be  no  more  than  conjecture,  that  such  groups  as  PI.  IV.  fig.  9  =  h.  2923,  &c. 
fig.  10  =  h.  3324,  &c.  and  fig.  11  =  h.  3908,  &c,  may,  in  the  progress  of  indefinite  ages,  have 
resulted  from  a  process  of  internal  segregation  from  nebulae  which  once  occupied  the  whole 
of  their  intermediate  space,  but  which  has  at  length  been  completely  absorbed  from  among 
them,  and  it  is  only  by  placing  on  record,  as  early  and  as  precisely  as  possible,  such  instances 
as  the  above,  that  any  chance,  however  slender,  of  exchanging  conjecture  for  knowledge 
can  be  looked  for.  The  group  IV.  fig.  10,  is  certainly  a  very  remarkable  and  interesting 
one  by  reason  of  the  variety  of  nebulous  forms  it  exhibits  in  so  small  a  compass ;  and  as 
it  occurs  in  a  region  which,  though  rich  in  clusters  of  distinct  stars,  is  nearly  devoid  of 
nebulae  of  any  of  these  particular  forms,  the  probability  of  their  systematic  connexion 
amounts  almost  to  certainty. 

(41)  Where  the  milky  way  crosses  the  18th  hour  of  right  ascension,  and  over  a  great 
many  degrees  of  its  extent  in  polar  distance  in  the  region  occupied  by  the  tail  of  Scorpio 
the  continuity  of  it  is  singularly  broken,  and  many  parts  of  its  borders  are  so  sharply  defined 
as  to  present  a  pretty  distinct  outline  so  as  to  divide  the  field  of  view  into  a  part  with  and 
another  without  milky  way.  In  these  spots  the  component  stars  are  usually  very  small, 
so  as  in  some  cases  to  put  on  the  appearance  of  a  barely  resolvable  nebula.  In  figures 
1,  2,  3,  Plate  V.  characteristic  specimens  of  these  appearances  are  represented  from  rough 
diagrams  made  at  the  time  of  their  occurrence. 

(42)  Plate  V.  fig.  4,  5,  6  =  h.  3641,  3707,  3644,  are  clusters  of  stars  in  which  only  general 
character  is  attempted  to  be  expressed  from  the  sweeping  diagrams.  They  are  of  no  peculiar 
interest  otherwise  than  as  they  may  elucidate  (as  in  the  case  of  fig.  5)  certain  aspects  of  nebulae 
which  may  by  possibility  be  supposed  to  originate  in  such  clusters  more  abundant  in  stars 
and  removed  to  such  a  distance  as  to  appear  nebulous. 

(43)  Plate  V.  fig.  7  =  h.  3504  is  the  noble  globular  cluster  o>  Centauri,  beyond  all 
comparison  the  richest  and  largest  object  of  the  kind  in  the  heavens.  The  stars  are  literally 
innumerable,  and  as  their  total  light  when  received  by  the  naked  eye  affects  it  hardly  more 
than  a  star  of  the  5th  or  5-4th  magnitude,  the  minuteness  of  each  may  be  imagined:  it 
must  however  be  recollected  that  as  the  total  area  over  which  the  stars  are  diffused  is  very 
considerable  (not  less  than  a  quarter  of  a  square  degree),  the  resultant  impression  on  the 
sensorium  is  doubtless  thereby  much  enfeebled,  and  that  the  same  quantity  of  light  concentred 
on  a  single  point  of  the  retina  would  very  probably  exceed  in  effect  a  star  of  the  3rd  magnitude. 

G 


22 


OBSERVATIONS  OF 


On  a  consideration  of  all  the  sweeping  descriptions,  as  well  as  from  a  great  many  occasional 
inspections  of  this  superb  object,  I  incline  to  attribute  the  appearance  of  two  sizes  of  stars 
of  which  mention  is  made  to  little  groups  and  knots  of  stars  of  the  smaller  size  lying  so 
nearly  in  the  same  visual  line  as  to  run  together  by  the  aberrations  of  the  eye  and  telescope ; 
and  not  to  a  real  inequality.*  This  explanation  of  an  appearance  often  noticed  in  the 
descriptions  of  such  clusters,  is  corroborated  in  this  instance  by  the  distribution  of  these 
apparently  larger  stars  in  rings  or  mesh-like  patterns,  chiefly  about  the  centre  where  the 
stars  are  most  crowded.  An  attempt  has  been  made  to  imitate  this  appearance  in  the  drawing, 
but  partly  from  the  difficulty  of  its  execution,  partly  from  defect  of  engraving,  the  plate 
fails  to  convey  a  just  idea  of  it.  Two  such  rings  on  an  oval  crossed  by  a  kind  of  bridge  is 
especially  conspicuous  in  the  central  part. 

(44)  Plate  V.  fig.  9  =  h.  3221,  fig.  11  =  h.  2621.  PI.  VI.  fig.  19  =  h.  2327.— These 
figures  exhibit  elliptic  nebulse  normal  in  their  character  —  that  is  to  say,  in  which,  as  the 
condensation  increases  towards  the  middle,  the  ellipticity  of  the  strata  diminishes,  or  in 
Avliich  the  interior  and  denser  portions  are  obviously  more  nearly  spherical  than  the 
exterior  and  rarer.  A  great  number  of  such  nebula?,  of  every  variety  of  ellipticity  and 
central  condensation  are  figured  in  my  Northern  Catalogue.  Regarding  the  spherical  as 
only  a  particular  case  of  the  elliptic  form,  and  a  stellar  nucleus  as  only  the  extreme  stage 
of  condensation,  at  least  nine-tenths  of  the  whole  nebulous  contents  of  the  heavens  will  be 
found  to  belong  to  this  class — so  that,  as  regards  a  law  and  a  structure,  the  induction  which 
refers  them  as  a  class  to  the  operation  of  similar  causes,  and  assumes  the  prevalence  within 
them  of  similar  dynamical  conditions,  is  most  full  and  satisfactory.  To  abstain  altogether 
from  speculation  as  to  what  may  be  the  nature  of  those  causes  and  conditions,  and  to  refuse 
all  attempts  to  reconcile  the  phenomena  of  so  large  and  so  definite  a  class  of  cosmical 
existences  with  mechanical  laws  taken  in  their  most  general  acceptation,  would  be  to  err  on 
the  side  of  excessive  caution,  and  unphilosophical  timidity.  The  time  is  clearly  arrived  for 
attempting  to  form  some  conception  at  least  of  the  possibility  of  such  a  system  being  either 
held  in  a  state  of  permanent  equilibrium,  or  of  progressing  through  a  series  of  regular  and 
normal  changes,  resulting  either  in  periodical  restorations  of  a  former  state,  or  in  some 
final  consummation. 

(45)  The  remarkable  object  h.  3145,  represented  in  Plate  V.  fig.  12,  is  by  no  means 
referable  to  this  normal  class.  It  is  expressly  described  as  brightest,  not  in  the  middle  of 
its  length,  but  at  one  end.  Neither  is  its  figure  elliptical,  but  broader  at  the  faint  than  at 
the  bright  extremity,  the  bounding  lines  being  nearly  rectilinear.  It  is  a  very  faint  and 
delicate  object,  and  I  regret  not  having  obtained  more  than  one  observation  of  it. 

(46)  Plate  V.  fig.  8  =  h.  3154,  and  VI.  5,  6,  7,  8,  9  =  h.  3248,  3675,  3610,  3594,  3228, 
represent  planetary  nebula;,  a  class  of  especial  interest,  and  of  which,  considering  their  general 
rarity,  the  southern  heavens  have  afforded  a  rather  unexpectedly  large  harvest.  Those  only 
are  here  delineated  which  have  either  accompanying  stars,  or  which  are  distinguished  by 
some  peculiarity,  as  PI.  VI.  fig.  5  =  h.  3248,  which  has  a  slight  chevelure  or  nebulous  haze 
exterior  to  its  large  oval  disc;  VI.  fig.  9  =  h.  3228,  which  has  a  star  or  a  small  disc  near  its 

*  The  perfect  roundness  of  the  disc  of  y  Virginis  under  a  magnifying  power  too  low  for  its  resolution,  noticed 
both  by  Captain  Smyth  and  myself  (see  the  details  further  on),  affords  an  excellent  illustration  of  this  expla- 
nation. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


23 


centre;  or  V.  fig.  8  =  h.  3154,  situated  in  the  midst  of  a  cluster  of  stars,  with  which  it 
contrasts  singularly,  and  with  which,  if  it  have  no  connexion,  it  is  strange  that  the  very 
same  combination  should  be  fortuitously  repeated,  in  the  case  of  M.  46  + H.  IV.  39  (not  here 
figured),  and  a  near  approach  to  it  in  h.  3100,  h.  3101,  observed  in  sweep  771,  as  in  the  field 
with  a  cluster  of  the  7th  class. 

(47)  A  most  remarkable  peculiarity  of  the  planetary  nebula,  PI.  VI.  fig.  5  =  h.  3248, 
but  which  cannot  be  represented  in  an  engraving,  is  its  very  decided  though  pale  blue 
colour,  which  is  noticed  in  three  out  of  the  four  observations  recorded  in  the  sweeps.  This 
and  the  beautiful  planetary  nebula  h.  3365,  in  which  the  blue  colour  is  much  more  striking 
and  intense,  are  the  only  objects  of  that  colour  in  the  heavens  so  situated  as  to  admit  of 
no  suspicion  of  contrast  with  a  red  star  influencing  the  eye.  It  is  true  that  in  the  latter 
instance  a  considerably  bright  red  star  is  near,  and  may  be  brought  into  the  same  field  of 
view,  —  and  that  its  presence  greatly  enhances  the  tint  of  the  nebula.  But  the  star  is 
remote  enough  to  be  easily  excluded,  and  the  nebula  does  not  cease  thereby  to  apjjear  of  a 
fine  blue  colour. 

(48)  Plate  VI.  fig.  10  =  h.  3548,  and  fig.  11  =  h.  2775,  are  nebulae,  centrally  involving 
double  stars.  Central  superposition  must  undoubtedly  be  held  strong  presumptive 
evidence  of  physical  connexion.  The  nucleus  of  M.  64  is  strongly  suspected  to  be  a  close 
double  star.  In  fig.  30  of  my  Northern  Catalogue  is  represented  a  very  remarkable 
example,  h.  2002,  of  this  combination  of  a  double  star  with  an  oval  nebula — the  direction 
of  the  two  stars  of  the  double  star  being  also  that  of  elongation  of  the  nebula.  Struve  in 
his  Dorpat  Catalogue,  No.  2332,  has  adduced  a  similar  example.  The  nebula  h.  2858,  R  A, 
5h  26m,  N  P  D  156°  44'  is  again  another  case  in  point,  as  would  also  h.  3122,  R  A,  8h  14m 
N  P  D  125°  41',  were  it  quite  certain  that  one  of  the  stars  is  anything  more  than  the  nucleus 
of  an  ordinary  nebula  which  has  upon  it  an  accidental  star.  No  such  supposition  applies  to 
h.  3548,  in  which  both  the  stars  are  sharply  defined,  and  of  the  10th  magnitude,  and 
have  been  repeatedly  made  the  subjects  of  micrometrical  measurement. 

(49)  Plate  VI.  fig.  12  =  h.  3131,  must  be  considered  as  adding  another  to  the  list  (a 
very  sparing  one)  of  "  nebulous  stars,"  as,  although  the  coma  is  not  perfectly  round,  the 
situation  of  the  star  is  precisely  at  the  general  centre  or  point  of  greatest  concentration. 
There  can  hardly  be  a  doubt,  we  may  presume,  that  objects  of  this  class  are  in  no  way  to 
be  regarded  as  of  an  exceptional  or  abnormal  character — but  simply  as  cases  where  the 
general  law  of  central  condensation  is  pushed  to  its  extreme,  i.  e.  up  to  a  nuclear  disc  of 
imperceptible  dimensions — in  other  words,  a  star. 

(50)  Plate  VI.  fig.  13  =  h.  3661,  fig.  14  =  h.  2487,  fig.  15  =  h.  3541,  and  V.  11  =  h.  2621. 
— The  frequent  association  of  nebulae  in  pairs  forming  "  double  nebulae,"  has  been 
dwelt  on  in  the  remarks  on  figures  68  ...  .  79,  appended  to  my  Northern  Catalogue,  and 
need  not  here  be  again  insisted  on.  Among  the  specimens  here  figured,  M.  62  (h.  3661) 
is  interesting  both  from  its  being  evidently  a  double  globular  cluster,  and  by  reason  of  the 
comparative  feebleness  of  the  condensation  about  the  southern  centre  and  the  small  interval 
(compared  with  the  total  diameter  of  the  object)  which  separates  them. — h.  3541  is  only 
remarkable  as  being  the  smallest  object  of  this  kind  which  has  yet  been  observed,  and 
this  figure  as  well  as  the  next  (fig.  16)  are  rather  intended  as  guides  to  the  eye  of  any  future 
observer  who  may  direct  a  telescope  on  this  and  the  very  minute  single  nebula  h.  3727, 


24 


OBSERVATIONS  OF 


than  to  express  any  peculiarities  in  the  ohjeets. — h.  2621  may  be  compared  with  h.  1397 
which  is  represented  in  fig.  76,  of  my  Northern  Catalogue,  and  which  it  very  strongly 
resembles.  These  combinations  will  not  fail  to  suggest  the  conception  of  a  globular  cluster 
revolving  round  a  very  oblate  spheroidal  one  in  the  plane  of  its  equator,  and  in  an  orbit 
which,  if  circular,  and  seen  obliquely,  like  the  central  nebula  itself,  would  have  a  diameter 
somewhat  more  than  four  times  that  of  the  latter — a  stupendous  system  doubtless,  but  of 
which  the  reality  can  hardly  be  considered  improbable. 

(51)  Plate  VI.  figs.  17,  18  =  h.  2535,  RA3h  16m  58s  and  h.  3688,  R  A  17h  22m  43s  repre- 
sent "  cometic  nebulae"  attached  to  stars.  Four  such  objects  are  represented  in  figs.  64,  65, 
66,  67  of  my  Northern  Catalogue. 

(52)  Plate  VI.  fig.  1  =  h.  3514,  and  fig.  2  =  h.  3241. —The  first  figure  in  this  plate 
represents  an  object  of  a  very  singular  nature  —  it  is  an  oval  nebula  pretty  well  defined, 
though  faint,  and  deviating  widely  from  the  normal  characters  of  such  nebula?,  so  as  to 
approach  in  some  degree  to  the  structure  of  M.  27,  as  figured  in  fig.  26  of  my  Northern 
Catalogue.  It  is  true  that  the  disposition  of  the  bright  axis  is  not  nearly  so  symmetrical, 
nor  are  its  two  terminal  masses  so  conspicuous  in  proportion  to  the  whole  size  of  the  object 
— nor  indeed  is  the  axis  straight.  A  general  similitude  however  exists  sufficient  to  warrant 
their  being  provisionally  classed  together,  and  our  class  so  extended  may  also  take  in  the 
small  but  interesting  nebula  fig.  2  =  h.  3241,  where  however  the  axis  is  wanting  to  connect 
the  terminal  masses,  so  that  possibly  this  object  may  be  nothing  else  than  a  very  close  double 
nebula,  whose  individuals  are  small  and  much  compressed.  For  another  analogous  structure 
confer  Dr.  Lamont's  thesis  of  August  25,  1837.    Fig.  IV. 

(53)  Plate  VI.  figs.  3,  4  =  h.  3680  and  3686.— These  are  Annular  Nebula,  of  which 
(not  to  speak  at  present  of  the  very  large  faint  object  V.  19)  we  have  already  two  examples 
in  the  northern  hemisphere,  M.  57  (the  annular  nebula  between  /3  and  y  Lyra)  and  IV.  13 — 
represented  in  figures  29  and  48  of  my  Northern  Catalogue.  It  is  not  impossible  that  the 
real  constitution  of  these  bodies  may  be  that  of  hollow  spherical  or  elliptical  shells,  of  which 
the  borders  appear  brighter  than  the  interior,  by  reason  of  the  greater  thickness  of  the 
luminous  matter,  or  starry  stratum,  traversed  by  the  visual  ray.  Certain  it  is  that  the  interior 
of  M.  57  is  very  far  from  totally  dark,  and  that  so  much  light  exists  within  the  annuli  of 
IV.  11  and  IV.  13,  that  they  are  set  down  by  my  Father  as  planetary  nebulae,  and  the 
latter  is  even  described  by  him  as  "  of  equal  light."  The  delicate  and  beautiful  annulus 
h.  3680,  appears  indeed  to  be  devoid  of  any  interior  illumination — but  the  object  is  so  faint 
that  a  nebulosity  filling  in  the  centre,  and  bearing  no  greater  proportion  in  respect  of  density 
to  the  ring  than  in  the  case  of  M.  57,  could  not  have  been  perceived.  The  tenuity  of  the 
ring,  as  well  as  the  feebleness  of  central  illumination,  will  of  course  in  our  hypothesis  be 
proportioned  to  the  thinness  of  the  shell,  and  the  law  of  degradation  of  its  light  will  be 
determined  by  the  ratio  of  the  radii  of  its  inner  and  outer  surfaces,  as  well  as  by  the  law  of 
density  of  the  strata  of  which  it  consists.  IV.  11  and  IV.  13,  would  therefore  seem  to  have 
the  central  hollow  smaller  in  proportion  than  either  of  the  other  two. — V.  19  is  probably 
not  a  hollow  shell,  but  a  real  annulus,  whose  actual  dimensions  must  be  indeed  enormous, 
being  described  by  my  Father  as  more  than  a  quarter  of  a  degree  in  length,  which,  supposing 
it  only  as  remote  as  61  Cygni,  would  correspond  to  a  real  diameter  1300  times  exceeding 
that  of  the  earth's  orbit. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


25 


Of  the  Great  Nebula  in  the  Sword-handle  of  Orion. 

(54)  It  may  easily  be  supposed  that  in  a  situation  so  favourable  for  viewing  this 
magnificent  object  as  the  Cape,  where  it  passes  the  meridian  at  an  altitude  of  60°,  with  the 
additional  advantages  of  a  sky  of  perfect  purity,  and  of  mirrors  in  a  constant  course  of 
repolishing,  I  should  eagerly  seize  the  opportunity  to  re-examine  my  earlier  delineation  of  it, 
with  a  view  to  the  detection  of  change,  the  correction  of  error,  and  the  observation  of  further 
particulars  as  to  its  form,  extent,  and  structure  which  had  escaped  previous  observation. 
Altbough  considerable  pains  had  been  taken  with  my  figure  of  1825  (engraved  in  the  2nd  vol. 
of  the  Memoirs  of  the  Astronomical  Society)  to  express  the  gradations  of  light  and  the  general 
form  of  the  nebula  and  its  principal  branches,  and  although  in  both  these  respects  that  figure, 
taken  altogether,  may,  I  believe,  fairly  claim  to  be  considered  more  correct  than  any  other  of 
the  same  object  which  has  yet  appeared,*  as  well  as  more  exact  in  many  of  its  details;  yet 
the  first  glance  obtained  of  it  under  these  more  favourable  circumstances  sufficed  to  convince 
me  of  the  necessity  of  executing  a  redelineation  of  it,  based  upon  a  micrometric  survey  and 
projection  of  the  stars  contained  within  its  area,  and  comprehending  a  multitude  of  nebulous 
branches,  convolutions  and  other  details,  of  whose  existence  I  had  never  before  had  the  least 
suspicion.    The  figure  of  1825  was  executed  without  the  aid  of  micrometric  measurements,  or 


*  I  am  aware  but  of  four  representations  of  this  nebula  which  have  appeared  since  1824, — one  by  Dr. 
Lamont,  published  with  his  thesis  "  Ueber  die  Nebelflecken,"  read  at  the  anniversary  sitting  of  the  Bavarian 
Academy  of  Sciences,  August  25,  1837;  and  two  by  Sig.  Rondoni,  a  Roman  artist.  The  former,  though 
rather  a  coarsely  executed  figure,  and  confined  solely  to  the  denser  part  of  the  nebula,  or  those  regions  which 
I  have  termed  the  Front,  Occiput,  and  Fauces,  yet  contains  some  valuable  particulars  respecting  the  apparent 
breaking-up  of  the  nebula  (especially  about  the  front  and  occiput)  into  patches  and  knots ;  particulars  very 
unsatisfactorily  expressed  in  my  figure  of  1824,  but  in  which  my  observations  of  1834  and  1837  fully  confirm 
Dr.  Lamont's  remarks.  In  his  figure  he  has  (perhaps  intentionally)  omitted  to  express  the  remarkable 
effusion  of  the  nebula  from  the  "  Front"  and  "  Proboscis"  into  what  I  have  termed  the  "  Subnebulous 
Region,"  and  he  has  filled  the  interior  of  the  trapezium  with  nebula,  a  particular  in  which  we  disagree 
decidedly.  The  two  figures  of  Sig.  Rondoni,  which  are  given  in  the  Report  of  Observations  made  at  the 
Collegio  Romano,  by  the  associated  astronomers  of  the  Gregorian  University,  for  the  years  1840  and  1841, 
are  perhaps  rather  to  be  regarded  as  curious  specimens  of  lithography  than  as  accurate  representations  of 
the  nebula  (such,  at  least,  as  I  have  ever  seen  it),  which  they  resemble  in  fact  hardly  more  than  they  do 
one  another.  Nor  should  I  have  thought  it  necessary  to  do  more  than  simply  mention  them,  were  it  not 
that  one  of  them  has  been  referred  to  by  Mr.  Hunt,  in  his  recent  work  entitled  "  Researches  on  Light,"  as 
an  instance  of  direct  photographic  representation  impressed  on  a  lithographic  stone  by  the  light  of  the  nebula 
itself.  Were  this  the  case,  the  high  authority  which  a  self-impressed  picture  would  claim  must  necessarily 
lead  to  the  absolute  rejection  both  of  Dr.  Lamont's  and  my  own  figures,  or  else  to  the  conclusion  of  changes 
both  in  the  nebula  itself,  and  in  the  situations,  relative  brightnesses,  and  nebulous  appendages  of  the  stars 
adjacent  to  it,  of  a  very  extraordinary  and  capricious  kind.  In  fact,  however,  the  inscription  on  the  margin 
of  Sig.  Rondoni's  figure  simply  expresses  (as  I  understand  it)  that  his  original  drawing  (probably  an  eye-draft) 
was  subsequently  transferred  to  a  surface  of  stone  by  a  photographic  process.  I  purposely  avoid  all  com- 
ment on  the  remarks  which  accompany  these  two  representations,  leaving  astronomers  to  form  their  own 
judgment  on  them.  The  other  representation  above  alluded  to  is  that  of  Sig.  Devico  himself,  in  the  year 
1839,  printed  in  the  Annals  of  the  Collegio  Romano  for  1838,  which,  though  much  less  inaccurate  in  many 
respects  than  Sig.  Rondoni's,  is  by  no  means  free  from  objection  on  that  score. 

H 


26 


OBSERVATIONS  OF 


at  best  of  very  rude  and  imperfect  ones,  which,  in  an  object  of  such  extent,  must  of  course 
afford  much  room  for  distortion  and  want  of  due  proportion  in  the  magnitudes  of  particular 
parts.  Nor  had  I  at  that  time  the  same  command  of  polish  and  figure  in  the  specula  which 
subsequent  practice  has  conferred,  so  that  imperfections  in  both  were  tolerated,  from  a  degree  of 
timidity  in  applying  the  remedy,  which  were  not  considered  endurable  at  a  more  advanced  period. 

(55)  Accordingly  a  series  of  equatorial  observations  of  differences  of  R  A  and  NPD 
was  set  on  foot  with  a  view  to  furnishing  the  requisite  data  for  the  construction  of  working 
skeletons  to  be  divided  into  triangles  and  so  filled  in  with  the  nebulous  details,  and  telescopic 
stars,  to  be  ultimately  transferred  to  a  general  drawing,  and  catalogued  in  order  of  right 
ascension,  according  to  a  regular  and  systematic  mode  of  proceeding.  These  differences  were 
obtained  chiefly  on  the  nights  of  December  18,  19,  1834;  December  17,  19,  22,  1836;  and 
February  18,  October  21,  23,  November  5,  14,  15,  16,  24,  1837.  One  set  of  observations  of 
this  nature  had  previously  been  procured  in  England  in  1831,  and  1832,  and  a  few  differences 
of  right  ascension  as  early  as  1825,  with  the  20  feet  reflector.  From  the  assemblage  of  these 
differential  measures  consisting  altogether  of  upwards  of  300  differences  of  R  A,  and  nearly 
as  many  (270)  of  Polar  distance,  the  details  of  which  it  is  unnecessary  to  give,  the  relative 
situations  of  those  stars  which  are  marked  in  the  annexed  Catalogue  as  of  the  first  class 
were  concluded,  with  as  much  precision  as  can  be  considered  requisite  for  such  a  purpose. 

(56)  By  the  aid  of  the  measures  of  December,  1834,  and  the  English  series  alluded  to, 
the  first  skeleton  was  laid  down  and  filled  in  on  the  4th  and  29th  January,  1835,  and  on  the 
27th  December,  1836,  and  a  number  of  curious  and  interesting  particulars  noticed  and 
delineated,  of  which  more  in  their  proper  place,  but  it  was  not  till  the  end  of  1837  that  the 
accumulation  of  the  micrometric  measures  had  enabled  me  to  lay  down  with  some  precision 
a  set  of  skeletons,  four  in  number,  extending  over  the  whole  nebulous  area  intended  to  be 
included  in  the  drawing.  These  were  completed  and  filled  in  on  the  19th,  23rd,  24th,  and 
30th  November,  and  on  the  1st  and  2nd  of  December,  1837,  on  the  former  of  which  nights 
also  a  set  of  micrometrical  position-angles  were  procured  for  the  purpose  of  ascertaining  the 
situation  of  two  small  but  important  stars  (marked  L  and  1  in  the  annexed  Catalogue), 
critically  situated  on  the  Messierian  Branch  (as  I  have  taken  the  liberty  to  call  it)  of  the 
nebula,  and  which  had  escaped  observation  in  the  equatorial,  owing  to  their  minuteness. 

(57)  The  triangles  of  all  the  skeletons  were  examined  seriatim,  and  all  the  stars  visible 
in  them  even  to  the  smallest  magnitudes  scrupulously  laid  down,  at  least  in  those  regions 
on  which  the  principal  interest  excited  by  the  object  is  naturally  concentrated.  It  must 
however  be  observed  that  in  the  denser  portions  of  the  nebula,  so  bright  is  the  diffused 
light,  that  it  is  extremely  difficult  to  fix  attention  on  such  minute  points,  and  that  glimpses 
are  often  caught  and  lost  again  in  a  manner  which  renders  it  impossible  to  say  positively 
that  a  star  has  or  has  not  been  seen.  No  star  however  has  been  laid  down  in  my  triangles 
and  entered  in  the  Catalogue,  but  such  of  whose  existence  I  am  certain,  from  repeated  and 
distinct  views ;  though  I  can  hardly  doubt  that  some  of  the  glimpses  above  referred  to  have 
been  caused  by  stars  really  existing.  The  suspected  star  marked  x  in  my  old  figure,  in 
the  middle  of  the  "  nebula  oblongata"  as  there  laid  down,  certainly  does  not  exist.  The 
nebula  was  lastly  carefully  worked  in  on  each  triangle,  bestowing  especial  regard  on  its 
configuration  with  respect  to  every  star  in  its  area. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


'27 


(58)  The  mode  of  "  reading  off  the  skeletons"  so  as  to  obtain  from  them  the  most 
probable  right  ascensions  and  polar  distances  of  the  unknown  stars  laid  down  in  them, 
requires  some  explanation.  The  places  of  the  "  skeleton  stars"  (those  of  the  first  class  in 
the  Catalogue)  finally  adopted  not  being  precisely  those  used  for  laying  down  the  skeletons, 
but  having  been  subsequently  deduced  from  the  observations  on  a  general  and  careful  revision 
of  their  whole  assemblage — there  will  necessarily  be  a  discordance  to  the  extent  of  a  few 
micrometer  parts  in  polar  distance,  and  a  few  tenths  of  a  second  in  right  ascension  between 
each  skeleton  and  the  adopted  catalogue,  even  for  those  stars  which  form  the  angles  of  the 
triangles  into  which  it  is  divided :  neither  will  the  amount  of  this  discordance  be  the  same  in 
every  part  of  the  same  skeleton.  Any  star  then  laid  down  within  a  triangle  whose  angles  we 
shall  denote  by  A,  B,  C,  will  have  its  place  as  referred  to  a  system  of  true  meridians  and 
parallels  supposed  to  be  drawn  across  the  skeleton,  affected  by  an  error  (and  requiring  a 
contrary  correction)  determined  by  and  calculable  from  the  errors  in  R  A  and  P  D  of 
A,  B,  and  C,  similarly  referred  to  the  same  system  of  co-ordinates.  Now  the  stars  being 
laid  down  within  each  triangle  by  the  sole  judgment  of  the  eye,  it  is  not  possible  to  eliminate 
the  errors  of  such  judgment  by  any  system  of  calculation — but  the  errors  produced  by  small 
displacements  of  the  angles  may  be  reasonably  enough  supposed  to  depend  on  the  proximities* 
of  those  angles  to  the  point  laid  down,  so  that  calling  the  proximity  of  that  point  to  A,  B, 
and  C,  respecting  a,  b,  and  c  the  formula 

Aa+Bb  +  Cc 
a  +  b  +  c 

will  express  the  error  of  its  place  either  in  R  A  or  P  D,  if  A,  B,  C,  represent  the  errors 
in  those  of  A,  B,  C,  respectively  in  the  same  directions.  The  proximities  in  question  are 
sufficiently  well  determined  for  the  purpose  without  measurement  (which  would  be  intolerably 
laborious)  by  the  mere  judgment  of  the  eye — and  when  the  unknown  star  lies  in  or  very  near 
one  side  (as  A  B)  of  the  triangle,  the  influence  of  the  opposite  angle  (C)  on  the  result 
must  be  proportionally  diminished  by  assigning  to  it  a  less  proximity. 

(59)  On  this  principle  then  each  skeleton  is  separately  read  off.  A  system  of  meridians 
at  10s  of  time  apart  in  R  A,  and  of  parallels  distant  from  each  other  by  1000  micrometer 
parts  (=  240//,44=4/  0//,44)  is  carefully  drawn,  the  zero  line  of  each  passing  through  the 
chief  or  fiducial  star  (01  Orionis)  and  upon  this  system,  by  a  diagonal  scale,  the  right 
ascension  and  polar  distances  of  every  star,  known  and  unknown,  of  the  skeleton  is  read  off. 
The  places  of  the  known  stars  thus  read  off  compared  with  their  catalogued  places  furnish 
the  corrections  required  for  each  of  them,  and  from  these  by  the  above  formula  those  to  be 
applied  to  the  readings  of  the  unknown  stars  are  derived.  The  same  process  being  repeated 
for  all  the  skeletons,  the  readings  are  arranged  in  order  of  right  ascension,  and  stars  which 
occur  in  different  skeletons  being  identified,  and  the  means  of  their  places  taken,  a  catalogue 
results,  as  free  from  error  as  the  nature  of  the  observations  will  permit.  The  magnitudes 
assigned  to  each  star  at  each  observation  are  in  like  manner  collected  and  a  mean  taken 
which  is  the  magnitude  finally  adopted.  The  following  is  the  result  of  this  process  for  the 
nebula  now  under  consideration. 

*  I  use  the  term  proximity  in  a  strict  sense,  to  express  the  reciprocal  of  the  distance  (^-)—  a  form  of 
expression  of  much  convenience  in  many  applications  of  algebra  to  geometry  and  physics. 


28 


OBSERVATIONS  OF 
CATALOGUE  OF  STARS  OBSERVED  IN  THE  NEBULA  ABOUT  9  ORIONIS. 


x  = 

y  = 

•n 

a 

x  = 

y  = 

•j. 

x  = 

y  = 

« 

No. 

Letter. 

s 

ARA 

ANPD 

DO 

cd 

No. 

Letter. 

ARA 

ANPD 

BO 
C3 

No. 

Letter. 

ARA 

AXPD 

on 

from  a. 

Sec.  Dec. 

from  a. 
Parts. 

O 

from  a. 

Sec.  Dec. 

from  a. 
Parts. 

O 

from  a. 
Sec.  Dec. 

from  a. 
Parts. 

O 

i 

Z 

8 

— 129.2 

-  599 

I 

51 

17 

-  6.7 

+  45 

3 

101 

1 

7 

4-  10. 1 

4-  395 

I 

2 

(x) 

12 

-  87-9 

+241 1 

52 

15 

-  6.5 

4-1526 

3 

102 

e 

12 

4-  10.4 

—2009 

3 

00 

8.9 

-  81.3 

+3291 

53 

a 

8 

-  6.2 

4 1 126 

1 

103 

J3 

4-  10.7 

4-  97i 

3 

4 

M 

9.IO 

-  80.6 

+3918 

54 

15 

-  6.0 

4-  71S 

3 

104 

X 

9 

4-  12.2 

4  728 

1 

5 

Q 

IO 

-  65  5 

-  55 

I 

55 

16 

-  5-7 

4-2008 

3 

105 

*5 

4-  12.4 

42882 

3 

6 

(?) 

IO.  1 1 

—  62.1 

— 2811 

56 

16 

-  5-6 

-1658 

3 

106 

12 

4-  13-5 

4-2345 

3 

7 

(?) 

IO 

-  61.6 

+  3422 

57 

17 

-  4.6 

+  8 

3 

107 

14 

+  n-5 

—3427 

3 

8 

12 

-  61.6 

+  1293 

3 

58 

J3 

—  4-3 

4-3809 

3 

108 

A* 

6.7 

+  14-4 

-1843 

1 

9 

12 

-  59-5 

+  3395 

2 

59 

12 

—  2.3 

4-4019 

3 

109 

16 

4-  144 

—  1 123 

3 

IO 

I  I 

-  57-2 

+  1018 

1 

60 

15 

-  2.3 

+  3200 

3 

1 10 

n 

8 

4-  15-° 

4-  453 

1 

1 1 

w 

IO.  1 1 

-  55-5 

+  3929 

1 

61 

15 

—  2.2 

+4889 

3 

in 

E 

10 

4-  15-5 

4-2417 

1 

12 

R 

II 

-  5*-5 

—  256 

1 

62 

15 

-  1.8 

+  1859 

3 

112 

12 

4-  16.9 

41891 

3 

'3 

14 

-  50.5 

+  226 

3 

63 

J3 

—  0.7 

+  3932 

3 

113 

b 

9.10 

4-  18.3 

—2760 

14 

H 

—  49.0 

+  239 

3 

64 

7 

!3 

—  o-7 

-  52 

1 

114 

16 

4-  20.0 

-  535 

3 

15 

—  49-° 

+  1944 

3 

65 

7 

—  0.7 

-  36 

1 

"5 

16 

4-  21.4 

43382 

3 

16 

12 

-  47.6 

+2376 

3 

66 

16 

-  0.6 

—2097 

3 

116 

18 

4-  23.6 

— 1601 

3 

17 

14 

-  47.2 

+  163 

3 

67 

8 

8 

—  0.4 

-  67 

1 

117 

P 

16 

+  24.4 

4-  985 

2 

18 

t 

IO.  II 

-  46-4 

+  1050 

1 

68 

15 

—  0.1 

4-4844 

3 

118 

16 

+  24.7 

-2875 

3 

J9 

14 

-  44-o 

-  7° 

3 

69 

a 

5 

0 

0 

1 

119 

4-  24.7 

-3518 

3 

20 

8 

-  43-6 

+  574° 

4 

70 

12 

4-  0.3 

—  396 

3 

120 

X 

1 1 

4-  25.1 

—  819 

1 

21 

'3 

-  4r-7 

+  I255 

3 

71 

a' 

'4 

+  0.3 

4-  5 

2 

121 

q 

17 

4-  25.4 

41069 

2 

22 

16 

—  41.0 

4-2282 

3 

72 

P 

15 

4-  0.5 

+4644 

3 

122 

16 

4-  25.8 

43086 

3 

23 

8 

—  40.6 

4-4990 

4 

73 

7 

4-  0.8 

-  28 

1 

123 

k 

12 

4  25.9 

4-1215 

2 

24 

(?) 

8 

-  38.8 

+4675 

4 

74 

B 

10 

4-  0.8 

4-3937 

1 

124 

a 

1 1 

4  26.0 

-2450 

25 

-  37.6 

—  3270 

75 

18 

4-  i-5 

—  J75 

3 

125 

»4 

4-  27.6 

4-3!79 

3 

26 

"3 

—  37-i 

+  809 

3 

76 

y' 

15 

4-  2.1 

—  692 

3 

126 

1 

J3 

4  27.6 

4-2135 

2 

27 

r 

1 1 

—  36-9 

+  294 

1 

77 

14 

4-  2.2 

4-4612 

3 

127 

13 

4-  27.9 

-3130 

3 

28 

14 

-  36.8 

—2689 

3 

78 

18 

-4-  2.2 

-  85 

3 

128 

'5 

4-  29.3 

-J534 

3 

29 

12 

-  36-6 

+4310 

4 

79 

15 

+  2.5 

-1665 

3 

129 

'3 

4  29.7 

— 1711 

3 

30 

16 

-  35-7 

—  198 

3 

80 

y" 

16 

+  2.6 

-  675 

3 

130 

16 

4-  33-4 

-1791 

3 

31 

(») 

-  34-3 

-3990 

81 

16 

4-  2.7 

4-  648 

3 

131 

16 

4-  33-5 

42871 

3 

32 

s 

1 1 

-  33-1 

-1 184 

1 

82 

X 

16 

4-  3-2 

—  901 

3 

J32 

(«) 

11 

+  33-8 

44222 

33 

M 

—  31.6 

4-  416 

3 

83 

16 

4-  3-2 

—  1756 

3 

!33 

e 

9.10 

4-  34-5 

41262 

1 

34 

8 

—  29.2 

4-2729 

1 

84 

w 

14 

4-  3-8 

-  583 

3 

J34 

17 

4-  35-6 

41327 

3 

35 

0 

10 

—  27.0 

— 1123 

1 

85 

J 

IO 

4-  3-9 

-3520 

1 

'35 

A 

6-7 

4  38-2 

43528 

1 

36 

K 

16 

—  26.3 

+  147 

3 

86 

d 

1 1 

+  3-9 

-2688 

1 

,36 

E 

8 

4  42.3 

—  261 

1 

37 

IO.  I  I 

-  24.3 

+  2460 

1 

87 

V 

IO 

+  4-3 

—  412 

1 

137 

J5 

4  42.4 

-1535 

3 

38 

13 

—  21.2 

-  61 

3 

88 

»7 

+  4-9 

4-  96 

3 

,38 

(0) 

11 

4  42.9 

4-4093 

39 

17 

—  20.9 

—21 19 

3 

89 

z 

16 

+  5-6 

-  686 

3 

139 

(r) 

11 

4-  5°-9 

4-4567 

40 

N 

7.8 

—  20.4 

4-1756 

1 

90 

*5 

+  5-9 

+  3033 

3 

140 

14 

4  52.1 

4-4637 

3 

41 

15 

—  19.8 

4-  101 

3 

91 

17 

4-  6.5 

+  238 

3 

141 

(X) 

16 

4-  52-5 

— 11 12 

3 

42 

15 

-  19-4 

—2883 

3 

92 

15 

4  6.8 

4-2798 

3 

142 

12 

4-  53-8 

4 1 1 10 

43 

15 

-  19-3 

4-2026 

3 

93 

f 

5 

+  6.9 

+  386 

1 

143 

X 

5.6 

4-  59-7 

+  3796 

1 

44 

17 

-  17-4 

-  114 

3 

94 

16 

4-  7-6 

—3027 

3 

144 

«5 

4-  70.0 

4-578o 

4 

45 

T 

1 1 

—  16.3 

4-  483 

1 

95 

12 

+  8.4 

+  1851 

3 

!45 

s 

8.9 

4  71. 1 

4  214 

1 

46 

16 

—  14.8 

-1959 

3 

96 

16 

4-  8.5 

-2978 

3 

146 

7? 

4-  72-3 

45630 

4 

47 

15 

-  12.3 

+  1583 

3 

97 

15 

4-  8.7 

-3321 

3 

H7 

T 

11 

4  76.4 

—  21 

1 

48 

h 

1 1 

—  12. 1 

—2120 

98 

>3 

4-  8.9 

-3625 

3 

148 

V 

9 

4  81.6 

-3888 

1 

49 

t 

7.8 

—  1 1.0 

— 2760 

1 

99 

c 

1 1 

4-  9-3 

-2524 

149 

Y 

10 

+  82.1 

41204 

4 

5° 

'4 

—  10.2 

4-  516 

3 

100 

G 

14 

4-  10.1 

+  548 

3 

150 

U 

10 

4  83.6 

-  935 

1 

Note. — The  following  stars  in  this  Catalogue  are  identified  with  stars  observed  by  others: — 


34  =  M  is  Bode's  131  Orionis,  and  is  identical  with 
Messier's  star  No.  1  in  his  figure  in  Mem. 
Acad.  Sci.  1771. 
40  =  N  is  Bode's  132  Ori.  =  Mess.  No.  2. 
49  =  1  is  Bode's  134  Ori.  =  Mess.  No.  3. 
53  —  (t  is  Bode's  135  Ori.  =  Mess.  No.  4. 
69  =  a  is  0'  Orionis  =  ASC.  679. 

Note  also,  the  star  No.  63  in  the  above  catalogue  is  perhaps  two  stars ;  at  least  in  one  diagram,  without 
a  date,  I  find  another  star  14m  laid  down  beside  it  on  the  same  parallel. 


93  =  £  is  92  Orionis  =  ASC.  681. 
101  =  I  is  Bode's  141  =  Mess.  No.  6. 
108  =  n  is  Bode's  143  =  Mess.  No.  7- 
110  =  n  is  Bode's  146  =  Mess.  No.  8. 
135  =  A  is  Bode's  153  =  Mess.  No.  10. 
143  =  X  is  Bode's  155  =  Mess.  No.  11. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


29 


(60)  In  constructing  the  figure  of  the  Nebula,  Plate  VIII. — The  stars  have  been  in  the 
first  place  carefully  laid  down  in  their  proper  places,  and  with  as  much  regard  to  their  relative 
magnitudes  as  might  consist  with  their  representation  by  mere  round  black  dots — every  other 
mode  of  expressing  them,  either  by  annexed  numbers  or  by  rays,  Sec,  being  objectionable,  as 
tending  to  confuse  the  details  of  the  nebula  and  draw  away  attention  from  them.  Among 
the  stars  so  laid  down  the  nebula  has  been  afterwards  worked  in,  from  all  the  evidence  of 
the  several  skeleton  projections,  and  of  other  drawings  from  time  to  time  obtained,  compared 
inter  se,  paying  very  particular  attention  to  the  due  expression  of  all  those  cases  where  some 
well  defined  portion  of  its  contour,  or  other  remarkable  point  of  it  were  found  to  coincide 
nearly  or  exactly  with  one  of  the  stars,  so  as  to  establish  authentic  landmarks,  or  fiducial 
points  by  which  at  any  future  time  a  perceptible  shifting  of  position  or  change  of  form  in 
the  nebula  may  be  certainly  detected.  The  area  of  the  figure  (half  a  square  degree  in  extent) 
comprises  all  the  nebulous  convolutions  and  appendages  which  I  have  been  able  to  trace, 
with  exception  of  a  faint  extension  of  the  terminal  effusion  of  the  greater  proboscis  beyond  the 
star  A  southwards,  which  may  be  traced  as  far  as  the  double  star  t  Orionis  which  it  involves, 
and  renders  nebulous.  It  is  however  of  little  intensity,  and  offers  nothing  remarkable  enough 
in  respect  of  form  to  have  made  it  worth  while  to  enlarge  the  dimensions  of  the  engraving 
sufficiently  to  take  in  the  whole.  Northwards,  between  this  nebula  and  that  about  C  Orionis, 
as  already  above  remarked  in  my  account  of  that  nebula,  no  nebulous  connexion  has  been 
traced.  An  attentive  consideration  of  our  figure  and  Catalogue  will  give  rise  to  some 
remarks  which  for  distinctness  we  shall  arrange  under  specific  heads. 

(61)  Of  the  Trapezium. — In  the  Catalogue,  the  four  large  stars  a,  j3,  y,  8  as  well  as  the 
fifth  star  y'  discovered  by  Struve  in  1826,  are  laid  down  from  the  "  micrometric  measures" 
of  that  excellent  observer,  which,  no  doubt,  exceed  in  accuracy  any  that  I  could  have  expected 
to  procure.  It  is  somewhat  remarkable  that  in  his  elaborate  discussion  of  the  measured  dimen- 
sions and  position  of  the  trapezium  and  this  star  in  the  "  mensurce  micrometricce  stellarum  composi- 
tarum"  p.  242,  no  mention  is  made  of  the  sixth  star,  (a'  Trapezii)  though  at  the  date  of  some- 
of  the  observations  there  recorded  which  come  down  as  low  as  1836,  its  existence  could  hardly 
have  been  unknown  to  him.  This  star  has  been  seen  by  me  on  several  occasions  in  the  20  feet 
reflector— viz.  on  December  25,  1832 ;  November  25,  and  29,  1834;  January  29,  1835,  and 
December  2,  1837,  besides  others  of  which  the  dates  are  not  specially  recorded.  On  the  two 
last  specified  occasions  micrometric  measures  were  procured  of  its  angular  position  from  a,  as 
compared  with  that  of  a  e  taken  as  a  fiducial  direction.  These  measures  gave  for  the  angle 
€  a  a'  respectively  20° .2  and  11°.5,  the  mean  being  15°.8.  If  the  disagreement  of  these 
should  appear  excessive,  it  will  be  recollected  that  in  this  case  every  circumstance  which  can 
add  difficulty  to  or  create  uncertainty  in  such  measurements  conspires— extreme  inequality, 
and  close  proximity  of  the  stars  directly  compared,  the  disturbing  near  neighbourhood  of 
three  other  very  bright  stars,  unsymmetrically  placed  with  respect  to  the  wires  and  to  each 
object — and  the  glare  of  the  surrounding  nebula,  very  different  in  its  effect  on  the  eye  from 
the  equable  illumination  of  the  field  afforded  by  a  lamp.  This  mean  15°.8,  subtracted  fro 
133°.0,  the  true  position  of  e  from  a  gives  117°.2  for  that  of  a'  from  the  latter.  Small  as 
this  star  is,  if  the  state  of  the  atmosphere  be  favourable  it  does  not  require  the  full  aperture 

i 


30 


OBSERVATIONS  OF 


of  18  inches  to  render  it  visible.  On  the  night  of  November  29,  1834,  I  find  it  recorded 
that  "  applying  the  aperture  of  12  inches  the  sixth  star  a'  was  finely  seen.  It  is  excessively 
minute,  and  very  close  to  a,  much  more  so  than  y'  is  to  y,  say  half  the  distance,  and  14  mag., 
while  y1  =  12  mag."*  This  estimate  of  distance  however  I  consider  too  small,  and  in  all 
probability  the  central  distance  a  a'  may  be  reckoned  at  about  3".  Appended  to  this  night's 
observations  I  also  find  the  following  note. — "  N.B.  In  the  interior  of  the  trapezium,  there 
exists  positively  no  nebulosity,  at  least  none  comparable  in  intensity  to  that  immediately 
without  it."  It  may  not  be  irrelevant  to  add  also  that  on  this  occasion  three  measures 
(220-5,  215*1  :  :  ,  222-8)  were  procured  of  the  difference  of  positions  between  the  lines  of 
direction  y  y'  and  a  e,  the  mean  of  which  219°  added  (as  in  this  case  is  necessary)  to  133*0  the 
position  of  a  e,  gives  for  the  position  of  y  from  y  3520,5  which  agrees  well  with  M.  Struve's 
position  of  this  star  (3530,6).  Had  only  half  the  weight  been  allowed  to  the  confessedly 
defective  measure  215.5,  the  coincidence  would  have  been  almost  perfect  (353°*3).  This  is 
also  the  proper  jdace  to  notice  that  the  stars  within  the  trapezium,  marked  Nos.  6,  7,  8,  by 
Signor  De  Vico,  as  having  been  observed  by  him  in  February  1839,  with  the  Cauchoix  refractor 
of  the  Collegio  Romano,  have  entirely  escaped  my  notice.  On  the  other  hand  no  indication 
of  the  star  a'  (whose  situation,  fairly  outside  of  the  trapezium  admits  of  no  possibility  of 
reconcilement  with  any  of  M.  De  Vico's  interior  stars)  appears  in  his  figure. — ("  Memoria 
intorno  ad  Alcune  osservazioni  fatte  alia  specola  del  Collegio  Romano  nel  corraente  anno 
1838.") 

(62)  Of  other  small  stars  near  the  Trapezium  or  otherwise  remarkably  situated,  not  noticed  in 
mH  figure  of  1824. — Two  exceedingly  minute,  but  undoubted  stars,  Nos.  75  and  78  of  our 
Catalogue  are  very  remarkably  placed  on  or  very  near  the  edge  of  the  nebula  at  the  bottom 
of  the  "  fauces"  or  "  great  sinus."  In  Dr.  Lamont's  figure  already  referred  to,  a  star  which 
may  be  supposed  identical  with  one  of  these  (No.  75),  from  its  allineations  with  other  stars, 
is  represented  as  deeply  immersed  in  the  nebula.  The  other  seems  to  have  escaped  his 
notice,  and  so  far  as  I  am  aware  that  of  every  other  observer. 

(63)  I  am  indebted  to  my  esteemed  friend  E.  Cooper,  Esq.  late  M.P.  for  Sligo,  in 
Ireland,  for  several  interesting  remarks  and  observations  at  various  times  communicated  by 
letter.  In  the  year  1833,  March  21,  he  was  so  good  as  to  forward  me  a  diagram  exhibiting 
the  situations  of  seven  small  stars  interestingly  situated,  which  had  escaped  my  notice  in  1824. 
Of  these,  six  occur  in  the  foregoing  Catalogue,  viz.  Nos.  41,  44,  91,  100,  114,  117.  The 
seventh,  whose  catalogued  co-ordinates  would  be  —  7S,75  and  +  227  Parts.  Micr.,  according 
to  the  place  assigned  to  it  by  Mr.  Cooper,  has  escaped  my  notice,  or  at  least  does  not  occur 
in  the  skeletons,  so  that  if  seen  at  all  it  has  been  only  by  transient  glimpses.  The  place  of 
this  star  is  half  way,  in  a  strait  line,  between  /3  (No.  73)  and  r  (No.  45.) 

(64)  The  star  marked  x  in  my  figure  of  1824,  suspected  to  exist  in  the  middle  of  the 
"  nebula  oblongata"  was  not  seen  by  Mr.  Cooper,  and  I  am  now  satisfied  does  not  exist.  On 
the  other  hand  I  find  in  his  diagram  a  star  very  distinctly  laid  down,  but  not  marked  by  him 

*  In  the  diagram  made  on  this  occasion,  the  letters  /3  and  y  are  transposed,  and  the  stars  y,  y1  are  called 
P,  /3>.    This  misnomer  is  of  course  rectified  in  the  text. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


31 


as  a  new  one,  though  no  such  star  occurs  in  my  former  figure  in  the  exact  place  of  No.  82,  in 
the  "  maxilla  inferior"  near  the  double  star  y'  y".  This  star  I  find  in  only  one  of  my 
skeletons,  and  though  quite  unequivocally  marked,  it  has  no  magnitude  attached,  and  the 
letter  y  is  placed  adjacent  to  it,  instead  of  being  affixed  to  the  double  star  y'  y",  both 
individuals  of  which  are  also  laid  down,  of  the  same  apparent  size  as  that  in  question.  Had 
it  not  been  therefore  for  the  insertion  of  this  star  (though  under  doubtful  circumstances)  in 
Mr.  Cooper's  diagram,  I  should  have  perhaps  hesitated  to  admit  it  into  my  Catalogue  as  I 
have  now  done,  transferring  to  it  the  letter  x  which  remained  otherwise  unoccupied. 

(65)  Mr.  Cooper  suspects  the  star  No.  41,  to  be  double.  No.  117  (p  of  the  Catalogue) 
affords  him  occasion  for  a  remark  of  considerable  interest  and  importance,  as  it  goes  to  prove 
that  the  relative  situation  of  the  nebula  and  this  star  underwent  no  change  in  the  interval 
between  1833  and  1837.  For  he  states  the  star  in  question  to  be  situated  "  on  the  very  edge 
of  the  stream  of  light"  (meaning  the  "  proboscis  major")  which  was  also  precisely  its  situation 
at  the  later  epoch.    He  makes  however  no  mention  of  its  minute  companion  q  (No.  121). 

(66)  The  two  small  stars  Nos.  51  and  57,  near  the  trapezium,  and  No.  81,  outside  of 
the  "  Front"  towards  its  rectangular  junction  with  the  "  occiput"  in  the  faint  (and  hitherto 
unnoticed)  effusion  of  the  nebula  which  prolongs  the  "  Sinus  Gentilii"  outwards,  have  in 
like  manner  eluded  the  scrutiny  of  all  other  observers  so  far  as  their  observations  are  known 
to  me.    Of  Nos.  88  and  91,  Dr.  Lamont  has  one,  and  Mr.  Cooper  the  other. 

(67)  Of  Evidences  of  change  in  the  Nebula. — To  the  reader  who  has  never  viewed  this 
object  through  powerful  telescopes,  but  who  is  familiar  with  the  various  representations 
which  have  from  time  to  time  been  made  of  it  (including  my  own  of  1824),  the  number 
and  complexity  of  the  various  branches  and  convolutions  now  first  exhibited,  and  the  different 
aspect  under  which  even  the  portions  best  known  are  now  presented,  will  no  doubt  tend  to 
convey  a  strong  impression  of  great  and  rapid  changes  undergone  by  the  nebula  itself.  I  am 
far  from  participating  in  any  such  impression.  Comparing  only  my  own  drawings  made 
at  epochs  (1824  and  1837)  differing  by  thirteen  years,  the  disagreements,  though  confessedly 
great,  are  not  more  so  than  I  am  disposed  to  attribute  to  inexperience  in  such  delineations 
(which  are  really  difficult)  at  an  early  period — to  the  far  greater  care,  pains,  and  time 
bestowed  upon  the  later  drawings — and  above  all  to  the  advantage  of  local  situation  and 
the  very  great  superiority  in  respect  both  of  light  and  defining  power  in  the  telescope  at 
the  latter  over  what  it  possessed  at  the  former  epoch,  the  reasons  of  which  I  have  already 
mentioned.  These  circumstances  render  it  impossible  to  bring  the  figures  into  comparison 
except  in  points  which  could  not  be  influenced  by  such  causes.  Now  there  is  only  one  such 
particular  on  which  I  am  at  all  inclined  to  insist  as  evidence  of  change ;  viz.  in  respect  of 
the  situation  and  form  of  the  "nebula  oblongata,"  which  my  figure  of  1824  represents  as 
a  tolerably  regular  oval  extended  very  nearly  in  a  right  line,  or  at  most  but  a  very  little 
curved  upwards  between  the  two  stars  x  =  No.  120 — and  k  =  No.  136  of  the  Catalogue. 
Comparing  this  with  its  present  appearance  as  exhibited  in  Plate  VIII.  it  seems  hardly 
possible  to  avoid  the  conclusion  of  some  sensible  alteration  having  taken  place.  No  observer 
now,  I  think,  looking  ever  so  cursorily  at  this  point  of  detail,  would  represent  the  broken, 
curved,  and  unsymmetrical  nebula  in  question  (lying,  as  it  does,  in  its  whole  extent,  clearly 
out  of  the  line  of  junction  of  the  two  stars  above  mentioned),  as  it  is  represented  in  the  earlier 


32 


OBSERVATIONS  OF 


of  the  two  figures:  and  to  suppose  it  seen  as  in  1837,  and  yet  drawn  as  in  1824,  would  argue 
more  negligence  than  I  can  believe  myself  fairly  chargeable  with. 

(68)  There  is  another  point  on  which  considerable  stress  might  be  laid,  were  I  satisfied 
that  the  earlier  diagrams  on  which  it  turns  were  done  with  sufficient  care.  In  1837,  the 
nebulous  spur  towards  the  end  of  the  great  proboscis,  which  terminates  at  E  (No.  Ill), 
certainly  was  neither  joined  to  the  proboscis  itself,  nor  directed  towards  the  star  A  (No.  135), 
but  rather  towards  a  point  about  one-third  of  the  distance  from  A  (No.  135),  to  C  (No.  126), 
near  to  where  there  is  a  small  star  16m  (No.  131).  Now  I  find  two  diagrams,  one  of  December 
25,  1832,  the  other  of  November  25,  1834,  in  which  this  spur  is  represented  as  running  directly 
from  A  to  E,  and  forming  a  complete  hook,  no  way  disjoined  from  the  proboscis.  But  the 
chief  attention  on  the  first  of  these  occasions  was  directed  to  the  magnitudes  and  situations 
of  the  stars,  and  the  hook  seems  to  have  been  only  roughly  sketched  in  as  a  novelty  to  be 
further  noticed  in  future,  while  on  the  last  it  is  only  very  faintly  indicated,  in  a  diagram  of 
the  stars  adjacent  to  6  Ononis  on  all  sides,  preparatory  to  the  formation  of  chart  intended  to 
take  in  both  t  Orionis  on  the  one  side  and  C  Orionis  on  the  other,  which  was  subsequently 
discontinued. 

(69)  Still  less  can  we  insist,  as  evidences  of  change,  on  such  particulars  as  the  curiously 
notched  outline  of  the  "  Nebula  Mairanni"  about  the  star  p  (No.  108),  now  for  the  first  time 
represented ;  or  on  the  intricately  rifted  and  broken  state  of  the  frontal  and  occipital  region 
of  the  principal  nebula.  I  ought  to  mention  here  that  (owing  no  doubt  to  the  difficulty  of 
properly  representing  on  paper  and  by  lamp-light  an  object  of  the  kind,  I  find  a  good  deal  of 
disagreement  in  respect  of  the  number,  size,  and  distribution  of  the  portions  into  winch  it  may 
be  considered  as  broken  up,  not  only  between  my  present  figure  and  Dr.  Lamont's,  but 
between  my  own  drawings  of  this  part  on  several  nights.  But  the  most  material  difference 
between  Dr.  Lamont's  figure  and  mine  consists  in  the  characteristic  forms  of  these  portions, 
which  he  represents  as  rounded  masses  more  or  less  detached  from  or  running  into  each  other 
and  into  a  general  nebulous  ground  ;  while  in  all  my  later  drawings  the  effect  is  rather  that  of 
a  tolerably  uniform  surface  marked  with  branching  rifts  or  channels,  like  roads.  There  is  one 
peculiarity  in  Dr.  Lamont's  figure  which  I  can  no  way  reconcile  to  my  own  impressions;  viz., 
the  strangely  different  form  and  magnitude  which  he  assigns  to  the  "  Sinus  Gentilii,"  from 
what  I  have  always  found  it.    This  is  a  point  which  I  trust  he  will  be  induced  to  re-examine. 

(70)  i]  Argus  and  the  great  Nebula  surrounding  it. 

Plate  IX.  r,  Argus  =  h.  3295  =  A.  309  =  Lac.  968  =  Brisb.  3198.  E  A.  10°  38' 38" 
N  P  D  148°  47'. 

There  is  perhaps  no  other  sidereal  object  which  unites  more  points  of  interest  than  this. 
Its  situation  is  very  remarkable,  being  in  the  midst  of  one  of  those  rich  and  brilliant  masses, 
a  succession  of  which  curiously  contrasted  with  dark  adjacent  spaces  (called  by  the  old 
navigators  coal-sacks),  constitute  the  milky  way  in  that  portion  of  its  course  which  lies  between 
the  Centaur  and  the  main  body  of  Argo.  In  all  this  region  the  stars  of  the  milky  way  are 
well  separated,  and,  except  within  the  limits  of  the  nebula,  on  a  perfectly  dark  ground,  and  on 


NEBULAE  AND  CLUSTERS  OF  STARS. 


33 


an  average,  of  larger  magnitudes  than  in  most  other  regions.  Some  idea  of  their  numbers 
may  be  formed  from  the  following  "  star-gages,"  or  numbers  counted  in  single  fields  of  view 
taken  without  partiality  or  selection  in  sweep  543  in  the  middle  of  the  zone  extending  from 
NPD  147°  to  150°,  which  is  almost  exactly  in  the  parallel  of  77  Argus,  viz. : — 

R  A  =  9h  38"'— Stars  in  field  .  .  93  R  A  10  30— Stars  .       .       .  .224 

9   50           „  .  125  11  24  ....  250 

10    10  .  .  106  11  35  .  14Q 

10   26  .  .  144 

The  mean  of  these  gages  which  extend  about  an  hour  in  R  A  on  either  side  of  the  Nebula, 
is  154,  which  being  the  number  of  stars  in  a  circle  15'  in  diameter  gives  an  average  of  3138 
to  the  square  degree  (in  the  denser  part  at  ll'1  24m,  the  gage  being  250,  the  number  to  the 
square  degree  would  amount  to  5093).  From  this  it  appears  that  in  these  two  hours,  during 
which  the  area  of  the  heavens  swept  over  consisted  of  3°  x  30°  x  sin  148°  30'  =  47.03 
square  degrees,  the  amazing  number  of  147,500  stars  must  have  passed  under  review. 

(71)  In  the  midst  of  this  vast  stratum  of  stars  occurs  the  bright  star  r?  Argus,  an  object 
in  itself  of  no  ordinary  interest  on  account  of  the  singular  changes  its  lustre  has  undergone 
within  the  period  of  authentic  astronomy.  For  while  in  Halley's  Catalogue  (constructed  in 
1677)  which  is  the  first  which  can  be  entirely  depended  upon,  it  is  marked  as  of  the  4th 
magnitude,  yet  in  Lacaille's  and  the  subsequent  Catalogues  of  Brisbane,  Johnson,  Fallows, 
and  Taylor,  it  is  made  to  rank  as  of  the  second.  When  first  observed  by  myself  in  1834, 
it  appeared  as  a  very  large  star  of  the  second  magnitude,  or  a  very  small  one  of  the  first,  and 
so  it  remained  without  apparent  increase  or  change  up  to  nearly  the  end  of  1837,  in  November 
of  which  year*  it  was  noticed  of  its  usual  brightness,  or  at  least  without  exciting  any  suspicion 
of  a  change.  Nor  had  any  such  suspicion  been  excited  during  a  series  of  photometric 
comparisons  set  on  foot  in  the  beginning  of  1836,  and  carried  on  whenever  fitting  opportunities 
occurred,  with  the  express  object  of  establishing  a  scale  of  southern  magnitudes,  and  in  which 
this  star  had  been  frequently  compared  with  others  both  superior  and  inferior  to  it  in 
brightness.  In  these  comparisons  its  rank  was  always  judged  to  be  superior  to  that  of  ft 
Crucis,  y  Crucis,  ft  Argus,  e  Canis,  and  Pollux,  and  always  inferior  to  Spica,  a  Crucis, 
Antares,  and  Aldebaran ;  equal  or  a  little  superior  to  Regulus,  and  a  good  match  with 
Fomalhaut.  Estimating  its  magnitude  numerically  from  these  data,  on  a  scale  in  which  each 
magnitude  is  supposed  to  be  divided  into  ten  degrees  or  decimals,  assigning  to  Rigel  the 
magnitude  1*0,  and  to  ft  Argus  2-0,  that  of  rj  would  be  1*4,  in  the  whole  interval  of  time 
from  February  1834  to  November  1837. 

(72)  It  was  on  the  16th  December,  1837,  that  resuming  the  photometrical  comparisons  in 
question,  in  which,  according  to  regular  practice,  the  brightest  stars  in  sight  in  whatever  part 
of  the  heavens  were  first  noticed,  and  arranged  on  a  list,  my  astonishment  was  excited  by 
the  appearance  of  a  new  candidate  for  distinction  among  the  very  brightest  stars  of  the  first 


*  Leaving  off  a  sweep  one  night  in  November,  I  noticed  it  rising  above  some  trees  in  the  S.E  ,  on  which 
occasion  I  remarked  to  my  attendant,  that  "  ?/  Argus  was  getting  up,  and  that  it  would  soon  be  time  to  begin 
another  year's  observations  on  the  nebula."  This  remark  was  subsequently  recalled  forcibly  to  recollection, 
but  the  precise  date  could  not  be  recovered. 

K 


34 


OBSERVATIONS  OF 


magnitude,  in  a  part  of  the  heavens  with  which  being  perfectly  familiar,  I  was  certain  that  no 
such  brilliant  object  had  before  been  seen.  After  a  momentary  hesitation,  the  natural 
consequence  of  a  phenomenon  so  utterly  unexpected,  and  referring  to  a  map  for  its 
configurations  with  the  other  conspicuous  stars  in  the  neighbourhood,  I  became  satisfied  of 
its  identity  with  my  old  acquaintance  r?  Argus.  Its  light  was  however  nearly  tripled. 
While  yet  low  it  equalled  Rigel,  and  when  it  had  attained  some  altitude  was  decidedly  greater. 
It  was  far  superior  to  Achernar.  Fomalhaut  and  a  Gruis  were  at  the  time  not  quite  so 
high,  and  a  Crucis  much  lower,  but  all  were  fine  and  clear,  and  t\  Argus  would  not  bear  to 
be  lowered  to  their  standard.  It  very  decidedly  surpassed  Procyon,  which  was  about  the  same 
altitude,  and  was  far  superior  to  Aldebaran.  It  exceeded  a  Orionis,  and  the  only  star  (Sirius 
and  Canopus  excepted)  which  could  at  all  be  compared  with  it  was  Rigel,  which,  as  I  have 
stated  already,  it  somewhat  surpassed. 

(73)  From  this  time  its  light  continued  to  increase.  On  the  28th  December  it  was  far 
superior  to  Rigel,  and  could  only  be  compared  with  a  Centauri  which  it  equalled,  having  the 
advantage  of  altitude,  but  fell  somewhat  short  of  it  as  the  altitudes  approached  equality. 
The  maximum  of  brightness  seems  to  have  been  obtained  about  the  2nd  January,  1838,  on 
which  night  both  stars  being  high  and  the  sky  clear  and  pure,  it  was  judged  to  be  very  nearly 
matched  indeed  with  a  Centauri,  sometimes  the  one,  sometimes  the  other  being  judged 
brighter,  but  on  the  whole  a  was  considered  to  have  some  little  superiority.  After  this  the 
light  began  to  fade.  Already  on  the  7th,  13th  January,  a  Centauri  was  unhesitatingly  placed 
above,  and  Rigel  as  unhesitatingly  below  it.  On  the  20th,  it  was  "  visibly  diminished — 
now  much  less  than  a  Centauri,  and  not  much  greater  than  Rigel.  The  change  is  palpable." 
And  on  the  22nd,  Arcturus  (the  nearest  star  in  light  and  colour  to  a  Centauri  which  the 
heavens  afford)  when  only  10°  high  surpassed  rj,  the  latter  being  on  the  meridian ;  ??  was  still 
however  superior  to  j3  Centauri,  a  Crucis  and  Spira,  and  continued  so,  (and  even  superior  to 
Rigel)  during  the  whole  of  February,  nor  was  it  until  the  14th  April,  1838,  that  it  had 
so  far  faded  as  to  bear  comparison  with  Aldebaran,  though  still  somewhat  brighter  than 
that  star. 

(74)  Beyond  this  date  I  am  unable  to  speak  of  its  further  changes  from  personal 
observation.  It  appears  however  since  that  time  to  have  made  another  and  a  still  greater  step 
in  advance,  and  to  have  surpassed  Canopus,  and  even  to  have  approached  Sirius  in  lustre,  the 
former  of  which  stars  I  estimate  at  double,  the  latter  at  more  than  the  quadruple  of  a 
Centauri,  so  that  Jupiter  and  Venus  may  possibly  come  to  have  a  rival  among  the  fixed  stars 
in  Argo,  as  they  have  on  recorded  occasions  had  in  Cassiopeia,  Serpentarius,  and  Aquila. 
This  subsequent  increase  was  first  communicated  to  me  in  a  letter  from  the  Rev.  W.  S. 
Mackay,  General  Assembly's  Mission,  Calcutta,  of  which  the  following  is  an  extract.  "To  my 
great  surprise  I  observed  in  March  last  (1843),  that  the  star  r]  Argus  R  A,  10h  39ra  decl.  58°  51' 
S.  had  become  a  star  of  the  first  magnitude  fully  as  bright  as  Canopus,  and  in  colour  and  size 
{sic  in  MS.)*  very  much  like  Arcturus.    This  has  been  observed  by  several  other  persons  to 


*  A  distinction  seems  here  to  be  taken  between  the  brightness  and  size  of  a  star,  which  I  do  not  understand. 
Canopus  has  at  least  double  the  light  of  Arcturus.  v  Argus  belongs  to  the  class  of  ruddy  or  yellow  stars,  as  do 
also  a  Centauri  and  Arcturus. 


NEBULiE  AND  CLUSTERS  OF  STARS. 


35 


whom  I  pointed  it  out.  Is  the  star  known  as  a  variable  star,  or  is  the  change  now  first 
observed  ?    a  Crucis  looked  quite  dim  beside  it." 

(75)  This  further  remarkable  increase  in  March  1843,  to  a  brightness  exceeding  that  of 
Canopus,  is  fully  established  by  a  series  of  comparisons  made  at  my  request  since  December 
29,  1842,  by  my  excellent  friend  Mr.  Maclear,  at  the  Cape,  from  which  it  appears  that  on  the 
last  mentioned  date  it  was  equal  to  /3  Centauri,  but  inferior  to  a,  and  that  during  the  first  half 
of  January,  Procyon  and  Rigel,  were  the  stars  with  which  it  was  most  comparable.  From 
this  time  until  March  8,  Mr.  Maclear's  observations  were  interrupted.  On  that  day  "  it  was 
particularly  brilliant  at  midnight,"  and  "  on  the  11th  and  14th,  it  was  "much  brighter  than 
a  Centauri"  and  Rigel,  "and  even  brighter  than  Canopus."  On  the  19th  it  had  become 
however  "  less  brilliant  than  on  the  last  three  nights,"  and  (as  appears  by  a  letter  from  Mr. 
Maclear,  dated  on  the  28th)  considerably  less  than  Rigel,  and  even  less  than  a  Crucis,  though 
still  much  greater  than  a  Hydras.  On  the  24th  it  had  begun  to  advance  again,  as  Mr. 
Maclear  states  it  to  have  been  on  that  night  "  decidedly  not  so  brilliant  as  Canopus,"  but 
still  "  brighter  than  a  Centauri" — and  on  the  28th  again,  "  still  less  brilliant."  We  have  here 
an  epoch  of  great  interest,  a  temporary  minimum,  with  a  kind  of  trepidation  or  fluttering  of 
light — followed  however  by  another  step  in  advance  even  yet  more  extraordinary — for  by  a 
subsequent  letter  dated  September  17,  1844.  Mr.  Maclear  referring  to  these  observations, 
says,  "  the  changes  of  77  Argus  are  curious,  for  last  April,  twelve  months  it  seemed  almost 
equal  to  Sirius, — I  speak  as  to  date  without  my  notes.  Now  the  star  is  stationary  and  scarcely 
so  bright  as  Canopus."  Lastly,  on  the  3rd  January,  1845,  Mr.  Maclear  writes  as  follows  to 
the  Astronomer  Royal — "  When  you  see  Sir  J.  Herschel,  tell  him  that  77  Argus  has  been 
for  some  time  rather  larger  than  Canopus,  and  seems  again  on  the  decline." 

(76)  Since  my  return  to  England,  the  following  memorandum  has  been  communicated  to 
me  by  the  late  Professor  Henderson,  from  which  it  would  appear  that  in  the  interval  between 
Lacaille's  observations  in  1751,  and  the  period  of  Mr.  Burchell's  residence  and  travels  in 
South  Africa,  the  star  had  receded  from  its  magnitude  as  observed  by  Lacaille  (2m  or  as  Bode 
states  it  3m)  to  the  fourth  magnitude,  as  in  Halley's  time,  and  again  increased  to  the  first, 
from  which  however  it  must  once  more  have  retrograded  previous  to  1834.  Mr.  Henderson's 
memorandum  runs  as  follows  : — 

"  Mr.  Burchell  wrote  July  17,  1827,  to  J.  Duncan  from  St.  Paulo,  near  Rio  Janeiro,  and 
said,  '  I  am  curious  to  know  whether  any  one  has  hitherto  noticed  that  the  star  77  Navis 
which  is  marked  as  being  of  the  fourth  magnitude  {and  which  was  always  so  when  I  was  in  Africa) 
is  now  of  the  first  magnitude,  or  as  large  as  a  Crucis.'"  On  further  inquiry  relative  to  this 
curious  observation,  I  have  been  favoured  by  Professor  Johnson  with  the  communication  of 
the  following  note  from  Mr.  Burchell  himself. 

"  Fulham,  9th  June,  1845. 

"  Dear  Sir. — I  regret  that  I  have  so  long  been  prevented  by  illness  from  complying 
with  the  request  you  made  when  I  had  the  pleasure  of  meeting  you  at  Dr.  Kidd's.  I  now 
find  on  reference  to  my  journal  of  Astronomical  Transactions  under  the  date  of  February  1 , 
1827,  when  I  was  at  the  city  of  St.  Paulo  in  Brazil,  that  the  star  77  Navis,  marked  as  a  star 
of  the  fourth  magnitude  by  Lacaille,  [  ?  Halley]  then  appeared  to  be  of  the  first  and  as  large 


36 


OBSERVATIONS  OF 


as  a  Cruris:  and  that  there  was  no  star  of  this  magnitude  in  that  part  of  the  heavens  when 
r  was  in  Africa  (in  1811—1815):  nor,  as  I  believed  when  I  was  at  Rio  de  Janeiro  (in  1825— 
1826)  as  I  think  it  would  not  have  escaped  iny  notice  in  the  latter  place.  And  that  on  the 
20th  February,  1828,  when  I  was  at  the  city  of  Goyaz  in  Brazil,  I  measured  the  angular 
distance  between  this  star  and  /3  Cruris,  which  I  found  to  be  15°  20'  19",  and  on  the  29th 
of  the  same  month,  its  distance  from  p  Navis,  which  was  13°  16'  29",  and  made  a 
memorandum  that  it  was  then  certainly  of  the  second  magnitude  at  least. 

"  If  these  memoranda  should  prove  of  any  use  it  will  give  me  great  pleasure,  and  I 
remain, 

"  Dear  Sir, 

"  Yours  very  truly, 

(signed)        "  War.  J.  Burchell." 

"  Mr.  Johnson,  Observatory,  Oxford." 


(77)  A  summary  of  the  observed  magnitudes  will  stand  as  follows  : — 


Date. 

Authority. 

Magnitude. 

Date. 

Authority. 

Magnitude. 

1677. 

Halley. 

4 

1838. 

Jan.  2. 

Herschel. 

7  1,  =  a  Crucis, 

1751. 

Lacaille. 

2 

very  nearly  =  a 

1811-1815. 

Burchell. 

4 

Centauri. 

1822. 

Fallows. 

2  * 

1842. 

Mar.  19. 

Maclear. 

L   1,  inferior  to 

1822-1826. 

Brisbane. 

2 

a  Crucis. 

1827.   Feb.  I. 

Burchell. 

1  =  a  Crucis. 

1843. 

April. 

Maclear. 

7  I,  nearly  equal 

1828.    Feb.  29. 

Burchell. 

2..1 

to  Sirius. 

1829-1833. 

Johnson. 

2 

1843. 

April  11-14. 

Mackay. 

Fully  as  bright 

1832..  1833. 

Taylor. 

2 

as  Canopus. 

1834  .  .1837. 

Herschel. 

1..2 

(78)  A  strange  field  of  speculation  is  opened  by  this  phenomenon.  The  temporary  stars 
heretofore  recorded,  have  all  become  totally  extinct.  Variable  stars  so  far  as  they  have  been 
carefully  attended  to,  have  exhibited  periodical  alternations  in  some  degree  at  least  regular, 
of  splendour  and  comparative  obscurity.  But  here  we  have  a  star  fitfully  variable  to  an 
astonishing  extent,  and  whose  fluctuations  are  spread  over  centuries,  apparently  in  no  settled 
period,  and  with  no  regularity  of  progression.  What  origin  can  we  ascribe  to  these  sudden 
flashes  and  relapses  ?  What  conclusions  are  we  to  draw  as  to  the  comfort  or  habitability  of 
a  system  depending  for  its  supply  of  light  and  heat  on  so  uncertain  a  source  ?  It  is  much  to 
be  regretted  that  we  are  without  records  of  its  changes  in  the  intervals  between  the 
observations  of  Halley  and  Lacaille,  and  those  of  Lacaille  and  Burchell.  Its  future  career 
will  be  a  subject  of  high  physical  interest.  To  this  account  I  will  only  add  that  in  the 
beginning  of  1838,  the  brightness  of  this  star  was  so  great  as  materially  to  interfere  with 


In  Fallow's  catalogue  the  star  is  mis-lettered  <j,  but  the  place  is  that  of 


NEBULAE  AND  CLUSTERS  OF  STARS. 


37 


the  observation  of  that  part  of  the  nebula  surrounding  it  which  is  situated  in  its  immediate 
vicinity,  and,  in  particular,  almost  to  obliterate  that  extremely  curious  oval  or  lacuna  which 
forms  so  conspicuous  a  feature  in  the  figure  of  the  nebula  annexed,  and  of  which,  had  I 
not  previously  secured  a  correct  representation,  I  should  then  scarcely  have  been  able  to 
have  done  so  to  my  own  satisfaction. 

(79)  The  accurate  representation  of  this  nebula  with  its  included  stars  has  proved  a 
work  of  very  great  difficulty  and  labour,  owing  to  its  great  extent,  its  complicated  convo- 
lutions, and  the  multitude  of  stars  scattered  over  it.  To  say  that  I  have  spent  several  months 
in  the  delineation  of  the  nebula,  the  micrometrical  measurement  of  the  co-ordinates  of  the 
skeleton  stars,  the  filling  in,  mapping  down,  and  reading  off  of  the  skeletons  when  prepared, 
the  subsequent  reduction  and  digestion  into  a  catalogue,  of  the  stars  so  determined,  and 
the  execution,  final  revision,  and  correction  of  the  drawing  and  engraving,  would,  I  am  sure, 
be  no  exaggeration.  Frequently,  while  working  at  the  telescoj>e  on  these  skeletons,  a 
sensation  of  despair  would  arise  of  ever  being  able  to  transfer  to  paper,  with  even  tolerable 
correctness,  their  endless  details.  However,  by  breaking  it  up  into  parts,  and  executing  each 
part  separately,  it  has  been  accomplished,  and  I  trust  with  such  exactness  as  may  afford  a 
record  capable  of  being  appealed  to  in  future  whenever  the  question  of  internal  changes  of 
the  form  and  situation  of  the  nebulous  branches  shall  be  gone  into. 

(80)  The  area  occupied  by  the  figure  Plate  IX.  of  this  nebula,  extends  in  right 
ascension  from  —  3m  45s  to  +  3m  0s  from  the  principal  star,  and  in  polar  distance  from 
—  24'  to  +  44',  comprising  in  the  whole  an  area  of  almost  exactly  a  square  degree.  Of 
this  about  four-sevenths  are  occupied  by  the  nebulous  branchings  and  their  included  vacuities, 
and  this  portion  only  I  have  thought  it  requisite  to  triangulate  and  catalogue.  The  number 
of  stars  within  this  area  whose  places  have  been  determined  is  1203,  being  at  the  rate  of 
2105  to  the  square  degree,  from  which  it  would  appear  either  that  small  stars  which  would 
have  been  conspicuous  on  a  dark  ground  have  escaped  notice  in  the  glare  of  the  nebula,  or 
that  the  nebula  itself  is  situated  in  a  spot  somewhat  less  crowded  than  the  general  average  of 
the  milky  way  in  its  immediate  neighbourhood. 

(81)  In  the  engraving,  those  stars  only  are  laid  down  which  are  entered  in  the  Catalogue 
accompanying  this  description  as  of  the  twelfth  magnitude  and  upwards,  with  exception, 
first,  of  such  stars  as  are  so  situated  with  respect  to  some  well  defined  edge  or  other 
remarkable  feature  of  the  nebula  as  to  serve  as  marks  by  which  any  future  change  of  form  in 
the  latter  may  be  certainly  recognised : — secondly,  of  small  stars  in  the  immediate  neigh- 
bourhood of  the  large  one  (especially  two  very  minute  ones  almost  close  to  it,  and  which 
the  increased  light  of  the  large  star  had  completely  obliterated  before  the  conclusion  of  my 
observations)  : — thirdly,  of  the  small  stars  of  the  clustering  groups  about  the  stars  O,  F, 
and  y  of  the  Catalogue,  and  of  two  remarkable  elliptic  groups  on  the  parallel  of  +  6000 
micrometer  parts  in  the  engraving  : — fourthly,  of  the  small  stars  immediately  adjacent  to,  and 
included  within,  the  remarkable  oval  vacuity  which  is  crossed  by  the  parallel  of  +  9000  Pts., 
and,  lastly,  of  a  few  others  nearly  adjacent  to  larger  stars,  with  which  they  may  be  considered 
to  form  double  stars.  To  have  laid  down  all  the  stars  observed  would  have  added  greatly 
to  the  probability  of  undetected  errors  in  the  engraving,  without  answering  any  adequate 


38 


OBSERVATIONS  OF 


purpose,  the  Catalogue  being  at  hand,  by  which  any  future  observer  may  satisfy  himself 
whether  any  particular  star  he  may  wish  to  identify  has  been  seen  by  me  or  not. 

(82)  It  would  manifestly  be  impossible  by  verbal  description  to  give  any  just  idea  of  the 
capricious  forms  and  irregular  gradations  of  light  affected  by  the  different  branches  and 
appendages  of  this  nebula.  In  this  respect  the  figure  must  speak  for  itself.  Nor  is  it  easy 
for  language  to  convey  a  full  impression  of  the  beauty  and  sublimity  of  the  spectacle  it  offers 
when  viewed  in  a  sweep,  ushered  in  as  it  is  by  so  glorious  and  innumerable  a  procession 
of  stars,  to  which  it  forms  a  sort  of  climax,  justifying  expressions  which,  though  I  find  them 
written  in  my  journal  in  the  excitement  of  the  moment,  would  be  thought  extravagant  if 
transferred  to  these  pages.  In  fact,  it  is  impossible  for  any  one  with  the  least  spark  of 
astronomical  enthusiasm  about  him  to  pass  soberly  in  review,  with  a  powerful  telescope  and 
in  a  fine  night,  that  portion  of  the  southern  sky  which  is  comprised  between  6h  and  13h  of 
R  A,  and  from  146°  to  149°  of  N  P  D,  such  are  the  variety  and  interest  of  the  objects  he 
will  encounter,  and  such  the  dazzling  richness  of  the  starry  ground  on  which  they  are 
represented  to  his  gaze.* 

(83)  There  are,  however,  certain  features  to  which  it  is  necessary  to  refer  more  particularly 
in  illustration  of  our  figure.  It  must  be  observed  in  the  first  place,  that  in  no  part  of  its 
extent  does  this  nebula  show  any  appearance  of  resolvability  into  stars,  being  in  this  respect 
analogous  to  the  nebula  of  Orion.  It  has  therefore  nothing  in  common  with  the  milky  way, 
on  the  ground  of  which  we  see  it  projected,  and  may  therefore  be,  and  not  improbably  is, 
placed  at  an  immeasurable  distance  behind  that  stratum. 

(84)  The  whole  extent  of  the  nebulosity  to  the  south  is  somewhat  greater  than  can  be 
included  in  the  figure,  but  it  grows  so  faint  beyond  the  oval  vacuity  in  the  upper  part  that  I 
have  not  considered  it  necessary  to  trace  it  beyond  that  limit.  Nor  am  I  quite  sure  that  the 
south  following  portion  of  the  area  of  the  figure  in  which  no  nebula  is  represented  is  in  reality 
absolutely  free  from  it.  The  interior  of  the  oval  above  mentioned  is  perfectly  so.  It  is  also 
nearly  devoid  of  stars,  four  very  minute  ones  (inserted  in  their  proper  places  in  this  figure) 
Nos.  243,  268,  274,  278,  of  the  Catalogue  only  having  been  perceived  within  it.  Great 
attention  has  been  paid  to  exactness  in  the  situations  of  the  minute  stars  Nos.  229,  235,  237, 
239,  and  309  (C )  of  the  Catalogue,  which  mark  out  the  form  of  this  oval  with  respect  to  its 
borders.  The  two  large  stars  ir  and  a>  on  its  south  following  side  are  fairly  immersed  in  the 
nebula,  as  are  also  No.  225  (  =  jtr)  on  its  south  preceding,  and  Nos.  276  and  297  at  its  northern 
extremity. 

(85)  Close  to  the  great  star  A,  is  situated  that  singular  lemniscate-oval  vacuity  which 
forms  so  strange  a  feature  of  this  nebula.    Its  area  is  not  entirely  devoid  of  light.    A  thin 


*  The  first  three  hours  of  the  zone  thus  marked  out  are  remarkable  for  their  fine  double  stars.  Among  the 
nebulae  which  occur  from  9!  to  12\  we  have  at  &h  17",  147°  36',  the  beautiful  planetary  nebula  h.  3163,  a  perfect 
planet  in  appearance,  with  an  attendant  satellite;  at  10"  llm,  147°  8',  the  falcated  nebula  h.  3239 ;  at  10h  38°, 
148°  47',  v  Argus  with  its  nebula;  at  101'  58m,  147°  49',  the  superb  cluster  h.  3315;  at  11 » 42"',  146°  14',  the 
blue  planetary  nebula  h.  33G5,  a  most  exquisite  and  unique  object ;  and  at  12"  44-,  149°  26',  the  beautiful 
cluster  of  various  coloured  stars  about  k  Crucis  (h.  3435),  figured  in  PI  I.  fig.  2. 


NEBULA  AND  CLUSTERS  OF  STARS. 


39 


nebulous  veil  seems  as  if  extended  over  its  northern  loop  on  the  preceding-  side.  Four  stars, 
Nos.  686,  603,  589,  and  670  (=  [w])  of  the  Catalogue  are  placed  precisely  on  its  edges,  and 
will  serve  as  excellent  detectors  of  change  in  its  form,  should  any  occur.  The  stars  Nos.  607, 
(=  [t] )  664  (=  [v]),  and  616,  though  near  the  edge,  are  yet  fairly  immersed  in  the  nebula. 
On  the  other  hand  [u]  No.  634,  situated  in  the  contraction  of  the  oval  towards  its  middle, 
though  also  near  the  edge,  is  yet  fairly  within  the  vacancy,  and  so  situated  that  the  slightest 
shifting  of  the  nebulous  contour  at  its  preceding  side  cannot  fail  to  be  rendered  sensible.  In 
like  manner  also  the  exceedingly  well  defined  outline  of  the  nebulous  mass  in  which  the  cluster 
and  double  star  O  occur  (between  —  50s  and  —  100s  in  R  A,  and  —  1000  and  — 2000  Pts.  in 
NPD),  has  its  situation  admirably  identified  by  the  double  star  v  (Nos.  322,  323),  which  is 
situated  very  close  to,  but  yet  fairly  within,  its  preceding  edge :  the  edge  actually  passing 
between  v  and  an  extremely  minute  star  of  the  seventeenth  magnitude  (No.  318),  and  being 
moreover  marked  out  by  the  two  stars,  Nos.  333  and  342,  the  former  of  which  is  precisely  on 
it;  as  also  by  the  stars  No.  311  and  No.  299  =  (p)  the  former  considerably  within,  the  latter 
considerably  without  the  nebula,  whose  edge  passes  between  them,  a  little  nearer  to  No.  311 
than  to  (p).  Similarly  the  star  o,  No.  803,  and  o',  No.  813,  one  on  each  side  of  the  remarkable 
nebulous  projection  whose  co-ordinates  are  +  25s  and  —  2500  Pts.,  afford  means  of  ascer- 
taining any  relative  movement  in  this  part  of  it. 

(86)  In  the  catalogue  of  stars  occurring  in  this  nebula,  hereto  subjoined,  the  letters 
variously  marked  and  accented  which  occur  in  the  second  column  indicate  (with  a  few 
exceptions  of  stars  otherwise  remarkable)  those  stars  which  have  been  used  as  the  summits  of 
triangles  into  which  the  nebulous  area  was  divided  for  the  formation  of  the  working  skeletons. 
Among  these,  such  as  exceed  the  12th  magnitude,  and  some  also  of  that  and  even  of  inferior 
magnitudes  have  had  their  places  determined  by  differences  of  R  A  and  NPD  taken  with 
the  equatorial.  It  would  merely  multiply  superfluous  figures  to  state  the  particulars  of  these 
differential  measurements.  Suffice  it  to  say  that  upwards  of  a  thousand  such  differences,  viz. 
544  in  R  A,  and  474  in  N  P  D,  were  taken  with  great  care  on  the  nights  of  the  25th 
December,  1834;  February  24,  1835;  April  1,  4,16,  25,  26,  28,  May  5,  June  27,  28,  1836; 
April  27,  May  8,  9,  14,  16,  17,  28,  and  29,  1837— from  which  the  places  of  the  stars  of  the  1st 
class  in  the  Catalogue  (138  in  number)  were  derived.  On  the  28th  February,  and  the  1st  and 
2nd  March,  1834,  also  a  series  of  angles  of  position,  90  in  number,  was  taken  with  the  position 
micrometer  of  the  20-feet  reflector  which  when  projected  graphically  on  a  scale  sufficiently  large 
to  afford  the  requisite  exactness,  furnished  the  co-ordinates  of  about  50  stars.  About  20  of 
these,  not  being  included  already  in  class  1,  or  whose  co-ordinate  in  R  A  only  could  be 
determined  by  differential  observations,  owing  to  their  faintness  not  allowing  bisection  by  the 
declination  wires  of  the  equatorial,  have  the  class  2  annexed  to  them  in  the  Catalogue.  Their 
places  are  probably  correct  to  0\7  of  time  in  R  A,  and  to  6"  or  7"  in  N  P  D,  judging  from 
the  mean  errors  of  such  stars  determined  in  this  manner  as  are  included  in  class  1. 

(87)  Classes  3  and  4,  result  from  the  reading  off  and  reduction  of  the  skeleton-diagrams, 
the  stars  of  class  3  being  summits  of  triangles  of  the  second  order,  formed  by  breaking  up  the 
larger  triangles,  whose  extent  was  judged  to  be  too  great  to  allow  of  a  sufficiently  precise  filling 
in  by  eye-draft.  Those  of  class  4  are  stars  simply  mapped  down  and  read  off.  The  former, 
from  the  use  to  which  they  were  to  be  applied,  having  been  laid  down  probably  with  more 


40 


OBSERVATIONS  OF 


deliberate  care  than  the  latter,  they  are  classed  separately.  A  few  stars  of  class  3  have  their 
right  ascensions  differentially  observed. 

(S8)  The  filling  in  of  the  triangles,  both  as  regards  the  small  stars  they  include,  and  the 
course  and  graduation  of  the  nebula  within  their  respective  areas,  was  performed  in  the  only 
way  in  which  such  an  operation  is  practicable,  that  is  to  say  by  eye-draft,  unaided  by  any 
process  of  measurement  other  than  mental  comparison  with  the  sides  and  angles  of  the  triangles. 
The  nature  of  the  process,  as  well  as  that  of  the  reading  off  and  correction  of  the  places  of  the 
stars  so  mapped  down,  has  been  already  described  in  speaking  of  the  nebula  of  Orion  ;  but  as 
in  this  case  a  much  greater  number  of  stars  had  to  be  determined,  and  in  consequence  the 
occasions  of  observation  were  much  more  numerous,  it  frequently  happened  that  only  single 
triangles,  or  perhaps  two  or  three  adjacent  ones,  could  be  executed  at  once,  and  that  in 
several  instances  before  the  data  for  the  construction  of  complete  skeleton  charts  were 
accumulated.  Thus  several  triangles  came  to  be  mapped  down  more  than  once,  and  when 
afterwards  a  series  of  skeletons  of  sufficient  precision  was  executed,  it  was  considered 
advisable,  not  indeed  to  reject  all  the  former  work,  but  to  go  over  it  de  novo  wherever  it 
seemed  likely  to  be  defective.  Thus  it  happened  that  on  the  final  reading  off  and  assemblage 
of  the  places  of  the  stars  for  the  purpose  of  arranging  them  in  a  Catalogue,  among  the  stars 
not  included  in  classes  1  and  2,  218  were  found  to  have  been  determined  by  two  such  skeleton- 
readings,  55  by  3,  5  by  4,  and  1  by  5.  In  all  such  cases,  means  were  taken,  unless  where 
good  reason  was  found  for  rejecting  one  or  more  of  the  readings  as  influenced  by  some  obvious 
cause  of  error ;  but  of  this  there  are  few  instances,  and  in  the  vast  majority  of  cases  the  devia- 
tions even  of  the  extreme  readings  from  the  adopted  mean  were  found  to  be  of  trifling 
importance.  Taking  for  instance  the  extreme  deviations  in  N  PD  in  the  279  cases  above 
enumerated,  their  numbers  and  amounts  stand  classed  as  follows. 


Deviations  in  Micrometer  Parts, 
of  which  50  =  12". 


0  and  under 
10 
20 
30 
40 
50 
60 
70 
80 

1 00  and  upwards 


10 

20 
30 
40 
50 
60 
70 
80 
100 


Number  of  Instances. 

60 
63 
54 
39 
22 
16 
10 
4 
3 
8 


279 

(89)  To  the  operation  of  filling  in  the  triangles,  and  otherwise  delineating  the  general 
aspect  or  minuter  particulars  of  the  nebula,  the  following  nights  were  wholly  or  partially 
devoted.  February  27,  28,  March  1,  2,  December  25,  1834;  April  15,  May  11,  June  7,  8,  10, 
14,  17,  21,  July  8,  1836;  April  24,  28,  29,  30,  May  1,  4,  6,  December  21,  22,  1837.  Angles 
of  position  were  also  measured  of  small  companions  near  the  central  star  in  sweeps  432,  433, 
434,  435  on  the  nights  of  March  14,  16,  31,  and  April  1,  1834. 


NEBULAE  AND  CLUSTERS  OF  STARS.  41 

(90)  The  magnitudes  assigned  to  the  stars  in  the  Catalogue  are  means  of  all  which  have 
been  found  ascribed  to  them  in  any  recorded  observation  or  diagram.  Some,  it  will  be 
observed,  are  noted  as  double.  A  summary  of  their  angles  of  position  and  distances 'is  contained 
m  the  following  Table. 


iNo.  in 
Catal. 

Letter. 

Mag. 

Angle  of 
Position. 

Distance 
measured  or 
estim. 

ARA. 
Sec.  Dec. 

ANPD. 
Pts.  Dec. 

Epoch. 

361 
37  J 

(g) 

10,12 

3o6°.4 

5"-4  skel. 

—0.56 

-'3-33 

1837.65 

451 
4-6/ 

P 

10,12 

352.8 

7".  10  skel. 

—0. 1 1 

—  29.26 

1837.71 

2361 
238J 

S 

8,15 

sf 

skel. 

+  0.  3 

+45 

1837 

3221 
323  J 

W 

13.13 

179.8 

3  est. 

+  0.00 

+  12.48 

1837.76 

354 1 
361/ 

z 

11,12 

226.7 

1 5".  1  skel. 

— 1.42 

+43.21 

1837.48 

37°  1 
381/ 

t 

I  1,12 

79-5 

15  -4  skel. 

-t-I.90 

—  11.75 

1837.34 

403-1 

404  L 
395  J 

0 

8,IO 

8,.. 

150.3 
309.3 

z\  est. 
10  est. 

-f-0. 10 

—0.97 

+  94° 
-26.35 

1837.02 
1837.97 

426 1 
430/ 

p 

9>»5 

156.2 

1 1.5  skel. 

+0.60 

+43-  5 

1837.34 

429-, 
434  J 

Z" 

9'1 1 

236.4 

7 ".8  skel. 

— 0.84 

4  J7-99 

is37-2o 

4331 
435/ 
4521 

Z' 
K1 

9,11 
8,  8 

199.3 
108.0 

8"-4  skel. 
13.4  meas. 

—0.36 

+1.64 

+  33-03 
+  17.22 

1837.22 
1836.30 

455  > 
458  J 

K2 

9=9 

116. 9 

2.4  nieas. 

+0.28 

+  4.66 

1836.89 

4681 
490/ 

C 

8,12 

sf 

skel. 

+  3.  2 

+96 

1837 

476-1 
486/ 

(P) 

10,17 

sf 

skel. 

+  '•  3 

+  30 

1837 

57n 

575  J 

D 

8,  9 

213.6 

17.9  meas. 

—  1.28 

462.02 

1836.91 

5971 
601/ 

1 1, 1 1 

199.4 

i3".8  skel. 

-0.59 

+  54-3° 

!837-34 

6181 
619/ 

r 

8,  9 

35i-8 

6.7  meas. 

—  0.12 

-27.59 

1837.03 

7231 
728  I 
730J 

A 

1,12 

46.8 
32.1 

12  est. 
14  est. 

+  I.I3 
+  O.96 

-34-J7 
-49-34 

1834.20 
Do. 

8621 
867/ 

|3 

8,12 

41.6 

13.2  skel. 

+  I.I4 

-40.91 

1837.76 

9181 
926  J 

m 

+  1.  3 

-78 

1836.... 

1013-1 
1018/ 

a 

10,13 

35-8 

17.8 

+  I-34 

—60.02 

1837.97 

1215-1 
1216  J 

e 

8,10 

115. 2 

9.1  meas. 

+  1.06 

+  16. 12 

1836.31 

M 


42 

A  GENERAL  CATALOGUE  OF  THE  STARS 
Known  to  exist  in  the  area  occupied  by  the  great  Nebula  about  r)  Argus,  within  the  limits  of  Right 
Ascension  and  Polar  Distance  comprised  in  the  Monograph  Chart. 


(N.B. — Interlined  words  refer  to  the  Star  immediately  above  them.) 


ARA 

ANPD 

ARA 

ANPD 

ARA 

ANPD 

from  J7 

from  rj 

o5 

til 

from  77 

from  t) 

from  Tj 

from  7} 

No. 

Letter. 

g 

Argus. 

X 

Sec.  Dec. 

Argus. 

y 

Micro.  Pts. 

cn 

s 

No. 

Letter. 

a 

Argus. 

X 

Sec.  Dec. 

Argus. 

y 

Micro.  Pts. 

Class 

No. 

Letter. 

Argus. 

X 

Sec.  Dec. 

Argus. 

y 

Micro.  Pts. 

Class 

i 

L 

7 

-224.5 

+4394 

I 

62 

*4 

-161.5 

+23°i 

4 

125 

15 

—  138.0 

+  6700 

4 

2 

X 

7 

—  22C.6 

-  35 

I 

63 

16 

— 161. 3 

+7889 

4 

126 

15 

-I37-S 

4-8341 

4 

3 

[b] 

12 

—  209.O 

+  732 

3 

64 

11 

— 160.3 

+  51 12 

4 

127 

16 

-136.8 

+3593 

4 

4 

e" 

11 

—  203.O 

+2408 

3 

65 

J3 

-J59-7 

+  6143 

4 

128 

16 

—  136.7 

+5992 

4 

5 

10 

—202.8 

-  253 

1 

66 

12 

-158.6 

4-5H8 

4 

129 

(0') 

10 

-136.6 

4-8057 

1 

6 

1 1 

-I98.7 

+3974 

4 

67 

15 

-158.5 

+4198 

4 

130 

16 

-136.3 

4-4908 

4 

7 

12 

—  I97.O 

+  3939 

4 

68 

!3 

-158.5 

+7055 

4 

131 

15 

—  136.2 

+6658 

4 

8 

M 

-I94.O 

+  1574 

4 

69 

14 

-158.3 

4-5032 

4 

132 

16 

—  1 36. 1 

+4282 

4 

9 

'3 

-I9I.9 

+  1363 

3 

70 

16 

-157-5 

+  8425 

4 

133 

15 

—  1 36.0 

+6566 

4 

IO 

1 

—  186.5 

+54U 

1 

71 

16 

-!57-4 

+7680 

4 

134 

16 

-135.8 

4-4928 

4 

ii 

00 

15 

—  185. 1 

+2300 

4 

72 

12 

-I57-I 

+4059 

4 

135 

13 

-135-4 

+  5942 

4 

12 

10 

-183.9 

+  84 

1 

73 

'5 

-157.1 
-156.7 

4-2572 

4 

136 

(e) 

9 

-135-3 

+3327 

1 

'3 

16 

-183.O 

+2598 

4 

74 

15 

+4668 

4 

137 

12 

-134.8 

+  5075 

4 

*4 

12 

—  182.O 

+  3804 

4 

75 

13 

-155-5 

+  6443 

4 

138 

15 

-134-5 

+4898 

4 

*5 

l6 

— 181.9 

+2875 

4 

76 

»4 

-155.2 

4-2542 

4 

139 

15 

-134-5 

4-6027 

4 

16 

12 

—  l8l. 5 

+  3894 

4 

77 

12 

-155.0 

+  7983 

4 

140 

13 

—  134.4 

4-8916 

4 

»7 

12 

—  l8l.O 

+  3944 

4 

78 

15 

-154.9 

+  8479 

4 

141 

14 

-134-3 

4-8606 

4 

18 

l6 

—  180.9 

+  5226 

4 

79 

16 

-154.9 

+  5894 

4 

142 

(0 

10 

-133-8 

+2842 

1 

*9 

14 

— 180.8 

+333° 

4 

80 

16 

-153-7 

+  5690 

4 

143 

15 

-133.8 

+  7794 

4 

20 

r 

IO 

—  179.6 

4-2270 

1 

81 

H 

-153.6 

+  2284 

4 

144 

14 

-133-1 

4-4908 

4 

21 

l6 

-178.3 

+  5"74 

4 

82 

15 

-*53-3 

+  8790 

4 

145 

16 

-133.0 

-j-9068 

4 

22 

14 

—  178.2 

+  3*45 

4 

83 

z" 

11 

-153.1 

+  254 

3 

146 

16 

— 132.6 

4-8444 

4 

23 

13 

-177.7 

4-3620 

4 

84 

J3 

—  152.4 

+  8I34 

4 

147 

(0) 

9 

—  132.2 

+7759 

1 

24 

l6 

-177.1 

+  5°73 

4 

85 

15 

-152.1 

+  8660 

4 

148 

14 

— 132. 1 

-1645 

4 

*5 

l6 

—  176. 1 

+  5384 

4 

86 

13 

-i5i-3 

+  6667 

4 

149 

13 

-132.1 

4-8556 

4 

26 

15 

-175-7 

+  337° 

4 

87 

15 

-151.2 

4-6727 

4 

150 

16 

-131-7 

+9058 

4 

27 

a" 

l6 

-175-5 

-j-2621 

4 

88 

16 

—  150.8 

+  5594 

4 

151 

16 

-13I-5 

+  7769 

4 

28 

9 

-175-4 

4-6931 

1 

89 

13 

— 150.2 

4-4852 

4 

152 

15 

-I3I-3 

+7799 

4 

29 

16 

-175-3 

4-4100 

4 

90 

13 

—  150.2 

+  3793 

4 

153 

13 

—  130.6 

+  3119 

4 

30 

'5 

-175.0 

+  348o 

4 

91 

13 

-150.1 

4-5058 

4 

154 

14 

—  130.5 

-f-9288 

4 

31 

(h) 

15 

— 174.1 

+  3542 

4 

92 

12 

— 150.0 

+  5360 

4 

155 

16 

—  1 30. 1 

+9153 

4 

32 

12 

-173.6 

+  3io4 

1 

93 

13 

-148.6 

+6553 

4 

156 

14 

— 130.1 

+  5914 

4 

33 

h~ 

9 

— 172.6 

—5227 

1 

94 

l6 

-148.3 

+  335° 

4 

157 

14 

—  129.9 

+7292 

4 

34 

15 

—  172.2 

4-6831 

4 

95 

w 

8 

—  148.0 

—  1332 

1 

158 

17 

—  129.8 

—  1777 

4 

35 

16 

-i7i-3 

+  5301 

4 

96 

15 

—  J47-7 

4-7722 

4 

159 

14 

—  129.8 

—2180 

4 

36 

(a\  \ 

12 

— 171.0 

+  336* 

4 

97 

15 

—  147.6 

+8010 

4 

160 

14 

—  129.5 

+9273 

4 

37 

9 

-170.4 

+3375 

1 

98 

11 

—  146.9 

+  5393 

4 

161 

15 

— 129.0 

— 1813 

4 

38 

double 

99 

f 

12 

-146.4 

4-1098 

3 

162 

15 

—  128.4 

+  3641 

4 

13 

-169.3 

4-4294 

4 

100 

15 

—  146. 1 

+7717 

4 

163 

16 

—  128.4 

+  5248 

4 

39 

15 

—  168.9 

+  5r39 

4 

101 

14 

-H5-7 

+8204 

4 

164 

13 

—  128.4 

+6381 

4 

40 

»3 

-168.6 

4-6641 

4 

102 

16 

-145-7 

+  3379 

4 

165 

x" 

1 1 

—  128.4 

-3498 

3 

41 

15 

-168.3 

+7949 

4 

103 

12 

-145.6 

+2265 

4 

166 

14 

-128.2 

4-6270 

4 

42 

—  168.2 

+5°49 

4 

104 

16 

-H5-3 

+  8S24 

4 

167 

16 

—  127.8 

+86oa 

4 

43 

16 

-167.8 

+35*7 

4 

i°5 

16 

-H5-3 

+  8749 

4 

168 

15 

—127.7 

+7757 

4 

44 

'i 

14 

—  167.7 

+  5169 

4 

106 

12 

-144.7 

+  7558 

4 

169 

15 

— 127.1 

+57I3 

4 

45 

12 

— 167.6 

4-4240 

4 

107 

14 

-144.5 

-1517 

4 

170 

15 

— 126.9 

+7198 

4 

46 

10 

—  167.5 

4-4269 

1 

108 

16 

-144.2 

+  8607 

4 

171 

15 

-126.8 

+7138 

4 

double 

109 

12 

—  144. 1 

-f-1340 

172 

16 

-126.8 

4-8856 

4 

47 

12 

— 167.0 

+6836 

4 

no 

15 

—  144-1 

+  8492 

173 

14 

-126.5 

4-8049 

4 

48 

00 

>3 

—  166.8 

+6701 

4 

1 1 1 

16 

-144.0 

+4973 

4 

174 

16 

-126.3 

4-5210 

4 

49 

11 

-166.6 

+  8425 

1 

112 

H 

-143.6 

+93°4 

1 

175 

15 

-125.9 

+  375I 

4 

5° 

13 

—  166.4 

+  3703 

4 

"3 

16 

-H3-5 

4-4882 

4 

176 

13 

-125.7 

4-6981 

4 

5' 

14 

-166.3 

+  5°49 

4 

114 

11 

— 142.6 

4-4667 

4 

177 

15 

— 125.2 

+  36-6 

4 

52 

16 

— 166.3 

4-5261 

4 

IT5 

15 

-142.5 

+  3697 

4 

178 

13 

-125.1 

+S6S3 

4 

53 

16 

-166.1 

+  3400 

4 

116 

k 

10 

— 142.2 

+  5421 

1 

179 

14 

—  124.9 

—2042 

4 

54 

14 

—  165.8 

4-4800 

4 

117 

z 

12 

— 142.2 

-2943 

3 

180 

e 

9 

—  124.7 

+5554 

1 

55 

13 

—  165.0 

4-5166 

4 

118 

12 

-I41-4 

+2644 

4 

181 

q 

10 

-124.6 

+4331 

1 

56 

11 

—  164.3 

+  7432 

4 

119 

16 

—  140.3 

+4275 

4 

182 

16 

-124.5 

+9197 

4 

57 

15 

— 163. 1 

4-4820 

4 

120 

v" 

12 

-139.8 

4-2015 

3 

183 

-124.5 

+4955 

4 

58 

13 

— 163.0 

+  8355 

4 

121 

11' 

-138.8 

4-2704 

4 

184 

15 

—  124.3 

—  108 

4 

59 

13 

—  162.8 

4-6756 

4 

122 

J3 

-138.6 

+  5082 

4 

185 

15 

—  124.2 

+7742 

4 

60 

14 

— 162.4 

+  6133 

4 

123 

14 

-138.4 

— 2771 
+4364 

4 

186 

14 

—  123.7 

-2234 

4 

61 

16 

-161. 8 

+7402 

4 

124 

16 

—  138.2 

4 

187 

16 

-123.3 

4-4184 

4 

A  GENERAL  CATALOGUE  OF  THE  STARS  IN  THE  GREAT  NEBULA. 


43 


ARA 

ANPD 

ARA 

ANPD 

ARA 

ANPD 

C3 

from  r} 

from  1) 

V, 

from  rj 

from  t] 

w 

from  rj 

from  Tj 

DO 

No. 

Letter. 

Argus. 

Argus. 

J. 

No. 

Letter. 

Argus. 

Argus. 

c§ 

No. 

Letter. 

Argus. 

Argus. 

X 

y 

X 

y 

0 

X 

y 

3 

Sec.  Dec. 

Micro.  Pts. 

Sec.  Dec. 

Micro.  Pts. 

Sec.  Dec. 

Micro.  Pts. 

188 

— 

—  123. 1 

-3698 

4 

259 

16 

— 101.7 

—  1940 

4 

327 

15 

-  79-8 

+  5413 

4 

189 

15 

—  122.8 

—  2481 

4 

260 

16 

— 101.5 

+  5983 

4 

328 

16 

—  79-7 

+  3694 

4 

190 

p" 

12 

—  122. 1 

+  6693 

1 

261 

7r" 

9 

— 101.4 

+  6757 

1 

329 

14 

—  79-5 

46090 

4 

191 

15 

— 121.7 

-I-4116 

4 

262 

14 

— 101.4 

—  1446 

4 

330 

14 

-  78.3 

—2814 

4 

192 

16 

-121.5 

+  9776 

4 

263 

15 

—  I0I.2 

4  484 

4 

33i 

12 

—  78.2 

47831 

4 

193 

16 

—  121. 5 

+  7809 

4 

264 

16 

— 101. 0 

43623 

4 

332 

1  I 

—  78.0 

— 2033 

4 

194 

14 

— 121. 2 

+  6000 

4 

265 

16 

—  IOO.9 

+  59H 

4 

333 

16 

-  77*8 

— 1205 

4 

195 

12 

— 120.6 

+  8327 

4 

266 

14 

—  I00.8 

+4433 

4 

334 

15 

-  77*7 

-3204 

4 

196 

l6 

—  120.6 

+4203 

4 

267 

12 

—  100.6 

+  3995 

4 

335 

12 

—  77.6 

47163 

4 

197 

l6 

—  120.6 

+  7882 

4 

268 

16 

—  IOO.5 

48483 

4 

336 

17 

—  77*2 

42971 

4 

198 

16 

— 120.5 

+4471 

4 

269 

16 

—  I00.2 

41421 

4 

337 

N 

10 

—  76*5 

41828 

1 

199 

l6 

— 120.4 

+4406 

4 

270 

15 

-  99-8 

44900 

4 

338 

l6 

—  76.4 

+  5542 

4 

200 

g" 

9 

— 120.2 

—  5120 

1 

27 1 

15 

—  99-6 

45058 

4 

339 

15 

—  76*4 

—  3154 

4 

201 

16 

— 120.2 

+4356 

4 

272 

14 

—  99-4 

44065 

4 

34° 

17 

-  76.3 

-  "5 

4 

202 

14 

—  II9-9 

-3858 

4 

273 

*3 

-  98*9 

47790 

4 

34i 

14 

—  76*3 

47027 

■  4 

203 

16 

—  II9-9 

49761 

4 

274 

16 

-  98.9 

48448 

4 

342 

l6 

—  76.0 

—  1 167 

4 

204 

16 

— 119. 6 

+  3575 

4 

275 

—  98.8 

41483 

4 

343 

n 

IO 

-  75-5 

4  3016 

1 

205 

1 1 

—  II9-5 

+2740 

4 

276 

1 1 

-  98*4 

+  7954 

4 

344 

y" 

8 

—  75-5 

+9843 

1 

206 

15 

-118. 8 

4-4141 

4 

277 

15 

-  98.2 

+  6757 

4 

345 

16 

—  74*7 

49000 

4 

207 

16 

-118.2 

+  3765 

4 

278 

16 

—  96*4 

48925 

4 

346 

14 

—  74*7 

-1833 

4 

208 

15 

— 117. 6 

+42 1 1 

4 

279 

14 

—  96.1 

44552 

4 

347 

14 

-  74-6 

48280 

4 

209 

16 

— 117.5 

44689 

4 

280 

14 

—  95-9 

46871 

4 

348 

15 

—  74*6 

46739 

4 

210 

14 

—  II7-3 

+  8475 

4 

281 

12 

—  95-3 

42948 

4 

349 

J7 

—  74*5 

—2143 

4 

211 

12 

117*1 

42952 

4 

282 

M 

I  I 

—  95-i 

—  880 

1 

350 

17 

—  74*5 

+  3352 

4 

212 

12 

117*1 

+4835 

4 

283 

l6 

—  95-1 

—2087 

4 

351 

14 

—  73*9 

—2739 

4 

213 

16 

— 117. 0 

+7697 

4 

284 

15 

-  94*8 

—4477 

4 

352 

17 

-  73.8 

—  3° 

4 

214 

rj" 

13 

—  1 17.0 

48670 

1 

285 

14 

—  94-6 

-1-7909 

4 

353 

13 

—  73*7 

46824 

4 

215 

-116.6 

-3988 

4 

286 

l6 

—  94*6 

+  5337 

4 

354 

Z'" 

12 

—  73*4 

46252 

4 

216 

16 

—  1 16.3 

+  34°3 

4 

neb 

dou- 

ble 

217 

15 

—  1 16.3 

+  353 

4 

287 

15 

—  94*i 

+  1195 

4 

355 

15 

—  72.9 

+  5873 

4 

218 

10 

— 116. 2 

+  5932 

4 

288 

l6 

—  94.0 

44241 

4 

356 

l6 

—  72.8 

+  8935 

4 

219 

13 

-116.1 

42690 

4 

289 

l6 

—  93.5 

—  1340 

4 

357 

16 

—  72.8 

—2118 

4 

220 

14 

— 116. 0 

46841 

4 

290 

l6 

—  93*4 

45302 

4 

358 

"3 

—  72.2 

+  659 

4 

221 

16 

-115.6 

44624 

4 

neb 

359 

15 

—  72.0 

+  3851 

4 

222 

— 115.4 

48292 

4 

291 

01 

7 

—  93.0 

4-9715 

1 

360 

14 

—  72.0 

—  1723 

4 

223 

15 

—  1 14.0 

+7485 

4 

292 

c 

10 

—  92*4 

46215 

1 

361 

Z'" 

1 1 

—  72.0 

46209 

4 

224 

15 

—  II3-3 

46775 

4 

293 

X 

1 1 

—  9i*7 

—2874 

1 

dou- 

ble 

225 

n" 

14 

— 112.8 

49876 

3 

294 

16 

—  91.0 

-1788 

4 

362 

15 

—  7i-9 

42381 

4 

226 

15 

—  1 12. 1 

4-7927 

4 

295 

16 

—  90.6 

46120 

4 

363 

12 

—  7i-9 

47601 

4 

227 

13 

—  1 1 1 .3 

49253 

3 

296 

15 

—  90.3 

46781 

4 

364 

15 

—  7i-9 

+  5796 

4 

228 

15 

—  1 10.8 

47560 

4 

297 

12 

—  9°*3 

48008 

4 

365 

12 

—  71*7 

+6957 

4 

229 

16 

— 110.6 

4-9353 

4 

298 

15 

—  89.8 

+  7J9 

4 

366 

15 

—  71*5 

48850 

4 

230 

15 

—  1 10.2 

46821 

4 

299 

(9) 

1 1 

—  89.5 

—  1456 

1 

367 

l6 

—  7i-5 

—  972 

4 

231 

— 110.0 

48472 

4 

300 

7T 

7 

—  89.4 

49469 

1 

368 

14 

—  71.4 

+  5175 

4 

232 

16 

—  109.4 

42930 

4 

301 

*4 

—  89.2 

47006 

4 

369 

14 

—  71.2 

46405 

4 

233 

15 

—  109.4 

+  8557 

4 

302 

1 5 

-  88.7 

42403 

4 

370 

t 

1 1 

—  71.2 

44079 

1 

234 

d 

10 

— 109. 1 

45295 

1 

303 

12 

-  88.6 

+  5601 

4 

dou- 

ble 

235 

S 

15 

-108.8 

+  8597 

4 

3°4 

14 

-  88.1 

—  443 

4 

37i 

—  70.8 

+  6479 

4 

236 

8 

—  108.7 

+  859 

1 

305 

15 

—  88.0 

44742 

4 

372 

(a) 

13 

—  70.7 

47276 

4 

237 

S' 

13 

—  108.5 

+8245 

4 

306 

15 

-  87.9 

46800 

4 

373 

I  I 

—  70.6 

45699 

4 

238 

15 

—  108.4 

+  9°4 

4 

307 

l6 

—  87.6 

+4558 

4 

374 

16 

—  70.4 

42331 

4 

239 

J4 

—  108. 1 

48988 

4 

308 

l6 

—  86.5 

43961 

4 

375 

16 

—  70.2 

— 2023 

4 

240 

15 

—  107.9 

48776 

4 

309 

r 

I  I 

—  86.1 

48761 

1 

376 

13 

—  70.2 

—2 108 

4 

241 

w" 

!3 

-107.4 

-2395 

3 

310 

lS 

-  85.9 

46991 

4 

377 

13 

—  70.0 

-1883 

4 

242 

13 

—  106.5 

48000 

4 

311 

15 

-  85.4 

-1553 

4 

378 

12 

-  69-9 

45030 

4 

243 

16 

—  106.4 

48484 

4 

312 

13 

-  85.3 

+  5699 

4 

379 

13 

-  69-9 

+  5297 

4 

244 

16 

-105.1 

+  3441 

4 

3i3 

14 

-  85.2 

-2854 

4 

380 

16 

-  69*5 

45861 

4 

245 

16 

—  104.9 

— 2215 

4 

3i4 

13 

—  85.0 

46058 

4 

381 

t' 

12 

—  69.2 

44067 

4 

246 

16 

-104.5 

+  7815 

4 

3i5 

16 

-  84.4 

49285 

4 

382 

I  I 

—  69.0 

— 2013 

4 

247 

12 

—  104.4 

46632 

4 

316 

15 

—  84.2 

41450 

4 

383 

14 

—  69.0 

-1923 

4 

248 

16 

—  104.4 

+  5077 

4 

3i7 

-  83.5 

4  906 

4 

384 

15 

-  68.7 

48215 

4 

249 

16 

-104.3 

—2987 

4 

318 

17 

—  83.2 

— 1269 

4 

385 

13 

-  68.5 

-r573 

4 

250 

T 

10 

— 104.1 

42548 

1 

319 

15 

—  83.0 

—  53° 

4 

386 

16 

—  68.5 

46410 

4 

251 

16 

— 104.0 

+  5978 

4 

320 

14 

—  82.6 

+  534i 

4 

387 

Z 

6 

—  67.9 

46499 

1 

252 

<P 

8 

-103.5 

47760 

1 

321 

0)  \ 

13 

-  82.2 

+3549 

4 

388 

13 

—  67.7 

—2063 

4 

253 

16 

-103.3 

— 1241 

4 

322 

13 

—  81.0 

— 1290 

1 

389 

14 

—  67.7 

+  5"4 

4 

254 

16 

— 103.0 

42809 

4 

323 

13 

—  81.0 

— 1302 

1 

390 

14 

—  67.6 

-1748 

4 

255 

iS 

— 103.0 

+  1945 

4 

dou- 

ble 

391 

16 

-  67.5 

45912 

4 

256 

16 

— 102.4 

— 2098 

4 

324 

15 

—  80.9 

44610 

4 

392 

13 

—  67.4 

+  775° 

4 

257 

14 

— 102.2 

+4547 

4 

325 

15 

-  80.7 

46065 

4 

393 

13 

-  67.3 

-4067 

4 

258 

16 

— 101.9 

4  299 

4 

326 

17 

—  80.1 

—  670 

4 

394 

16 

-  67.1 

42109 

4 

A  GENERAL  CATALOGUE  OF  THE  STARS  IN  THE 


ARA 

ANPD 

ARA 

ANPD 

ARA 

ANPD 

to 

tS 

from  tj 

from  r) 

be 

from  jj 

from  rj 

>j 

to 

from  rj 

from  t] 

• 

No. 

Letter. 

Argus. 

Argus. 

No. 

Letter. 

Argus. 

Argus. 

09 

No. 

Letter. 

Argus. 

Argus. 

S 
0 

X 

Sec.  Dec. 

y 

Micro.  Pts. 

0 

z 

Sec.  Dec. 

y 

Micro.  Pts. 

6 

X 

Sec.  Dec 

y 

Micro.  Pts. 

395 

14 

-  66.5 

—  2049 

4 

459 

1 1 

-  53-7 

-3863 

4 

527 

14 

-  37-3 

-3013 

4 

396 

14 

-  66.6 

— 1813 

4 

doubt- 

ful 

528 

17 

-  36.8 

44187 

4 

397 

[L] 

14 

-  66.0 

—  445 

2 

460 

16 

-  53-6 

+3106 

4 

529 

13  : 

—  36.1 

-1755 

4 

398 

b" 

8 

-  66.0 

+9609 

1 

461 

15 

-  53-4 

+  28 

4 

530 

H 

-  35-9 

4 1230 

4 

399 

»4 

-  65.8 

+6327 

4 

462 

16 

-  53-4 

+7459 

4 

531 

H 

11 

-  35-9 

0 

1 

400 

16 

-  65.8 

+  1679 

4 

463 

'3 

-  53-3 

— 2670 

4 

532 

14 

-  35-6 

-3140 

4 

401 

12 

-  65.6 

+  7444 

4 

464 

!3 

—  53-3 

+  8689 

4 

533 

12 

-  35-4 

—4862 

4 

402 

J3 

-  65.6 

— 1813 

4 

465 

15 

—  53-° 

+7309 

4 

534 

15 

-  35-1 

—  1 124 

4 

403 

c 

°) 

-  65-5 

— 202.3 

1 

466 

16 

—  52-7 

+  i855 

4 

535 

to" 

10 

-  34-7 

+  79°4 

1 

7 

dou- 

ble 

467 

13 

—  52-4 

+4900 

4 

536 

[p] 

15 

—  34-7 

-  137 

2 

404 

I 

—  65-3 

— 2014 

2 

468 

C 

8 

-  51.6 

+  539 

1 

537 

17 

—  34-4 

+  5695 

4 

405 

15 

—  65.2 

—2348 
-3817 

4 

dou- 

ble 

538 

15 

—  34-3 

41786 

4 

406 

1 1 

—  65.2 

4 

469 

16 

—  51.4 

+  6360 

4 

539 

16 

—  34-3 

+  675 

4 

doubt- 

ful  star 

470 

15 

—  51.2 

+  1761 

4 

540 

Q 

9 

—  34-2 

43003 

1 

407 

10 

—  64.2 

+  6130 

4 

47i 

16 

—  51.2 

+43*8 

4 

54i 

16 

-  34-i 

—  1890 

4 

408 

14 

—  64.1 

—  1973 

4 

472 

J7 

—  51.0 

—  i860 

4 

542 

16 

—  33-9 

4  680 

4 

409 

14 

—  64.0 

-1878 

4 

473 

17 

—  5°-9 

+  2546 

4 

543 

14 

-  33-8 

+  358 

4 

410 

r4 

—  63.9 

— 2098 

4 

474 

16 

—  50.7 

+  7398 

4 

544 

r3 

—  33-7 

-2571 

4 

411 

>4 

-  63.8 

+  ^91 

4 

475 

12 

—  50.5 

-(-2906 

4 

545 

r3 

—  33-6 

4 1042 

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4 

728 

13 

4-  1.0 

-  49 

2 

799 

+  J 

7-9 

-3615 

4 

659 

17 

-  12.5 

+  1470 

4 

729 

15 

+  1.0 

+2207 

4 

800 

+  1 

8.0 

—  214 

4 

660 

14 

—  12.2 

+  4*5 

4 

730 

12 

+  1.1 

-  34 

2 

801 

+  1 

8.0 

+  1048 

4 

661 

15 

—  12.2 

-4558 

4 

731 

H 

4-  1.2 

+  8858 

4 

802 

+  1 

8.4 

— 1814 

4 

662 

-  11. 8 

+  3354 

4 

732 

13 

+  1.3 

4-2971 

4 

803 

0 

+  J 

9.0 

+  2400 

1 

N 


4fi 


A  GENERAL 


CATALOGUE  OF  THE  STARS 


IN  THE 


ARA 

ANPD 

ARA 

ANPD 

ARA 

ANPD 

No. 

Letter. 

si 

from  jj 

from  t] 

hfj 
cS 

from  r\ 

from  jj 

cS 

from  jy 

from  jj 

5! 

Argus. 

Argus. 

3 

No. 

Letter. 

Argus. 

Argus. 

m 
OB 
CS 

No. 

Letter. 

Argus. 

Argus. 

CO 

cd 

X 

Sec.  Dec 

y 

Micro.  Pts. 

0 

X 

Sec.  Dec 

y 

Micro.  Pts. 

X 

Sec.  Dec 

y 

Micro.  Pts 

5 

804. 
805 

600 
807 

»5 

4-  19.2 

4-  340 

4 

874 

14 

+  S°-i 

-1255 

4 

940 

13 



+  63-9 



-3115 

4 

15 

+  i9-2 

4-4366 

4 

875 

14 

+  5°-2 

-1237 

4 

941 

14 

+  63-9 

+  6094 

4 

17 

+  19-5 

+  946 

4 

876 

14 

+  5°-3 

-1394 

4 

942 

13 

+  641 

-  655 

4 

13 

+  21-4 

4-3065 

4 

877 

12 

+  5°-4 

4-6092 

4 

943 

14 

+  64.1 

+  2838 

4 

808 

14 

+  21-4 

+  5312 

4 

878 

12 

+  5°-5 

+4778 

4 

944 

16 

+  64.2 

4-3841 

4 

809 
0  10 

13 

4-  21.7 

-3140 

4 

879 

1 1 

+  5°-7 

-f-5962 

4 

945 

15 

+  64-5 

—  3630 

4 

17 

+  23.1 

-  718 

4 

880 

15 

+  5»-° 

4-4708 

4 

946 

16 

+  649 

-  65 

4 

811 

16 

4-  23.8 

+  122 

4 

881 

IS 

+  5i-5 

— 4622 

4 

947 

15 

+  65.2 

+  1775 

4 

812 

nt 

14 

+  23-8 

—  3681 

4 

882 

16 

+  5i-6 

+  1333 

4 

948 

+  65.2 

4-4888 

4 

813 

8  14 

0 

13 

+  24.0 

+  2665 

4 

883 

14 

+  52-o 

+  1901 

4 

949 

15 

+  65.5 

4-3867 

4 

+  24-3 

+  5379 

4 

884 

15 

+  52-i 

-4143 

4 

950 

+  65-7 

+  1418 

4 

8l5 
8l6 

13 

4-  24.8 

+  5564 

4 

885 

12 

+  52-6 

+  3982 

4 

95i 

1 1 

+  65-9 

—4601 

4 

16 

+  25-5 

-3951 

4 

886 

15 

4-  52.6 

— 1402 

4 

952 

14 

+  66.3 

—  3130 

4 

817 
8l8 

16 

+  25.5 

+  55 

4 

887 

15 

+  52-9 

+  1333 

4 

953 

S 

8 

+  66.7 

-5486 

1 

15 

+  27.4 

+  1936 

4 

888 

14 

+  53-1 

—  2264 

4 

954 

15 

+  67.6 

+4778 

4 

819 
82O 
821 
822 

823 

16 

+  27.6 

+  4DI 

4 

889 

12 

+  53-6 

-4153 

4 

955 

n" 

12 

+  67.7 

+  1274 

1 

IS 

+  27-8 

4-3701 

4 

890 

14 

+  54-i 

+  5374 

4 

956 

16 

+  67.9 

—  132 

4 

16 

4-  28.8 

—  60 

4 

891 

15 

+  54-6 

—  3 162 

4 

957 

13 

+  67.9 

+4922 

4 

1 5 

+  29.5 

+4584 

4 

892 

12 

+  54-7 

+  6163 

4 

958 

14 

4-  68.0 

+  1470 

4 

s 

13 

+  29.7 

+  1520 

2 

893 

15 

+  54-8 

-1530 

4 

959 

1 1 

4-  68.4 

-4513 

4 

024 

825 

820 
827 

V 

12 

4-  29.9 

+  6119 

4 

doubt- 

ful 

960 

12 

4-  68.8 

4-5891 

4 

10 

+  3°-7 

+4077 

1 

894 

13 

+  55-o 

+  39J7 

4 

961 

16 

+  69.2 

-3370 

4 

15 

+  3r-° 

4-  687 

4 

895 

14 

+  55-i 

+  5897 

4 

962 

12 

4-  69.8 

— 2129 

4 

14 

+  3i-8 

— 1005 

4 

896 

l6 

+  55-2 

-3534 

4 

963 

15 

+  7°-3 

4-4836 

4 

828 
829 
83O 

14 

+  32-o 

—  908 

4 

897 

13 

+  56-1 

+  1239 

4 

964 

w 

10 

+  7°-3 

+4660 

1 

14 

+  32-6 

— 1851 

4 

898 

13 

+  56-3 

+4042 

4 

965 

13 

4-  71-1 

+  5991 

4 

16 

+  32-6 

+  35° 

4 

899 

15 

+  56-6 

-3198 

4 

966 

1 1 

+  7i-3 

4-2175 
-  487 

4 

83I 

14 

4-  32-7 

+  1745 

4 

900 

13 

+  56.6 

+  5374 

4 

967 

12 

+  72.6 

4 

832 

13 

+  32-7 

4-4690 

4 

901 

IS 

+  56.7 

+2075 

4 

968 

15 

+  72.7 

+  1760 

4 

833 

15 

+  32-8 

4-4187 

4 

902 

12 

+  56.8 

— 4210 

4 

969 

12 

+  73-o 

4-5298 

4 

834 

835 
836 

837 

13 

+  32-9 

+  59°4 

4 

903 

14 

+  56.9 

+  1346 

4 

970 

1 1 

+  73-3 

-1977 

4 

1 1 

+  33-3 

+  6249 

4 

904 

16 

+  56.9 

-1438 

4 

97i 

15 

+  73-3 

-3674 

4 

v 

i 

IS 

+  33-7 

+4299 

4 

doubt- 

ful 

972 

15 

+  73-8 

-4465 

4 

9 

+  33-9 

—4440 

1 

905 

16 

+  56.9 

—  160 

4 

973 

[2] 

12 

+  74-6 

-  371 

4-6053 

3 

838 
839 

1 1 

+  33-9 

+  59°9 

4 

906 

14 

+  57-o 

+  5452 

4 

974 

10 

+  75-9 

1 

iS 

+  34-6 

-  949 

4 

907 

13 

+  57-5 

+4245 

4 

975 

17 

+  76-° 

—  1869 

4 

840 

14 

+  34-9 

4-6254 

4 

908 

15 

+  57-8 

—4850 

4 

976 

14 

+  764 

-3730 

4 

841 

1  j 

+  37-o 

+  S859 

4 

909 

16 

+  57-8 

—4930 

4 

977 

16 

+  76.5 

4-6089 

4 

84a 
843 

14 

+  37-2 

4-1305 

4 

910 

14 

+  57-9 

—  3860 

4 

978 

12 

+  76-9 

+4155 

4 

IS 

+  37-3 

-  294 

4 

911 

16 

+  58-0 

— 3317 

4 

979 

IS 

+  77-3 

4-3380 

4 

844 

\ 

7 

+  37-8 

-4143 

1 

912 

J 

13 

+  58-o 

+  335 

2 

980 

14 

+  77-7 

+  5373 

4 

845 

16 

+  37-9 

+2634 

4 

913 

14 

+  58.7 

4-2270 

4 

981 

14 

+  78-o 

4-2813 

4 

846 
847 

17 

+  38-6 

-2055 

4 

914 

14 

+  58.7 

—2234 

4 

982 

V 

10 

+  78.3 

4-3041 

1 

16 

+  38-9 

-1952 

4 

9l5 

12 

+  58.8 

+  2544 

4 

983 

a 

9 

+  784 

-359° 

1 

848 

13 

+  39-1 

4-1605 

4 

916 

13 

+  59-2 

4-1564 

4 

984 

14 

+  78.7 

+3H3 

4 

849 
850 
851 

14 

+  39-2 

+2383 

4 

917 

1 3 

+  59-3 

4-6174 

4 

985 

a 

9 

+  78.9 

4-5014 

1 

14 

+  39-6 

-2645 

4 

918 

m 

12 

+  59-5 

—  1799 

1 

986 

H 

+  79-i 

4-4238 

4 

M 

IS 

+  39-8 

-3689 

4 

dou- 

ble 

987 
988 

15 

+  79-9 

+  5500 

4 

852 

14 

+  41-2 

+  33°3 

3 

919 

17 

+  59-9 

—  1408 

4 

13 

4-  80.2 

+  79 

4 

853 

f 

12 

+  4i-3 

+  5799 

1 

doubt- 

ful 

989 

17 

4-  80.8 

—2134 

4 

854 

855 
856 

12 

+  42-2 

+2353 

4 

920 

12 

+  59-9 

4-2008 

4 

990 

15 

+  81.9 

+4974 

4 

17 

+  42.2 

-  795 

4 

921 

!4 

+  60.2 

+  3722 

4 

99i 

16 

+  82.7 

—3545 

4 

14 

4-  42.4 

+  5794 

4 

922 

16 

+  60.3 

—4880 

4 

992 

15 

4-  82.9 

+  537o 

4 

857 

O  _  O 

IS 

+  42.6 

+4382 

4 

923 

16 

+  6°-3 

+  36 

4 

993 

H 

+  83.5 

+  726 

4 

859 
860 

1 1 

+  43-3 

-I-6209 

4 

924 

14 

4-  60.4 

+  5994 

4 

994 

g' 

10 

+  83.8 

4-2020 

4 

13 

+  43-7 

-3997 

4 

925 

13 

+  60.5 

—  586 

4 

995 

16 

+  83.9 

—3068 

4 

14 

+  43-8 

4-3401 

'4 

926 

m' 

12 

+  60.8 

-1877 

4 

996 

16 

+  84.1 

-1-6024 

4 

861 
862 

13 

+  43-8 

—2078 

4 

dou- 

ble 

997 
998 

14 

+  84.6 

+  3331 

4 

8 

+  44-6 

-2937 

1 

927 

+  60.8 

-4- 1229 

4 

4-  84.6 

+  833 

4 

863 

dou- 

ble 

928 

17 

4-  61.0 

+  3996 

4 

999 

4-  84.8 

-338i 

4 

11 

+  44-7 

+  59°9 

4 

929 

h 

IO 

+  61.5 

4-2399 

1 

1000 

+  85.0 

-1047 

4 

864 
865 
866 

14 

+  45-i 

+  5889 

4 

930 

14 

+  61.5 

4-4104 

4 

1001 

+  85.3 

-I-6014 

4 

+  45-5 

—  11 14 

4 

93i 

+  61.7 

4-4409 

4 

1002 

4-  86.6 

4-3623 

4 

P 

IS 

+  45-6 

+4512 

4 

932 

4-  61.8 

-4478 

4 

1003 

4-  86.9 

+  4J2 

4 

867 

12 

+  45-7 

-2978 

4 

933 

00 

+  62.0 

4-3870 

1 

1004 

g 

4-  88.0 

+  2156 

1 

868 

14 

+  46-3 

— 1229 

4 

934 

(t) 

4-  62.1 

+  H94 

1 

1005 

4-  88.4 

+  32 

4 

869 
870 

4-  46.8 

+4672 

4 

935 

4-  62.2 

+  5297 

4 

1006 

+  88.4 

4-30I7 

4 

+  47-2 

+455I 

4 

936 

+  63-2 

-45i8 

4 

1007 

4-  88.8 

+4472 

4 

871 

(x) 

+  47-7 

+  1921 

4 

937 

+  63.2 

+  3946 

4 

100S 

4-  89.0 

+  5745 

1 

872 

8 

+  49-4 

+7585 

1 

938 

+  63-5 

-2234 

4 

1009 

r 

4-  89.0 

4-  686 

3 

873 

14 

+  5°-i 

+  1718 

4 

939 

iS 

+  63-9 

-393° 

4 

1010 

13 

+  89.9 

+  55H 

4 

AREA  OCCUPIED  BY  THE  GREAT  NEBULA. 


47 


A IV  A 

ASS  FL) 

ARA 

ANPD 

AKA 

AT\PD 

T 

-Letter. 

to 

TO 

from  tj 
Argus. 

from  7] 
Argus. 

Vi 
03 

No. 

Letter. 

ca 

from  t) 
Argus. 

from  Tj 
Argus. 

en 

is 

No. 

Letter. 

cS 

from  7] 
Argus. 

from  tj 
Argus. 

DO 
C3 

X 

Sec.  Dec* 

y 

Micro.  Pts. 

0 

& 

X 

Sec.  Dec. 

y 

Micro.  Pts. 

X 

Sec.  Dec. 

y 

Micro.  Pts. 

O 

IOI I 

12 

-f-  90.0 

-2509 

4 

1079 

13 

+  117.4 

+  496 

4 

1 148 

!5 

+  142.9 

— 1813 

4 

1    1  z 

b 

9 

-f  90-2 

— 1040 

1 

1080 

l6 

+  "7-5 

+  5766 

4 

1 149 

J5 

+  143.2 

+  5O30 

4 

1013 

a 

9 

+  9°-5 

—2190 

1 

1081 

14 

+  118.3 

+  2644 

4 

1150 

(1) 

1 1 

+  143-4 

+  56° 

1 

dou- 

Die 

1082 

M 

I  I 

+ 1 18.4 

+4353 

3 

1151 

17 

+  H3-5 

+2788 

4 

1014. 

*4 

+  9°-5 

-  599 

4 

1083 

[g] 

12 

+ 1 18.4 

+4987 

3 

1152 

13 

+  143-5 

+  897 

4 

1015 

'4 

+  90.0 

+26 14 

4 

1084 

'5 

+  118. 8 

+2446 

4 

1153 

16 

+  144.2 

+5255 

4 

1016 

'4 

+  9'-3 

+4256 

4 

1085 

12 

+  119.1 

+2190 

4 

1154 

13 

+  144-4 

+4891 

4 

1017 

'4 

1      ^  .  O 

+  445 

4 

1086 

13 

+ 120.5 

+  1830 

4 

"55 

'5 

+  144-7 

+  3789 

4 

1018 

& 

13  : 

+  91-8 

— 2250 

4 

1087 

12 

+  121.5 

—21 14 

4 

1156 

(y) 

1 1 

+  145.2 

+  1596 

1 

10 1 9 

'5 

+  9r-9 

+2664 

4 

1088 

16 

+ 122.4 

+  187 

4 

1157 

12 

+  145.6 

+4643 

4- 

1020 

14 

+  92-1 

+  3470 

4 

1089 

14 

+  122.5 

+  3933 

4 

1158 

16 

+ 146.6 

+  125 

4 

1 02  I 

J5 

+  92.2 

— 1560 

4 

1090 

15 

+  122.5 

-  789 

4 

"59 

13 

+  147.2 

+2462 

4 

1022 

16 

+  93-1 

—  908 

4 

1091 

V 

9 

+  123.5 

+  1551 

1 

1 160 

16 

+  147.3 

—2682 

4 

IO23 

I D 

+  93-4 

+  1947 

4 

1092 

J5 

+  124.2 

+  5887 

4 

1161 

*5 

+  H7-5 

+2938 

4 

IO24 

!5 

+  94-3 

+  2458 

4 

1093 

16 

+  124.4 

+  232 

4 

1162 

(v) 

1 1 

+  148.3 

+5848 

3 

1 02  5 

10 

+  95-° 

+  1897 

4 

1094 

14 

+  124.4 

—  1846 

4 

1163 

J4 

+  148.3 

-  590 

4 

IO26 

12 

+  95-3 

+2496 

4 

1095 

16 

+  125.3 

+ 1610 

4 

1 164 

14 

+  149.0 

—  627 

4 

IO27 
I02o 

x5 

+  90.6 

4-2559 

4 

1096 

H 

+  125.3 

-2565 

4 

1165 

16 

+  149. 1 

—  3160 

4 

[d] 

J5 

+  96-7 

+  983 

4 

1097 

13 

+  126.2 

+  1381 

4 

1166 

12 

+  150.0 

-1731 

4 

IO29 

r3 

+  97-° 

—  287 

3 

1098 

16 

+  126.3 

—  1986 

4 

1 167 

x3 

+  150.1 

—  445 

4 

IO3O 

'5 

+  97-2 

+  5683 

4 

1099 

13 

+  126.5 

-  705 

4 

1168 

12 

+  150.3 

+4619 

4 

IO3I 

15 

+  97-2 

—  1754 

4 

1 100 

15 

+  126.6 

+  5998 

4 

1 169 

14 

+  151-2 

+478o 

4 

IO32 

'3 

+  97-7 

+  5983 

4 

I  IOI 

16 

+  127.2 

+  1343 

4 

1170 

13 

+  152.5 

—  1768 

4 

IO33 

10 

+  98.0 

—  921 

4 

1 102 

15 

+  127.4 

— 3181 

4 

1171 

16 

+  152.6 

-2987 

4 

IO34 

I  I 

4-  98.3 

—2753 

4 

1 103 

r 

9 

+  127.8 

+6133 

1 

1172 

1 1 

+  153.2 

+4780 

4 

IO35 

12 

+  98-9 

+  5988 

4 

1 104 

'5 

+ 128.0 

+  3898 

4 

"73 

16 

+  153.3 

+2542 

4 

IO36 

JS 

+  99  4 

+2057 

4 

1105 

16 

+  128.3 

+  809 

4 

"74 

14 

+  153-3 

-  370 

4 

IO37 

*3 

+  99-8 

—  857 

4 

1 106 

r5 

+  128.5 

+  5787 

4 

"75 

»S 

+  153.6 

+  1970 

4 

IO38 

10 

+  99-9 

—  418 

4 

1 107 

H 

+  128.5 

+2989 

4 

1176 

15 

+  154-3 

—  238 

4 

IO39 

*5 

+ 100.2 

+  5626 

4 

1108 

15 

+  129.0 

+  5!7 

4 

"77 

K 

8 

+  155-9 

— 1726 

1 

IO4O 

:S 

4-100.3 

— 1000 

4 

1 109 

1 1 

+  129.0 

-3421 

4 

1178 

+  157-4 

—4628 

4 

1 04 1 

1 1 

4- 102. 1 

-3256 

4 

1 1 10 

14 

+  129.4 

-3038 

4 

"79 

16 

+  157.5 

— 1132 

4 

IO42 

'4 

+ 102. 1 

+  2866 

4 

1111 

16 

+  129.8 

-2570 

4 

1180 

1 1 

+  157.8 

-1733 

4 

IO43 

J5 

+  102.5 

+  999 

4 

1 1 12 

1 1 

+  130.0 

+  6173 

4 

1181 

11 

+  158.1 

—  1788 

4 

IO44 

10 

+  102.7 

-1323 

4 

1113 

16 

+  130.4 

+  1708 

4 

1182 

13 

+  158.3 

+  92 

4 

IO45 

'3 

+ 102.8 

+  5593 

4 

1 1 14 

15 

+  131. 1 

+  5797 

4 

1183 

w 

6 

+  158.3 

+2782 

1 

IO4O 

P" 

14 

+  102.9 

— 3171 

4 

1115 

+  13 1.2 

+  5366 

4 

1 184 

16 

+  158.8 

— 1260 

4 

IO47 

1 1 

+  103.2 

+  1172 

3 

1116 

1 2 

+  i3!-5 

+  6088 

4 

1185 

12 

+  160.3 

+  32 

4 

IO48 

15 

+  103.2 

+2414 

4 

1117 

15 

+  132.2 

+  3823 

4 

1186 

13 

+  161. 1 

—  814 

4 

IO49 

1 1 

+  103.3 

+2564 

4 

1 1 18 

15 

+  132.2 

+  2935 

4 

1187 

r3 

+  162.6 

+4493 

4 

IOJO 

15 

+  103.4 

+  3684 

4 

1119 

12 

+  132.4 

+  1151 

4 

1188 

1 2 

+  162.6 

-2558 

4 

IO5I 

r5 

+  103.5 

+  3593 

4 

1 120 

1 1 

+  132-9 

+  6098 

4 

1189 

[1] 

1 1 

+  163.0 

+4002 

3 

IO52 

J3 

+  103.6 

—  1658 

4 

1 121 

16 

+  133-3 

—  3208 

4 

1 190 

16 

+  163.2 

— 1136 

4 

IO53 

16 

+  103.8 

+  957 

4 

1 122 

16 

+  133-4 

+  768 

4 

1191 

15 

+  164.0 

+  3118 

4 

IO54 

u 

+  104.6 

+  3958 

1 

1123 

14 

+  133-9 

-  589 

4 

1 192 

12 

+  170.2 

+4032 

4 

IO55 
IO56 

W 

!5 

+  104.7 

+2460 

4 

1 124 

r5 

+  133-9 

+ 1090 

4 

"93 

r3 

+  170.2 

+4142 

4 

I  I 

4-105.5 

+2776 

1 

1125 

M 

1 1 

+  J34-4 

+4918 

3 

"94 

12 

+  171-4 

+  3677 

4 

IO57 

tnri? 

+  105.7 

—2762 

4 

1126 

M 

1 1 

+  r34-5 

+  5396 

3 

"95 

H 

+  171-3 

—  1898 

4 

14 

+  105.8 

—  465 

4 

1 127 

16 

+  135.3 

+  '573 

4 

1 196 

15 

+  172.4 

—  526 

4 

1059 

1061 
1062 

1 1 

+  106.4 

+6136 

3 

1128 

1 1 

+  136.1 

—  3018 

4 

"97 

z 

8 

+  17+1 

-  556 

1 

14 

+  107.7 

+2519 

4 

1129 

8" 

16 

+  136.2 

+  1603 

4 

1198 

[m] 

11 

+  1746 

+4663 

3 

13 

+  108.1 

+  553I 

4 

1130 

1 1 

+  137-7 

—  842 

3 

"99 

+  177-4 

+4072 

4 

+ 108.6 

+  3494 

4 

1 1 3 1 

12 

+  I37.8 

—  327 

4 

1200 

12 

+  178.1 

—2430 

4 

1063 

q" 

1 1 

+  108.9 

—  1 120 

3 

1132 

!5 

+  137.8 

+  3017 

4 

1201 

a" 

+  178.7 

+  986 

1 

1064 

9 

+  109.3 

+  5866 

1 

"33 

14 

+  138.2 

— 2000 

4 

1202 

14 

+  178.7 

-J953 

4 

1065 

1066 

'3 

+ 1 10.5 

+  3269 

4 

1134 

1 1 

+  I38.3 

+4838 

4 

1203 

Y 

7 

+  178.9 

+3441 

1 

13 

+ 1 10.9 

+6045 

4 

1135 

13 

+  I38.7 

—  347 

4 

1204 

12 

+  180.6 

-2539 

4 

1067 

1068 

14 

+ 1 10.9 

+  5634 

4 

1136 

15 

+  I38.8 

+  5977 

4 

1205 

1 1 

+  183.9 

— 21 12 

4 

V 

(w) 

1 1 

+  111.0 

—3402 

1 

1137 

10 

+  139-8 

-3535 

1 

1206 

V 

8 

+  1940 

—2192 

1 

1069 

1 1 

+  113-0 

+  753 

1 

1138 

'5 

+  140.5 

+  5037 

4 

1207 

w 

11 

+  194-8 

+2134 

1 

1070 

12 

+  "3-7 

—  623 

4 

1139 

15 

+  140.6 

+4833 

4 

1208 

10 

+  >97-5 

-2997 

4 

1071 

13 

+  114.1 

818 

4 

1 140 

T4 

+ 140-7 

+  3849 

4 

1209 

+  198.2 

-2816 

4 

1072 

13 

+ 1 14.3 

+2395 

4 

1 141 

13 

+  141-4 

—  1 140 

4 

1210 

12 

+  199-8 

-3187 

4 

1073 

15 

+  115.1 

+  5786 

4 

1 142 

17 

+  141.6 

+2485 

4 

1211 

+201. 1 

+  846 

1 

1074 

T3 

+  "5-3 

+  506 

4 

1 143 

15 

+  142. 1 

— 1041 

4 

1212 

•3 

+209.2 

—2879 

4 

1075 

14 

+  "5-3 

+4028 

4 

1 144 

15 

+  142.2 

+2960 

4 

1213 

9 

+209.2 

— 19 10 

1 

1076 

14 

+  115.8 

+2264 

4 

1 145 

14 

+  142.5 

+2786 

4 

1214 

15 

+211.9 

-3H5 

4 

1077 

12 

+  116.9 

+2526 

4 

1 146 

+  142.9 

—  967 

4 

1215 

e 

7 

+224.2 

-3631 

1 

1078 

13 

+  117-3 

-1756 

4 

1 147 

15 

+  142-9 

+  3138 

4 

1216 

B' 

12 

+225.3 

-3615 

2 

REDUCED  OBSERVATIONS 

OF 

NEBULJ1  AND  CLUSTERS  OF  STARS, 

MADE  WITH  THE  TWENTY  FEET  REFLECTOR, 

IN  THE 

Years  1834,  1835,  1836,  1837,  and  1838, 
AT  FELDHAUSEN, 

ARRANGED  AS  A  CATALOGUE,  IN  ORDER  OF  RIGHT  ASCENSION, 

FOR 

THE  EPOCH  1830. 


o 


51 


Reduced  Observations  of  Nebula  and  Clusters  of  Stars  made  with  the  20  feet  Reflector, 
in  the  years  1834,  1835,  1836,  1837,  and  1838,  at  Feldhausen. 


Synon. 


III.  461 


A.  507 


A.  18 

B.  38 


R  A.  1880.0. 
h.   m.  s.  d. 


o  1  15.4 
o    1  25.3 

35.8 

o    1  54.2 

O     2  7.2 

9-5 

O     2  51.3 

o    5  16.2 


o  6  23.8 
o    6  26.4 


28.3 


34.2 

O   12  49.4 
49.6 
O  12  59.2 

59.2 

o  13  0.4 
1.6 

o  13  7.9 
8.1 

o  14  26.6 
o  15  25.1 
26.7 
o  16  24.4 


25.9 


26.5 


26.5 


N  P  D.  1830.0. 


115  55  O 
147  58  II 
58  21 
147  56  26 
147  56  56 

55  5i 
147  53  47 
114   7  16 


151  16  15 

130    9  58 


9  4i 

9  5 

x39  34  35 

34  5° 
139  35  8 

35  20 
139  36  35 

36  40 
139  34  15 

34  3° 
136  13  13 
123  28  44 

30  o 
163    1  58 


1  5i 


1  15 


Description,  Remarks,  &c. 


F ;  v  L  ;  v  m  E  ;  v  g  b  M  ;  4'  1 ;  1'  br  

F;  R  ;  30'  

e  F;  S;  R  

e  F;  preceding  of  2.    Requires  attention,  but  no  doubt  remains  

e  e  F ;  the  following  of  2.    Requires  attention,  but  leaves  no  doubt   

ee  F;  S;  R   

e  F;  S;  R  

e  F ;  L  ;  R  (by  diagram) ;  v  g  v  1  b  M  ;  attached  to  and  nearly  involving  a 
L  star  ;  the  following  of  2.  A  very  F  object  of  singular  appearance,  3  or 
4'  diam. ;  forms  a  kind  of  cometic  appendage  to  the  star,  which,  however, 
is  quite  at  the  edge. 

e  F;  R;  vlb  M;  30"  

B;  vL;  vmEina  long  irregular  train,  the  preceding  end  being  much  the 
brightest.  Whole  length  =  i\  diam.  of  field,  or  22'.  The  nucleus  is 
either  a  double  star  or  a  much  more  sharply  terminated  nebulous  mass, 
elongated  in  a  different  position  (i46°.5)  from  that  of  the  nebula  (i09°.8). 

vB;  vL;  vmE;  at  least  25'  1  and  3'  br.  The  following  part  is  Faint, 
the  preceding  and  shorter  trinuclear  the  2d.  nucleus  taken.  A  strange 
object. 

v  B  ;  v  L ;  a  very  long  irregular  crooked  ray  with  3  nuclei,  the  second  of 
which  appears  to  consist  of  stars.    See  Plate  IV.  fig.  8. 

e  F  ;  S  ;  R.    The  first  of  a  group  of  4  nebula?  

eF;  vS;  R;  g  b  M.  istof4  

e  F ;  v  S ;  R.  The  2nd  of  a  group  of  4 ;  in  centre  of  gravity  of  the 
triangle  formed  by  the  other  three. 

e  F  ;  v  S  ;  R ;  2nd  of  4,  in  centre  of  gravity  of  the  others  

v  F  ;  S  ;  R.    The  3rd  of  a  group  of  4  

v  F  ;  S  ;  R  ;  g  b  M.    The  3rd  of  4   

F  ;  S  ;  R.    The  last  of  a  group  of  4  

F  ;  R ;  g  b  M  ;  20".    The  last  of  4   

v  F  ;  R ;  b  M  ;  40" ;  r  

v  F;  R  or  vlE;  gb  M;  15"  

p  B  ;  p  L  ;  IE;  45"  ;  precedes  a  star  14  m  

©  47  Toucani.  A  most  magnificent  globular  cluster.  It  fills  the  field  with 
its  outskirts,  but  within  its  more  compressed  part,  I  can  insulate  a 
tolerably  defined  circular  space  of  90"  diameter  wherein  the  compression 
is  much  more  decided  and  the  stars  seem  to  run  together  ;  and  this  part 
I  think  has  a  pale  pinkish  or  rose-colour. 

The  great  cluster  preceding  the  Nubecula  Minor.  Estimated  diameter  of  the 
denser  portion  5' ;  of  the  whole  (not,  however,  including  loose  stragglers) 
8'.  Stars  14 ....  16  m  and  one  =  12  m,  n  p  the  centre.  Excessively 
compressed.  (N.  B.  In  a  sweep  below  the  pole,  when  of  course  owing 
to  the  low  altitude  much  of  the  light  was  lost.) 

47  Toucani.  A  most  glorious  globular  cluster.  The  stars  are  =,  14  m, 
immensely  numerous  and  compressed.  Its  last  outliers  extend  to  a  dis- 
tance of  2m  16s  in  R  A  from  the  centre.  It  is  compressed  to  a  blaze  of 
light  at  the  centre,  the  diameter  of  the  more  compressed  part  being  30s 
in  R  A.  It  is  at  first  v  g,  then  p  s  v  m  b  M.  It  is  completely  insulated. 
After  it  has  passed,  the  ground  of  the  sky  is  perfectly  black  throughout 
the  whole  breadth  of  the  sweep.  There  is  a  double  ^  11  m  preceding  the 
centre  (Pos.  226°-5 — A  R  A  =  6s-s  from  centre  of  neb). 

Fills  the  field  with  its  stragglers,  condensation  in  three  distinct  stages,  first 
v  g,  next  p  s,  and  finally  v  s  v  m  b  M  up  to  a  central  blaze  whose  diameter 
in  R  A  is  13". 5  and  whose  colour  is  ruddy  or  orange-yellow,  which  con- 
trasts evidently  with  the  wliite  light  of  the  rest.  The  stars  all  nearly 
equal  (12  .  .  .  14  m).    A  stupendous  object.    See  Plate  III.  fig.  1. 


52 


REDUCED  OBSERVATIONS  OF 


No. 

2323 

2324. 

2325 
2326 

2327 


2328 
2329 


2330 

2331 
2332 

2333 


2334 
2335 

2336 

2337 
2338 


2339 
2340 

2341 
2342 

2343 


2344 


Synon. 


R  A.  1830.0. 
h.  in.  s.  d. 


A  590  ? 


h.  27 


II.  478 

h.  30 


III.  223? 


A.  2 


o  18  19.7 
23.5 

o  18  50.5 
52.1 

o  19  4.5 

O  21  12.8 

o  21  57.8 
58.9 

o  23  6.7 
o  24  52.2 

53.2 

o  25  26.7 

o  23  48.3 
o  26  37.2 

39.6 

o  28  30.0 

34-9 
35.2 
o  28  50.5 


o  29  7.3 

8.9 

o  30 

o  32  23.8 

30.3: 

o  33  0.8 
5-3  = 
0  33  51. 1 
51.2 

53-i 

o  33  55.3 
o  34  40.7 

o  35  29.2 
o  37  5.1 

o  37  7.2 
9.9 
13-7 

o  39  3.7: 
8.7 


N  P  D.  1830.0. 


124  37  43 
37  0 
147  55  26 

55  '8 
162  28  23 

124  11  52 
12  11 

124  11  42 
11  47 

96  5  19 
122  43  13 

43  55 
100  38  24 

164    3  8 

146  43  46 

42  53 
120  24  31 

24  53 
23  58 
no  52  6 


164    6  28 

6  23 

164  27  . . 

147    6  6 

6  13 

147    8  26 

8  18 

164  18  30 

20  54 
19  58 

164  23  56 

164  17  10 

141    6  36 

164  31  32 

164  22  22 

22  18 

21  50 

164  18  9 

18  47 


Description,  Remarks,  &c. 


e  F ;  S  ;  has  a  small  faint  double  *  n  p,  2'  dist  

F ;  L ;  v  1  E  ;  60" ;  has  a  double  H«  2'^  dist.  n  p  

p  B;  R;  p  s  b  M;  25"   

pB;vS;  R;gmbM;  15"  

p  B  ;  IE;  v  g  b  M  ;  40"  

v  F ;  the  preceding  of  two.    The  other  v  L  and  B  

p  B  ;  p  L  ;  p  m  E  ;  v  g  b  M  

B  ;  L  ;  v  m  E  ;  p  s  1  b  M  ;  4'  1 ;  1'  br ;  pos  =  2270 ;  the  f  of  2   

vB;  vL;  vmE;  psmbM;  8'1;  1'br;  pos  =  47°.9  ;  dies  away  gra- 
dually at  both  extremities ;  has  a  star  10  m,  dist  45",  pos  =  327°9.  See 
Plate  VI.  fig.  19. 

v  F ;  v  1  E  ;  g  1  b  M  ;  60"  1  

v  B  ;  S  ;  1  E  in  parallel ;  smbMtoajfc  11m   

[Obs.  makes  R  A  25  m  but  as  this  and  the  neb  of  620,  are  certainly 
identical,  the  earlier  minute  is  preferred.] 

p  B  ;  S  ;  E  in  parallel ;  v  s  b  M  almost  to  a  star  

p  F ;  R ;  g  b  M  ;  60"   

vF;  L;  R ;  v  g  1  b  M  ;  2'  

v  F;  S;  R;  15";  precedes  3  stars  

v  F;  R;  gib  M;  20"  

v  F ;  R  ;  25" ;  near  one  or  two  stars   

v  F;  S;  R  

F ;  S  ;  IE  among  several  B.  stars   

p  B  ;  p  L  ;  E  ;  g  b  M  ;  r  ;  80"  1,  50"  br.  If  this  nebula  be  really  III.  223, 
the  P  D  assigned  to  that  nebula  by  my  Father's  Observations  must  be  i° 
in  error.  The  error  cannot  lie  in  this  observation,  the  109th  degree  of 
Polar  distance  being  beyond  the  possible  reach  of  the  instrument  in  sweep 
641 

e  F  ;  R  ;  near  a  jfc  8  m.    (At  the  beginning  of  the  Nubecula  Minor)  

e  F;  S;  IE;  r  

Here  comes  on  the  preceding  edge  of  the  Nubecula  Minor,  seen  as  a  mere 
nebula — the  sweep  being  below  the  pole  and  vision  imperfect 

v  F;  S  ;  R;  15"  the  preceding  of  two   

e  F ;  S.  (Owing  to  some  unknown  cause  of  unsteadiness  the  Right  Ascen- 
sions of  this  sweep  are  liable  to  an  error  which  may  amount  to  several 
seconds  of  time). 

p  F ;  S  ;  R ;  20" ;  the  following  of  two   

F ;  R ;  v  g  b  M  ;  among  stars.    (See  the  above  remark  respecting  R  A) 

F ;  v  g  b  M  ;  irreg  figure  

F ;  R ;  the  field  is  full  of  the  nebulous  light  of  the  Nubecula  Minor   

The  first  of  an  irregular  string  of  nebulce  and  stars  which  descends  at  an 
angle  of  about  450  from  the  centre  to  the  edge  of  the  field  (i.  e.  in  a  n  f 
direction). 

v  F  ;  R  ;  outlying  

An  irregular  train  of  stars  and  nebulosity  in  the  Nubecula  Minor.  (Evidently 
that  referred  to  in  f  625. 

e  F ;  p  L ;  R  ;  gvlbM;  50"   

a  v  F,  R  nebula  or  group.  (We  are  now  fairly  in  the  Nubecula  Minor,  and 
the  field  begins  to  be  full  of  a  faint  perfectly  irresolvable  nebulous  light). 

A  binuclear  nebula,  or  two,  v  S,  R,  running  together   

A  small  irresolvable  knot  in  the  bright  part  of  Nubec.  Min  

pL;  vF;  R;  vgbM;  (in  a  sweep  below  the  pole  and  ill  seen)  the  R  A 
is  probably  also  in  error. 

v  F.  (Below  the  pole,  and  the  sweep  otherwise  irregular.  R  A's  not  good) 
F ;  E  or  binuclear  ;  S  ;  v  g  1  b  M   


NEBULAE  AND  CLUSTERS  OF  STARS. 


53 


No. 


2345 


2346 


2347 


2348 


2349 


2350 
2351 


2352 

2353 
2354 


2355 


2356 


2357 
2358 


2359 


Synon. 


V.  1 

h.  61 


A  19  ? 

or 
A  21  ? 


A  3  ? 

A  4? 

or 
A  21  ? 


VI.  20 
h.  74 


A.  5 

A.  530  ? 


R  A.  18S0.0. 
h.  m.  s.  d. 


o  39  3.9 


II.6 


o  39  9.5 
1 0.0 
1 1.1 

o  39  11. 1 
13.9 
14.2 

o  39  33.5 
34.6 

39-5 
42.7 
o  40  13.0 

13.4 
23.6 

o  40  15.4 
o  40  53.6 

56.7 
59.2 

62.0 
o  41  43.9 

o  42  15.7 
o  44  22.5 


o  44  29.4 
29.9 
32.3 

0  44  55-3 


46  3.7 


o  45  12.8 
o  46  1 1.7 
11. 8 

o  46  51.9 

53-5 
12. 1 


NPD.  1830.0. 


Il6  13  57 


J3  45 


164    1  8 

o  38 
o  52 

122  21  17 

21  31 

21  13 

164  26  33 

25  45 

26  18 
26  43 

164    2  8 


1  37 

129  10  12 
164  24  7 

25  53 

24  28 

25  13 
164  12  28 

164  27  52 
117  30  33 


122    8  4 

7  34 

7  28 

164  13  22 


19  23 

164    4  37 
164  18  17 
18  46 

128  37  20 


36  13 

36  14 

37  56^ 


Description,  Remarks,  &c. 


v  v  B  ;  v  v  L ;  v  m  E  ;  30'  1,  3'  or  4'  br  ;  has  several  stars  in  it ;  g  m  b  M  to 
a  centre  elongated  like  the  nebula  itself.  The  neb.  is  somewhat  streaky 
and  knotty  in  its  constitution  and  may  perhaps  be  resolvable. 

vvB;  vvvL;  a  superb  object ;  3I  radii  of  field  in  length  (24') ;  breadth 
about  3' ;  posn  =:  i43°-8  very  exact.  Its  light  is  somewhat  streaky,  but  I 
see  no  stars  in  it  but  4  large  and  1  very  small  one,  and  these  seem  not  to 
belong  to  it,  there  being  many  near. — The  difference  of  R  Ascensions  of 
this  and  the  former  obs.  arises  in  great  part  from  the  undefined  nature  of 
the  object.    I  prefer  this  however. 

p  B  ;  p  L  ;  oval ;  r ;  2'  diameter  

F;  R  30"  

F  ;  L  ;  R  ;  v  g  b  M  ;  2'.    Here  begins  a  starry  region  of  the  Nubecula  Minor 

vB;  S;  pmE;  smbM;  has  a      9  m  5'  dist  n  f   

B;  pS;  IE;  vsvmbM;  has  a  s|!  7' m  5'  dist  n  f  

v  B  ;  R ;  g  m  b  M  ;  40".  has  a  *  8  m  dist  5'   

F  ;  S  ;  R  ;  g  b  M  ;  40"  South  of  a  *  8  m.  (In  Nubec.  Minor)   

Not  v  F  ;  S  ;  R  ;  has  a  star  9  m  n  f .   

F ;  1  E  ;  30" ;  precedes  a  star  9  m   

F;  S;  R;  18";  a  star  9  m  n  f  

p  B  ;  R ;  60"  has  a  star  13mm  centre.  Occurs  in  a  field  illuminated  by 
the  Nubecula  Minor  and  many  stars. 

p  F;  R;  90"  

v  F ;  R ;  g  b  M  ;  2' ;  r.  There  has  probably  been  an  error  of  io<  committed 
in  reading  the  chronometer.    Reduction  re-examined  and  found  correct. 

F;S;  R;  vsvmbM  to  a  $  13  m.    A  trapezium  of  L.  st.  follows  .... 

v  F  ;  situated  on  the  edge  of  the  Nubecula  Minor  

F  

v  F;  R;  30*  

F;  S;  R;  40'  

A  F,  p  L,  cluster  of  v  S  stars.  It  is  the  preceding  knot  (or  centre  of  con- 
densation) of  the  resolvable  portion  of  the  Nubecula  Minor  which  fills  the 
subsecpient  field  and  consists  of  irregularly  clustered  stars  12. . .  .20  m. 

v  F ;  S  ;  R ;  30"   

©  ;  B  ;  L  ;  R ;  g  b  M  ;  all  resolved  into  stars  12  ...  16  m  ;  5'  diam. 
N.B.  This  observation  decides  the  doubt  raised  in  the  obs.  of  sweep  292 
(see  Catal.  of  Nebulae,  &c.  h,  No.  74)  respecting  the  Right  Ascension  of 
this  object  in  favour  of  the  latter  of  the  two  results  there  set  clown,  which 
is  consequently  to  be  adopted  as  the  correct  result  of  that  observation. 

vB;  L;  mE;  sbM;  has  a  j|c  nmnp   

B  ;  L  ;  R  ;  g  1  b  M  ;  90"  

v  B  ;  L  ;  p  m  E,  oval;  has  a  *  11  mnp  

Hereabouts  seems  to  be  placed  the  main  body  of  the  Nubecula  Minor  which 
is  a  Faint,  Rich,  Large  Cluster  of  very  small  stars  (12....  18)  filling 
many  fields,  and  broken  up  into  many  knots,  groups,  and  straggling 
branches.    But  the  whole  is  clearly  resolved  into  stars. 

I  should  consider  this  to  be  about  the  main  body  of  the  Nubecula  Minor, 
which  is  here  fairly  resolved  into  excessively  minute  stars,  which  are  how- 
ever certainly  seen  with  the  left  eye. 

eF   

pF;  pL;  R;  vglbM;  r   

e  F.  [This  obs.  gives  47  for  the  minute  of  R  A.  The  earlier  minute  pre- 
ferred.]   In  a  sweep  below  the  Pole. 

B;  vL;  vgpmbM;  vmE;  irreg  fig ;  8'  to  10'  1 ;  3'  or  4'  br ;  has 
subordinate  nuclei.    See  PI.  V.  fig.  10. 

F ;  v  L  ;  v  g  b  M  ;  4'  1,  2'  br ;  has  another  neb  attached  

A  very  faint  nebula  attached  to  the  large  one  of  f  488  No.  36,  or  a  subor- 
dinate nucleus. 

A  large  oval  nebula  containing  3  stars.  [N.B.  Mr.  Dunlop's  neb  530  is 
described  by  him  as  easily  resolvable  into  very  minute  stars.  Its  iden- 
tity with  this  is  therefore  very  doubtful.] 


494 
625 


482 

44! 
625 
441 

486 

488 
488 

803 


P 


54 


REDUCED  OBSERVATIONS  OF 


Svnon. 


2360 


2361 
2362 


2363 

2364 
2365 


2366 
2367 


2368 


2369 
2370 


2371 

2372 
2373 

2374 
2375 


A  23 


A.  25 


A  ss? 
A  62 


R  A.  1830.0. 
h.  m.  s.  d. 


o  47  17.0 
17.6 
18.8 
20.8 

o  48  1 1.8 
o  48  44.0 
44-5 

o  48  42.0 
44.4 
o  49  16. 1 

o  49  16.7  : 


o  49  31.5 
o  50  23.3 

24.0 
25.1 

25.9 

26.4 
o  50  44.9 

45.1 

o  51  .. 

o  52  16.2 
o  53  17.0 

19.5 

19.6 
19.6 
o  53  25.0 
27.8 
o  56  17.6 
o  56  19.2 

19.9 

o  56  24.4 
31.6 
o  57  21.5 

25.3 
26.1 
28.8 


N  P  D.  1830.0. 


163    6  52 

7  4 
7  28 
7  16 

163    9  48 
122  52  23 
S3  36 

143  41  52 

4«  55 
131  22  23 

H3  S3  45 : 


H3  49  45 
163  23  18 

23  20 

22  49 

23  12 

24  10 
126    3  9 

3  6 

162  55  .. 
165  22  12 

163  5  21 

5  54 
5  58 

5  37 

6  42 
144    9  24 

9  42 
156  31  12 
126    3  15 

3  41 
162  32  42 
31  48 
161  45  42 

45  » 
45  52 
45  48 


Descriptioo,  Remarks,  &c. 


pB;  v  S  ;  R ;  v  1  b  M  ;  15';  r  

F;  v  S;  R;  glbM;  r;  15"  

An  extremely  small  bright  knot  of  the  Nubec.  Min.  15"  diam  

p  B  ;  v  S  ;  R ;  12" ;  r.  Situate  at  the  upper  limit  of  the  nubecula  which 
here  is  starry.    At  the  other  it  is  nebulous. 

An  extremely  small  faint  knot  of  the  Nubec.  Min.  1 5"  diam   

F;  eS;  R;  sbMtoa  stellar  nucleus  

e  e  F ;  v  S  ;  almost  doubtful  whether  really  the  object  looked  for.  Has  a 
p  B  s(s  following  2'  dist.  (N.B.  The  coincidence  of  the  places  destroys 
this  doubt.) 

F,  S,  R,  15"  follows  a  star  12  m  on  same  parallel  

yF;S;  R  

F ;  S  ;  Stellar  ;  the  bad  definition  of  a  south-easter  prevents  certainty,  but 
I  think  it  is  not  a  star. 

v  F  ;  S  ;  R.  The  R  A  may  err  several  seconds.  The  P  D  also  is  not  very 
good. 

Viewed;  found  exactly  in  place  of  No.  29  f  498.  p  B.  S.  R.  b  M.  15". 
there  is  also  another,  pos  =  3  6°.  8  A  P  D  =  4'. 

v  F,  1  E,  v  g  b  M.    Place  from  No.  29/298  pos  36°.8  A  N  P  D  =  4'  

© .  A  small  v  B,  highly  comp.  oval  cluster  2'  1 ;  1'  br ;  v  g  b  M  stars 
=  13  m. 

A  resolved,  v  comp.  somewhat  oval  cluster  of  close-wedged  stars  13  ...  15  m 

©  ;  S  ;  B ;  little  Elliptic  ;  g  b  M  ;  2'.  Fairly  resolved  into  rather  large  and 
not  very  crowded  stars. 

©  ;  vB;  S;  IE;  ror  resolved ;  90"  1,  60"  br ;  a  close  compressed  knot  of 
stars  with  outliers. 

p  B  ;  S  ;  oval ;  resolved ;  60"  

F ;  S  ;  R ;  glbM;  makes  a  triangle  with  2  st.  s.  of  neb   

e  F  ;  S  ;  R ;  at  the  northern  angle  of  an  equilateral  triangle  formed  with  two 
stars  11  m. 

The  upper  edge  of  the  Nubecula  Minor. — Resolvable   

v  F ;  L  ;  R  ;  v  g  b  M  ;  3'  or  3  J'  diam  

Cluster ;  imperfectly  resolved ;  rather  irregular  figure ;  5'  diam.  Not 
equally  condensed  about  centre ;  fades  imperceptibly  ;  has  a  double  star 
(12  =  12  m)  in  centre. 

B  ;  L  ;  irreg  fig,  with  a  %  ijmin  most  comp.  part   

B,  L  neb  with  r  centre  ;  irregularly  E  into  a  kind  of  broad  train  as  in  figure 
(PL  IV.  fig.  6)  gently  graduating  away  to  the  borders.    6'  diameter. 

B  ;  L  ;  irreg  R ;  g  m  b  M  ;  3'  or  4'  in  extent ;  fades  away  insensibly  

B;  L;  pmE;  pgmbM;  5';  r  (ill  seen,  below  the  pole)   

e  F;  S  ;  R.    (N.B.  The  R  As  in  this  sweep  open  to  error  of  some  seconds) 

e  e  e  F  seems  to  have  a  v  F  star  involved   

eF;  vmE;  vlbM;  a  Ray  nebula,  pos  =  i45°-4   

F;  R;  lb  M  

F ;  S  ;  R ;  g  b  M  ;  20"   

v  F ;  L ;  oval ;  vgvmbM   

eF;  pL;  R;  vgbM   

© .  vB;vL;pgvmbM.  Diam.  of  more  condensed  part  =  60'  + 
in  R  A  ;  but  there  are  loose  stars  to  a  considerably  greater  distance,  st.  1 3 
or  14  m  all  nearly  equal  and  distinct,  but  run  into  a  blaze  in  centre. 

©  ;  v  B  ;  v  comp  ;  p  s  v  m  b  M  ;  4' ;  all  resolved  into  stars  13  . .  15  m  .... 

vB;  vL;  psvmbM;  R;  5  or  6'  diam.    All  resolved   

A  fine,  highly  condensed  © .    p  s  b  M  ;  diam  4'   


NEBULA  AND  CLUSTERS  OF  STARS. 


55 


No. 


2376 


Synon. 


R  A.  1830.0. 
h.   m.   s.  d. 


NPD.  1830.0, 


A.  31  ? 


2377 
2378 

2379 
2380 


2381 
2382 
2383 

2384 

2385 

2386 
2387 

2388 

2389 
2390 

2391 

2392 
2393 
2394 
2395 

2396 


A.  36 


o  57  50.7 
57-i 
57-5 

60.0 

61.3 
o  58  5.8 
o  58  30.0 

30.4 

0  59  47.6 

1  O  45.1  : 


I  I  38.4 
I  I  45.2 
I    2  1 1.7 

14.7 
I    2  29.1 

31.6 
1    2  30.6 

3 1.6 

33-8 
1    2  42.3 
42.9 

4-3-9 
44.6 

1  3  7.1 
9.1 
10.1 
13.0 

1  3  14.1 
17.7 

1    3  34.6 

1    4  17.2 

20.8 
1    5  6.1 


5  23.8 
30.1 

5  43-2 
45.2 

5  46.4 
48.9 

5  5 1-4 

52.4 

6  59.9 
60.9 


162  57  43 
57  57 

57  32 

58  58 

58  33 

121    5  34 

163  44  3 
44  6 

162  54  18 

J37  35  13 


160  47  7 
126  41  4 
126  23  45 
24  41 

162  40  1 r 

40  32 

121  7  36 

7  45 
6  58 

163  15  56 
16  23 
16  7 

15  39 
163  47  47 

47  44 
47  48 

47  8 
120    8  39 

8  6 
128  59  16 

122  59  33 

59  13 
152  33  30 
27  ± 

149    9  25 

9  3i 
128  48  51 

48  20 
122  38  49 

39  13 
122  44  4; 

41  3 
149  1 1  20 

II  21 


Description,  Remarks,  &c. 


Cluster,  6th  class  ;  F;  R;  10' diam.    Stars  15  18  m  (below  pole)  ... 

v  F,  L,  p.  rich  cluster;  6th  class.    Stars  14  .  .  .  15  m  


F,  L,  p  comp.  cl  of  6th  class.     10'  diam.  g  b  M  ;  stars  12  16  m; — 

in  some  parts  almost  nebulous. 

Cluster  6th  class;  stars  12  ...  15  m,  a  few  =  10  m  and  one  of  9  m; 
m  comp.  M  ;  fills  field  and  has  loose  straggling  lines  and  crooks  branch- 
ing off. 

F,  L,  cl ;  1.  comp ;  g  b  M ;  7'  diam ;  resolved  into  st  14  .  .  .  .  16  m  

v  F;  S;  R;  gib  M;  15"   

p  F ;  S  ;  R ;  r ;  pretty  compact  

©  ;  a  v  S,  v  B  knot  of  visible  stars  15  or  20"  diam.  almost  like  a  solid  mass 

v  F;  p  L;  R;  gib  M;  2'  

A  star  7m?  After  a  long  and  obstinate  examination  with  all  powers  and 
apertures  I  cannot  bring  it  to  a  sharp  disc  and  leave  it,  in  doubt  whether 
it  be  a  star  or  not.  The  star  B  137  immediately  preceding  offered  no 
such  difficulty,  giving  a  good  disc  with  320.  [No  doubt  a  "  Stellar 
Nebula".  ] 

F;  R;  vL;  vglbM;  3'  

e  F ;  R ;  S  near  a  v  S  star   

v  F  ;  R ;  g  b  M  ;  20"   

vF;  S;  R;  gib  M;  15"   

v  F;  p  L;  R;  v  lb  M;  2'  

eF;  pL;  R;  glbM;  2'  

F;  p  L;  R;  gb  M;  60"  

F ;  R  ;  vglbM;  40"  the  preceding  of  two  

Not  v  F;  p  L;  R;  gb  M;  60"  

p  F ;  R ;  g  b  M  ;  40"  in  a  field  rich  with  stars  11....  15m  

p  B  ;  R  ;  g  b  M  ;  60"   

F;  R;  40"  

F;  S;  R;  30"   

B;  R;  g  b  M.  80"   

pB;  L;  R;  vglbM;  r;  3'   

B;  R;  gbM;  2'  

p  B  ;  p  L ;  R  ;  2'.    Has  two  stars  near  

e  F ;  S ;  IE;  20' ;  foil,  of  2   

v  F;  S;  E;  gib  M   

vF;  S;  R;  glbM;  18"  

The  suspected  Nebula  of  f  493  re-examined.  I  believe  it  is  only  3  v  F  st. 
but  yet  there  remains  a  suspicion  of  nebulosity. 

Rather  doubtful,  but  I  strongly  incline  to  the  suspicion  of  its  being  a  v  F 
neb  with  2  v  S  stars  near  it. 

p  F;  S;  R,  g  b  M ;  15"  has  a  ^  1:  m  following.  Place  liable  to  some 
error  owing  to  some  temporary  unsteadiness  in  the  apparatus. 

F.  S.  R.  Observed  when  past  meridian  so  that  no  R  A  and  only  a  very 
rude  P  D  could  be  obtained. 

p  B ;  S ;  R ;  b  M ;  30"  (R  A  uncertain)   

B  ;  R  ;  p  s  b  M  ;  40"   

v  F;  S;  R,  g  1  b  M.  18"  

pB;  R;  pgbM;  20"   

p  B;  S;  R;  gbM   

p  B  ;  R  ;  b  M  ;  20"  

vF;S;R;gbM.  (PDa  rough  estimate  from  that  of  the  nebula  imme- 
diately preceding). 

p  B;  R;  b  M;  20'   

F;vS;R;  12"   

Fj  S;  R;  15"  


Sweep. 

441 
482 
625 

738 


745 
495 
482 
625 

745 
490 


5°9 
802 
486 
803 
625 
745 
495 
645 

494 

625 

738 
745 
441 

745 
482 

738 
441 
645 
643 
803 
635 

493 
501 

734 

735 
504 
803 
486 
645 

494 
645 

494 
735 
504 


56 


REDUCED  OBSERVATIONS  OF 


No. 

2397 
2398 
2399 

2400 

2401 
2402 


2403 
2404 

2405 

2406 

2407 

2408 

2409 

2410 
241 1 

2412 

24i3 
24x4 
2415 
2416 


Synon. 


2417 
2418 
2419 

2420 


A.  7 


A.  60 


A.  9 


R  A.  1830.0. 


h. 

ra, 

s.  d. 

0 

/ 

I 

7 

20.7 

.  .  r 
I40 

IS 

12 

I 

8 

8.0 

164 

12 

1 1 

I 

8 

12.7 

j  J 

164 

I  j 

O2.7 

II 

38 

66.5:: 

II 

30 

I 

9 

3O.6 

124' 

IS 

44 

I 

9 

43-4 

l62 

26 

46 

50.2 

26 

46 

I 

9 

56.9 

164 

12 

45 

57.8 

12 

18 

59.2 

II 

42 

62.5 

12 

1 1 

I 

10 

32.3 

I49 

48 

18 

I 

10 

53-4 

164  14 

8 

I 

1 2 

42.8 

131 

5* 

1 

12 

55.2 

149  25 

20 

58.3 

24 

46 

I 

13 

29.3 

124 

57 

31 

31.4 

58 

0 

I 

16 

9.0 

125 

57 

10 

12.7 

58 

46 

10.2 

56 

49 

I 

16 

12-5 

126 

0 

20 

I4.2 

0 

46 

ia.7 

0 

x4 

I 

17 

0.3 

I29 

0 

56 

31 

2 

21 

I 

17 

29.6 

128 

58 

26 

30.4 

58 

21 

1 

17 

30.6 

128 

57 

6 

31.9 

56 

2 1 

I 

17 

45.6 

128 

54 

6 

I 

20 

15.6 

126 

36 

24 

I 

21 

0.2 

130 

11 

46 

I 

21 

21.8 

126 

28 

40 

35± 

28 

58 

3° 

± 

1 

22 

1.6 

142 

28 

14 

I 

22 

18.0 

113 

33 

5 

I 

24 

3!-3 

124 

23 

13 

31.4 

22 

29 

I 

24 

55.6 

129 

34 

■4 

N  P  D.  1830.0. 


Description,  Remarks,  &c. 


v  F  ;  S ;  R ;  b  M  ;  15".  R  A  may  err  several  seconds  being  only  roughly 
determined  by  an  auxiliary  star,  having  passed  beyond  the  field. 

Chief  centre  of  condensation  at  southern  edge  of  an  irreg.  figured  nebulous 
mass  2'  diameter. 

F;  p  L;  irreg  fig;  r;  2'.    Nebula  and  stars  the  first  of  an  irregular  line  . . 

p  B  ;  p  L  ;  irregular  nebula  with  many  stars.  [The  first  of  an  irregular  line 
of  3  nebulae  and  many  stars], 

A  resolved  nebula  or  cluster  of  irregular  figure  

p  B;  R ;  g  1  b  M  ;  20".  [This  nebula  was  looked  for  in  the  place  here  set 
down  in  siveep  635,  but  was  not  seen.  The  observation,  however,  in  sweep 
493  is  distinct  and  regular,  so  that  there  is  no  doubt  of  the  existence  of 
such  a  nebula,  at  this  R  A,  within  the  zone  swept  (1230  ....  1260).  In 
all  probability,  therefore,  the  degree  was  wrong  read  off,  and  instead  of 
124  should  be  123  or  125.    The  minute  can  hardly  be  wrong.~\ 

pB;pL;  R;  gbM   

F ;  L  ;  R ;  v  g  b  M  ;  4'  diam  

irreg  R ;  r ;  60"  The  second  of  a  train  of  F.  nebulous  clustering  patches 
which  run  across  the  field. 

p  B  ;  p  L ;  irreg ;  the  2nd  of  an  irreg.  line  of  mixed  neb  and  st  

S  ;  R  ;  a  resolved  nebula  or  cluster  

F.R;gbM;r;  60'   

?F;  R;  gbM;  30"   

The  third  mass  in  an  irregular  line  of  loose  stars  and  nebula.  pB;  pL; 
irreg  fig. 

e  F  ;  IE;  20°.  A  difficult  object  but  certain  after  long  attention  with  the 
left  eye. 

vB;S;lE;psbM  

v  B;  S;  IE;  p  s  m  b  M  

p  B;  S  ;  R;  1  b  M   

B ;  v  1  E  ;  p  g  m  b  M  ;  near  a  v  S  star  

p  B ;  S  ;  rather  a  doubtful  object.    The  preceding  of  two   

F;  S;  1  E   

v  F  ;  S  ;  IE;  this  is  the  "  doubtful"  neb  of  a  former  sweep   

p  B  ;  S  ;  E  ;  b  M  ;  20".    The  following  of  two   

F;  S;  RorlE  

p  F;  S;  1  E   

eeF;  S;  R;  vgbM  

eeF;  S;  bM  

eeF;  S;  R;  vgbM   

eeF;  the  s  p  of  two  which  form  an  equilateral  triangle  with  a  star  13m.. 

eeF;  S;  R;  vgbM   

eeF.    The  n  f  of  two   

eeeF;  S;  R;  vgbM.    The  4th  of  a  group  of  4  

v  F;  S;  R  

e  F  ;  S  ;  attached  to  a  minute  star,  and  very  near  a  bright  one   

A  Double  Star.    The  left  eye  leaves  no  doubt  of  its  being  involved  in  v  F. 

neb.  diffused  over  15".    An  extremely  delicate  and   difficult  object. 

Pos.  of  the  double  #  2250. ;  dist  4"  ;  15  and  16  magnitudes. 

v  F;  S  ;  R;  R  A  only  rough  being  already  beyond  the  field   

There  is  a  nebula  but  I  perceive  no  D  *  in  it.    Obs.  past  merid  and  R  A 

not  taken. 

F ;  S  ;  R ;  b  M  among  5  or  6  stars  11  m   

B  ;  L  ;  p  m  E  ;  g  p  m  b  M  ;  3'  1,  2'  br  

v  F;  R;  25"  

F;  S;  R;  b  M;  15"   

vF;  pL;  R;  vlbM;  2';  has  a  double  *  5'  or  6'  n  f   


NEBULAE  AND  CLUSTERS  OF  STARS. 


57 


No.  Synon. 


z 42  I 


A.  17 


2422     I.  281 
h.  139 


24.23 

2424 
2425 

2426 


2427 
2428 
2429 

2430 


2431 


2432 


2433 


2434 
2435 


A.  479 


2436  II.  481? 

2437  III.  459 
h.  155 

2438 
2439 


2440 
2441 


R  A.  1830.0. 
h.  m.  s.d. 


I  25  42.8 
46.9 

I  26  22.4 

23.9 
25.8 


I  26  23.8 

I  27  17.3 
I  27  29.8 

I  27  38.8 
41.2 

I  27  43.2 
I  28  8.5 
I  28  49.1 
50.6 
I  31  7.4 
8.5 

1 1.6 
1  31  15.5 
15.9 
18.1 
1  31  2 1. 1 

21.8 

1  31  32+ 

35-5 
1  3i  57-9 
1  32  12.7 

12.9 


1  40  48.2 
1  40  57.1 

1  41  12.0 
1  41  45.8 
54-9 


1  42  13. 1 
1  42  22.4 


N  P  D.  1330.0. 


164  26  25 

25  27 

I20  16  27 

»7  5 

17  13 


127  22  44 

127  21  36 

127  21  56 

132  18  19 

18  3 

19  .. 
130  1  6 
130  12  58 

128  11  20 
11  35 

120  47  17 
48  10 
46  43 

120  46  30 
46  12 
46  38 

133  23  19 

23  33 

24  + 
133  27  ± 

26  8 

J5S  45  49 
166  24  47 

25  45 


101  16  4 
114  38  33 

H3  38  5 
139  28  30  ; 
29  30 


i*5  47  53 
I25  43  5 


Description,  Remarks,  ice. 


B;  RorlE;  p  s  b  M  to  a  *  ;  has  also  a  involved  which  looks  like  a 
second  nucleus  and  several  small  st  about  it. 

pB;  S;  irreg  R ;  p  s  b  but  not  to  M,  but  rather  to  a  point  near  the 
southern  edge.  Is  decidedly  resolved,  and  has  scattered  St.  (This  is  an 
outlier  of  the  Nubecula  Minor.) 

pB;  vmE;  p  sib  M;  2^'l.  No  other  near  it  within  3  fields  in  R  A  and 
1  field's  breadth  in  declination. 

tB;  L ;  vmE;  pspmbM;  has  a  H<  iom;nf   

v  B  ;  v  L  ;  v  111  E  pos  1 18.3  ;  1st  g  then  s  m  b  M  to  nucl  4'  1  15'  br  has  a 
♦  9  m  n  f. — (N.  B.  The  place  assigned  to  I.  281  in  my  former  Catalogue 
is  R  A  i1'  27"'  22.9"  N  P  D  1200  22'  in  which  it  is  now  evident  that  the 
minute  in  R  A  is  there  mistaken,  and  the  N  P  D  materially  in  error,  since 
by  the  remark  in  sw  644  it  appears  that  there  are  not  two  distinct  nebulae 
in  this  place.  The  difference  of  the  descriptions  is  explained  by  the  low 
situation  of  the  object  in  the  latitude  of  Slough.) 

F ;  R;  12"  follows  a  s|e  12  m.  This  is  possibly  identical  with  the  next 
but  one,  with  a  mistaken  minute. 

eeF;  v  S ;  R ;  the  preceding  of  two  in  field  together  

F ;  S ;  R ;  the  following  of  two.  Possibly  identical  with  the  last  but  one. 
(Both  rightly  reduced.) 

B ;  p  L  ;  m  E,  nearly  in  the  parallel ;  pmbM   

B ;  L ;  mE;  gbM;  i\'  long   

B  ;  m  E  ;  gbM;  80"  P  D  rough  being  taken  2  fields  past  the  meridian  . . 

pF;  S;  R;  bM;  15'  

pF;  S ;  R ;  b  M  ;  15'.    Precedes  2  st  1 1  m   

pB;  S  ;  R;  gbM;  15".    Follows  a  pretty  bright  D  star  

NotvF;  R;  30".    Has  a  double  star  n  p  

v  F;  (sky  cloudy).    The  preceding  of  two  


v  F ;  v  S.    The  preceding  of  two   

v  F;  p  L   

v  F ;  (sky  cloudy).    The  following  of  two  

F ;  S  ;  R ;  gbM;  15".    Has  a  star  near  it,  following   

pB;  S;  R;  gpmb  M.    The  preceding  of  two  

F ;  S  ;  R ;  20"  

F ;  S ;  R ;  P  D  rough,  being  taken  when  considerably  past  merid  

e  F  ;  R.  Place  roughly  obtained  from  that  of  the  foregoing  neb  from 
which  its  position  is  1440  (=  540  s  f). 

F  ;  S  ;  1  E ;  g  1  b  M.    The  following  of  two  

v  F;  irreg.  R;vglbM  

e  F ;  R ;  vglb  M;  40"  

v  F ;  R ;  v  g  b  M  ;  40".  Reduced  on  the  supposition  of  a  mistaken  wire 
(1st  for  2nd).  And  there  can  be  no  doubt  that  this  supposition  is  correct ; 
as  (independent  of  the  coincidence  of  results)  were  it  otherwise  this  nebula 
must  have  been  in  the  field  of  view  at  the  moment  of  observation  in  sweep 
622,  and,  being  at  least  equal  in  brightness  to  that  actually  observed, 
could  not  fail  to  have  been  noticed. 

F;  R;  glbM;  35"   

v  F ;  v  S.    Requires  attention  to  distinguish  it  from  a  star   

F;  vL;  R;  vgvlbM;  3'  

v  F  ;  R ;  gbM;  20"   

B;  R;  gbM;  30'. — (N.  B.  Both  observations  are  correctly  reduced,  but 
there  is  an  obvious  error  of  10"  in  one  or  other,  arising  from  mis-reading 
or  mis-registering  of  the  chronometer  ;  and  I  consider  the  obs.  in  sweep 
744  to  be  more  open  to  that  mistake  than  that  of  sweep  497.) 

*i  S;  Rj  15"   

vvFj  S  


745 
441 

644 

645 
494 


822 

803 
803 

489 
753 
75* 
488 
638 
486 
802 
644 
645 

494 
645 
644 

494 
489 

753 
75* 
753 

489 
508 
622 
746 


650 
646 

498 
744 
497 


802 
802 


58 


REDUCED  OBSERVATIONS  OF 


No.  Synon. 


2442 

2443 
2444 

2445 

2446 
2447 
2448 


2449 
2450 
2451 

2452 
2453 


2454 

2455 
2456 


2457 
2458 
2459 
2460 
2461 

2462 


2469 


2470 


I.  62 
h.  160 

I.  105 
h.  165 

III.  460 
h.  166 


III.  266 


III.  464 
h.  178 
III.  468 


h.  192 
h.  196 


2463 

II.  482 

h.  199 

2464 

II.  483 

h.  200 

2465 

II.  484 
h.  201 

2466 

II.  485 
h.  202 

2467 
2468 

R  A.  1830.0. 
h.  m.  s.  d. 


I  42  39.I 

I  44  45.2 
I  45  50.3 

I  46  24.5 

I  46  31.5 
I  46  48.0 
I  47  58.7 
60.2 
61.9 
I  48  9.0 
I  48  24.5 
I  48  28.7 

I  50  32.7 
I  50  36.5 
46.0 


I  51  56.1 

1  53  52-4 
1  54  37-4 
40.5 
43.1 

'  55  3-3 

1  56  6.5 

1  57  46.1 

1  59  34.9 

1  59  38.1 
44.8 

1  59  40.0 

42.8 

2  1  2.2 

2    1  3.7 

2    1  17.4 

2    1  22.9 

2    3  16.0 
2    4  17.4 
17.7 
24-8 

2  5  11. 5 
12.7 

2  6  9.8 
13.1 


N  P  D.  1830.0, 


100  32  34 

104  34  46 
114  35  52 

126  43  20 

126  40  56 

99  53  24 
120  45  12 

45  6 
45  33 
147  31  38 

T47  35  43 
96  14  18 

102  19  41 
117    7  18 
7  18 


148  36  58 

146  39  13 
165    3  9 

3  5 

3  o 

158  41  26 
114   7  20 

159  16  1 
116  16  17 

131  58  33 
57  13 

126  16  46 
18  55 
100  56  14 

100  56  24 

100  57  14 

100  59  24 

147  32  8 
126  39  30 

37  4° 
40  16 

39  ± 
122  45  3 
44  22 

132  50  2 
49  23 


Description,  Remarks,  &c. 


e  F ;  p  L  ;  certainly  not  entitled  to  a  place  in  the  1st  class. — (N.B.  The  Right 
Ascension  here  set  down  is  of  course  to  be  preferred  to  the  rough  R  A 
(1.42.54+)  of  my  former  Catalogue.) 

p  B ;  IE;  p  s  m  b  M  ;  40'  

pF;  R;  gbM;  25".  No  other  neb  within  15' all  round.— (N.B.  This 
remark  shows  that  the  nebula  No.  167  of  my  former  Catalogue  is  really 
identical  (as  there  suspected)  with  III.  460.) 

F;  S;  R;  bM;  15".  [It  is  barely  possible  that  this  and  the  next  nebula 
■may  be  identical  with  Nos.  2441  and  2442  by  a  mistaken  deyree  mPD.] 

eeeFSR.    RA  only  rudely  taken  by  a  star,  being  out  of  the  field  

eeF;  40"  

p  B;  IE;  p  s  b  M;  35"  

pB;  pmE;  pgpmbM;  30*   

B;  S;  E;  p  s  b  M   

pB;  R;  gbM;  30'   

v  F;  S;  R;  b  M  

vF;  E;  vlbM;  30"  

F;  R;  gib  M;  20'  

p  B;  S;  R;  gbM;  18"  

F;  S;R;glbM;  the  reductions  having  been  examined  and  found  correct, 
a  mistake  of  10"  must  have  been  committed  in  reading  or  registering  the 
chronometer  in  one  or  other  of  these  observations.  There  is  no  apparent 
reason  for  preferring  either. 

p  B  ;  p  L  ;  IE;  attached  to  a  star  12  m   

p  F ;  S  ;  R ;  makes  an  obtuse  angled  triangle  with  2  st  1 1  m  

Somewhat  doubtful,  but  I  believe  it  is  a  v  F  neb  involving  a  v  F  %   

F;  v  S;  R;  has  a      12  m  25"  dist.  450  n  p  

eF;  S;  R;  10"  close  to  a  v  S  star  

eeF;  v  S ;  R ;  has  a  %  13  m  preceding,  dist  100"  

vF;  IE;  gbM;  25   

p  F ;  R;  gbM;  30'   

A  v  F  double  He  involved  in  a  v  F  nebula   

F  ;  R  ;  s  b  M  ;  r ;  15"  a  difficult  object  

v  F;  v  S;  R;  12"  

F;  R;  30";  v  s  v  m  b  M  to  a  jfc  13  m  

F ;  R  ;  40" ;  vsvmbMtoa  H«  12m  

e  F ;  S  ;  R ;  1st  of  a  group  of  4  

v  F ;  S ;  R.    The  2nd  of  a  group  of  4   

v  F ;  S ;  R.    The  3rd  of  a  group  of  4  

v  F  ;  S ;  R.    The  last  of  a  group  of  4  

p  F;  R;  gib  M;  40";  r   

p  B  ;  1  E  in  inerid  ;  40"  1 ;  gbM  

vF;  S;  IE;  15"  1  12'br   

pF;  IE;  gbM(RA  correctly  reduced)  

v  F  ;  R ;  place  roughly  taken  being  past  the  meridian  

pB;  S;  psmbM  

B;  S;  E;  psmbM;  18"  

pF;  vS;  svmbM,  like  a  blurred  star  

F;  R;  gbM;  30"   


NEBULA  AND  CLUSTERS  OF  STARS.  59 


No. 


2471 

2472 

«473 
2474 

z475 


Sjnoo. 


II.  474 
h.  209 


III.  224 
III.  239 


II.  487 
h.  225 


III.  472 


A.  519  i 


II.  284 
h.  249 


II.  488 
h.  253 


I.  63 
h.  254 

V.  48 


III.  449 

h.  269 


R.  A.  1830.0. 
h.  in.  s. d. 


2    8  15.3 

15-3 

16.9 
2  12  16.2 

21.4 
2  12  26.9 
2  13  8.3 

10.2 
2  13  52-5 

2  14  3.0 
2  15  10.7 
2  17  23.4 
2  19  50.0 
52.1 
2  20  22.7 

2  20  37.6 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


102     8  40 

8  24 
8  1 
132  31  35 
31  10 
150  38  30 
132  11  15 

11  22 
124  29  49 

in  35  30 
in  28  50 
115  34  27 
135  12  8 

12  45 
101  18  14 

109  48  12 


2  22  6.1 

132  10  15 

6.6 

9  43 

10.7 

9  r5 

14.0 

9  *7 

2  24  3.2 

126  47  3s 

10.7 

48  30 

47  3° 

45  47 

2  24  13. 1 

107  57  42 

14. 1 

57  37 

2  24  49.4 

101  30  39 

2  25  15.3 

135  16  25 

22.4 

16  21 

2  26  47.4 

129  47  13 

48.5 

47  19 

2  30  47.1 

145  36  39 

2  31  8.8 

98  52  14 

2  31  12.1 

145  36  9 

2  32  17.4 

102    1  15 

2  32  43.2 

125    0  10 

2  32  45.3 

98  59  9 

2  36  26.0 

119  43  33 

2  39  4.1 

120  59  12 

5-5 

59  6 

2  39  34.2 

15°  37  53 

2  41  10.7 

107  42  40 

2  45  42.5 

145  39  58 

F;  R;  b  M  ;  60";  ill  observed  in  a  south-east  cloud   

F;  R;  gib  M;  40"  

Not  v  F;  p  L;  R;  v  gb  M;  50"  

eF;  vS;  R ;  psbM;  has  a  sje  7  m  s  f  and  6  other  S  st  intermediate   . . 

F;  R;gbM;  20"  

e  F  ;  S ;  R ;  has  two  small  stars  very  near  it  

p  F  ;  R  ;  p  s  1  b  M  ;  40"  has  a  *  8  m  following  in  parallel   

Not  v  F ;  R ;  pgbM;  3  5"  has  a  *  9  m  foil  4'  dist   

p  B  ;  S  ;  R ;  p  s  b  M.  Has  a  s)c  10  m  exactly  foil  in  the  parallel  just  at 
the  edge  or  35*  dist  from  centre. 

p  B ;  IE;  gbM;  r ;  30".    Has  a  coarse  double  %  prec  

F ;  E  in  parallel ;  g  1  b  M  ;  20"  1   

pB;  R;  gpmbM;  60"   

vF;  S;  R;  glbM;  15'  

eF;  S;  vlbM;  20"  

eF;  L ;  R ;  glbM;  2'   

p  B;  E;  gb  M;  50"  1,  35"  br   

vF;  IE;  gbM;  25"  

F ;  p  L ;  1  E ;  has  a  *  8  m  3'  dist,  s  f  

e  e  F ;  p  L ;  R  ;  40"  n  p  a  1 1  ni. — (N.B.  The  night  appears  to  have  been 
hazy  and  was  interrupted  by  cloud.) 

v  F;  R;  20". — (N.B.  An  extraordinary  discordance  in  the  observed  Right 
Ascensions  of  this  object,  for  which  I  can  assign  no  reason. — The  reduc- 
tions are  correct.) 

B  ;  pm  E  ;  p  s  b  M;  30"  1 ;  position  2I5°.7  

pB;  mE;  gbM;  80"  1,  15"  br  

p  B  ;  S  ;  IE.    Transit  lost  owing  to  a  passing  cloud   

No  description — observation  evidently  hurried   

pF;  S;  R;  pgmbM;  25"  

e  F ;  irreg  R;  1  b  M  

e  e  F;  S;  R  

Not  v  F  ;  S  ;  R ;  almost  stellar ;  between  2  st  nearly  in  the  parallel  

F;  S;  R;  g  b  M.  15".    [Both  R  A's  correctly  reduced]   

pB;  L;  psbM.  3'  1,  2'  br ;  either  Binuclear  or  more  E  on  the  n  f  side 
than  on  the  opposite.    iVb  other  neb  near  it. 

B;  L;  pmE;  vsmbM;  100"  1,  60"  br.  Unecpially  bright,  and  ex- 
hibiting an  approach  to  the  Binuclear  form  (See  Plate  VI.  fig.  14). 

eF;  S;  R.    j  5"  the  preceding  of  two   

v  F  ;  p  m  E  ;  has  a  v  F  star  at  the  s  f  extremity   


F ;  S  ;  R ;  gbM;  20"  ;  the  following  of  two   

p  B  ;  R;  b  M;  35".    Observed  in  a  south-east  cloud-drift. 


p  B  ;  S ;  R  ;  like  a  star  12  m  a  very  little  rubbed  at  the  edges,  a  curious 
little  object  and  easily  mistaken  for  a  star,  which,  however,  it  certainly 
is  not. 

p  B ;  R ;  g  p  m  b  M ;  30"   


B ;  p  m  E ;  s  b  M  ;  90*  1,  40"  br   

B;  L ;  vmE;  pspmbM;  3'  long;  pos  =  I5i°.l   

B;  L;  vmE;  psvmbMtoapL,  R  nucleus  ;  4'  1,  40"  br 

F;  R;  glbM;  30"  

p  B ;  L ;  p  m  E ;  v  g  1  b  M ;  2'  1,  40"  br  


F;  R  ;  gbM;  taken  for  No.  3  sw  520,  but  proves,  on  reduction,  to  be  a 
different  nebula. 


635 

650 

643 
644 
645 
736 
652 

732 


60 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R.  A.  1830.0. 


h. 

s.  d. 

0 

2 

4-5 

51-3 

145 

45 

59 

% 

4.6 

18.2 

100 

A  .1 

2 

46 

44-9 

109 

20 

32 

2 

5° 

50.7 

103 

4 

51 

2 

51 

40.8 

122 

47 

13 

43.6 

46 

5 

2 

55 

49 

113 

32 

2 

55 

29.2 

102 

44 

56 

46 

± 

2 

55 

48.1 

102 

40 

5° 

48.2 

39 

41 

2 

57 

58.5 

100 

12 

J9 

2 

59 

39-4 

129 

40 

58 

42 

3 

2 

5.6 

in 

14 

42 

7-3 

J4 

7.6 

13 

10 

3 

2 

59-4 

99 

33 

59 

3 

3 

8.9 

99 

35 

20 

3 

4 

16.8 

157 

25 

16 

20.8 

26 

9 

3 

4 

52.1 

1 5  / 

59.6:: 

36 

38 

3 

5 

4.4 

143 

59 

8 

3 

6 

23.3 

148 

27 

9 

3 

6 

26.9 

112 

37 

35 

1 

7 

•?  ?.4. 

JJ  T 

I4.C 

c  1 

A  A 
TT 

37-8 

51 

33 

3 

8 

35.6 

131 

43 

11 

3 

9 

35-5 

IOO 

55 

24 

10 

21.4 

121 

1 2 

2? 

J 

3 

11 

4-3 

I3I 

43 

II 

14.4 

43 

43 

3 

12 

0.3 

110 

1 

35 

2.0 

1 

59 

3 

12.6 

106 

0 

25 

3 

14 

32.2 

I27 

48 

40 

32.6 

43 

45 

33-i 

43 

12 

3 

15 

7.8 

I42 

47 

33 

3 

15 

347 

III 

58 

5° 

N  P  D.  1830.0. 


Description,  Remarks,  &c. 


2499 
2500 

2501 
2502 
2503 

2504 
2505 

2506 

2507 
2508 

2509 


2510 
2511 
2512 

2513 

2514 

2515 
2516 
2517 


2518 
2519 
2520 
2521 


2522 


2523 
2524 


2525 
2526 


II.  470 

h.  275 

III.  469 

III.  245 


II.  475 

II.  285 
h.  285 


II.  258 


II.  286 

h.  289 

III.  591 

h.  291 

A.  205  ?  ? 


A.  337 

III.  956 
A.  487 

I.  106 


F;  R;  gbM;-C   

F;  tS;  R;  psb  Mj  stellar 


F  ;  v  m  E  ;  90"  1,  10"  br ;  has  2  st  10  mag,  f 

pFj  R;  glbM,  25"  

v  F;  IE.  18"  

vF;  p  m  E ;  v  1  b  M  ;  60'  1,  30"  br  


B  ;  v  L;  p  m  E  ;  v  g  b  M ;  3^'  1,  2J'  br.    Has  in  or  near  the  middle  a 
star  16  m. 


The  sp  of  two  

p  B  ;  L  ;  R;  80".    The  n  f  of  2,  dist  about  7^',  pos.  450 

pF;  R;  b  M   

F;  R;  gbM;  25  to  30'   


Not  v  F ;  R ;  p  s  1  b  M ;  20".    Has  a*  nnii'ii  

Viewed  past  merid.    Seen  in  place  but  v  v  F,  as  it  began  to  cloud  

pB;  L;  R;  t  g  in  b  M  4'  diam   

pB;  vL;  R ;  gmbM;  4'  diam  

B ;  v  L ;  R ;  r ;  3'  first  v  g  then  psb  M.     With  the  left  eye  I  see  it 
mottled.    (N.B.  This  is  no  doubt  a  distant  $). 

F  ;  p  m  E  j  50'  the  preceding  of  two  


e  F ;  R ;  the  following  of  two  ;  pos  from  the  other  =  1200 


pF;  IE;  gbM;  25'  

F;  S;  pmE;  gbM  (growing  cloudy)  

Seen  found  in  sweeping  for  A  205  below  the  sweep.  It  has  about  the  same 
R  A  but  farther  south.    Only  this  neb  found. 

pF;  R;  glbM;  15"  

Not  v  F  ;  S ;  R ;  b  M.  (R  A  roughly  taken  by  the  intervention  of  an 
auxiliary  star,  being  past  meridian  when  observed). 

B ;  L  ;  v  m  E  in  pos  8o°;  v  g  b  M  to  an  axis;  l\'  1,  x'  br   

Found  in  place  and  viewed  p  M,  but  very  faintly  seen   

Star  8  m  the  chief  of  a  cluster  of  18  or  20  stars  

F  ;  S ;  almost  stellar ;  but  E  ;  has  a  *  8  m  prec  72',  2'  n  

p  B  ;  R ;  v  g  b  M ;  3';  resolved  into  st  15  m.  A  very  faint  nebula  (?  ?) 
precedes. 

(J)  ;  B ;  L  ;  irreg  R  ;  2  J'  diam  ;  all  resolved  into  equal  stars  14  m. — Has  a 
*  9  m  450  n  f  3'  dist. 

vB;  R;  gmbM  (hazy)  

e  e  F ;  barely  perceptible  

v  F ;  L  ;  R ;  v  g  1  b  M  ;  2 \'  diam  

v  B ;  R  ;  gmbM;  90"  (hazy)   

0  ;  v  B  ;  R  ;  1st  g,  then  s  v  m  b  M  ;  r,  mottled,  but  not  resolved.  (N.B. 
There  must  have  been  a  mistake  of  10'  in  reading  or  registering  the  chro- 
nometer in  one  or  other  of  these  observations.  The  reductions  of  both  are 
correctly  performed.) 

p  F  ;  v  L ;  1st  g  then  p  s  b  M  to  a  F  nucleus ;  m  E  8  or  10'  1,  2'  br  

B ;  v  L ;  1st  v  g  then  p  s  v  m  b  M ;  3'  1,  2'  br.  m  E.  (N.B.  These  dimen- 
sions can  only  refer  to  the  brighter  portion.) 

p  F ;  R  ;  glbM;  pos  from  a  *  7  m  =  3i°.o  ;  A  R  A  =  7'-5  5  *  4' s 

v  F ;  R;  p  L  ;  v  1  b  M  ;  90".    (P  D  evidently  5'  too  large)   

0 ;  v  F ;  R ;  p  L ;  v  g  v  1  b  M  ;  r  ;  90"  2'  diam  

F;  L;  R;  glbM;  2'   

F  ;  m  E  in  position  37°-3  ;  gbM;  2'  1,  15"  br   

pB;  R;  gbM;  25"   


NEBULA  AND  CLUSTERS  OF  STARS. 


61 


No. 


Synon. 


2527 

2528 
2529 

2530 

2531 

2532 
2533 
2534 


2535 
2536 
2537 


2538 

2539 
3540 
2541 
2542 

2  543 

2544 
2545 


2546 

2547 
2548 

2549 

2550 
2551 

2552 


A.  548 

A.  206 
A.  547 


III.  197 

h.  298 

III.  196 

h.  297 


IY.  77 


I.  257 


A.  591 


III.  246 

III.  487 
II.  290 


III.  559 


2553 


III.  857 


R.  A.  1830.0. 
h.  m.  s.  d. 


3  16  H-3 
12.4 
3  16  13.2 
3  16  I3-8 
14.9 

3  16  18.0 

3  16  18.5 

3  16  20.5 
3  16  25.7 
3  16  58.2 

58.2 

3  17  28.4 
3  !8  17-3 
3  J9  57-6 
58.0 
65.7 
3  21  16.3 
18.9 
3  21  25.3 
3  21  31.3 
3  21  48.3 
3  21  49.. 

3  23  55.9 

3  23  58.3 
3  23  ± 


3  24  31.7 

32.5 
3  24  38.7 
3  25  19.4 

20.3 
3  25  35.6 

38.5 
3  26  7.9 
3  26  18.0 

18.7 
3  27  8.4 


3  27 


N  P  D.  1830.0 


127  50  49 

49  3° 
157    6  9 

107  42  49 
43  ° 

93  38  4 

93  37  4 

93  32  24 
112  7  30 
112    8  10 

8  25 

127   4  50 

108  11  25 

126  17  38 
19  30 
19  39 

122  52  28 
52  42 
121  29  32 

127  44  31 

108  22  29 
121  41 

109  51  52 

125  26  24 
124  19  + 


in  23  50 
24  8 

105  47  45 

104  15  11 
16  2 

140  52  33 

5i  43 
no  4  48 
no  52  51 

5i  35 
126  42  37 


42  43 
121  47  .. 


Description,  Remarks,  &c. 


v  B  ;  v  L ;  4'  diam,  1st  g,  then  v  s,  v  m  b  M  to  a  stellar  nucleus   

vB;  p  L ;  IE;  vsvmbM,  toa  nucleus  2"  diameter   

p  B ;  irreg  RorlE;  v  L ;  vgbM;  r;  3'  

p  B  ;  p  L  ;  1'  diam  ;  a  miniature  of  the  last  neb  of  this  sweep  

p  B;  S;  R;  p  s  b  M   

F ;  R ;  b  M  ;  20".    The  first  of  3   

Not  v  F  ;  v  S ;  E  ;  6  or  8"  ;  2nd  of  3.  Query  if  not  a  nebulous  double 
star. 

F;  R;  b  M  15".    The  3rd  of  3   

F  ;  S  ;  R ;  b  M  ;  15" ;  precedes  IV.  77   

F.  Attached  cometically  to  a  9  m  which  forms  its  head.  It  is  an  exact 
resemblance  of  Halley's  comet  as  seen  in  the  night  glass.  Pos.  of  tail 
=  239°.i. 

A  complete  telescopic  comet ;  a  perfect  miniature  of  Halley's,  only  the  tail  is 
rather  broader  in  proportion  ;  m  E  ;  90"  1 ;  the  star  at  the  head  =  10  m. 
See  fig.  17,  PI.  VI. 

60"  diam  ;  v  s  v  m  b  M  to  nucleus ;  ?  a  disc  

F;  R;  glbM;  30"   

F;S;R;gpmbM;  15"   

v  F ;  R.    (Clouding  over  rapidly)   

v  F ;  IE;  40"  

B;R;psmbM.    A  double  star  precedes  

p  B ;  R ;  p  s  1  b  M  ;  40"  

v  B ;  IE;  p  s  b  M  ;  45"  

F ;  S  ;  R ;  has  a  s|!  12  m  s  f   

v  F  ;  R  ;  p  s  1  b  M  ;  20"  

R  A  by  working  list ;  P  D  roughly  taken  ;  Transit  missed  while  observing 
another  nebula. 

eF;  S;  pslbM;  has  a  ^  8  m  s  f .  Very  difficult  and  probably  not  to 
be  seen  without  a  recently  polished  mirror,  such  as  was  used  in  this  ob- 
servation. 

p  B  ;  R ;  p  s  b  M  ;  30"   

B  ;  L  ;  m  E,  but  with  a  R  nucleus  much  brighter  than  the  environing  F 
atmosphere.  P  D  roughly  taken.  Transit  missed,  the  observation  having 
been  lost  by  relying  on  the  R  A  given  in  Mr.  Dunlop's  Catalogue  (3h  25"') 
which  is  too  great.  That  here  set  down  is  assumed  at  random  as  probably 
nearer  the  truth. 

B;  L;  pmE;  psmbM;  2'1   

B  ;  m  E  ;  g  m  b  M  ;  90"  1,  40"  br  

vF;  S;  IE;  glbM;  25"   

p  F  ;  p  L  ;  R  ;  40"  near  3  st,  2  of  which  are  10  m   

p  B  ;  R ;  first  v  g  then  more  s,  b  M  ;  70"  

vF;  R;  gbM;  4°"   

v  F ;  p  L  ;  irreg  ;  near  stars   

F;  L;  R;  vglb  M;  2'  

vF;  S;  R  

v  F;  S;  R  

A  very  remarkable  neb.  A  decided  link  between  the  nebula;  M  5 1  and 
M  27.  Centre  v  B  ;  somewhat  extended ;  gvmbM;  13  m  near 
the  edge  of  the  halo  involved.  The  area  of  the  halo  v  F  ;  general  position 
of  the  longer  axis  20°.8  whole  breadth  =  3'.    See  PI.  IV.  fig.  1. 

v  B,  E,  resolvable  nucleus  ;  or  has  2  or  3  st  involved  ;  the  preceding  Arc  is 
the  brighter.    I  think  the  oval  is  in  some  degree  filled  up  to  the  south. 

Place  from  working  list.  Seen  sweep  644,  but  under  circumstances  not 
admitting  an  observation  of  its  exact  place. 


R 


642 
641 

651 
649 

757 
806 
807 

74i 
652 
642 


802 
644 


62 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


2554     III.  960 


2555 

2556 

2557 
2558 

2559 


2560 

2561 

2562 
2563 
2564 


2565 
2566 

2567 
2568 
2569 


2570 
2571 

2572 
2573 

*574 
2S7S 


2576 

2577 

2578 

2579 
2580 


II.  262 


A.  574 


III.  961 


II.  263 


III.  45I 

I.  58 

II.  593 

III.  247 


I.  107 

II.  267 

II.  291 

III.  248 

A.  426 


H.  A.  1880.0. 
h.  m.  s.  d. 


3  27  38.4 
41.0 

41.9 
3  27  44-5 

3  28  41.3 
3  28  51.3 
3  28  51.3 
3  29  ± 


3  29  8.3 
9-7 

3  29  33.5 


3  29  58.5 
3  30  9.6 
3  30  25.8 


3  30  58.6 
3  3i  5-9 
5-9 

3  31  5°-° 
3  3i  55-7 
3  31  57-2 
68.5 

3  32  34-3 
3  32  34-4 

3  32  37-6 
3  33  4-7 
5.0 

3  33  20.6 
3  33  3°-S 

33-4 

33.8 
3  34  22.6 

23.4 
3  34  32-° 

33-5 
3  35  22-° 

24.9 

3  35  5i-4 
3  36  40.1 
42.7 


N  P  D.  1880.0. 


no  57  2 

56  50 

56  45 

115  30  28 

125  48  29 

125  47  9 

125  49  49 

125  35  ± 


in  27  15 
28  21 
126    1  5 

108  54  20 
115  4  6 
126    4  35 


108  59  34 
i'3  34  15 

35  35 

109  15  27 
113  16  45 
126    1  45 

125  59  58 

109    8  18 

126  8  45 

121  52  22 

134  39  39 

38  51 

116  46  3 

113    6  30 

6  o 

7  24 
I28    3  55 

5  o 

104    2  36 


3  o 
112  38  50 

39  33 
125  56  40 

137  45  5i 
46  53 


Description,  Remarks,  &c. 


e  F  ;  S  ;  R ;  between  2  very  faint  stars   

v  F  ;  R ;  situated  exactly  between  2  stars  14  m  (about  one  semi-diameter 

from  either  edge  by  diagram). 
eF;  S ;  R;  vlbM.    Situate  between  2  v  S  stars  

B  ;  L ;  R ;  psbM;  2'.  (The  P  D  differs  4'  from  the  working  list,  but  it 
is  expressly  stated  in  the  obs.  that  the  index  was  correctly  read,  the  dif- 
ference having  doubtless  been  noticed  at  the  time.) 

e  F  j  v  S  ;  the  preceding  of  3   

v  B  ;  p  L ;  IE;  g  m  b  M  ;  the  2d  of  3  

B;  S ;  IE;  pmbM;  the  3d  of  3  of  the  same  R  A  as  the  second   

vB;L;R;psbM.  A  fine  nebula.  The  obs.  of  the  place  like  that  of 
A  591  above  was  lost  by  setting  the  instrument  on  the  place  given  in  Mr. 
Dunlop's  Catalogue,  and  relying  on  his  R  A  (3h  31")  which  is  too  great, 
instead  of  sweeping  over  them,  when  they  could  not  have  escaped  being 
regularly  taken. 

F;  S;  R;  gbM;  15"   

F;S;RjbMj  15"   

®;  pB;  R;  gpmbM;  70"  

v  B.    Seen  but  no  place  or  description  further   

pF;  vS;  R;  psmbM   

B ;  R  ;  gpmbM;  40"  

0;  vB;  R;  g  m  b  M ;  90".  A  globular  cluster  in  all  probability  iden- 
tical with  this,  was  also  seen  in  sweep  636,  while  searching  beyond  the 
meridian  for  A  562. 

v  B  :  the  1st  of  3,  seen  but  no  place  or  further  description   

pF;  R;  glbM;  30"   

v  B  ;  pmE;  psmbM;  60"  1  

B  ;  R  ;  psmbM;  50"  

B  ;  R ;  psmbM;  30"  

v  F;  S;  R  

® ;  vB;  p  L;  psbM;  ror  resolved  ;  2'  

v  B  


v  B ;  the  2d  of  3,  seen  but  no  place  or  further  description   

v  B ;  L ;  R ;  first  v  g,  then  v  s,  v  m  b  M ;  3'   

vB;  R;  psmbM;  40" ;  has  asfcnf   

v  B ;  the  3d  of  3,  seen  but  no  place  taken  or  further  description .... 
F;  vmE;  vglbM;  2'  1,  20"  br  ;  a  *  7  m  precedes  in  parallel 

B;  R;  vsvmbM;  20"   

B;  R;  psmbM;  40"  

F;  S  ;  E ;  gpmbM;  15";  has  a  *  s  f  (list  2'  

PB;lE;pgmbM;  35"   

pB;  pmE;  gbM;  25"  

p  F ,  E  ;  p  s  1  b  M  ;  40"  1   ,  

F;  S;  R;  15"  

pB;  vS;  psbM;  15"  (clouded)   

F;  vmE;  vlbM;  3'  1,  20"  br;  pos  =  i84°.2  

F;  L;  m  E;  v  g  v  1  b  M;  90"  1   

F ;  S ;  IE;  gbM;  20"  

B;  IE;  psbM   

pF;  S;  R;  psmbM;  20"  

B;  L;  pmE;  smbM;  100"  1,  60"  br  

vB;  L;  mE;  vsvmbM  to  nucleus  =  *  i°m  


Sweep. 

741 

652 

642 
646 

802 
802 
802 
635 


NEBULyE  AND  CLUSTERS  OF  STARS. 


63 


No. 


Synon. 


E.  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


2581 


A.  562 


2582   

2583  II.  458 


2584 


2585 
2586 


2587 
2588 
2589 


2590 
2591 
2592 

z593 
2594 


2595 


!596 
2597 


2598 
2599 

2600 


2601 


III.  249 


II.  460 


III.  962 


A.  427  ?  ? 


A.  480 


A.  438 


3  37 


3  .37 

3  37  22-5 
24.2 

3  37  22.7 
25.6 
25.9 
3  38  5-6 
3  38  54-5 

58-  4 

59-  4 
3  39  52-7 
3  41  2.6 

3  42  55-3 
61.4:: 


126  45  i 


126  23  49 
108  48  21 

48  16 

112  26  34 

27  48 

*7  55 
135  11  6 
135  10  31 
10  5s 
"  53 

127  13  33 
106  55  o 
150  19  58 


3  45  25.9 

162  12  10 

3  46  34-2 

J35    2  13 

37-5 

2  16 

3  46  40.8 

158  44  20 

42.8 

43  3i 

3  46  59-5 

110  57  55 

3  47  6.8 

no  59  22 

8.8 

60  56 

10.5 

60  30 

3  47  35-4 

137  59  4 

36.9 

59  37 

3  48  2-7 

127  29  42 

3  50  2.6 

132  51  37 

3.0 

51  22 

4.2 

53  - 

3  5i  52-2 

125  57  1 

3  52  7-2 

156  30  1 

10. 1 

31  58 

3  S2  7-3 

136  42  5 

12.2 

42  11 

3  52  42-1 

139  23  50 

45.8 

24  5 

Description,  Remarks,  &c. 


B ;  p  m  E ;  pgbM.  The  place  is  taken  from  Mr.  Dunlop's  Catalogue, 
but  I  have  reason  to  believe  this  R  A  too  great  and  the  N  P  D  also  mate- 
rially in  error— perhaps  126  35  would  be  preferable.  It  was  found  by 
sweeping  past  the  meridian. 

®;  v  B,  and  evidently  a  globular  cluster.  Observed  past  meridian,  clouds 
having  prevented  its  place  being  secured  at  the  time  of  transit. 

F;  v  L;  gib  M;  R;  4"   

p  B ;  R  ;  g  m  b  M  ;  40"   

pB;  R;  vsmbMtoa  nucleus  =  %  13  m;  60".  (N.B.  Both  observa- 
tions agree  in  making  the  degree  of  P  D  108 — whereas  it  appears  in  the 
reduction  of  my  Father's  observations  as  109.) 

Fj  S;  R;  gbM;  15'   

pF;  S;  R  j  b  M  ;  20"   

p  B ;  R ;  gpmbM;  40"   

pB;  vL;  vmE;  3'  1,  20"  br ;  pos  =  22i°.6  

F;  v  m  E  in  pos  ==  39°-5  ;  3'  long  

A  ray  nebula  (vmE)vgpmbM;  2'  1 ;  pos.  42°.3  ;  380  is  no  measure. . 

p  B;  vmE;  glbM;  a  ray  nebula,  4'  1,  20"  br ;  pos  =  38°.o   

F  ;  S  ;  R  ;  15"  ;  attached  to  a  star  14  m   

p  B  ;  v  1  E  ;  p  m  b  M  ;  25"   

v  F ;  R ;  g  1  b  M  ;  15".  In  a  constellation  of  B  st  forming  almost  a 
cluster. 

F;  S;  R;  bM;  15";  one  of  a  constellation  with  7  B  stars   

F ;  irreg  R  ;  glbM;  30"  ;  has  a      7  m  f ,  and  others  near  

Viewed  past  merid  ;  found  in  place  ;  pB;  R;  gbM;  30"   

v  F  ;  IE;  gbM;  25"  

F  ;  S  ;  p  m  E  in  the  parallel ;  gbM;  15"  1  

F ;  p  L  ;  R  ;  v  1  b  M  ;  50"  

p  F;  R;  glbM;  25"  

e  F  ;  S  ;  R ;  precedes  2  B  st  and  the  nebula  III.  962  

e  F  ;  S  ;  makes  an  obtuse  angled  nearly  isosceles  triangle  with  two  st  10  m 
n  of  it. 

p  B  ;  IE;  gbM  (newly  polished  mirror)  ;  makes  an  obtuse  angled  triangle 
with  2  st  10  m  to  its  north 

F ;  S ;  R ;  makes  an  obtuse  angled  triangle  with  2  B  st,  the  one  preceding, 
the  other  following  it. 

p  F ;  R  ;  v  1  b  M ;  20".  (Newly  polished  mirror,  but  the  sky  dull  and 
haze  forming ;  so  that  this  may  very  possibly  be  A  428.) 

vF;  pL;  R;  vglbM;  80".  I  feel  convinced  this  nebula  is  too  faint 
to  have  been  seen  by  Mr.  Dunlop.  Put  on  the  9 -inch  aperature, 
could  not  discern  the  least  trace  of  it.  Mirror  polished  yesterday,  and  in 
high  beauty.    Sky  superb. 

vF;  L;  E;  vgvlbM;  2'  

p  B  ;  R ;  gbM;  2'  has  2  st  12  m  near  it   

p  B  ;  p  L  ;  R  ;  90";  makes  a  triangle  with  2  stars  13  m  about  1  radius  of 
nebula  (by  diagram)  from  its  edge. 

p  B  ;  R  ;  2'  near  a  star  

v  F;  v  S;  R;  10'  

p  B;  S;  1  E;  p  m  b  M;  18"  

pB;  S;  R;  bM;  15*   

F;  L;  R;  vglbM;  2^'.  With  9  inches  aperture,  and  a  mirror  newly 
polished  yesterday,  and  in  high  beauty,  it  is  barely  possible  to  discern 
with  the  utmost  attention  that  this  nebula  exists;  but  to  have  discovered  it 
with  that  aperture  and  power  180  would  have  been  quite  out  of  the 
question  ;  possibly,  however,  90  might  show  it  better. 

F;  vL;  R;  vglbM;  3'.    Sky  dull,  a  haze  forming  

F  ;  L ;  R ;  vglbM;  2^' ;  has  north  of  it  a  triangle  of  st  12  m  

F ;  L ;  R ;  vgvlbM;  70"   


Sweep. 


663 


636 

801 

741 
652 

647 
641 
642 
654 
805 
752 

639 
801 
651 
756 

501 
5H 
745 
805 
654 
512 
508 
642 
647 

652 

642 

654 

805 


801 

752 
639 

804 
801 
508 
51s 
805 


654 

744 
526 


64 


REDUCED  OBSERVATIONS  OF 


Svnon. 


2602 


2603 
2604 
2605 


2606 
2607 

2608 
2609 


2611 
2612 
2613 

2614 
2615 

2616 


2617 
2618 


2619 
2620 


2621 


2622 

2623 

2624 
2625 


A.  369  ?  ? 


A.  466 


&.  348 


III.  499 


A.  409  ?  ? 


IV.  26 


A.  600 


R  A.  1830.0. 

h. 

3 

5^  53-7 

543 

58.7 

3 

53  464 

3 

55  "-6 

2 

<;<;  <;8.-? 

3 

57  59± 

63.3 

3 

58  20.0 

21.2 

22.8 

3 

58  55.2 

56.1 

584 

3 

59  56-° 

3 

59  57  o 

58.! 

4 

0  25.6 

4 

0  51.8 

4 

1  48.6 

5°-3 

4 

2  4.9 

4 

3  8-9 

4 

3  23-8 

26.O 

4 

3  54-o 

*r 

A  AQ.O 

4 

5  11.0 

4 

5  23-7 

24.9 

27.9 

4 

5  29.2 

30.4 

32.4 

4 

6  1 1.4 

12.8 

4 

6  37.1 

6  37.6 

4 

7  7-8 

4 

7  26-3 

N  P  D.  1830.0. 


134  58  37 

57  37 

58  18 

142  48  47 
156  30  55 

143  2  44 
3  4i- 

133  52  37 

S2  38 

133  48  57 
49  37 

49  38 
158    6  5 
6  25 

6  47 

144  33  48 
35  ± 

99  17  15 

17  19 

in  37  55 

in  30  30 

143    7  39 

7  3° 
*44  33  29 
167  17  58 

138  21  11 

20  13  : 

156  17  o 
17  56 
103  10  13 


153  20  51 
123  17  + 

17  6 

*7  55 
123  19  14 

18  11 

19  10 

*46  34  5 
33  55 
153  13  11 

15  1 
121  59  22 
146  55  6 


Description,  Remarks,  &c. 


Sweep 


F ;  E  in  the  parallel ;  v  g  v  1  b  M  ;  60"  1,  40'  br  

e  F;  IE;  S  

F ;  p  m  E  ;  precedes  2  bright  stars  

F  ;  v  S  ;  R ;  p  m  b  M  ;  12" ;  has  *  8  m  i5'.5  prec  in  R  A,  to  northward 

e  F;  S  ;  R;  (a  doubtful  object.)    Has  a     n  p,  10  m,  3'  dist  

e  e  e  F  ;  S  ;  R ;  between  2  st  12  and  13m   , 

eeeF;  S;  R;  RA  not  taken  on  the  wires ;  requires  a  negative  swing 
correction,  being  past  meridian. 

F;  R;  vgpmbM;  80".    Not  resolved.   A  companion  to  A  466  

F;  R;gpmbM   

© .    B  ;  p  L ;  R ;  3'  diam.    Resolved  into  stars  barely  perceptible  

B  ;  L  ;  1  E  ;  p  s  b  M  ;  3'.    It  is  just  north  of  a  great  group  of  large  stars 

6,  7,  and  8  m,  scattered  over  two  or  three  fields, 

B;  R;  gpmbM   

p  B ;  m  E  ;  v  g  b  M ;  90"  1 ;  pos  i25°.5   

B  ;  m  E  ;  p  g  b  M ;  90'  1,  15"  br ;  pos  1 17°.6   

pB;  pmE;  S;  glbM;  25  or  30".  (Cloudy.)  

B;  L;  vmE;  gbM;  3'  1,  40"  br  

B;  L;  vmE;  s  b  M  (by  diagram) ;  pos  =  io°.o  +  ;  P  D  rough. 
Transit  missed. 

v  F ;  first  v  g,  then  p  s,  v  m  b  M  ;  20"  

eeeF.    So  very  faint  that  I  almost  doubt  the  observation  

B  ;  L ;  p  m  E  ;  gbM;  has  a  s(c  8  m  s  p  3'  or  4'  dist   

p  B  ;  R  ;  b  M  ;  barely  in  time,  and  too  late  for  a  good  observation  

e  e  F ;  v  S  ;  R  ;  12".    In  a  very  dark  field  ;  no  *  13  m  within  5'   

vF;  vS;  R;  vlbM;  12"  

vF;  R   

A  poor  cluster  of  about  a  dozen  stars  9  ...  12  m  within  a  space  of  about  5', 
the  largest  taken. 

B  ;  E  ;  spmbM,  growing  more  R  internally  ;  60"  1,  30"  br ;  pos  770  . . 

p  B  ;  E  ;  v  s  b  M  to  a  roundish  nucleus  

pB;  pmE;  vsvmbM;  seen  in  sweeping  in  vain  for  A  409   

F  ;  R  ;  glbM;  among  B  st ;  one  =  9  m,  3'  n  

eF;  vS;  R;  glbM;  12"  

B ;  S  ;  R  ;  first  p  s,  then  v  g  b  M  ;  20".  A  mottled  disc,  but  so  hazy  at 
the  borders  that  I  have  no  doubt  of  its  being  a  very  distant  and  highly 
compressed  (f).  It  is  not  a  planetary  nebula,  though  a  near  approach  to 
one  :  does  not  bear  magnifying.  A  power  of  320  is  of  no  use.  A  very 
remarkable  and  interesting  object.  (N.  B.  The  minute  of  R  A  certainly 
correct.) 

vF;  S;  R;  gbM;  15"   

B  ;  R  ;  p  s  b  M  ;  60".    The  n  p  of  two.    (PI.  V.  fig.  11.)  

p  B  ;  R ;  p  s  1  b  M  ;  pos  from  the  following  neb  =  3i7°-9   

F  ;  R ;  b  M  ;  60".    The  preceding  of  two  

a  B  ray  ;  p  s  m  b  M  ;  4'  1 ;  the  s  f  of  two.    See  fig.  11,  Plate  V  

p  s  b  M  ;  full  7'  long  ;  position  32°.2  

B  ;  v  L  ;  vmE;  5'  long.  A  fine  and  curious  object.  The  following  and 
brighter  of  2.    In  the  ray  is  either  a  v  F  *  or  a  knot  in  the  nebula. 

v  B  ;  R  ;  has  2  st  n  f   

vB;  pL;  R;  smbMtoa  stellar  nucleus.    Has  2  st  10  m  n  f  

F  ;  S  ;  R.    Has  a  v  S  star  foil.    Dist  1 J  rad  of  neb  (by  diagram)  

F ;  S  ;  R.    Has  a  v  S  star  1  diam  s  f  

vB;  IE;  psvmbM;  50"  1 ;  40"  br   

v  F  ;  R ;  p  L ;  v  1  b  M  ;  60"  


NEBULjE  and  clusters  of  stars. 


65 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


2626 

2627 
2628 

2629 
2630 

263 1 

2632 

2633 
2634 

2635 

2636 

2637 
2638 
2639 
2640 

2641 

2642 

2643 
2644 


2645 
2646 
2647 
2648 

2649 
2650 

2651 


2652 
2653 


A.  338  ?  ? 


A.  339? 


4  8 

4  9 
4  10 

4  11 
4  12 

4  13 

4  14 

4  14 

4  15 


19.5 
20.7 
23.5 
57.8 
60.1 
30+ 
32.2 

7.6 
8.0 
0.5 
0.8 
11.3 

34.6 
35.8 


4  16  11. 1 

12.8 
4  16  17.9 

4  16  44.8 

4  16  48.2 

4  16  58.8 

4  18  37-7 

4  19  25-7 
27.0 
27.1 

4  20  57.2 
58.1 

4  2 1  59-4 
4  22  26.8 


4  22 
4  23 
4  23 
4  23 

4  24 

4  27 


4  27 


35-3 
35-1 
39-4 
33-5 
45.0 
55.6 
56.0 
8.3 
9.6 
21.8 
23.9 
25.4 

53-  7 

54-  3 


4  31  2.1 
4  3i  36-7 


N  P  D.  1830.0. 


Il8  54  31 

55  16 

148  10  10 

146  29  20 

29  42 

146    o  18 

146  12  1 

12  38 
140  34  40 

34  35 
135  26  23 

26  16 
160  50  55 

153  12  30 
1 1  52 

145  20  39 


J38  39  43 

133  51  49 

134  1  19 
130  59  22 
147  22  7 

141  59  22 
59  4 

59  39 
145  19  47 

20  8 
132  31  47 
117    5  2 

4  58 

4  36 

117  20  + 

138  11  9 

138  9  24 
145  24  16 

24  24 
145  26  25 

25  42 
134   4  54 

4  44 
3  37 
144  57  42 

58  33 

no  59  17 
162  11  55 


Description,  Remarks,  &c. 


v  F ;  E  ;  r.    Rather  a  doubtful  object   

The  suspected  nebula  of/  511.    Certainly  verified  ;  v  F ;  g  v  1  b  M  ;  15" 

B;  pL;  pmE;  smbMtoa  round  nucleus  =  sfc  n  m  

p  B  ;  R  or  1  E  ;  b  M  to  an  elongated  nucleus   

pB;  IE;  g  b  M  to  an  extended  nucleus.    AD*  precedes  

B;  R;  40"  

v  B  ;  R ;  g  m  b  M  ;  60"  between  3  stars   

B  ;  R ;  in  a  triangle  formed  by  3  stars   

vF;  S;  R;  vglbM;  20"   

F;  R;  25"  

pF;  IE;  glbM;  25"  long  

pF;  pmE;  gpmbM;  25"  1,  15"  br.    [Min  of  R  A  by  obs  15]  

A  star  7  m  chief  of  a  cluster  8th  class — about  20  in  number,  loose  and 
straggling. 

v  B  ;  L  ;  m  E  ;  g  m  b  M  ;  r ;  2'  1,  1'  br   

B;  L;  mE;  vgpmbM;  90"  1,  40"  br ;  has  a  *  14  m  at  the  southern 
edge. 

B  ;  v  L  ;  first  v  g  then  s,  m  b  M  to  a  stellar  nucleus.  Diameter  in  R  A  = 
15s.  A  star  11  m  involved,  n  p,  gives  it  a  distorted  appearance.  A  curi- 
ous object. 

p  B  ;  L  ;  R  ;  v  g,  then  p  s,  b  M  

vF;  S;  R;  glbM;  20"  (hazy)  

Found  in  place  and  viewed  past  merid  ;  not  vF;  S;  R   

F;  S;  R;  gbM;  20"  

v  F ;  S  ;  R  ;  1 5"  g  b  M  ;  has  a  double  star  n  f  

p  F  ;  S  ;  R ;  15";  has  a*  13  m,  1'nf  

p  B  ;  S  ;  R ;  p  g  b  M.  Has  a  sfc  10  m  60"  dist  and  one  14  m  dist  one 
radius  of  neb  from  its  edge,  both  s  f. 

nor  vF;  R;  gpmbM;  20"  

vF;  S;  R;  pslbM  

vF;  S;  R;  pgbM,  dilute  at  the  borders   

F;S;  E;  gbM   

F;  S;  1  E;  glbM  

p  F ;  S  ;  R ;  g  b  M  a  #  12  m  prec  i\o  ;  pos  from  centre  of  neb  =  287°.8 

not  vF;pL;R;gbM.    (N.B.  Time  of  transit  somewhat  confusedly 

stated  in  MS.,  which  renders  a  mistake  of  10s  not  improbable.)     See  the 

next  observations. 

vvF;  R;  gbM;  15"   

pF;  S;  R;  gib  M  15"  

v  F;  v  S  

v  F  ;  R ;  b  M  ;  15"  

F ;  R ;  b  M  ;  20"  

B;  mE;  pL;  psmbM;  60"  1.   The  preceding  of  2  

B  ;  m  E  ;  s  m  b  M  ;  60";  pos  =  1 5°.o  

e  F  ;  L  ;  roundish  undefined.    The  following  of  2   

e  F  ;  p  L  ;  IE;  the  following  of  2  

pF;  S;  psbM  

F;  S;  vlE;  vlbM;  20"   

F;  pmE;  vglbM;  20"  

p  B  ;  L  ;  m  E  ;  s  b  M  ;  3'  1,  2'  br  ;  pos  i05°.8  

B  ;  L  ;  m  E  ;  first  v  g  then  v  s,  m  b  M  to  a  nucleus  5"  in  diameter ;  3'  1 ; 
i'  br. 

A  nebula.    No  description   

v  F  ;  R  ;  g  1  b  M  ;  60"   


S 


66 


REDUCED  OBSERVATIONS  OF 


No. 


2654 

z6SS 
2656 

2657 


2658 
2659 

2660 
2661 


2662 


Synon. 


II.  522 
h.  326 


A.  296  ?  ? 


Nubecula 
Major 


R  A.  1830.0. 
h.  m.  s.  d. 

N  P  D.  1830.0. 
0      /  // 

4  32  30.4 

98  56  6 

4  33  16.3 

107  19  40 

4  35  22.1 

ic6    8  2.1 

4  36  58.0 

I  c6   71  CO 

60.9 

31  27 

64.0 

30  56 

4  38  30.2 

131  48  31 

4  38  39.1 

131  50  20 

4  38  43-3 

!59    8  37 

4  38  47-9 

!58  59  54 

49.9 

59  32 

49.9 

60  21 

A      1  5  r"Q 
4"     3°  5"'® 

160  55  1 

_  Q  _ 

5<).2. 

54  53 

58.3 

55  12 

4  4'  5-4 

'35    5  26 

4  42  13-3 

156    7  25 

4  43  2.8 

J49  33  33 

5-5 

33  8 

4  43  29.2 

122  15  14 

32.4 

16  42 

4  43  46-8 

160    7  20 

4  43  49-9 

138    6  48 

52.2 

6  19 

52.4 

7  5 

4  44   

i6o°45'..i6i° 

4  44  26.0 

159    7  48 

4  45  °-9 

124  13  21 

4.6 

13  47 

4  45  48-7 

150    5  11 

52.8 

5  22 

55-4 

5  16 

4  48  31-5 

!59  37  57 

35-3 

38  44 

4  48  40.0 

159  40  7 

41.3 

40  13 

4  48  5i-4 

158  3°  31 

4  49  5-9 

T  C  8     f  O    A  T 

7.6 

50  42 

8.0 

5i  4 

8.8 

49  51 

9-7 

5°  39 

4  49  I4-1 

120    9  23 

14.8 

8  42 

17.0 

9  21 

4  49  51. 1 

159  23  46 

Description,  Remarks,  Sec. 


F ;  R ;  gbMj  40";  near  some  small  stars 


e  F ;  v  S  ;  R  ;  between  2  stars   

p  L;  p  rich;  irreg  R  cluster;  p  m  comp  M;  5';  stars  11  16  m.... 

F;  R;  gb  M;  30"  

p  B;  S;  R;  gbM;  15"  

v  F  ;  R ;  gbM;  30"   

F;  p  m  E;  gib  M;  40"  

v  F  ;  1  E  ;  g  1  b  M  ;  20"  

F  ;  R  ;  g  b  M  ;  30"  

v  F;  S  ;  R  

v  F ;  S;  R;  gbM;  12"  

F;  R;  gbM;  35"  

p  F;  L  ;  R;  gv  1  b  M;  2'  diam  

v  F  ;  L  ;  R  ;  v  g  1  b  M  ;  l\'  diam  

pF;L;  lE;gbM   

e  F ;  R  ;  attached  to  a  star  14  m  

e  F;  S;  R  

B;  L;  pmE;  svmbMtoa  nucl ;  z\'  1 ;  1 \'  br  ;  a  %  12  m  involved . . 
B  ;  L  ;  m  E  ;  first  g,  then  p  s  m  b  M  ;  4'  1 ;  1  ^  br  

p  B ;  L  ;  irreg  R ;  surrounds  a  ^  i:  m,  touches  two  1 1  m  and  has  a  fainter 
just  at  the  edge. 

p  B  ;  L  ;  irreg  R ;  involves  4  stars,  and  is  v  g  b  about  the  chief  of  them  . . 

v  F  ;  S;  attached  to  a  star  10  m.    A  doubtful  object   

e  e  F ;  R  ;  r,  or  else  stars  seen  on  it.    Well  defined  (hazy)  

v  F ;  S  ;  R  ;  very  near  a  star  15m  

F  ;  R  ;  r,  or  has  some  v  F  stars  involved   

Lower  part  of  zone  begins  to  be  filled  with  the  faint  light  of  the  Nubecula 
Major.  At  4h  47  "  this  light  increases,  and  we  are  evidently  on  the 
skirts  of  the  Nubecula.  At  4h  50'" ;  N  P  D  =  1600  2'  stars  from  12  to 
15m  are  now  very  numerous. 

v  F  ;  irreg  R  ;  90"  ;  r  

v  F ;  R  ;  gbM;  20"  

e  F;  R;  v  lb  M  

B  ;  R ;  first  g,  then  p  s  1  b  M  ;  60"  

vF;  pL;  R;  gbM;  50"  

p  B  ;  irreg  R ;  p  g  m  b  M  ;  60"  

F;  S;  R   

F;  S;  R.    (Sky  hazy.)   

F;  S;  R  

F;  S;  R.    (Sky  hazy.)   

v  F;  E  ;  vlb  M  

p  B  ;  R  ;  v  g  1  b  M  ;  40"   

®.  p  B ;  R ;  g  1  b  M  ;  90".  Resolved.  With  the  left  eye  I  see  the 
stars.  (N.  B.  The  degree  is  159  in  the  original,  but  this  is  a  manifest 
error,  the  zone  swept  not  extending  so  far  as  159.50.) 

pB;  pL;  R;  gbM;  50"   

p  B ;  R  ;  g  1  b  M  ;  70".    Has  a  *  10  m  3' s  f   

p  B;  L;  R;  gib  M;  80"   

F ;  S ;  R ;  g  1  b  M  ;  20".    Has  a  *  9' m  s  f,  90"  dist   

p  F ;  IE.    Has  a  if.  10' m  sf  dist  60"   

F;  S ;  R ;  20".  A  star  10  m  sf  and  a  small  D  *  s  p.  (N.  B.  The  R  A 
is  4.50  17.0  by  the  original  obs. ;  but  this  must  be  presumed  erroneous, 
as  the  three  observations  manifestly  refer  to  the  same  nebula.) 

B:  R:  elb  M:  60":  r  


Sweep. 

758 

651 

517 
658 
508 
761 
804 
804 
523 

653 
508 

759 
523 
509 

75> 
804 
658 

5i9 
665 
645 

644 

523 
526 
805 
744 
75« 


653 
662 
663 
756 
519 
524 
523 
509 

523 
509 
508 
508 
653 


759 
522 

512 
645 
644 

511 


523 


NEBULA  AND  CLUSTERS  OF  STARS. 


67 


No. 


Synon. 


E  A.  1830.0.  N  P  D.  1830.0. 
h.  m.  s.  d. 


Description,  Remarks,  &c. 


Sweep. 

5'9 
524 

520 
807 
525 
75i 
652 
808 
75i 
523 
748 

75 1 

523 
653 
522 
657 
508 
760 
508 
658 

522 
653 
508 
760 

523 
509 

748 

748 

509 

523 
522 

653 
658 
646 
761 

512 

759 
512 
508 
760 


759 
748 


2678 


2679 


A.  73  ? 


A.  76  i 


4  50  21.5 

24.0 

4  5°  25-9 
28.7 
30.1 

4  5°  4°-3 
4  50  58.6 

4  5°  59-° 
4  5i  5-4 
7.6 

4  51  56.0 
61.4 

4  5i  57-2 
4  5i  58.5 
58.9 
59.0 
59.1 
60.2 

4  5i  59-1 
62.0 

62.4 
4  52  18.8 
19.7 
20.6 

4  52  5M- 
51.6 

55-2 
4  53  8.8 
12.6 

!3-5 
4  53  21.4 

21.5 
21.7 

4  53  37-9 
4  53  47.0 

4  53  5°-3 
50.3 
4  54  16.2 
4  54  18.2 


4  54  23-3 
4  54  42± 


150 


o  51 


143  38  10 
38  10 

38  H 
160  8  32 
no  37  36 
153  16  25 

l6o     2  2 

2  26 

160   15  43 

l6  12 

159  42  46 
157   12  O 

11  II 

12  45 

11  12 

12  7 
157  10  + 

11  40 

10  31 
157  19  46 

19  31 
19  36 
x59  4o  55 

39  47 
39  36 

159  37  26 
36  43 

36  55 
157  11  1 

11  45 
11  40 

116  17  25 

156  56  36 

>58  55  9 

55  20 

159    2  8 

157  21  31 
22  4 


158  20  11 

159  27  .. 


F  ;  L  ;  R ;  v  1  b  M  ;  90" ;  very  dilute  at  borders.    A  star  9' m  s  f  almost 
involved. 

F;  pL;  R;  vglbM;  50".    Has  a  very  delicate  and  beautiful  1st  class 
double  star  attached. 

B;  S;  R;  pmbM;  20"  

pB;  S;  R;  gpmbM;  15"   

vF;  S;  R;  psbM;  20" ;  very  dilute  at  borders   

A  v  F,  S,  cluster   

pF;  pL;  R;  glbM;  50"  

F;  R;  vglbM;  40"  

eF;  S;  E;  40"  1;  r  

B;  R;  b  M;  90"  ,  

B;  S;  R;  r  

0 ;  B  ;  irreg  R  ;  g  b  M.    Resolved  into  st  14  m,  with  outliers  as  far  as 
4'  diam. 

A  p  B,  S,  cluster   

vB;  S;  IE;  psbM.    Double  or  extended  wedge-shaped   

v  B  ;  E  or  binuclear ;  in  b  M  ;  40"  1.    The  s  p  of  two   

vB;S;pmE   

v  B  ;  S  ;  E  ;  b  M  ;  1 5".    Has  another  v  F  neb  nearly  north  

v  B  ;  R  with  an  appendage  ;  g  m  b  M  ;  30"  

v  F  ;  the  n  f  of  two   

e  F;  R ;  pL;  the  2nd  of  2,  making  a  lozenge  with  the  other,  and  two 
stars. 

v  F  ;  S  ;  R  ;  s  b  M  ;  the  n  f  of  two   

F;  R;  b  M;  20"  

F;  R;  b  M   

pF;  R;  vglbM;  60"  

p  B  ;  S.    A  knot  of  clustering  stars   

F  ;  S  ;  R.    (Sky  hazy.)   

The  second  of  a  series  of  clustering  patches   »  

The  third  of  a  series  of  clustering  patches.  Oval  

A  rather  poor  irreg  R  cluster.    (Sky  hazy.)   

A  cluster,  p  B  ;  p  m  E  ;  3'  1,  90"  br ;  stars  12  m  

A  double  star,  the  chief  of  a  p  Rich,  p  L,  cluster  of  loosely  scattered  st ; 
1  comp  M  ;  8' ;  stars  11  15  m. 

A  poor  loose  cluster  8'  diam  ;  stars  10  ....  15  m  ;  chief  D  sfc  taken  

A  double  star,  the  chief  of  a  poor  loose  cl  3  or  4'  diam   

v  F ;  v  L  ;  v  m  E  ;  v  g  v  1  b  M  ;  4'  1,  2^'  br  


e  F  ;  R ;  g  b  M ;  40".     A  very  starry  field  follows  this,  and  hereabouts 
may  be  said  to  commence  the  denser  part  of  the  Nubecula  Major. 

A  S  double      ist  class  in  centre  of  a  S.  R.  neb   

v  S  ;  R ;  12"  

pB;  L;  R;  gmbM  

F  ;  v  S  ;  R  ;  has  two  or  three  stars  appended   


pB;  S;  R;  has  two  stars  appended  forming  an  arc  with  the  nebula.  (N.B. 
This  obs  makes  the  R  Ah.  54.2.1,  but  having  been  made  in  a  hurried 
and  somewhat  irregular  manner  when  the  nebula  was  leaving  the  field,  it  is 
most  likely  that  the  sliding  eyepiece  was  not  brought  fully  up  to  its  bear- 
ing ;  a  source  of  error  which  has  on  more  than  one  occasion  produced  em- 
barrassment.   The  R  A  adopted  is  liable  to  no  objection.) 

B;  R;  r  

v  F ;  S  ;  the  first  of  a  trapezium  of  4  neb.  Place  estimated  from  those  of 
the  2nd  and  4th. 


68 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


2699 

2700 
2701 

2702 
2703 
2704 
2705 
2706 
2707 
2708 
2709 

2710 


2711 


2712 

2713 
2714 

2715 


27 16 


2717 

2718 
2719 
2720 

2721 
2722 


A.  114 


A.  167 


III.  500 
h-  345 
A.  169 


R  A.  1830.0. 
h.  111.  s.  d. 


4  54  58-8 
60.5 

4  55  4-4 
4  55  n-3 
14.0 

4  55  i8± 

4  55  21.5 

4  55  24-° 

4  55  33-1 

4  55  41-5 

4  55  48-3 

4  55  54-3 

4  56  13.0 


4  58 


N  P  D.  1830.0. 


159  28  O 

28  14 

128  57  46 

157  26  29 
26  IO 

159  26  .. 

158  27  14 

159  27  54 

160  4  47 

158  28  29 

159  30  9 

160  42  37 
156  46  38 


14.6 

156 

43 

49 

1 5.0 

43 

19. 1 

43 

45 

22.1 

156 

40 

19 

23.6 

40 

5 

28.3 

39 

31 

30.5 

39 

46 

39-4 

40 

10 

32.0 

152 

J7 

4 

33-6 

16 

46 

44.8 

i57 

57 

23 

IO.I 

99 

*3 

10 

14. 1 

158 

40 

17 

51.2 

40 

31 

24.5 

156 

42 

46 

26.2 

42 

10 

27.1 

43 

3 

27.5 

4* 

1 1 

29.2 

43 

0 

27.7 

160 

28 

43 

35.2 

29 

17 

27.8 

158 

30 

47 

32.7 

102 

6 

40 

32.7 

153 

33 

25 

47.1 

156 

36 

4i 

0.5 

159 

48 

*9 

i-5 

48 

57 

2.3 

48 

57 

Description,  Remarks,  ice. 


R  ;  g  b  M  ;  2'  (thick  haze)   

B  ;  R  ;  resolvable  ;  No.  2  in  a  group  of  four  forming  a  sort  of  lozenge  .  — 

vF;  pL;  vglbM;  90"   

A  star  9  m  in  a  faint  cluster  of  6th  class  

A  H«  9  in  in  the  centre  of  a  poor  cluster  of  v  S  stars  4'  diam   

F ;  S  ;  No.  3  in  a  group  of  4.    Place  estimated  from  No.  2   

v  F  ;  R ;  the  preceding  of  two  in  the  field  

p  B  ;  v  S  ;  R  ;  No.  4  in  a  group  of  4  

e  F  ;  irreg  R  ;  2'   

v  B ;  R ;  g  b  M  ;  60".    The  following  of  two  in  the  field  

v  F  ;  S;  R  

F ;  S  ;  R  ;  20".    Has  a  :|!  13  m  close  to  edge  (about  450  sf  by  diag.)  .... 

A  very  faint  small  nebula  with  3  v  S  st  involved ;  place  deduced  not  from  a 
sweep  but  from  a  drawing  carefully  made  of  its  configuration  with  the 
neighbouring  nebula,  especially  of  the  cluster  f  653,14.  See  fig.  3.  PI.  III. 

Chief  s|{  9' m  in  a  L  loose  cluster   

Place  of  a  very  close  double  star  in  a  cluster  class  6  

A  cluster,  6th  class.    (Plate  III.  fig.  3)  

A  v  B,  v  L  neb  with  stars  (the  chief  of  which  in  the  anterior  part  of  the  neb 
taken)  of  a  crooked  rounded  oblong  shape.  A  fine  object.  See  fig.  3.  PI. 
III. 

B  ;  4'  1 ;  a§'  br  

v  B  ;  v  L  ;  m  E  ;  stars  seen  

v  B  ;  v  L  ;  irreg  oval  figure  with  stars  in  it   

v  B  ;  v  L  ;  irregularly  extended,  irresolvable  but  thickly  dotted  with  many 
distinct  stars.  (N.B.  The  discordance  in  R  A  arises  in  part  from  the 
great  magnitude  and  irregular  shape  of  the  object,  and  the  want  of  a 
natural  centre  of  reference :  partly,  however,  to  the  state  of  the  reductions 
in  this  sweep  which  are  not  very  satisfactory.) 

F;  S;  R;  b  M;  15"   

vF;  S;  R;  glbM;  15"  

v  F  ;  S  ;  R  ;  15".    The  zone  here  is  full  of  grouping  and  clustering  stars  .  - 

p  B  ;  R  ;  g  b  M  ;  It  is  visible  in  strong  3  and  is  much  brighter  than  II.  522 
or  III.  399. 

Cluster  of  6th  class;  p  Rich;  L;  irreg  fig ;  b  M  ;  st  11  ....  18;  fine 
object. 

A  star  9  m  the  chief  of  a  cluster  of  6th  class  4'  in  diam  ;  nebulous.  The 
most  condensed  part  is  1'  south  of  the  stars.  (N.B.  In  the  former  obs 
it  does  not  appear  that  this  particular  star  was  taken,  nor  what  centre  of 
reference  was  fixed  upon.) 

p  B  ;  p  L  ;  with  one  conspicuous  star.    See  fig.  3.  PI.  Ill  

A  star  10  m  involved  in  F  neb  2'  diameter  

A  star  in  the  centre  of  a  B,  L,  R  nebula   

vB;  vsmbMtoasfc  10  m  which  is  double  or  triple.  Other  clusters  and 
nebulas  in  field. 

B  ;  irreg  R ;  2' ;  has  a  ^  10  m  in  centre  

F;  S  ;  R;  g  b  M  ;  25"   

v  F  ;  R  ;  30".  Taken  at  leaving  the  field,  which,  in  so  faint  an  object,  is  a 
source  of  uncertainty  in  R  A. 

F ;  R  ;  g  b  M  ;  20"  

p  B ;  p  L  ;  irreg  R;  orvlE;  vgbM;  80"  among  p  B  st  

vF;  mE;  glbM;  25"!;  in  field  with  many  B  and  1  v  B  *  7' m  n  p  the 
neb. 

p  F  ;  p  L  ;  irreg  R  with  2  or  3  B  st   

An  irreg  R,  comp  cluster,  b  M  ;  40"  diam  

p  B  ;  S  ;  R  ;  40";  r  ;  preceded  by  a  hook  of  stars  12  m   

p  F ;  R  ;  r  ;  among  numberless  stars  


NEBULAE  AND  CLUSTERS  OF  STARS. 


69 


No. 


2723 


2724 
2725 
2726 

2727 

2728 
2729 


2730 


2731 
2732 

2733 
2734 
2735 

2736 

2737 

2738 
2739 


2740 


2741 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


A.  531 ? 


A.  81 


A.  549 


A.  233  ? 


2742 
2743 
2744 

2745 
2746 


A.  235 


N  P  D.  1830.0. 


4- 

58  1 1-4 

157  29  55 

11.7 

29  51 

12.2 

29  36 

A 

58  20.4 

156  40  41 

4 

58  36.3 

160  41  7 

4 

58  38.1 

156    14  l8 

40.7 

14  I5 

4 

58  54.9 

159    38  4O 

55-6 

39  12 

4 

59  15-1 

164  32  25 

4 

59  20.6 

J57  59  H 

25.1 

59  4° 

_  c  * 
20.5 

00  0 

4 

59  20.7 

128  13  4 1 

23.8 

14  36 

h  ± 

4 

59  47-o 

156  5  15 

c 

J 

O  -3.1 

122  11  11 

c 

0  2.Z.1 

162    8  14 

5 

0  36.5 

160  24  25 

5 

0  37-3 

151  21  58 

42.1 

22  1 1 

5 

0  46.2 

159  48  11 

52.2 

47  43 

5 

1  5.2 

139  48  18 

c 

J 

1  12.9 

160    2  12 

c 

5 

1  45-3 

T  CO    CO    A  CI 

AC  8 
45. s 

51  I4 

48. 1 

C  T  IT 

CO. I 

CO  CI 

c 

I  48.0 

127    AA  1A 

46  ± 

5 

I  56.2 

156  20  56 

57.0 

20  46 

58.3 

20  II 

59.2 

20  15 

59-7 

20  48 

5 

2  1.0 

159    19  14 

3-4 

19  40 

5 

2  6.3 

II9  29  44 

7± 

31  ± 

5 

2  17.0 

119  28  51 

17.3 

28  14 

5 

2  36.3 

158    13  47 

5 

3  5-i 

156   37  I 

5-4 

36  30 

6.5 

36  55 

7-5 

36  31 

7-9 

36  38 

Description,  Remarks,  &c. 


p  F;  R;  pgb  M  

vb;  S;  R;  smbM;  20"  (evidently  better  seen)  

B ;  R  or  oblong ;  pretty  evidently  a  double  star  with  a  nebula  about  it  ... . 

v  F  j  S;  R;  g  b  M  

ttF;  irreg  R  ;  2'   

pB;  L;  R;  gbM;  2'   

B;  L;  R;vgpmbM;  r;  3'  

B  ;  R;  pmbMj  35";  r   

©;  B;  S;  R;  r  

e  F  ;  E  ;  attached  to  and  following  a  D  H:  (9  =  9  m)  

vB;  R;  v  s  m  b  M ;  30"   

v  B  ;  E  ;  S.    Stellar,  like  a      9  m  blurred  

vB;  S;  R;  svmbM;  15"  

B  ;  v  L  ;  m  E  ;  regular  elliptic  ;  res.    I  see  several  small  st  in  it  

v  B  ;  v  L  ;  m  E  ;  g  1  b  M  ;  5'  1,  2'  br ;  pos  3 140  stars  seen  in  it.  Visible 
with  C  and  lamp  illumination. 

vB;  vL;  vmE:  gbM;  4'L    Taken  as  A  531  but  too  late  for  transit, 
the  observation  having  been  missed  by  relying  on  Mr.  Dunlop's  place. 

p  Rich  cl  of  S  stars  which  fills  field.   In  northern  edge  of  the  Nubecula  Major. 

pB;  pmE;  gpmbM;  has  a  ^c  1 3  m  following  

v  F  ;  R  ;  v  g  1  b  M  ;  40"  

e  F;  R;  25'  

pB;  pmE;  vglbM;  40"  1  

F ;  pmE;  gbM;  70"  1  25"  br  

v  F ;  S  ;  R  ;  g  1  b  M  ;  30"  insulated  

p  B  ;  R  ;  b  M  ;  60"  

F;  S;  R;  vglbM;  query  whether  a  ^  11.12  m  near  it  s  f  be  not  also 
nebulous. 

F;  pij  IE;  2'   

F ;  R ;  gbM;  40"  

F;  R;  gbM;  90"  

F ;  S  ;  R  ;  g  1  b  M  ;  45".    The  preceding  of  two  in  the  field  

B;  L;  R;  vgbM;  2*'  

B ;  E ;  3'  1,  90"  br ;  in  a  field  strongly  illuminated  by  the  C  in  her  first 
quarter. 

B ;  L  ;  IE;  first  g,  then  p  s  m  b  M.    Transit  missed,  P  D  very  rough .... 

B;  S;  R;  p  sb  M  

vB;  vS;  vsvmbM;  a  condensed  knot  of  stars,  two  of  which  (one  on 
either  side)  are  exterior. 

B  ;  S  ;  R  ;  s  b  M  ;  25";  has  2  st  very  near,  one  n  p,  one  s  f  

A  v  S  compact  cl  of  st  11  m'  with  (?)  nebulosity ;  20"  

B ;  S  ;  R  ;  has  s|c  12  m  n  p  

F  (?) ;  R  ;  b  M.    (Thick  haze  in  sky)  

F;  S;  R;  30"  ..  

p  F  ;  S  ;  IE  the  preceding  of  2   

v  F ;  E  ;  place  roughly  deduced  from  that  of  its  companion  

F;  S;  R;  glbM;  1 5"  the  following  of  2   

F  ;  S  ;  R  ;  the  following  of  2   

pb;  L;  gbM;  3'   

Nebula  ;  no  description  but  that  it  has  a  ©  following  it   

p  F;  R;  lbM;  25"  

e  F  ;  S  ;  R  ;  15"  precedes  a  globular  cluster  

v  F;  R;  lb  M;  40"  

F;  S;  R  


X 


70 


REDUCED  OBSERVATIONS  OF 


No. 

2747 
2748 

2749 


Synon. 


R  A.  1880.0. 

N  P  D.  1830. 

h. 

m. 

s.d. 

0 

s 

3 

18.1 

159  51 

40 

5 

3 

55.2 

157  32 

IS 

58.9 

31 

59 

s 

3 

58.5 

156  39 

35 

59-5 

39 

15 

59.6 

39 

27 

59.6 

39 

40 

60.3 

39 

3i 

60.5 

39 

26 

5 

4 

0.1 

157  29 

28 

5 

4 

10.2 

127  1 1 

38 

5 

4 

12.4 

160  33 

10 

5 

4 

*5-3 

160  50 

57- 

15-5 

Si 

2 

5 

4 

23.6 

157  29 

13 

5 

4 

24.3 

149  56 

55 

32.3 

^6 

j 

16 

5 

4 

44.8 

156  26 

10 

5 

5 

7-7 

156  27 

20 

5 

5 

9-7 

160  34 

17 

5 

5 

26.2 

155  8 

18 

28.8 

9 

45 

5 

5 

28.0 

158  16 

37 

5 

5 

28.0 

159  36 

4 

28.4 

36 

44 

28.5 

37 

19 

31.9 

36 

45 

5 

5 

43-5 

159  34 

8 

44-5 

34 

9 

4.7.5:: 

36 

5o 

48.5 

34 

5 

5 

0 

14.2 

J59  37 

44 

16.0 

37 

28 

16.0 

37 

34 

18.5 

37 

35 

5 

6 

14.7 

159  26 

17 

5 

6 

16.6 

160  57 

27 

5 

6 

20.8 

158  51 

1 

5 

6 

40.2 

158  39 

48 

s 

6 

45-7 

158.  50 

54 

47.8 

Si 

1 

s 

6 

47-7 

160  56 

11 

49.0 

56 

22 

5 

7 

47-5 

160  45 

1 

68.1 

48 

55 

Description,  Remarks,  Sec. 


2750 
2751 
2752 
2753 

2754 
2755 


2756 
2757 
2758 
2759 

2760 
2761 


2762 


2763 


2764 
2765 
2766 

2767 
2768 

2769 


2770 


A.  236 


A.  246 


B.  895 
A.  170  ? 


p  F  ;  S  ;  R ;  g  b  M  ;  40"  the  second  of  two  in  field  

v  F ;  R  ;  a  nebulous  knot  in  the  s  p  part  of  a  cluster   

The  southern  of  two  nebula?  in  the  same  cluster  of  stars   

0  ;  B  ;  Rich,  compact :  v  m  compressed   

v  B  ;  S  ;  R  cluster  of  distinct  stars  ;  m  b  M  ;  2'  diam  

v  B  ;  R ;  g  m  b  M  ;  30";  has  several  small  st  near  it   

0;  vB;  L;  R;  gpmbM;  100";  resolved.    I  see  the  stars  

vB;  R;  psmbM;  2'  diam  ;  resolved.    The  stars  well  seen   

0;  vB;  S;  R;  vmbM;  resolved ;  has  several  outliers  

v  F  ;  R  ;  another  nebulous  knot  in  the  cluster   

v  F  ;  v  m  E  ;  a  long  ray  through  a  star  11  m  

v  F;  S  ;  R;  r  

F;  R;  b  M   

pF;  vS;  R;  vlbM  among  many  stars  

A  p  L,  Rich,  6th  class  cluster ;  irreg  fig  ;  in  radiating  streaks.  Place  that 
of  a  s):  10  m  (one  of  3  such).  It  is  within  this  cluster  that  the  two  nebulse 
No.  2748  and  No.  2750  occur. 

v  F ;  v  m  E  ;  g  v  1  b  M  ;  90"  1   

v  F  ;  v  m  E  ;  2'  1,  20"  br  ;  pos  =  162.0.  I  prefer  the  former  R  A  as  the 
Zeros  in  f  756  are  more  numerous  than  in./"  524,  and  the  extrameridian 
correction  evanescent  in  the  former  sweep,  whereas  in  the  latter  it  amounts 
to  several  seconds. 

v  F  ;  20";  the  preceding  of  2   

v  F;  20";  the  following  of  2  

The  most  compressed  part  of  a  p  F ;  L  ;  branching  cl  of  stars  12  .  .  .  15  m 

B;  L ;  R ;  g  1  b  M ;  90"  

B ;  R ;  r  with  left  eye ;  25'  diam  

F;  R;  60";  r   

v  F ;  S  ;  R ;  g  b  M ;  20"  

F;  S;  R;  20";  the  first  of  3   

F  ;  the  preceding  of  3   

F;  S  ;  R;  15";  the  preceding  of  3  

F;  p  L;  R;  gib  M;  80"  

F;  S;  R;  25";  the  second  of  3   

The  second  of  3.  Place  roughly  estimated  from  a  diagram  made  at  the  time 
from  those  of  the  others. 

F  •  St ;  R ;  20" ;  the  second  of  2  

vB;  S;  R;  pmbM;  40";  the  last  of  3  

B ;  R;  gbM;  60'   

vB;  R;  pgvmbM;  60";  the  following  of  3   

B ;  R>;  g  m  b  M  ;  30";  the  following  of  3  

B ;  v  v  S  ;  IE;  uniform  in  light ;  10"   

v  F ;  pL;  runs  into  and  forms  the  first  mass  of  a  series  of  clustering  groups 

The  first  nucleus  of  a  clustering  group  of  mixed  stars  and  neb  

Seen.  No  place  or  description  

A  star  7' m,  the  chief  of  a  large  very  loose  clustering  mass   

p  B  ;  irreg  fig  ;  the  following  of  2  in  field  together   

The  second  nucleus  of  a  binuclear  clustering  group  of  mixed  nebula  and  stars 

The  last  of  three  clustering  groups  (hazy)   

The  most  condensed  part  of  a  large  rich  cluster  of  scattered  stars  which  more 
than  fills  field. 

The  general  middle  of  the  same  cluster   

A  star  9  m  the  second  in  magnitude  and  near  the  centre  of  clustering  groups 
which  run  together  and  form  a  cluster  which  fills  the  whole  field,  v  1  comp 
M;  St  11  16.  m 


NEBULAE  and  clusters  of  stars. 


71 


No. 


2771 

2772 
2773 


Synon. 


2774 


2775 

2776 

2777 


A.  508 


2778 
2779 


2780 


A.  170 
or  172 


2781 


2782 


2783 


R  A.  1830.0. 
h.  m.  s.  d. 


5    7  13-5 


7  20.2 
25.1 
7  32-9 

39.6 
39.6 
42.3 


5  7  47-6 
47-9 
47-9 


5    8  5-8 
7.6 

5  8  29.4 
5    8  29-7 

31.7 


9  iS-5 
9  I9  S 
20.3 
23.2 
9  30.6 


33.2 
34.6 

35-4 
36.7 
36.7 

9  44-4 
44.8 
46.0 
48.5 

7-5 
11.5 
11.6 
12.4 
17.7 
5  10  17-9 


5  10 


N  P  D.  1830.0. 


161  58  26 

157  29  20 
29  46 
157  32  31 

31  36 

32  II 
32  9 
32  40 

J57  39  3i 
40  9 
40  21 
4°  55 


159  10  59 
11  21 
161  24  8 
130  14  47 

14  12 


15  ± 

156  30  56 
H7  35  49 

35  5° 
35  5° 
158  57  48 

57  49 

58  2 

58  20 
58  9 

57  48 

157  59  30 

58  58 

58  51 

59  23 
3  21 


159 


'59 


3  o 
3  28 
3  22 

3  45 
2  49 


Description,  Remarks,  &c. 


F ;  R ;  b  M  ;  r.  Hardly  visible  through  a  thick  haze.  The  observation 
makes  the  R  A  6m  13.5,  but  this  is  impossible  from  the  context.  It  may 
be  8m. 

e  F ;  the  preceding  of  2  

v  F  ;  R  •  the  preceding  of  2  

F  ;  R.  FThere  has  been  most  probably  a  mistake  of  105  in  reading  or  register- 
ing tlie  chronometer  committed  here.] 

p  F ;  R ;  gbM;  25";  has  2  s  t  12  m  to  the  north  

pB;  R ;  g  b  M ;  40";  the  following  of  2  

pB;R;gbM;  60"   

F ;  R ;  b  M  ;  the  following  of  2.  [The  seconds  of  R  A  come  out  on  reduc- 
tion 48.3,  but  the  nebula  was  taken  on  leaving  the  field,  and  the  observa- 
tion is  noted  as  unsatisfactory  in  the  MS.] 

p  F ;  vL;  R ;  vgbM;  r ;  3'   

B;  L;  R;  ghM;  3'  

pB;  L;  R;  gib  M;  2'  

pF;  vL;  R;  vgbM;  3';  a  fine  nebula.  [The  R  A  comes  out  jm  27'-^, 
but  this  cannot  be  admitted.  The  nebula  was  taken  at  leaving  the  field, 
and  no  doubt  the  slider  of  the  eye-piece  could  not  have  been  brought  up 
to  its  contact.    The  P  D,  however,  is  good.] 

B ;  E ;  30";  has  a  double  star  in  the  centre  (PL  VI.,  fig.  11)  

B;  S;  R;gbM;  15"  

The  first  and  brightest  star,  9  m,  of  a  cluster  of  loosely  scattered  stars  .... 

Superb  $;  v  B;  R;  first  v  g,  then  svmb  M;  4';  resolved,  the  stars 
barely  visible  in  strong  twilight. 

Superb  0 ;  all  resolved  into  stars  14"' ;  v  s  m  b  M  to  a  blaze  or  nucleus  of 
light ;  diam  in  R  A  =  15  seconds  of  time.  Difference  of  left  and  right 
eyes  in  resolving  this  cluster  very  remarkable.  Returning  from  the  left  to 
the  right  eye,  the  object  (in  comparison)  appears  as  if  glazed  over  with  a 
kind  of  dull  film. 

v  B  ;  R;  v  s  v  m  b  M  ;  3';  all  clearly  resolved  into  stars  from  14  to  16  m 
except  at  the  centre,  where  they  are  massed  together  into  a  blaze  of  light. 

v  F  ;  1  E  ;  g  1  b  M  ;  25"  

F;  mE;  vgvlbM   

F ;  E ;  towards  a  star  11  m  ;  g  1  b  M  30";  has  another  *  9  m,  n  

F  ;  S  ;  m  E  ;  pos  450  n  f  to  s  p.    Has  a*  nmnf  

0;  a  fine  large  cluster  of  st  =  13  m  ;  m  b  M.  [The  preceding  of  3  objects, 
all  of  which  were  taken,  and  the  R  A  therefore  probably  hurried  and  some- 
what anticipated.] 

0 ;  B  ;  R  ;  gbM;  3'  diam  ;  resolved  into  stars  

v  B  ;  L  ;  IE;  v  m  comp  M  ;  3';  r   

v  B ;  L  ;  oval ;  resolved   

p  B ;  S  ;  R  ;  a  cluster  of  s  t  12  m;  diam  1'  

0 ;  v  B  ;  v  m  comp  3'  diam   

pF;  R;  g  1  b  M  ;  30"  

F ;  R  ;  v  g  1  b  M  ;  90"  

F;  R;  gb  M;  2'  

p  F ;  p  L  ;  R  ;  vgbM;  90"  

B;  S;  R;  35"   •  

B  ;  E  ;  gbM;  2' ;  r.    The  second  of  3  objects   

0;  B;  S;  R;  25';  r  

A  cluster  nebula  ;  S  ;  R  ;  p  B  ;  40"   

F ;  R ;  g  b  M  ;  40"  

A  v  B;  L,  Round  cluster  of  stars  12  m,  5'  diameter.  (N.  B.  This  obs. 
must  refer  to  the  general  cluster  in  which  the  former  is  situated  as  a 
nebulous-looking  knot  —  a  combination  of  the  most  ordinary  occur- 
rence in  the  Nubecula  Major,  though  very  rare  in  other  parts  of  the 
heavens.) 


523 
512 
748 
508 


72 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


2784. 


2785 


2786 
2787 
2788 

2789 
2790 
2791 


2792 


2793 


2794 


2795 
2796 

2797 


2798 


2799 


2800 


A.  172  ? 


A.  172 
or  173? 


A.  247 
or  248 

A.  173  ?  ? 


A.  210 


E  A.  1880.0. 
h.  m.  s.  d. 


5  10  3!-S 

32.1 

5  10  41-7 
43.0 
44.8 
46.5 

49-5 
51.9 
53.6 


5  10  52.8 

5  11  3" 
S  11  52.1 


5  12 
5  12 
5  12 


5  " 

5  13 
5  i3 


3-3 
23.5 
27.0 

28.0 
28.4 
29.5 
29.8 

59-5 
60.8 

5-7 

14.8 
15.1 
16.9 


5  13 

5  13  25.0 
5  13  28.9 

31-5 
5  13  29.9 

5  !3  55-2 

5  13  5^-4 

63.9 
S  14  S-6: 


J5-7 
5  14  7-9 
9.4 

5  H  "4 


NPD.  1830.0. 


159  19  40 
20  41 
20  6 

159    6  31 
6  10 

4  57 
6  1 

5  19 

6  24 

5  5° 


155  26  54 
158  57  45 
i74  15  5 

156  20  50 
160  59  2 

158  55  35 

55  26 
55  35 
55  3 
55  36 

157  49  11 

49  25 

155  39  37 

158  57  31 
58  4 

57  25 

159  .... 

156  29  6 
154    8  48 

8  27 
122  19  42 

157  22  33 

157  34  10 

34  3 

159  16  38 


18  21 
157  39  23 

38  9 
157  31  23 


Description,  Remarks,  &c. 


v  B  ;  R  ;  g  m  b  M  ;  50"  

B  ;  R ;  g  b  M  ;  12  seconds  diam  in  R  A  in  time.    Has  a  bright  star  to  s  . . 

B;  p  L;  R;  gb  M;  90"  

Centre  of  a  L  ;  oval ;  r  ;  neb  3'  or  4'  1,  2  J'  br   

A  L,  irregularly  E  cluster  and  neb.    Has  2  bright  neb  n  p  

The  preceding  part  of  a  nebulous  cl  of  irreg  fig  

B  ;  L  ;  irreg  fig ;  Binuclear ;  3'  1,  2'  br.    The  s  f  of  3  

A  bright  cl  of  irregular  figure  

Two  oval  nebulae  joining  

An  irregular  cluster  with  a  nebulous  knot. — [N.B.  This  object,  by  diagrams, 
made  in  several  of  the  observations,  appears  to  consist  of  a  resolvable  and 
irresolvable  portion,  the  general  form  being  that  of  a  somewhat  crooked 
oblong  extended  from  n  p  to  s  f  at  an  angle  of  60  or  jo°  with  the  parallel, 
the  northern  end  being  nebulous,  the  southern  starry.  This  anomalous 
form  and  constitution  will  serve  to  explain  the  apparent  disagreement  of 
these  descriptions  and  places."] 

F ;  S  ;  R ;  v  g  b  M  ;  20";  has  a  *  7  m  n  f,  dist  6'  

F;  R;  vgb  M;  60"   

p  F ;  L ;  irreg  R ;  v  g  b  M  ;  r ;  3'  diam.  (R  A  open  to  much  error  for 
want  of  zero  stars  to  be  depended  on.) 

vF;  R;  30"  

eF;  R;  gvlbM;  90"  

v  B  ;  v  S ;  stellar  ;  has  a  ;jc  np  

B  ;  v  S  ;  R  ;  r ;  15";  has  a  small  star  very  near  the  edge   

avB;  vS;  knot  of  stars  

vB;  S;  R;  20"   

B;  S;  R  

F;  R;  b  M;  60"  

F;  irreg  R;  r;  query,  if  not  a  knot  of  v  S  stars  

vB;  L;  R ;  v  g  m  b  M  ;  2';  r  

vF;  pL;  R;  vglbM;  45"   

tF;  R;  40"  

v  F ;  R ;  20"  

The  southern  part  of  the  field  is  here  illuminated  by  the  faint  light  of  the 
Nubecula  Major. 

eF;pL;R;  2'.   (Sky  dull)  

pF;  pL;  R;  vglbM;  80"   

pB;  R ;  g  b  M ;  30"   

v  F;  L;  R;  v  g  v  1  b  M  ;  2';  has  a  *  12s  prec  and  3'  n  

The  star  (L  C  409,  B  922  6  Doradus  of  the  Brisbane  Catalogue)  marks  the 
northern  limit,  and  the  commencement  in  R  A  or  nearly  so  of  a  great  ir- 
regular series  of  clusters,  more  or  less  connected  by  scattered  stars. 

Cluster  of  7th  class ;  a  fine  L  cluster  of  sc  st  which  fills  the  field.  The 
point  taken  is  in  the  middle  of  3  groups  in  the  most  condensed  part. 

The  first  of  the  series  of  clusters  which  extends  northwards  as  far  as  B  922. 

B;  S;  R;  1  b  M;  in  the  general  irresolvable  illumination  of  the  Nubecula 
Major.  Beyond  the  limit  of  the  sweep,  and  the  right  ascension  in  con- 
sequence liable  to  error  ;  [besides  which,  the  reductions  of  this  sweep  run 
badly.] 

B;  S;  R;  gib  M;  25"  

The  second  of  a  series  of  clusters  which  extend  northwards  as  far  as  B  922 

A  poor  cluster ;  the  southern  of  three  or  four   

The  third  of  a  series  of  clusters  extending  to  B  922   


NEBULAE  AND  CLUSTERS  OF  STARS. 


73 


No. 


Synon. 


2803 
2804 


2805 

2806 

2807 

2808 

2809 
2810 

2811 

2812 
2813 
2814 
2815 

2816 
2817 


2818 
2819 

2820 
2821 
2822 
2823 


2824 
2825 


II.  289 
h.  352 


A.  124  ? 


B.  A.  1830.0. 
h.  m.  s.  d. 


5  H  19-9 

20.1 
20.9 
21. 1 
5  14  22.6 

5  H  27-i 
27.9 
30.7 
31. 1 
5  14  32.0 
5  H  39-° 
5  H  45-7 
5  M-  51-0 

5  15  i3-° 
5  15  15-7 

5  IS  !7-i 

5  IS  42-5 
S  iS  Si-9 
5  15  S8-3 
5  16  24.4 
24.5 
5  16  36.3 
5  17  M 
49 
6.7 
9.1 

5  17  104 
5  17  46.2 
47.6 

5  17  47-4 

5  18  3.8 

5  18  6.0 

5  18  11. 8 

I3-I 
13.3 
15.0 

15-3 
5  18  16.9 

S  I8  33-3 
34.0 

35-4 
36.5 
37.0 


N  P  D.  1830.0. 


159  30  25 

30  13 

30  22 

29  50 

i59  33  55 
159  32  45 

32  55 

33  2 
33  " 

159  33  5° 
101  40  13 

160  39  52 

159  33  46 

156  18  31 
159  29  o 

125  53  26 

156  20  41 

156  30  11 
159    9  21 

155  8  55 
8  20 

162  15  51 

157  3°  25 

30  8 
30  35 
30  49 

159  38  35 

i53  11  4i 

12.  28 

157  37  11 

158  2  57 

159  49  35 

156  47  55 
48  16 

47  44 
47  46 
47  31 

158  45  56 

159  30  19 
30  24 
30  10 

3°  55 
30  37 


Description,  Remarks,  &c. 


p  B  ;  S  ;  R ;  insulated  in  the  recess  of  an  arc-formed  nebulous  cluster.  (See 
plate  III,  fig.  6,  for  this  and  several  following  objects.) 

B ;  R ;  g  b  M  ;  the  preceding  nebula  

p  B  ;  R  ;  g  b  M  ;  2'.    An  arc  of  faint  stars  connects  it  with  another  

p  F ;  R ;  gb  M;  insulated  within  an  arc   

The  south  preceding  of  two,  forming  a  binuclear  nebula  at  the  southern 
extremity  of  an  arc-formed  cluster  of  stars. 

The  north  following  of  two,  forming  a  binuclear  nebula  at  the  southern  ex- 
tremity of  an  arc-formed  cluster. 

p  B ;  r ;  the  most  compressed  part  of  an  irregularly  figured  cluster,  whose 
outliers  form  an  arc. 

The  second,  or  northern  nucleus  of  an  irregular  binuclear  nebula  which  ter- 
minates, to  the  south,  an  arc-formed  cluster. 

B ;  irreg  R ;  (the  following  of  two  very  close)  connected  by  an  arc-formed 
cluster  with  another  (No.  28  of  same  sweep). 

A  3rd  and  v  F  nucleus  of  the  nebular  group  at  the  southern  extremity  of 
the  arc-formed  cluster.    From  figure  of  Jan.  17,  1838. 

p  b  ;  R ;  g  b  M.    Very  visible  in  strong  C  light   

vF;  IE;  gvlbM;  r.    (N.  B.  The  Nubecula  Major  is  here  very  poor, 

and  hardly  any  tiling  of  it  seen.) 
A  fourth  nucleus  at  the  southern  end  of  the  arc-formed  nebula  and 

cluster,  as  laid  down  in  the  figure  of  Jan.  17,  1838.    PI.  III.  fig.  6. 

pF;  R ;  vgvlbM;  3'  diam  mottled  (resolvable)  

v  F ;  follows  a  double  star.     An  outlier  of  the  arc-formed  nebula  and 

cluster.    Laid  down  in  drawing  Jan.  17,  1838,  whence  also  its  place.  See 

Plate  III.  fig.  6. 

A  large  scattered  cluster,  which  more  than  fills  the  field.  Stars  10  ...  12  m. 
Place  that  of  a  double  star,  the  chief  star. 

e  F ;  2'  diam   

v  F ;  v  S ;  R  ;  has  a  %  p  25"  dist   

pB;  R;  bM;  15'  

v  F ;  p  L ;  1  E  in  parallel ;  vglbM;  2'  1 ;  90"  br  

p  F;  p  L ;  E  in  parallel ;  90",  50" ;  has  a  ^  or  two  in  it   

v  F;  S;  R;  gib  M   

p  B;  R;  g  1  b  M  ;  40'  

pF;  PL;  R;  glbM;  40"  

F ;  p  L  ;  R ;  glbM;  70"  

pF;  R;  vgb  M;  80"   

F ;  R ;  g  b  M ;  80" ;  r.    On  a  ground  of  small  stars   

p  B  ;  irreg  R;  gbM;  25".    Among  many  st,  one  =  7' m,  n  p   

eF;  pL;lE;  vgvlbM   

e  F;  S;  R  

F ;  R ;  vgbM;  40" ;  3  stars  10' m  precede  

F  ;  R  ;  40"  

pB;  R;  bM;  60"  

pB;  S;  R;  bM;  15"  

L;  R; b  M   

0;  pB;  R;  psmbM;  2'  diam.  Resolved  

p  B  ;  S ;  R ;  g  p  m  b  M ;  40"  

A  star  7  m.    The  most  southern  and  largest  of  a  L,  brilliant  but  poor 

cluster  which  fills  the  field.    Stars  8,9  12  m. 

vB;  R;  gmbM;  25"   

B;  R;  gbM;  40"  

B;  E;  gmbM;  25'  

v  B ;  R ;  gbM;  40" ;  r  

vB;  S;  R;  gbM;  30"  


U 


REDUCED  OBSERVATIONS  OF 


No. 


?ynon. 


2826 
2827 


A.  129 


2829 


2830 

2831 
2832 

2833 


2834 
2835 
2836 

2837 
2838 


2839 


A.  131 


2840 
2841 


5  '9  13-5 

156  55 

5i 

5  19  18.0 

159  23 

2 

19.6 

23 

29 

20.3 

22 

58 

33-9 

23 

45 

R  A.  1830.0. 
h.  m.  s.  d. 


5  18  19 


5  J9  37-2 

5  19  5'  i 
53.6 
53.8 

5  20  0.7 
0.8 

5  20  4.7 
5  20  16.0 

5  20  32.0 
32.2 

32-  5 

33-  8 

34-  3 
34-5 
34-7 

5  20  49'7 
5  2«  i-5 
5  21  12.5 
13.4 
5  21  18.8 
5  21  36.7 
52.1 
56.5 

5  21  57-i 


N  P  D.  1830.0. 


160. . 161 


156  58  8 

159  34  47 
34  15 
34  37 

161  25  57 
25  o 

159  10  o 

157  2  41 

156  56  5 
56  38 
56  41 

55  58 

56  47 
56  35 
56  34 

159  56  52 

155  38  4° 
136  52  52 

52  37 

156  1  58 
159  42  o 

4i  35 
41  o 

159  38  50 


74-4 

38 

21 

5  22  7.8 

158  s 

J3 

5  22  10.8 

156  17 

38 

10.8 

18 

25 

j  2.0 

18 

41 

14.7 

17 

48 

15.1 

18 

1 

Description,  Remarks,  &c. 


Sky  black  in  all  the  southern  part  of  the  degree  swept,  but  the  5'  at  the 
upper  end  (1600  2'. . .  1600  7')  marks  the  edge  of  the  nebulous  light  of 
the  Nubecula  Major. 

F ;  R ;  gbM;  30".    Among  many  stars  

Fine  cluster.  Irreg  fig.  The  chief  nucleus  (which  seems  to  be  a  close 
double  star,  9  m)  taken. 

The  most  condensed  knot  (=  12")  in  a  pretty  rich  L,  s  c,  cl   

The  brightest  v  S  knot  in  a  L  irreg  cl  of  st  11  m  16  n  

p  rich  L  cluster  10'  diam.  It  has  in  it  a  close  triple  star,  easily  taken  for  a 
nebulous  knot.  (N.  B.  This  is  doubtless  the  knot  taken  in  the  three 
foregoing  observations,  but  it  does  not  appear  what  point  in  the  cluster 
was  taken  in  this  obs ;  probably  the  general  middle.) 

eF;  p  L.  (Possibly  the  same  with  No.  2826,  but  the  nebula;  are  so 
crowded  that  they  may  with  equal  probability  be  different  ones.) 

B;  S;  R;  gb  M;  25";  r  

B;  S ;  R;  vgvmbM;  15"  

vB;vS;R;gbM;  20"  

v  F;  L ;  irreg  R  ;  3'  

F ;  p  L ;  irreg  fig ;  r ;  2'  1,  90"  br  

vF;  L;  R;  gvlbM;  60"   

Cluster,  6th  class ;  eF;  L ;  irreg  R ;  4'  diam.  Resolved  into  S  st  with 
nebulous  light. 

pB;  RjglbM;  40"   

pL;  b  M.    Seen  through  cloud  

pF;  R;  glbM;  2'   

pB;  S;  R;  vgbM;  20"  

pF;  R;  gbM;  60"   

pB;R;bMj  45"  

p  B  ;  R ;  p  m  b  M.    (In  the  body  of  the  Nubecula  Major.)   

v  F ;  oval ;  r ;  40"  

v  F;  R;  30".    A  faint  and  poor  cluster  precedes  

v  F;  S ;  RjglbM;  15" ;  has  4  B  st  prec  

B ;  R ;  first  g,  then  s  b  M  ;  a  group  of  B  st  prec  

Cluster  8th  class;  poor;  sc  st ;  a  *  10  m  the  chief,  in  southern  part  taken 

p  F;  irreg  R;  gbM.    (See  remark  on  the  next  neb.)   

p  B  ;  R;  60".    Situated  in  the  main  body  of  the  Nubecula  Major  

p  B ;  p  L  ;  irreg  R ;  r.  Field  full  of  light,  consisting  partly  of  stars,  and 
partly  of  resolvable  nebula. 

v  F ;  R ;  g  b  M.  Field  full  of  the  nebulous  light  of  the  greater  Nubecula. 
[Note. — As  it  is  hardly  possible,  without  sotne  perceptible  slip  of  the 
apparatus,  to  make  so  great  an  error  in  P  D,  in  an  object  of  this 
nature,  as  this  observation  would  imply,  I  cannot  help  supposing  that 
an  error  of  20-  +  has  been  committed  in  R  A,  and  that  the  places  of 
the  nebula  f  748,  Nos.  25  and  26,  should  stand  as  follows : — 748,  25 — 
RA  c,n  56.7,  PD  159  42.0 ,•  end  748,  26—^^  522  17.1,  NPD 
159  38.50.  This  would  reconcile  everything.  Note  both  these  nebula' 
were  observed  in  quick  succession  in  this  f  at  leaving  the  field,  where 
there  is  always  a  liability  to  an  anticipation  of  the  R  A,  from  the 
sliding  eye-piece  not  being  urged  up  to  full  contact ;  and  the  quantity 
in  question  (at  this  P  D)  does  not  exceed  what  might  very  well  arise 
from  that  cause.'] 

p  B ,  R ;  60".    Situate  in  the  main  body  of  the  Nubecula  Major   

F.    The  preceding  nucleus  of  the  compound  nebula  figured  in  fig.  2,  PI.  III. 

Place  by  ARA  and  PD,  from  the  chief  nucleus  measured  on  diagram. 
A  double  neb;  pos.  2600;  dist  80".    The  first  pB;  S;  R;  30".  The 

second  e  F  ;  R ;  almost  stellar. 

p  F;  irreg  R;  b  M  ;  25"  

p  B;  R;  p  s  b  M  

B;eS;bM;  10"   

pB;  S;  R;  s  v  m  b  M,  to  a  *  ;  30"  


NEBULiE  AND  CLUSTERS  OF  STARS. 


75 


No.  Svnon. 


2842 
2843 


2844 


2845 
2846 
2847 


2849 
2850 


2851 
2852 
2853 
2854 


2855 
2856 

2857 
2858 


A.  175 


A.  89 


A.  90 


III.  590 

A.  237 


E  A.  1880.0. 
h.  m.   s.  d. 


5  22  27.2 
5  22  28.6 
29.8 

32.O 

33-5 

5  22  35.8 

5  22  45.8 

46.6 
46.9 
48.0 

49-5 
50.0 


5  22  49.5 
5  22  54.1 
5  22  56.4 
57-6 
5  22  59-8 
62.2 
63.5 
64.6 

5  23  39-7 
41.7 
5  24  10.4 
11. 3 
13.2 
5  2+  47-5 
5  25  0.7 
5  25  2.4 
5  25  7.5 

5  25  •• 
5  25  29.8 

5   2S  38.8 

5  25  56.3 
5  26  2.5 

5  -4 


NPD.  1830.0. 


158  4  31 
158    6  47 

6  49 

7  * 
7  13 

158  4  3 
I58    7  52 

7  39 

8  7 

7  52 

8  8 
8  20 


158    3  27 

156  32  10 

157  20  11 
20  37 

160    5  52 

5  54 

6  25 
6  57 

154    7  16 
4  26 
160  18  10 
18  5 
18  57 
156  36  16 
162  37  50 
104  11  24 
156  32  1 
160  23  . . 

154  54  9 
156  24  36 

158  37  2 
156  44  10 

43  51 


Description,  Remarks,  &c. 


The  2nd  nucleus  of  the  composite  nebula  of  fig.  2,  PI.  III.,  from  diagram. . 

F;  S;  R.    The  third  of  a  group  of  4  nebulae  connected  by  stars   

The  first  bright  nebulous  head  of  a  large  beautiful  irregular  cluster  of 
resolved  stars. 

The  second  nebula  of  a  group  of  three  

B ;  S ;  R.  One  of  the  chief  nuclei  or  knots  of  a  large  irregular  cluster 
nebula.  (See  remarks  on  this  nebula  further  on,  and  refer  to  figure  2, 
PI.  III.) 

Hereabouts  may  be  placed  the  general  middle  of  the  group  of  3  nebulae 
referred  to  in  No.  311/653. 

The  second  of  the  two  nebulous  heads  of  the  cluster  referred  to  in  No.  36  of 
this/. 

The  last  of  3  nebulae  in  a  zig-zag  formed  cluster  

p  B ;  S  ;  R.    The  4th  of  a  group  of  4  connected  by  stars,  &c  

The  third  nebula  in  a  group  of  3  

p  B  ;  S ;  R.    Another  chief  nucleus  or  knot  of  the  cluster  neb   

The  southern  and  brightest  nebular  nucleus  of  a  great  branching  cluster. 
[Note. — A  reference  to  fig.  2,  PI.  III.  which  is  a  very  careful  and 
exact  representation  of  this  highly  characteristic  object,  will  explain  all 
the  apparent  discordances  of  these  descriptions.  It  is  proper  here  to 
observe,  that  each  observation  lias  been  referred  to  its  proper  point  by 
sketches  made  at  the  moment  of  observation  in  the  sweeping  book.  In 
fact  the  places  of  the  two  principal  nebulous  masses  only  in  the 
southern  part  of  the  object  have  been  taken,  none  of  the  others  beirig 
sufficiently  prominent  or  definite.  The  diagram,  however,  from  which 
the  figure  is  taken,  affords  data  for  measurement  equal  to  direct 
observation  in  a  sweep.~\ 

An  outlier  of  the  group  figured  in  III.  2.    Place  from  diagram.    vF;  p  L 

A  nebulous  group  or  knot  

p  B  ;  S  ;  R  ;  b  M.    Has  2  st  9  and  10  m  following  

p  B  ;  vS;  R;  10"   

pB;  S;  R ;  glbM;  a  double  neb.    It  has  a  v  F  neb  attached  n  p  .... 

B;  R;  a  double  nebula.    (Clouding  over.)   

A  double  neb.    Pos.  339.1 ;  50"  dist ;  each  F ;  R;glbM;  35" and  30".. 

p  B  ;  binuclear  (by  diagram,  double) ;  gb  M;  30"  

A  star  14.n1,  with  an  e  F  nebula  about  it   

v  F.    (Cloudy.)    (N.  B.  The  P  D  has  been  probably  spoiled  by  the  cloud.) 

pB;  R ;  glbM;  50"   

v  F  ;  40" ;  has  a  %  15  m  at  60"  dist  pos  =  i9°.6  

p  B  ;  irreg  R ;  vgbM   

e  e  F ;  v  v  L.    Great  blotches  of  diffused  nebulosity  

p  B ;  R ;  b  M ;  90"  

v  F;  R;  25"  

pF;  R;  gbM;  r   

The  southern  edge  of  Nubecula  Major.  All  the  zone  south  of  this  is  dark 
and  starless. 

pB;  L;  R ;  glbM;  2^'  diam ;  a  star  9mnp  

A  rich,  discrete  cluster,  class  VII.  Not  much  comp  M ;  10'  diam  stars 
13  m. 

pB;  S;  R;  psbM;  20"  

A  close  first  class  D  star,  10  and  1 1  m,  with  a  thick  nebulous  mist  like  dust 
about  it. 

B  ;  R ;  or  1  E  ;  binuclear  or  s  b  M  to  a  double  star  10  and  1 1  m.  [Note. — 
The  obs  gives  22  "  for  the  R  A,  but  this  is  impossible.  From  the  context 
it  is  presumed  to  be  26,  being  evidently  the  same  object  with  No.  2S, 
/MO 


Sweep. 


538 
759 

653 
512 

653 


76 


REDUCED  OBSERVATIONS  OF 


2859 

2860 
2861 
2862 

2863 
2864 

2865 
2866 
2867 


2869 


2870 
2871 

2872 
2873 
2874 

2875 
2876 
2877 


Synon. 


IV.  21 


A.  211 


A.  136 
A.  136 


A.  77  ?  ? 
A.  136 


A.  136 


A.  213 


E  A.  1830.0. 
h.  m.  s.  d. 


5  26  7-3 

7-3 

5  26  9-9 

5  26  14.4 

5  26  26.3 

29.0 
5  26  35-i 

5  27  2.0 
2.0 
6.0 

5  27  7-3 
5  27  10.0 

5  27  2S± 
29.3 


5  27  35-7 
5  27  45-° 

47.8 
48.8 

5  27  45± 

5  27  48.2 

5  27  56.0 

57-3 
58.0 
S  28  3.2 

5  28  5.6 

5  28  10.5 
14.5 
5  28  17-7 

5  28  18.7 
5  28  20.3 


N  P  D.  1830.0. 


160     3  7 
2  40 

112     4  3 

126   30  12 

158  58  43 

58  I9 

157  38  50 

159  59  O 
58  34 
58  57 

160  4  19 

158  58  34 
158  57  ± 

56  45 


158  57  3 

158  57  37 

57  28 

57  37 

158  58  ± 


*57  35  34 

120  55  2 

54  4° 
56  12 

!59  59  4 

121  o  50 

167  52  45 
53  23 
'59  59  49 

159  58  59 
157  33  57 


Description,  Remarks,  Sec. 


A  large  ill-defined  patch  at  the  lower  edge  of  the  Nubecula  Major,  which 

is  pretty  definite  here,  and  very  bright. 
The  first  of  several  nebulae  running  together  and  forming  a  very  remarkable 

group,  which  fills  the  field  with  a  faint  diffused  nebulosity.    See  fig.  7, 

PI.  IV. 

F ;  irreg  R ;  vsbM;  to  a  st  12  m ;  2  or  3  st  involved,  and  several 
bright  ones  near. 

The  cusp  of  a  cluster  of  stars,  8 . . . .  1 1  m ;  arranged  pretty  exactly  in  a 
figure  of  3  with  appendages.    ^  8min  cusp  taken. 

p  B  ;  S  ;  R ;  insulated,  but  has  a  group  of  4  nebulae  following  in  the 
parallel. 

p  F;  S;  R;  g  1  b  M  ;  40"  

The  second  of  a  great  line  of  rich  clusters  which  are  connected  by  abundant 
scattered  stars.    (The  first  not  taken.) 

The  second  of  the  group,  fig.  7,  PI.  IV.    L  ;  F  ;  v  g  b  M   

F;  R;  gbM;  40"   

p  F ;  p  L;  irreg  R   

F  ;  v  L  ;  v  g  b  M  ;  the  third  of  several  whose  borders  join,  forming  the 
group  in  fig.  7,  PI.  IV. 

v  F  ;  p  L  ;  R  ;  the  first  of  a  group  of  4  neb  with  stars.  (N.B.  The  mirror 
newly  polished.    See  fig.  20,  PI.  VI.) 

F  ;  S  ;  the  second  of  a  group  of  4  nebulas  with  stars.  The  place  inter- 
polated from  those  of  the  1st  and  3rd  by  the  aid  of  a  diagram  made  at  the 
time.    PI.  VI.,  fig.  20. 

The  first  nebulous  knot  of  a  large  fine  nebulous  cluster  3'  in  extent.  (N.B. 

This  is  doubtless  identical  with  what  is  called  the  second  in  f  538, 
as  it  does  not  appear  that  in  this  obs  the  separate  nebula  of  which  the 
group  is  composed  were  so  well  distinguished  as  in  that  f  where  a 
freshly  polished  mirror  was  used.  The  diagram  of  sweep  535  represents 
the  {really)  first  as  much  fainter  and  more  diffused  than  the  others.) 

The  third  of  a  group  of  4  nebula?  with  stars  ;  p  B  ;  R  ;  p  s  1  b  M.  PI.  VI., 
fig.  20. 

A  star  9  m,  the  chief  of  a  curious  cluster  of  mixed  stars  and  nebulas  5'  in 
diameter. 

The  brightest  star  in  a  p  L  irreg  cluster  with  nebula;  mixed  

The  chief  star,  9  m  of  a  large  irregular  cluster.  (Note.  The  cluster  referred 
to  is  obviously  the  "group  of  4  nebula;  with  stars"  of f  538.)  PI. 
VI.  fig.  20. 

The  last  nebula  in  the  group  of  4  with  stars.  Place  concluded  (with  no 
precision)  from  the  1st  and  3rd  by  the  aid  of  a  diagram.  [N.B.  I  suspect 
all  the  nebula  of  this  group  to  be  placed  several  seconds  too  early  by 
f  538  in  R  A.  The  reductions  in  that  f  are  not  good,  and  the 
group  lies  at  the  southern  limit  of  the  zone  beyond  the  fair  grasp  of  the 
reductions.] 

The  third  of  a  great  line  of  rich  clusters  all  connected  by  abundance  of 
irregularly  scattered  stars. 

e  e  F ;  S  ;  R  ;  south  of  several  bright  stars   

F  ;  R  ;  1  b  M  ;  30";  at  the  apex  of  a  sort  of  cusp  of  stars   

v  F  ;  S  ;  R  ;  at  the  apex  of  a  converging  parcel  of  distant  st   

The  4th  of  several  running  together  (fig.  7,  PI.  IV.).  F  ;  S  ;  attached  to  a 
larger  (the  5th). 

e  e  F  ;  v  S ;  certainly  not  to  be  seen  except  in  a  superbly  clear  night,  as 
this  is. 

e  F ;  IE;  40";  has  a  coarse  double  star  n  f,  6'  distant  

eF;  S;  R;  gbM;  15"  

The  5th  of  several  running  together  (fig.  7,  PI.  IV.) ;  attached  to  a  smaller, 
No.  4. 

The  6th  of  several  running  together  (fig.  7,  PI.  IV.).  This  also  is  a  double 
nebula,  having  a  very  small  one  attached  n  p  (No.  7.). 

The  following  part  of  a  large  irregular  cluster  which  extends  obliquely  across 
the  field.  (Note.  This  is  one  member  of  the  collection  of  clusters  whose 
details  are  noted  in  f  760.) 


NEBULAE  and  clusters  of  stars. 


77 


No. 


Synon. 


R  A.  1830.0. 
h.    in.  s.d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 


761 


2878 


2879 


2881 
2882 
2883 


2884 
2885 

2886 
2887 


2889 


2891 
2892 
2893 


5  28  30.9 


156  22  l6 


A.  178; 


A.  214 


A.  215 


32.8 

34-3 
5  28  37.6 

5  28  49-3 
51.4 

5  28  51.3 
5  28  52.4 
5  29  12.9 
14.5 
15.6 
17.1 
5  29  16.8 

5  29  20.4 
22.7 
5  29  22.2 
5  29  32-9 

34-9 

5  30  .. 
30  3.2 

5  3°  14-9 
5  30  25.6 

27.6 


5  3°  49-3 
5  3°  53-8 
5  3°  55-3 


56.1 
57-9 
S8.3 


59-5 
60.0 


21  12 

21  36 

138  48  15 

138  48  20 

49  18 

159    7  12 

159  *5  35 

160  6  28 
6  7 

5  S3 

6  47 

157  33  42 

160  52  28 
52  3 

153  20  o 

159  16  40 

16  5 

158  52  .. 

52  29 

161  59  55 
iS7    °  5° 


5  31  i-9 


156  3s  25 
141    2  25 

157  24  35 

24  28 

24  21 

25  1 


24  35 
24  32 
141    4  s 


v  B  ;  v  L  ;  oval ;  v  g  p  m  b  M  ;  a  beautiful  nebula  ;  it  has  very  much  re- 
semblance to  the  Nubecula  Major  itself  as  seen  with  the  naked  eye,  but  is 
far  brighter  and  more  impressive  in  its  general  aspect  as  if  the  nubecula 
were  at  least  doubled  in  intensity.  (Note. — July  29,  1837.  I  well  remem- 
ber this  observation,  it  was  the  result  of  repeated  comparisons  between  the 
object  seen  in  the  telescope  and  the  actual  nubecula  as  seen  high  in  the 
sky  on  the  meridian,  and  no  vague  estimate  carelessly  set  down.  And 
who  can  say  whether  in  this  object,  magnified  and  analysed  by  telescopes 
infinitely  superior  to  what  we  now  possess,  there  may  not  exist  all  the 
complexity  of  detail  that  the  nubecula  itself  presents  to  our  examination  !) 

vB;vL;E;gbM:  3'   

pB;  vL;  IE;  gbM;  3'  

e  e  F  ;  R  ;  b  M  ;  exceedingly  difficult  and  delicate.  (Sky  perfectly  clear.) 
The  preceding  of  two. 

F ;  R ;  gbM;  north  of  a  v  B  group  of  2  st  g  m,  1  =  9',  3  or  4  =  1 1 

e  e  F  ;  R  ;  b  M  ;  the  following  of  two ;  in  field  to  s  is  a  brilliant  group  of 
stars. 

A  pretty  rich  irregular  cluster  which  fills  the  field ;  a  knot  in  it  taken  .... 

A  cluster  ;  a  double  star  in  it  taken  

pB;  R;  gbM  

B;  pL;  R;  gbM;  2'  

p  F;  p  L;  R;  g  1  b  M;  2'  

vB;  L;1E;  gmbM;  3'  

The  4th  of  a  great  line  of  rich  clusters  connected  by  abundant  irregularly 
scattered  stars. 

v  F ;  L  ;  irreg  R ;  3  B  st  precede   

p  B  ;  R ;  gbM;  2';  3  st  precede  

e  F  ;  R  ;  30 "  

The  second  knot  in  a  rich  cluster  of  irregular  figure  of  stars  11  ....  16  m. 
The  knot  seems  to  be  a  close  double  or  triple  star. 

A  little  knot,  a  triple,  perhaps  a  quadruple  star,  forming  a  point  of  refer- 
ence in  a  cluster  of  the  7th  class.  The  knot  looks  like  a  nebula  till 
analysed. 

Here  commences  a  very  starry  or  resolved  region  of  the  greater  Nubecula  . . 

The  middle  of  the  most  condensed  part  of  a  cluster  of  stars  13  m  which  runs 
off  to  the  s  p  and  joins  No.  39  of  this  sweep. 

F  ;  R  ;  v  1  b  M  ;  60"   

Place  of  a  double  star  class  I,  (h  3779),  the  chief  of  a  great  cluster  of  S  st 
loose  and  filling  the  field.  It  is  the  forerunner  of  the  great  cluster-region 
of  the  nubecula. 

v  B  ;  S  ;  R.  Here  comes  on  the  richest  and  brightest  part  of  the  starry 
and  clustering  portion  of  the  nubecula.  (Note. — From  this  object  being 
described  at  one  time  as  a  double  star,  and  at  another  as  a  nebula,  it  is 
probable  that  it  is  in  one  of  those  singular  close-knotted  groups  which 
especially  characterize  the  nubecula?.] 

A  B  S  stellar  neb,  or  very  close  cluster  15"   

e  e  F;  pL;  R;  40"  

A  very  condensed  pellet  of  stars  2'  diam  with  stragglers.  The  nucleus  is 
10  or  12". 

B  ;  S ;  irreg  R;  s  m  b  M.    A  close  compressed  cluster,  stars  12  . . .  14  m 
0 ;  B ;  S ;  R ;  comp  M  to  a  blaze  of  stars.    Many  stragglers   

(g ;  vB;  R;  psvmbM;  resolved.  (Note. —  This  obs  makes  the 
minute  of  R  A,  31,  but  the  united  testimony  of  all  the  rest  shows  this 
to  be  a  mistake ;  and  it  appears  by  this  very  f  that  there  are  not  two. 
The  zone  swept  being  only  i°  in  breadth;  and  2,  or,  according  to  the 
MS.,  3  minutes  having  elapsed  without  an  object  before  this  came  to  be 
taken.) 

0  ;  B ;  irreg  ;  R ;  2'.    The  stars  easily  distinguishable   

B  ;  pretty  rich,  compressed  cluster  of  stars  12  m  

eF;  pL;  R;  vlbM;  30"  


508 
522 
526 

762 
526 

748 
657 
523 
748 
5i3 
75i 
760 

509 
5i3 
5i5 
748 

657 


759 
759 

672 
658 

760 


512 
525 
653 

538 

522 

760 


512 
508 

525 


x 


78 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


l895 


2896 
2897 


2899 
2900 


2901 

2902 
2903 

2904 
2905 


2906 

2907 
2908 


2909 
2910 


29 1 1 

2912 
2913 


A.  218 


A.  98 


A.  241 


A.  240 

A.  100  ? 
A. 219  ? 


2914 
2915 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


5  31  28.1 
28.6 

5  3i  3&4 
5  32  11. 1 
IT.9 
12.3 
12.7 
5  32  38.8 

5  32  454 
5  32  46.8 

56.i 
57-i 
5  33  54 

5  33  *5-° 
5  33  36-3 
37.1 

5  33  414 
5  33  46-7 


494 
5  33  Si-i 

5  34  54-i 

5  34  594 


64.6 


73-9 

5  35  i6-7 
5  35  *3-8 
26.1 

5  35  23.8 
25.0 
5  35  38.8 
5  35  35-^ 
45-3 
46.6 

47-5 
50.1 

5  35  53-5 

5  35  56-3 
59.6 


157    6  16 

4  3i 

107  56  54 

159  17  49 
18  10 
18  3 
18  25 

160  57  12 
157  38  13 
157  48  10 

48  50 

48  49 

159  22  28 

160  4  17 
157  49  11 

49  4i 

161  11  30 
160  16  3 


16  3 
157  34  7 

169  58  40 
157    3  17 


1  19 

161  48  30 

157  40  11 

39  25 

156    8  10 

7  4i 

160  3  32 

»S7  4°  51 

40  30 

4°  57 

40  56 

41  3 

156  59  46 

161  s  54 

7  o 


Description,  Remarks,  &e. 


A  small  highly  condensed  knot  in  an  immensely  large  and  very  rich  cluster, 
which  fills  much  more  than  the  field,  and  is  like  the  Milky  Way. 

A  very  small  nuclear  knot  in  an  extremely  rich  assemblage  of  stars  and 
clustering  groups  which  fill  the  field. 

A  fine  clustering  group  of  large  stars   

p  F;  R  ;  b  M ;  2o"j  in  a  field  full  of  stars  

p  B ;  R  j  b  M ;  40" ;  in  a  field  rich  with  clustering  stars  

pB;  R ;  g  1  b  M  ;  80"  in  the  n  p  part  of  a  cluster  

F;  R;  3°";  r   

F;  R;  vglbM;  3'   

vB;  S;  R;  psmbM;  25"  

A  pretty  L,  irreg  cluster  7th  class ;  chief  *  9  m  taken  (at  leaving  the  field)  ; 
the  rest  are  10 ....  1 5  m. 

Chief  *  9  m  of  a  v  irreg  cluster,  4'  long,  3'  br  

A  cluster,  6th  class   

The  general  middle  of  a  cluster  of  loose  stars  11  16  m.    It  is  rich,  and 

fills  the  whole  field. 

F ;  v  L  and  diffused ;  irreg  R ;  gbM   

pB;  vL;  vglbM;  IE;  4'.    A  fine  cluster  precedes  it  

v  F ;  vL;  R;  vglbM;  4'  diam  

p  B;  R;  pglbM;  2';  a  star  10  m  involved,  p  

B;  R;  gbM;  60".  [Note.  —  The  obs  makes  the  degree  159,  but 
although  the  zone  swept  in  this  f  was  intended  to  be  onlg  of  1°  in  extent 
(159. .  .  .to  160),  yet  as  the  star  B  1065  (P  D  160.15)  u'as  taken  shortly 
after,  in  it,  it  appears  to  have  overlapped  considerably  into  the  next 
degree,  on  which  account  I  am  induced  to  regard  this  neb  as  identical 
with  No.  33,  f  75 1,  in  which  no  mistake  of  the  degree  was  possible.] 

B  ;  R  ;  gbM;  60".    See  note  on  the  last  obs  

v  S  ;  F  ;  R;  12".  In  the  northern  part  of  a  cluster  of  stars  14  m,  8'  long, 
3'  br. 

vF;  S;  IE;  bM;  2  st9  m  follow  toward  the  north  

A  very  L,  v  rich  cluster  of  separate  stars  9 . . . .  1 1  m,  which  fills  the  whole 
field. 

Cluster  7th  class.  The  2nd  of  two  stars  9  m,  which  may  be  considered  the 
leading  stars  of  the  very  large  and  fine  cluster  of  the  Nubecula  Major, 
which  fills  many  fields,  is  of  all  degrees  of  condensation,  and  much 
broken  up  into  groups  and  patches. 

An  ill  defined  nebuloid  group  of  stars  15  m.  (N.  B. — Clouds  very  trouble- 
some.)   The  field  full  of  grouping  stars. 

vB;S;lE;gmbM;r.    Almost  a  ©   

B  ;  L ;  gbM.    The  first  of  3  neb  which  ran  together  

v  F ;  p  L  ;  irreg  R.  The  first  of  3,  which  run  together.  See  Plate  III. 
fig-  5- 

p  B  ;  R ;  gbM;  60" ;  resolved  into  stars  13... 15m   

A  rich,  R,  p  L  cluster  of  stars  12  m;  1  comp ;  5'  1 ;  one  if  11m  

v  F  

B  ;  L ;  gbM.    The  second  of  3  which  run  together   

B  ;  L ;  E.    The  middle  of  3  which  run  together   

v  B  ;  v  L  ;  gbM.  The  second  of  a  train  of  3.  The  first  is  a  large 
irregular  nebula. 

v  B  ;  v  L.    A  singular  figure  like  3  nebulae  lumped  together   

p  B  ;  irreg  fig  ;  g  1  b  M.  (By  a  diagram  made  at  the  time,  it  consists  of  3 
pretty  distinct  masses  which  extend  over  a  considerable  space  in  R  A. 
Plate  III.  fig.  5.) 

A  more  condensed  part  of  the  great  cluster  (761,  39),  of  a  crescent-like 
form,  occupying  one  field.    Rich  and  fine. 

©;  B;  R;  gbM;  2'.    Resolved  into  stars  

F(?)j  R;  gbM;  3'.    (Hazy  sky.)  


NEBULAE  AND  CLUSTERS  OF  STARS. 


79 


No. 
2916 

2917 
2918 

2919 

2920 

2921 
292a 
2923 

2924 

2925 
2926 

2927 
2928 

2929 
2930 
2931 
2932 
2933 

2934 
2935 

2936 
2937 
2938 

2939 
2940 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 

N  P  D.  1830.0. 

0      1  u 

157  41  II 

57-1 

AI   A  7 

CO  0 

AI    I  5 

C    ifl  IOC 

1 59    9  42 

5  36  3°-3 

157  40  4 

31.0 

40  16 

31.6 

40  7 

31.9 

39  48 

38.8 

40  11 

5  36  36-7 

IS7    5  23 

37.1 

5  56 

37-7 

4  46 

40.7 

5  35 

5  36  43-8 

160  39  26 

44-3 

38  57 

46.2 

39  52 

S  36  43-8 

120    9  33 

AA  -7 
TT  / 

O  AI 
y  tj 

5  37  13-3 

159     I  18 

5  37  30.4 

l6o  20  O 

5  37  44-4 

124      I  59 

5  37  46-1 

l60   17  IS 

5  37  51-5 

I59  42  40 

5  38  8.1 

157  31  6 

5  38  9.0 

159  29  10 

159  S3  10 

T  fi  T       n    t  Cl 

1  cn    m    c  *7 

f   t  2   a  n  ft 

160  46  13 

5  38  43-2 

160  15  IO 

43-9 

15  52 

5  38  43-5 

112     4  50 

5  38  43-9 

160  21  24 

49± 

21  54 

5  38  46± 

160   13  24 

5  38  59-° 

156   57  46 

5  39  29-° 

160   l8  54 

3 1.6 

19  50 

5  39  4°± 

160  16 

5  39  S°-i 

i59    5  37 

Description,  Remarks,  &c. 


Sweep. 


A.  220 


A.  102 


III.  241 


A.  103  ?  ? 


A.  143 


B  ;  L  ;  b  M.    The  3d  of  3  which  run  together.    (Plate  III.  fig.  5.)  

v  B  ;  L ;  g  b  M.    The  third  of  a  triplet  

p  B  ;  L  ;  R.    The  third  of  3  which  run  together  

v  F;  R  ;  g  b  M  ;  90".  [There  is  strong  ground  to  suspect  an  error  of 
a  degree  in  the  P  D.    It  should  most  likely  be  160.] 

p  F  ;  L  ;  R  ;  follows  a  group  of  3  running  together  

F ;  irreg  R  ;  g  1  b  M  ;  r  ;  2'.    (PI.  Ill,  fig.  5)  

Irreg  R  ;  r  ;  2'  diam  

F  ;  irreg  R;glbM  

v  F ;  R ;  follows  3  v  B  L  nebula?  which  run  together   

B  ;  R  ;  v  g  1  b  M  ;  20";  a  rich  clustering  part  precedes  

vB;  R;  vgvlbM;  20"  

B  ;  S  ;  v  g  b  M  ;  20"   

B  ;  R  ;  g  b  M  ;  40"  

p  B  ;  S  ;  R  ;  g  b  M  ;  insulated   

B  ;  R  ;  g  1  b  M  ;  25";  has  a  H«  9  m,  5',  n  p  

p  B;  S;  R;  gb  M;  20"  

vF;  S;  R;  gpmbM;  20" ;  in  a  rich  field   

vF;  S;  R;  pslbM;  25"   

The  chief  (9  m)  of  a  L,  irreg  figured,  looped  or  hooked  cluster  of  stars 
12  ...  15  m  ;  rich  and  various,  and  filling  the  field 

v  F  ;  R ;  g  b  M  ;  the  first  of  a  group  of  six  nebulae.  See  PI.  IV,  fig.  9. — 
(N.B. — In  the  original  obs  all  the  nebula?  of  this  group  in  the  748th  sweep 
have  the  PD  1590,  but  this  having  been  satisfactorily  proved  to  be  a 
mistaken  reading  for  160  ;  it  is  corrected  accordingly  here  and  subse- 
quently.) 

Cluster,  8th  class  ;  coarse,  loose,  and  filling  the  field;  stars  10  ....  13  m. 
Place,  that  of  a  double  star  in  a  vacant  part. 

The  second  of  a  group.  PI.  IV,  fig.  9  

A  very  faint  large  oval  ill-defined  nebula  ;  not  taken  in  sweeping,  but  laid 

down  from  a  careful  drawing.    See  Notes  on  the  Catalogue  of  Nubecula 

Major. 

F;  IE;  gbM;  2'   

Cl  VI  ;  v  F  st  and  nebulosity  of  irregular  branching  figure,  or  rather  3 

clusters  connected.    See  Notes  on  Catal  of  Nubecula  Major, 
v  v  F ;  vvL;  vglbM.    See  do.  do. 

p  B  ;  S  ;  R ;  gbM;  30"  ;  insulated  

A  v  L  v  rich  cluster  of  sc  st  10  .  .  .  .  15  m  which  more  than  fills  the  field  . . 

p  B  ;  R  ;  b  M  ;  the  preceding  of  2  on  the  same  parallel ;  a  star  9  m  between 

B ;  R ;  gbM;  90";  the  3rd  of  a  group  of  6  

v  B  ;  R;  the  3rd  of  a  group  of  7.    PI.  IV,  fig.  9  

e  F  ;  R  ;  gbM;  20"   

p  F  ;  the  4th  of  a  group  of  7.    PI.  IV,  fig.  9  

p  F  ;  S  ;  R  ;  g  b  M  ;  the  5th  (4th  properly)  of  a  group  of  6,  R  A  only  esti- 
mated from  a  rough  diagram  incorrect  (as  it  would  seem)  in  the  order  of 
the  objects. 

v  F ;  the  5th  (4th  in  MS)  of  a  group  of  6.    PI.  IV,  fig.  9   

v  F ;  E  ;  g  1  b  M  ;  40";  north  of  2  stars  10  m  

p  B  ;  R ;  last  of  a  group  of  6.    PI.  IV,  fig.  9   

B  ;  the  6th  of  a  group  of  7   

v  F  and  S  ;  the  last  of  a  group  of  7  ;  this  nebula  escaped  notice  in  /  748. 
PI.  IV,  fig.  9. 

The  middle  of  a  large  extended  faint  nebulous  mass  which  forms  the  north- 
ern branch  of  the  great  looped  nebula,  and  is  almost,  or  entirely,  detached 
from  it.    See  the  next  object. 


522 
760 
538 
748 

538 
508 
760 
512 
522 
653 
761 
508 
658 
523 
5i3 
75i 
645 

535 
759 

748 


663 
748 

760 


523 
5*3 
523 
748 

75i 
647 

75  J 
748 

748 
761 
748 
751 
751 

513 


80 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R  A.  1830.0. 

N  P  D.  1830.0. 

h.  m.    s.  d. 

0      1  11 

5  39  5!-3 

159  II  17 

s-2.8 

II  21 

53-4 

II  22 

II  14. 

53-9 

11  6 

53-9 

11  9 

S4-o 

11  2 

54.0 

11  5 

5  40  16 

159  34  28 

5  40  31-2 

160  46  13 

5  40  48.6 

124  18  47 

55-2 

19  28 

5  4°  58-4 

154  22  18 

62.7  : 

22  35 

66.1 

22  29 

5  4i  5-i 

145    36  20 

5  41  5-6 

I  CO   AA  1Q 

*  jy  TT  jy 

5  4i  9-8 

JS9  49  43 

5  41  10.9 

i59  51  33 

5  4i  12-7 

159  44  13 

5  41  25.0 

159  29  10— 

5  41  28.3 

I  ZCi    An  1A 

*iy  *4 

5  41  32.2 

159  50  41 

5  4i  34-9 

!S9  45  47 

5  41  48.2 

158  32  42 

49.8 

32  21 

5  41  49.7 

159  45  19 

5  42  20.0 

'59  3i  55 

5  42  29- 1 

142    9  0 

5  42  324 

158  26  25 

5  42  5°-9 

152  51  26 

52.1 

51  24 

52.6 

51  3 

5  42  Si-o 

157  24  20 

52.4 

24  4 

54-5 

26  25 

5  42  52-0 

159  17  20 

5  42  54-9 

159    0  4 

5  43  8.2 

141  36  58 

Description,  Remarks,  &c. 


Sweep. 


2941 


A.  142 


2942 

2943 
2944 

2945 

2946 
2947 

2948 
2949 

2950 
2951 
2952 

2953 

2954 

2955 
2956 

2957 

2958 
2959 
2960 

2961 

2962 
2963 

2964 


A.  594 


A.  152?? 
A.  145  ? 


A.  iE 


The  nucleus  of  the  great  looped  nebula  about  30  Doradus  

The  chief  star  of  the  great  nebula  

Do  

Do  

Do  ;  the  great  nebula  ;  an  assemblage  of  loops   

Do  

Do  

See  PI.  II.  fig.  4,  and  the  explanation  

p  L,  p  B,  m  E,  of  irreg  rounded  and  somewhat  serpentine  figure,  much 
brighter  in  its  foil  part ;'  E  generally  in  parallel.  Involves  5  stars,  2  of 
which  are  10  m.    See  Catal  of  Nubecula  Major. 

B  ;  R  ;  b  M  ;  resolved  ;  the  following  of  two  on  the  same  parallel,  a  star  9  m 
intervening. 

0;  B;  R;  with  an  appendage  to  northward  ;  i\'  diam.  (N.B. — I  have  no 
confidence  in  this  R  A.  The  reductions  of  this  f  run  badly,  and  the  object 
was  taken  at  leaving  the  field.) 

B  ;  irreg  R ;  g  b  M  ;  3'  1 ;  2'  br  with  stars  appended.  This  R  A  to  be  pre- 
ferred. 

B  ;  L  ;  R  ;  g  1  b  M  ;  90";  has  a  j|e  10  m  2'  dist  25°  s  f  

pFj  L;  R;  vlbMj  2'  

F;  R;  gib  M;  40"  

e  F;  R;  v  1  b  M  ;  40"  

The  preceding  of  two  forming  a  double  nebula.  The  place  deduced  from 
that  of  the  following  and  brighter,  by  A  R  A  =7*.  1,  A  N  P  D  =  20",  as 
they  result  from  the  drawing  of  Dec.  4,  1837.    PI.  III.  fig.  4. 

The  north  preceding  of  the  four  principal  nuclei  of  the  nebula  of  PI.  III.  fig.  4 

The  most  southern  of  a  group  of  4  or  5  nebulae,  5'  diam  mixed  with  stars. 
This  is  the  south  preceding  of  the  four  chief  nuclei  of  the  complex  group 
of  PI.  III.  fig.  4. 

B  ;  R  ;  double  ;  the  other  sp  is  F  ;  R  ;  followed  by  clustering  stars. 

Cluster  VI  of  v  F  st  and  nebula.    See  Catal  of  Nubecula  Major. 

The  north  following  nucleus  of  the  complex  group  of  PI.  III.  fig.  4,  from 
drawing. 

The  south  following  nucleus  of  the  complex  group  of  PI.  III.  fig.  4,  from 
drawing. 

A  very  faint  nearly  round  nebula  close  to  a  star  10  m,  not  observed  in  sweep- 
ing, but  laid  down,  Dec  4,  1837,  in  the  drawing  fig.  4,  PI.  III.  whence  its 
place  is  derived. 

pF;  S;  R  

e  F  ;  S  ;  R  ;  insulated   

B  ;  p  S  ;  R  ;  1  b  M  ;  follows  a  star  ion  with  other  S  st  about  it.  Not  ob- 
served in  sweeping,  but  laid  down  in  the  drawing  of  Dec  4,  1837,  whence 
its  place  is  derived,  III,  4. 

vF;  S ;  mE;  glbM;  i'I;  perhaps  a  v  F  double  neb.  See  Catalogue  of 
Nubecula  Major. 

e  F ;  R  ;  40";  a  line  of  3  st,  10  m  to  s,  points  nearly  to  it   

v  F;  S;  R;  12"   

F  ;  irreg  R  ;  psbMj  sfa  small  group   

e  F  ;  S  ;  R ;  has  a  star  16  m  in  centre   

p  F,  R  ;  p  s  1  b  M  ;  50"  

A  star  9  m,  chief  of  a  F  irreg  oblong  cluster  3'  in  extent  

Cluster,  irregularly  elongated  ;  not  very  rich  

F;  S;  R  

CI  VI.  v  F,  R,  60",  partially  resolved.  See  Catal  of  the  Nubecula  Major 
v  F  ;  S  ;  R.    This  nebula  forms  an  appendage  to  the  skirts  of  the  great 

looped  nebula  30  Doradus,  which  hang  down  in  visible  fringes  from  the 

upper  (southern)  part  of  the  field. 

p  B  ;  R  ;  vlbM;  30"   


NEBULA  AND  CLUSTERS  OF  STARS.  81 


No. 


Synon. 


E  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 


2965 


2966 


2967 
2968 
2969 

2970 
2971 

2972 


2973 

2974 
2975 


2976 
2977 
2978 


2979 
2980 


2982 
2983 


A.  185 


A.  147  ?  ? 
A.  151  ? 
or 

A.  154 


A.  153  ?  ? 


A.  155 


Nubec. 
A.  106 


5  43  15.8 


5  43  20.6 
22.0 
24.9 
25.0 


158  20  55 
20  25 

159  17  21 
17  23 
17  12 

16  50 

17  1 1 


s 

43  32.9 

in 

3  6 

54 

5 

44  «-3 

161 

-4 

3i 

5 

44  25-5 

156  58 

46 

34.6:: 

58 

37 

5 

45  "-5 

159 

*4 

40 

5 

45  14.0 

160 

42 

41 

19.5 

43 

7 

5 

45  *5-* 

158  36 

19 

15.8 

36 

31 

18.8 

36 

39 

5 

46  ^1.2 

161 

3 

52.7 

3 

47 

5 

46  52.1 

158 

6 

1 1 

c 
3 

46  54.3 

'59 

5° 

35 

5° 

5 

57"* 

49 

5° 

59-3 

5° 

54 

5° 

16 

5 

47  13-3 

140 

37 

35 

5 

48  6.8 

158  33 

43 

5 

48  IO.I 

i57 

29 

46 

10.4 

30 

21 

1 1.2 

29 

45 

13.4 

30 

8 

14.4 

30 

25 

5 

48  50.1 

i59 

10 

57 

54-5 

10 

5° 

5 

49  3°-i 

i53 

42 

49 

30.3 

43 

27 

S 

50  .... 

158' 

..1 

59 

5 

5°  34-3 

160 

6 

30 

34.8 

7 

2 

35-i 

6 

39 

35-4 

7 

8 

37-5 

6 

20 

5 

50  43.2 

161 

31 

11 

5 

51  12.4 

155 

21 

0 

13.1 

21 

9 

13.2 

21 

29 

A  small  close  knot  or  cluster,  40"   

B  ;  S  clustering  group  or  0 ;  30"  stars  visible.  [N.  B. — This  obs  makes 
RA  5  42  48.1,  but  this  must  have  been  observed  by  mistake  on  the 
moveable  wire.    See  Catal  of  Nubec  Major.] 

The  cluster  s  f  the  great  looped  nebula  

A  bright  S  cluster  of  distinct  stars.    (Thick  haze.)   

0  ;  B  ;  R  ;  3' ;  all  resolved  into  stars  13  ....  16  m  

0  irreg  R ;  psmbM;  2'  

B  ;  S ;  m  comp  ;  not  m  b  M  ;  irreg  oval ;  3' ;  stars  distinct  13  m.  [This 
obs  makes  the  R  A  io\3,  which  I  have  not  allowed  to  stand  against  the 
united  weight  of  the  rest.  The  object  was  taken  at  leaving  the  field,  and 
the  slider  probably  not  brought  fully  home  to  the  stop.] 

vF;  S;  RorlE;  gbM;  15"  

pB;  L;  pmE;  glbM;  has  a  if.  13  mm  the  middle   

p  F  ;  R ;  gbM;  80"  

v  F  ;  R  ;  30".    The  obs  in  R  A  is  marked  as  uncertain   

eF; pL;  IE   

F;  R;  g  vlbM;  60"  

B  ;  R ;  g  m  b  M ;  40"  

pFjpL;  R;  vgvlbM;  35"  

F;S;R;gbM;  20"  

p  F ;  p  L ;  R ;  vglbM;  80"   

v  F;  S;  R;  gbM   

v  F;  R;  gb  M;  40*   

eF;  pL;  irreg  R  

A  p  B  cluster  nebula  90"   

F  (?)  L ;  R ;  thick  haze   

F  cluster;  irreg  fig;  gbM;  2';  resolved  

F ;  irreg  fig ;  r  ;  one  star  seen ;  90"  

Irreg  oval  cluster ;  v  F ;  2'  diam ;  v  1  comp  M ;  almost  nebulous.  Stars 
=  16  m.  [This  obs  gives  the  R  A  46"  39^.5  which  must  evidently  be  re- 
jected. Taken  at  leaving  field,  the  eye-piece  having  remained  untouched 
since  No.  42  of  the  same  f.    See  note  on  that  obs.] 

eeF;  vS;  nfa  triangle  of  stars  10  m  which  form  part  of  a  bright  group 

F ;  S ; '  R.    A  star  1 1  m  precedes   

p  B ;  E  ;  resolved.    I  see  the  stars  in  it ;  2'  1   

p  F ;  irreg  R ;  40  or  50";  vlbM  

F ;  irreg  R ;  with  small  stars   

p  B ;  S  ;  resolved  

F;  irreg  fig;  90' 1;  15"  br;  r  

A  v  S,  B  knot,  probably  6  or  8  v  S  stars  wedged  into  a  close  group   

0;  v  s  m  b  M  ;  15"  

F;  R ;  vgvlbM;  60"  

v  F;  p  L;  R;  glbM;  80"  

Here  follows  a  legion  of  v  small  scattered  stars  all  indefinite  and  loose   

B,  L  neb ;  6'  1,  5'  br ;  resolved,  in  part ;  chief  *  1 1  m  taken  

Cluster  6th  class ;  F  ;  oval  or  irreg  fig ;  v  m  comp ;  st  =  15m  

p  B;  L;  irreg  R;  glbM;  3';  resolved  into  st  15  m  

CI ;  irreg  fig ;  consists  of  3  or  4  disjoined  clusters,  the  middle  one  the 
largest  and  brightest ;  of  3  or  4  L  st  and  nebulosity ;  chief  *  taken. 

CI  6th  class ;  irreg  R ;  F ;  glbM;  3'  barely  resolved  into  v  S  stars  and  a 
few  large  ones. 

v  F 
pB 


PB 
pB 


vglbM;  3'   

v  S;  R;  vglbM;  12" 
v  S;  g  m  b  M;  15"  .. 
eS;  R;  gbM;  10".. 


759 
538 


522 

509 

673 
657 
748 


647 
523 
761 
760 
657 
673 
75' 
538 
522 
512 
673 

75i 
538 
523 
509 
657 
673 
748 


762 

759 
522 

538 
760 
512 
658 
748 
657 
539 
5i5 

5'3 
75i 
523 
673 

657 

673 
5'5 
539 
5i8 


Y 


82 


REDUCED  OBSERVATIONS  OF 


No. 

2984 
2985 
2986 

2987 


Synon. 


2988 
2989 

2990 


2991 


2992 


2993 
2994 

2995 


2996 
2997 

2998 
2999 

3000 
3001 
3002 
3003 


3004 


A.  160 


R  A.  1830.0. 
h.  m.  s.  d. 

N  P  D.  1830.0. 

0      1  11 

5 

51 

59.9 

116 

40  8 

5 

52 

14.8 

I  ?0 

31  38 

5 

52 

41.6 

J7 

25  4.8 

43.2 

23  40 

43-9 

24  14 

5 

5* 

42.6 

157 

21  53 

42.8 

21  58 

43-9 

21  56 

44-5 

21  53 

46.4 

21  35 

46.9 

21  47 

48.0 

22  23 

5 

52 

59.1 

149 

56  IO 

5 

S3 

51.0 

l6l 

12  45 

52.5 

12  25 

5 

53 

5O.2 

157 

27  28 

58.3 

26  52 

58.5 

27  21 

58.9 

27  31 

59-5 

27  15 

5 

54 

.£  _ 
ID.7 

l6l 

7  45 

I7-7 

7  4° 

18.8 

8  14 

22.8 

8  57 

5 

54 

2I.3 

159 

31  32 

22.0 

30  52 

22.3 

30  48 

24.4 

31  15 

S 

54 

3I.9 

155 

51  45 

5 

54 

38.O 

1 59 

30  42 

38.9 

3°  35 

5 

55 

I  I.3 

158 

37  0 

II.4 

37  16 

12.3 

37  25 

5 

eft 

5° 

149 

7  42 

c 
J 

■;6 

J 

2Q.4. 

1f.Q 
158 

13  29 

32.1 

!3  J5 

5 

56 

37-3 

l60 

56  47 

5 

56 

50.5 

I4O 

4-3  55 

5i-3 

44  27 

5 

57 

16.4 

'59 

35  3 

5 

57 

26.2 

J59 

2  8 

5 

57 

45.8 

156 

25  1 

5 

57 

55-3 

157 

16  16 

56.2 

16  24 

56.5 

16  19 

56.6 

16  1 1 

5 

58 

5-3 

i55 

28  49 

5.6 

28  33 

6.0 

28  56 

Description,  Remarks,  &c. 


e  F  ;  S ;  R ;  has  a  He  1 3  m  in  centre   

v  F;  R;  50";  gb  M   

B;  S;  R;  15*   

pB;vS;R;  12"   

pF;  tSj  gmbM  

pF;  S;  R  

F;  R;  gbM;  30"  

pF;  Sj  R;  giM;  18"  

pF;  R;  gbM  

pB;  R;  glbM;  45"  

F ;  R ;  lbM;  30"   

F;  R   

Chief  *  of  a  cluster  8th  class  of  about  a  dozen  bright  and  some  smaller  stars 

pB;  pL;  R;  gbM;  60*  

F ;  R;  pmbM;  50'  

pF;  S;  R  

pF;  R;  bM;  30"  

F;  R;  gbM;  r   

pF;  R;  gpmbM;  r   

v  F ;  R ;  glbM;  60".    Among  stars  

B  ;  L  ;  R ;  gbM;  90"   

vB;  R;  gvmbM;  80";  r   

©;  B;  R;  gbM;  40";  r  

B  ;  R;  gmbM;  80'  

p  B;  R  ;  30";  the  preceding  of  2  

0;  pB;  R;  gmbM;  resolved ;  stars  14  .  .  .  16  m ;  has  a  v  v  F  neb  n  f 

p  B  ;  R ;  b  M  ;  60" ;  has  a  afc  10.1 1  m,  n  p  (thick  haze)  

p  F  ;  R ;  40".    Remarkably  situated  in  a  triangle  of  S  stars  ;  the  preceding 
of  two. 

e  F ;  S  ;  R  ;  has  3  3  st  pretty  distinct  towards  the  south  

v  F ;  R ;  30";  the  following  of  2  

v  F  ;  R;  25";  the  following  of  2  

F;  IE;  gbM  

p  F ;  irreg  RjpsbM  

p  F ;  R ;  b  M ;  30'   

e  F  ;  S  ;  R;  20";  has  a  *  12  m,  s  f  very  near  

F ;  R ;  b  M  ;  20";  connected  with  stars,  &c  

v  F;  R;  b  M;  30"   

F;  IE;  r   

e  e  F ;  attached  to  a  star  15m  

e  e  F ;  R  ;  attached  to  a  v  S  star.    [In  the  obs  this  is  called  "  rather  a  doubt- 
ful object,"  but  all  doubt  is  removed  by  the  subsequent  obs  off  762.] 

F;  v  S;  R;  v  s  b  M;  stellar  

Fj  R;  bM;  45'  *  •  • 

e  e  F ;  R  or  1  E  ;  attached  to  a  *  16  m  

pB;  R;  gbM;  20"  (?)  

pF;  R;  v  g  b  M;  90'   

F;  L;  R;  glbM;  100"   

F;  L;  R;  gbM;  90"   

p  B;  L;  R;  v  g  1  b  M;  80"  

vF;  pL;  R;  vlbM;  80';  in  a  rich  field  

F ;  L ;  g  v  1  b  M  ;  90" ;  in  a  rich  field  . . .  ^  


NEBULAE  AND  CLUSTERS  OF  STARS. 


83 


No. 


Synon. 


R  A.  1830.0. 
h.  m.   s.  d. 


NPD.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 


3005 


3006 


A.  196 


A.  161  ?  ? 


3007 

3008 
3009 

3010 
301 1 


A.  193 


3012 
3013 
3014 
3015 

3016 
3017 
3018 
3019 
3020 

3021 
3022 
3023 
3024 


3025 


3026 
3027 
3028 


A.  194 


A.  223  ? 


II.  265 


5  58  39-9 
39-9 
40.8 
42.3 
44-5 

5  58  47-4 

49.1 
50.3 
50.5 


5  58  58.8 
59.2 
60.3 
63.2 
5  58  59-3 
5  59  !7-3 
20.8 

5  59  24-4 
25.7 
25.7 

5  59  46-5 
47.8 

47-9 
50.6 
51.6 
o  1 1.6 
o  24.8 

0  50.0 

1  0.5 

4-5 
1  7.1 
1  28.9 
1  35.2 

1  45-3 

1  46.7 
48.9 

2  23.8 
4  0.6 
4  36.6 

4  57-3 
57-9 
58.6 
59.6 

5  17-9 


19.8 

20.3 

5  4J-7 

6  1.6 
6  23.1 

24.7 


158  28  8 
27  39 

27  38 

28  46 
28  29 

159  11  56 

12  o 
12  7 
12  10 


158  38  13 
38  11 

37  48 

38  24 
158  17  52 
172    9  41 

7  47 
153  43  35 
43  11 
43  14 
158  31  4 
30  48 

30  32 

31  36 
31  10 

157  56  54 
164  21  25 
in  43  46 

158  38  54 

38  39 
160  43  10 

156  51  16 
162  58  40 

153  45  49 

157  43  3i 
43  42 

155  15  8 

124    4  15 

142  29  5 

1 1 1  46  7 

45  55 

46  20 
46  1 1 

159  33  28 

33  43 
33  4° 
155    3  54 
164  42  15 

157    4  27 
3  45 


B;  S;  R;  20"  

pB;  R;  gbM;  30"  

B;  R;  gbM;  30'   

F ;  R ;  the  preceding  of  three  

pF;  S;  irreg  R;  psbM;  25"  

v  B ;  R;  g  m  b  M  ;  60"  (in  a /of  1°  continued  to  6h  4'",  in  which  no  other 
nebula  occurs  after  this.) 

vB;  R;  gbM;  30"   

$;  B;  S;  Rj  gmbM;  70";  resolved  

0;  vB;  R ;  vgvmbM;  r. — [Note.  The  minute  of  R  A  given  by  this 
obs  is  59,  but  this  is  decidedly  mistaken.  (See  the  remark  on  J"  748 
above,  no  nebula  under  those  circumstances,  however  faint,  to  say  no- 
thing of  so  conspicuous  a  one,  could  by  possibility  have  escaped  notice.)] 

pB 

pF 

PB 

pF 

pF 


?e,  n  f . 


;  R;  gb  M;  40"   

;  S  ;  R  ;  the  second  of  three  

;  S ;  R ;  has  a  *  1 5  m  close  to  the  1 

;  S  ;  irreg  R;  psbM;  25"  

;  R;  gbM;  30"   

F;  S;R;gbM;  18"  

F  ;  irreg  R  ;  pslbM;  40"   

F;  R;  g  1  b  M ;  40*;  .-1*9111  follows  in  parallel,  and  3  more  11  m  near 

v  F ;  p  L ;  RjvglbM;  80"   

F;  R;  v  g  1  b  M;  40"  

0;  no  other  description   

v  B ;  R;  psmbM;  60"   

v  B ;  R ;  m  b  M ;  40"  

0;  B  ;  R ;  psbM;  resolved  ;  much  compressed ;  the  3rd  of  3   

v  B;  R;  g  m  b  M;  90";  r  

F;  S;  R;  gbM;  15"  

F ;  p  L  ;  R ;  g  p  m  b  M ;  2'  

F  ;  p  m  E ;  g  1  b  M ;  40"  

p  F;  R;  lb  M;  50'  

vF;  L;  R;  gbM;  2'   

eeF;  vL;  R;  glbM;  4'   

e  e  F;  R;  p  L;  gbM;  2'  

p  F ;  R ;  gmbM;  90"   

«F;  v  S ;  R ;  10"  \   

F;R;lbM;  15"  

p  F  ;  irreg  R;  r  

v  F;  S;  R  

pF;  vmE;  gvlbM;  2'  1  

pB;  vS;  E;  vsbM;  a  ruddy  star  9  m  prec  about  5s  in  R  A  

F;  R;  p  s  1  b  M;  60"  

pB;  R 
B;  pL 
pF;  R 


Many  stars  near  it 


gmbM;  40"  . 
R  ;  p  s  p  m  b  M 

gbM;  60";  r  

Double  nebula,  pos  i2°-5  ;  larger  p  B  ;  R ;  gbM;  40";  smaller  v  F  ;  R  ; 
glbM. 

F ;  irreg  R;  gbM   

v  F ;  irreg  R  ;  gbM;  50';  r  

F ;  irreg  fig ;  glbM;  has  2  or  3  stars  in  it  

v  F;  R;  gbM;  2'  

v  F  ;  R ;  40"  

vF;  R;  gbM;  40"  


538 
656 

759 
522 
512 
748 

523 
673 
657 


759 
522 

538 
512 

759 
668 
666 
5i8 
515 

539 
656 

759 
538 
522 
512 
760 
672 
647 

538 
512 
657 
761 
672 

539 
653 
760 

5i5 
663 
765 

533 
647 
532 
768 
523 

673 
657 
5i8 
672 
538 
760 


84 


REDUCED  OBSERVATIONS  OF 


No. 


Svnon. 


E  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


3029 

3030 

3031 
3032 

3033 


3034 

3°3S 
3036 


3037 

3039 

3040 
3041 

3042 
3043 


3044 

3°45 
3046 
3047 
3048 


3049 
3050 


3051 
3052 
3053 


3°54 


A.  201 


A.  616? 


8  91 
12.8 
8  24.1 

*5-3 

8  40.0 

9  6.3 


6    9  11. 3 
12.5 
12.9 
6    9  58± 
6  10  28.4 
6  12  41.5 
44-5 
5i-5 


6  12  50.8 
6  13  12.6 
6  13  42.3 

42.6 
6  14  20.9 
6  14  52.1 

54.2 
6  16  12.8 

6  17  27.2 
28.3 

30.1 
6  17  32.0 
6  17  32.4 
6  18  45.3 
6  20  24.2 
6  20 

20  42.5 
6  20  48.5 
6  21  4.2 
4.2 
6.2 

6  21  4.4 
6  21  42.4 
6  23  2.7 
8.9 

6  23  51.3 
54.1 
54-7 


i33?36  57 
i34?37  o 
i33?39  16 
134? 38  45 
163  21  50 
in  19  17 

116  42  54 

43  18 

43  2 

152  29  23 

165  23  59 

JS9  4  34 
4  4° 
4  11 


163  47  25 
161  28  58 
158  12  35 
12  38 
112  o  15 
117  10  20 
9  28 
134  41  8 

112  45  27 
44  10 

46  14 
H7  *8  47 
147  26  42 

113  54  3° 
154  22  27 
154  51  41 

52  10 

iS4  54  3° 

157  26  51 
26  1 1 
25  35 

154  57  14 
154  5°  48 
121  10  17 
10  29 

158  49  27 
49  55 
49  H 


e  F;  R;  vlb  M;  40"  

ee  F;  R.    P  D  mistaken  i°  in  one  or  other  of  these  obs  

eF;  vS;  pslbM;  rather  a  doubtful  object  

e  F  ;  R  ;  P  D  i°  mistaken  in  one  or  other  of  these  obs  

F;vS;R;  bM  

p  B  ;  p  L  ;  m  E  in  pos  =  870  ±  ;  pslbM;  2j'  1,  40"  br,  to  a  tolerably 
well  defined  round  nucleus. 


PB 
v  F 
p  F 
PF 
PB 
v  B 
v  B 
v  B 


E 


R ;  v  1  b  M ;  50"   

R;  pslbM;  25"  

R ;  b  M  ;  20"  

irreg  R ;  vgpmbM;  2';  r   ,  

R;  gmbM;  30"  

R ;  p  s  m  b  M  ;  60"  

S;  R;  pgvmbM;  35";  not  resolvable.  [This  observation  makes 
the  degree  of  polar  distance  158,  but  the  similarity  of  descriptions  and 
other  particulars  of  general  agreement,  together  with  the  want  of  any  other 
observation  of  such  a  nebula  in  a  part  of  the  heavens  thoroughly  examined, 
in  the  168th  degree,  render  it  almost  a  certainty  that  the  nebula;  are 
identical.] 

vF;  L;  R;  gvlbM;  3'  

v  F  ;  R ;  g  1  b  M  ;  30".    A  triple  star  precedes   

B;  S;  R;  or  1  E ;  resolved  into  stars  14  ...  .  16  m ;  50"  

B ;  irreg  R  ;  or  1  E  ;  g  b  M  ;  80" ;  r  

vF;  pL;  R ;  vglbM;  40"   

B ;  R  ;  p  s  m  b  M  ;  30"  

v  B ;  R ;  psmbM;  30";  r   

A  poor,  very  coarsely  scattered,  but  brilliant  cluster  of  8th  class.  Place  of 
a  star  8  in  =  B  1222,  the  chief  in  cl. 

vF;  S ;  R ;  has  a  v  S  star  at  n  f  edge,  and  a  double  #  n  f   

F ;  R ;  g  1  b  M  ;  has  1  or  2  st  on  it  and  a  small  close  double  star  (dist  3", 
12  and  12  m)  north. 

F;  L;  R ;  vglbM;  80  or  90";  has  1  or  2  st  in  or  near  M  

v  F  ;  IE;  v  g  b  M  ;  the  preceding  of  2  

vF;  IE;  vgvlbM;  the  following  of  2  

e  F ;  R ;  has  a  coarse  D  star  preceding  on  same  parallel  90"  dist  

F;  R;  glbM;  20"   

Place  doubtful,  clouded  before  transit  over  wire  and  bisection,  the  approx 
R  A  given  by  the  obs  is  34  . 8,  which  must  be  too  little. 

e  F ;  v  S ;  R ;  the  preceding  of  3   

e  F ;  S ;  IE;  the  middle  of  3  

F;  pL;  R;  gvlbM;  precedes  a  double  star   

F  ;  p  L ;  irreg  R;  glbm;  2'   

F ;  L  ;  R  ;  50" ;  among  10  or  12  stars  10  and  11  m  

e  F ;  S  ;  the  last  of  3   

v  F  ;  S  ;  R  ;  near  a  star  10  m  

p  B  ;  R  ;  g  b  M  ;  4'  diam  ;  r  or  resolved,  among  B  stars   

pB;  R;  vglbM;  all  evidently  resolved  into  stars,  not  very  rich.  Some- 
thing between  a  cl  and  a  ®.  [This  obs  makes  the  R  A  24"1  8.9,  but  it  is 
pretty  clear  that  this  is  a  misreading  of  the  chronometer.] 

F  ;  p  L  ;  R  ;  30"  

v  F  ;  R ;  glbM;  20"   

v  F;  S  ;  R  


NEBULAE  AND  CLUSTERS  OF  STARS. 


85 


No. 


3°55 
3056 

3°57 

3058 

3°59 
3060 

3061 


3062 
3063 

3064 
3065 


3066 
3067 
3068 

3069 


3070 

3071 
3072 

3073 

3°74 
3075 

3076 
3077 
3078 

3079 


Synon. 


A.  578 


VII.  14 

h.  422 


V.  21 


VII.  12 
h.  440 

VII.  17 
h.  441 


R  A.  1830.0. 


h . 

III . 

S.  U. 

0  / 

* 

6 

26 

47.6 

158  48 

45 

47.6 

49 

4 

5O.O 

49 

16 

50.6 

48 

6 

*7 

52.1 

124  41 

51 

56.9 

41 

6 

29 

14.9 

154  12 

19 

15.4 

12 

1 1 

17.9 

11 

47 

6 

31 

27.9 

114  42 

28 

6 

34 

24.4 

122  19 

15 

6 

j  j 

4.7.0 

113  18 

22 

47.8 

18 

55 

50.1 

18 

30 

6 

35 

53.6 

117  18 

4 

55.6 

17 

28 

56.6 

18 

23 

6 

38 

5.0 

117  28 

23 

6 

*i.8 
j 

116 

?8 

6 

40 

50.9 

116  32 

28 

6 

42 

55-i 

125  48 

30 

58.5 

49 

17 

59-3 

48 

5i 

59-3 

49 

23 

6 

43 

10.8 

153  32 

23 

47 

34-3 

T  C/t  A. 

6 

T/ 

46.0 

154  8 

12 

48.3 

7 

23 

6 

48 

24.1 

130  39 

58 

24.9 

38 

40 

6 

S1 

40.7 

103  28 

33 

6 

ss 

56.4 

118  27 

43 

6 

57 

8.8 

131  49 

7 

10. 1 

49 

40 

7 

0 

28.7 

102  54 

22 

7 

3 

6.8 

157  8 

25 

7 

9 

39-7 

102  54 

48 

N  P  D.  1830.0. 


i-3 

105  20 

12 

40.0 

114  38 

48 

40.0 

152  2 

17 

40.1 

2 

46 

6.2 

117  12 

3i 

Description,  Remarks,  &c. 


Sweep.  I 


B;  pL;  R;  vgmbM;  50"  

p  B  ;  R  ;  g  b  M  ;  50";  has  a  double  star  preceding  

F;  R;  vglb  M   

pB;  R  ;  g  b  M  ;  30"  

e  F;  R;  v  1  b  M  ;  25  .  .  .  30'  

e  F  ;  IE;  25".    Some  right  in  field  from  rising  moon  

F;  L;  R;  vglbM;  2'   

pB;  L ;  R;  vgbM;  r;  diam  in  R  A  =  175  of  time   

F  ;  v  L  ;  R;  gvlb  M;  3'  

Not  vF;  R;  or  IE;  pslbM;  E  between  2  v  S  st,  and  has  two  stars 
8'msp  pointing  to  it. 

p  B  ;  S  ;  R  ;  20";  has  2  or  3  S  st  close  to  it  

p  F  ;  S  ;  R ;  in  a  field  with  numerous  stars.    1 1 30  is  the  right  P  d   

F;  S;  R;  gpmb  M;  12"   

p  B  ;  S  ;  R  ;  1  b  M  ;  20".  [This  obs  makes  the  P  d  1120,  but  this  was  ex- 
amined in _/"  533,  and  declared  erroneous  as  above.] 

pF;  R;  pslbM;  35"  

F  ;  E  ;  b  M  ;  20"  

pB;  R;  gpmbM;  80";  r  

p  F  ;  L  ;  irreg  R  ;  or  1  E  ;  g  b  M  ;  2'   

A  double  nebula  the  preceding  e  F  ;  the  following  (whose  place  is  here  set 
down)  p  B  ;  both  R  ;  g  b  M  ;  in  a  field  full  of  stars,  among  which  is  also 
a  third  nebula. 

e  F  ;  S  ;  R  ;  between  stars.    A  double  nebula  precedes   

B;  R;  gpmbM;  3' all  resolved  into  st  14  m.  In  the  centre  is  a  s(c  13m 

p  B  ;  R  ;  g  b  M;  90";  resolved  into  st  14  m   

B  ;  irreg  R  ;  g  b  M  ;  3';  resolved  into  st  14  . . . .  16  m  with  stragglers,  and 
some  large  stars  near. 

0;  pB;  irrR;  gbM;  2j';  resolved  into  sti3m   

v  F;  R;  v  gl  b  M  ;  30"  

F ;  v  S  ;  R ;  makes  a  small  triangle  with  2  stars   

e  F ;  R ;  50"  

v  F ;  p  L  ;  IE;  in  the  parallel   

p  B  ;  m  E  ;  in  pos  43° ;  pslbM;  7  5"  1 ;  among  many  stars   

p  B  ;  v  m  E  ;  pos  46°.6  ;  p  s  b  M  ;  90"  1 ;  10"  br ;  in  a  field  very  full  of 
small  stars. 

A  large  region  full  of  scattered  stars,  forming  a  cluster  of  which  the  chief 
(=  8  m)  taken.  It  seems,  however,  to  be  only  a  clustering  part  of  the 
milky  way  which  here  comes  on  rather  suddenly. 

pB;  pL;  IE;  gbM;  r;  2'  long   

vF;  pL?  IE?  gmbM;  in  field  with  many  stars  

F ;  v  S  ;  R  ;  pslbM;  15";  like  a  blotted  star  ;  in  field  with  many  small 
stars. 

A  pretty  rich  cluster  ;  irreg  fig  ;  7'  diam  ;  g  b  M  ;  stars  10  . . .  14  m  ;  place 

that  of  a  D  star  the  chief 
Coarse  loose  cluster  of  about  30  stars  ;  many  11  m  ;  one  10  m  taken  

A  very  singular  nebula,  much  like  the  profile  of  a  bust,  (head,  neck,  and 
shoulders,)  or  a  silhouette  portrait,  very  large,  pretty  well  defined,  light 
nearly  uniform,  about  12'  diam.  In  a  crowded  field  of  milky  way  stars, 
many  of  which  are  projected  on  it.    See  fig.  4,  PI.  IV. 

Middle  of  a  fine  L ;  rich  cluster  not  m  comp  M.    Stars  9  12  m;  fills 

field. 

The  No.  905  A  S  C  is  the  chief  of  a  fine  cluster  of  discrete  stars,  6o°  or 
70  in  number.    R ;  gbM;  8'  diam. 

p  F;  p  L;  gbM;  90"  1 ;  60"  br  

p  B  ;  E ;  or  irreg  fig  ;  g  1  b  M   

pF;  R;  vgmbM;  40"  ;  in  a  rich  field  


538 
653 
522 
545 
54i 
663 
5i8 
539 
515 
53° 

678 

533 
768 
532 

53i 

530 
769 
769 
530 

530 

54i 
801 
663 


539 
5i5 
539 
5i5 
754 
529 

757 

769 
804 
52 

676 

538 
757 


675 
530 

6S2 

524 
771 


Z 


86 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


3080 
3081 

3082 
3083 


3084 
3085 

3086 

3087 
3088 


3089 

3090 

3091 
3092 

3093 


VIII.  35 


3094 
3095 

3096 
3097 


E  A.  1830.0. 
h.  m.  s.  d. 


VIII.  38 

h.  459 


VII.  67 


VII.  28 


VI.  36 


I\.  39 

+ 

M.  46 

h.463 
+  464 


IV.  64 


7  16  8.2 

7  17  17.7 
25.9 

7  17  2cH- 

7  17  374 

46-  3 
7  18  8.5 

7  21  45-5 

47-  7 
7  24  0.9 

7  28  2.9 
7  28  49.6 

7  28  51.5 

7  29  14.8 

7  31  39-3 
7  33  "-9 

7  34 

3.8 

7  34  16.4 
7  34  20-9 


7  35  J0-8 
1 1.1 

13-5 
14.9 
16.5 
7  36  38.8 

50.9 
5i-5 

53.2 


N  P  D.  1830.0. 


102  56  II 

no  36  33 
31  32 

117    3  - 

no  41  43 

41  21 

152  45  26 
158  40  27 
40  26 
106  50  35 

151  54  o 
104    6  50 

no  14  8 

103  29  1 

137  14  31 
108  41  35 

104  20  50 

20  18 


121  15  40 
IO7  49  l6 


158  54  13 

53  3i 

54  13 
54  13 
53  55 

159  8  55 

8  32 

8  42 

8  45 


Description,  Remarks,  &c. 


The  most  comp  part  of  a  great  sc  cl  or  rather  region,  more  crowded  with 
stars  than  the  rest  of  the  milky  way,  though  hardly  entitled  to  rank  as  a 
cluster.    The  st  run  in  singular  lines  and  curves  on  a  dark  ground. 

Cluster ;  irreg  R  ;  p  m  comp  6'.    Stars  of  mixed  magnitudes  

Cluster;  7th  class;  p  comp;  4'  or  5'  in  extent.  Stars  12  m.  [One  or 
other  of  these  observations  seems  to  have  been  mis-read  by  5'  in  P  D.] 

p  F  ;  R  ;  b  M  ;  30";  nearly  on  meridian  of  n  Canis,  or  perhaps  somewhat 
preceding. 

A  cluster  composed  of  two  groups  of  bright  stars  separated  in  R  A  by  a  dark 
interval.    Chief  He  of  preceding  group  taken. 

Place  of  a  D  star,  chief  of  a  cluster  8th  class  

v  F ;  v  S  ;  R.    In  a  field  full  of  stars  

F;  pL;  pmE;  pslbM;  90" ;  pos  of  extension  =  1 170  

B  ;  L  ;  m  E  ;  g  b  M  ;  2'  1 ;  1'  br   

A  small  but  brilliant  group  of  6  or  8  large  stars,  8,  9,  and  10  m,  within  a 
very  small  compass. 

v  F  ;  L  ;  R  ;  g  b  M  ;  r.    Is  no  doubt  a  very  distant  cluster  of  6th  class  . . 

A  very  L,  pretty  rich,  splendid  cluster,  which  more  than  fills  the  field. 
Place  of  the  chief  s(c  a  fine  double  star.  [N.B. — P  D  by  obs  103°,  but 
this  is  a  mistake.  The  cluster  is  VIII.  38,  and  not  VII.  38,  as  mis- 
printed in  h.  459. 

A  large  fine  rich  cluster,  not  much  compressed,  but  nearly  filling  the  field. 
Stars  1 1 ....  13  m,  no  conspicuous  star,  place  that  of  a  coarse  D  star  11 
and  11  m. 

A  very  large  rich  fine  cluster  of  small  stars  which  nearly  fills  the  field.  Place 

that  of  a  D  star,  class  II. 

eF;  L;  pmE;  vlbM;  involves  2  stars  

A  rather  irreg  cluster  of  8th  class  ;  p  m  comp.    The  most  comp  part  forms 

a  ridge  or  body  of  stars  elongated  in  the  meridian.    Stars  12. ...  15  iu 

with  larger  outliers. 

O.  A  very  fine  Planetary  Nebula,  oval,  uniform  in  light,  and  of  a 
very  fiat  appearance  ;  rather  faint ;  diam  in  R  A  =  4'.o  ;  has  a  15m 
on  it,  and  one  13  m  close  to  its  border.  This  object  is  excentrically 
situated  in  a  superb  cluster  of  stars  12 . .  . .  16  m  (46  Messier). 

O.  A  fine,  nearly  uniform,  slightly  elliptic  Planetary  Nebula,  40" 
diam.  A  *  14  m,  is  excentrically  situated  in  or  on  it,  which  is  doubt, 
less  only  superposed  and  belongs  to  the  fine  cluster  Mess  46,  in  which 
(somewhat  north  of  the  most  compressed  part)  this  object  is  situated.  A 
very  uncommon  and  indeed  unique  combination,  if  No.  3154  be  not  a  case 
in  point. 

A  cluster  of  about  150  st ;  B;  p  L ;  p  rich ;  not  much  more  comp  M  ;  8' 
diam  ;  has  one  H<  8  m  (place  taken),  one  red  one  9  m,  the  rest  12  ....  14  m. 

O .  An  object  which,  owing  to  general  bad  definition  to-night,  and  not  be- 
ing able  to  follow  beyond  its  transit  (being  north  of  zenith),  I  could  not 
perfectly  make  out.  Certainly  not  a  star  ;  but  if  a  Planetary  Nebula, 
it  is  one  of  the  less  sharply  defined  ones. 

F  ;  S  ;  R ;  15";  near  3  B  stars   

pB;  R;  gpmbM;  35"   

pB;  S;  R;  gmbM;  25"   

p  B  ;  R  ;  b  M  ;  near  3  stars  1 1  m   

B  ;  S  ;  R  ;  p  s  m  b  M  ;  30" ;  south  of  3  st  1 1  m  

A  double  nebula ;  v  L  ;  v  F  ;  position  of  centres  =  400 ;  diameters  4'  and  3' 
running  together,  and  having  a  star  13  m  at  their  junction.  (N.B. — The 
R  A  here  set  down  seems  to  be  that  of  the  preceding  neb.) 

F  ;  v  L  ;  m  E  ;  1st  g,  then  p  s  m  b  M   

e  F ;  v  L ;  pmE;  has  a  coarse  double  *  (13  and  16  m  dist  =  12")  in 
middle. 

F  ;  v  L  ;  m  E  ;  v  s  1  b  M  ;  to  a  *  13  m,  like  a  very  faint  atmosphere, 
about  a  nucleus  31'  1 ;  1^'  br ;  pos  of  its  extension  =  39°-8.  I  think  it 
has  some  sort  of  hooked  appendage.— [N.B.— /»  these  three  last  observa- 
tions the  nature  of  the  object  appears  to  have  been  misapprehended.  In 
/523  it  was  evidently  better  seen  and  more  satisfactorily  made  out.} 


NEBULAE  AND  CLUSTERS  OF  STARS. 


87 


No. 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 

768 
540 

771 


3098 
3099 

3100 


3101 
3102 
3103 


535 


3104 

3i°5 
3 106 

3017 


3108 


3109 
3110 
3111 


VII.  10 

VII.  23 

h.  479 
A.  626 


7  37  22-9 
7  39 

7  4°  33-° 


34-5 


7  4°  43± 
7  4i  33-9 
7  46  8-7 


7  46  33-6 
7  47  48-2 
7  48  1-3 

7  49  '9-9 
27.1 

7  5°  37-o 
42.8 

7  51  25.0 
7  54  52-6 
7  55  l6-4 

29.6 
31.4 

34.6 
61.5 
62.4 


113  28  30 
127  33  59 

116  55  49 


55  43  = 


116  50  ± 
110  52  41 
128    7  27 
5  43 


160  59  5 
117  25  22 
113  51  16 

119  37  29 
3«  7 

103  53  59 
54  38 

141  50  26 
101  49  51 
150  21  36 

24  46 
24  30 


23  39 

21  16 

22  7 


A  fine  cluster,  scarcely  scattered,  pretty  rich,  not  much  more  comp.  M. 
Nearly  fills  field.    Stars  8  13  m. 

The  chief  star  (4' m)  of  an  orange  colour,  of  a  very  large  and  very  diffused 
cluster  of  large  stars,  too  loose  to  be  a  fit  object  for  the  ordinary  magni- 
fying power. 

O  •  In  the  field  with,  and  south  of  a  cluster,  and  on  a  rich  ground  is  the 
undefined  object  of  f  769.  (See  the  next  observation.)  It  is  no  doubt  a 
very  faint  small  round  Planetary  Nebula,  4",  or,  at  the  very 
utmost,  5"  diameter,  and  =  in  light  to  a  star  11  m.  There  is  an 
appearance  of  elongation,  but  this  is  probably  owing  to  one  or  more 
e  e  S  stars,  as  the  field  is  full  of  such.  It  is  dim,  faint,  and  a  very 
little  hazy.  All  the  other  stars  are  sharp,  and  the  definition  to-night 
is  perfectly  good. 

An  object  whose  nature  I  cannot  make  out.  It  is  certainly  not  a  star,  nor 
a  close  double  star  ;  but  it  is  not  round,  and  I  should  call  it  an  oblong 
Planetary  Nebula,  by  reason  of  its  decidedly  marked  though  some- 
what dim  outline,  were  there  not  some  suspicion  of  its  being  double,  as 
if  a  very  close  and  highly  condensed  double  nebula.  It  is  very  small, 
and  rather  faint,  8"  long,  5"  broad,  and  equals  a  star  10  m.  In  a  field 
with  at  least  60  or  80  stars,  all  sharp  and  well  defined  but  this. 
[N.  B. — The  P  D  open  to  uncertainty,  as  the  telescope  rests  on  the 
gallery,  and  I  cannot  get  it  low  enough  for  bisection.  An  estimated 
allowance  of  2'  made  for  this.] 

A  small  but  condensed  cluster,  class  VII.  p  Rich,  diam  3'.  [This  is  the 
cluster  referred  to,  as  in  the  field  with  the  Planetary  Nebula.] 

Irregular  cluster,  p  Rich,  not  m  comp  M,  10',  stars  12  m  nearly  equal. 
General  middle  taken. 

Superb  cluster,  g  b  M,  20'  diam,  much  more  than  fills  the  whole  field. 
Stars  10  and  11  m  all  nearly  equal. 

Cluster  6th  class  ;  B  ;  L  ;  Rich,  not  very  highly  condensed  in  the  middle. 
Stars  very  remarkably  equal.  All  12  or  13  m.  Very  few  14  m; 
none  11.    A  fine  object. 

Viewed.  A  very  beautiful  large  cluster,  very  rich  ;  stars  nearly  equal,  and 
um;  g  b  m  ;  not  m  comp  M ;  more  than  fills  the  field.  [N.  6. — It  is 
visible  in  the  finder  of  the  equatorial,  and  in  the  telescope  of  that 
inst  appears  as  a  fine  cluster.'] 

vF;  R;  lb  M;  25"   

Cluster  8th  class.    L ;  loose  and  straggling.    A  milky  way  cluster  

A  very  rich  milky  way  cluster,  or  mass  of  stars  10,  11,  and  12  m;  diam  20'. 
The  neighbourhood  is  rich,  but  much  less  so  than  this  cluster. 

Cluster  7th  class.    R  ;  5'  diam ;  stars  12  m  

A  R  ;  p  comp  cluster  of  stars  11  13  m;  6th  or  7th  class  ;  g  b  M  ; 

pretty  rich ;  7'  diameter. 
F  ;  R  ;  g  b  M  ;  30"  ;  in  a  field  full  of  stars   

pF;  IE;  in  parallel;  glbM;  25"  long.  [N.  B.— Both  observations 
correctly  reduced.    Perhaps  5'  mistake  in  one  or  other.] 

pF;  R;  vgpmbM;  25"   

F  ;  v  S  ;  R  ;  between  3  stars  13  and  14  m  

An  orange-coloured  *  8  m,  in  middle  of  a  L  and  magnificent  cluster  of 

perhaps  200  or  250  stars  8  16  m.    Many  of  the  larger  magnitudes, 

and  really  a  superb  object.    Very  visible  to  the  naked  eye,  &c. 

A  double  star  in  the  same  cluster  

Place  of  a  double  star  in  a  fine  sc  p  rich  cl  of  L  st,  which  fills  field,  and 
may  contain  150  stars,  large  and  small.  No  other  remarkable  double 
star  in  it. 

Chief  D  star  in  a  fine  cl  7th  class,  stars  7  12  m.    Fills  field,  and  has 

outlying  stars  two  or  three  fields  preceding. 

A  star  6  m,  one  of  the  chief  of  a  large  splendid  cluster,  coarse,  filling  field. 

20'  25'  diam  ;  stars  9 ....  13  m. 

A  star  6  m,  in  a  superb,  v  L  cluster.    Rich  and  brilliant.    In  the  northern 

part  about  20'  ;  following  this  *  is  a  star  5  m,  ruddy.    Has  two  or 

three  neat  double  stars  in  it.    The  whole  region  round  is  rich  in  large 

stars. 


769 


771 
677 
661 
540 

659 


545 
53i 
768 

771 
531 

676 
687 

763 
687 
524 

524 
664 

764 
681 
682 


88 


REDUCED  OBSERVATIONS  OF 


No. 

3112 
3113 

3114 
3115 

3 1 16 

3117 

3118 

3T19 
3120 

3121 
3122 


3123 

3124 

3125 
3126 
3127 

3128 
3129 

3130 


Synon. 


VIII.  30 
h.  488 


VII.  11 


A  S  C. 
1 00 1 


A.  563 


A.  411 


VII.  64 

h.  503 


III.  902 


R  A.  1830.0. 
h.  ra.  s.  d. 


IV.  35 
h.  513 


II.  266 


7  55  35-* 

8  o  7.5 

1 1.7 

8    2  42.6 
2  43.8 
8    3  17-7 


8  5  15.5 
21.4 
22.9 

8    5  21.4 

56.1 

8  10  6.1 

8  11  8.9 
8  11  44.2 

46.8 
8  13  23.4 

25.6 
8  14  25.2 

27.1 


27.3 
27.9 

14  31.2 
16  25.2 

16  28.1 

24  18.6 

25  33-5 

25  45-5 

25  53-5 
56.9 
57.8 

26  12.2 
15.0 


N  P  D.  1830.0. 


117  42  45 
119  24  41 
24  56 

102    19  48 

19  47 
102  25  41 


126  55  1 

51  48 

52  32 
138  44  9 

47  23 

116  56  43 

in  17  3 

120    6  57 

6  40 

102  47  o 

46  58 

125  41  8 

40  51 


4>  5 

40  50 

119  46  31 

118  56  49 

122  25  26 
157  33  28 
105  33  35 

102  35  42 
1 12  23  11 

24  55 
23  10 
150  32  6 
32  52 


Description,  Remarks,  &c. 


Cluster  7th  class,  distinguished  among  milky  way  clusters  ;  p  rich  ;  bright. 
The  star  taken  is  the  chief  of  a  condensed  hook  in  the  following  part. 

p  comp  cl  sixth  class ;  irreg  R  stars  1 3  ...  14  m.  One  =  8'  m  near  the 
middle  taken. 

Place  (R  A  doubtful)  of  a  9m;  chief  of  cl  p  rich  ;  irreg  R  ;  g  1  b  M  ; 
5' ;  stars  13  m.  Belongs  to  milky  way,  but  is  a  much  more  compressed 
part  of  it. 

A  large,  E,  rich  cl.    Fills  field  ;  st  12  m  ± ;  a  B  st  (6  m)  s  f  

A  fine  rich  cluster  of  stars  1 1 . . . .  1 3  m,  which  fills  the  field  

A  fine  nebulous  star  6' m,  in  the  following  part  of  the  cluster  VII.  11,  and 
almost  unconnected  with  it.  The  nebula  is  faint,  but  I  feel  confident  that 
it  is  not  the  nebulous  haze.  [Notandum. — Nothing  more  difficult  than 
to  prove  a  nebulous  star  of  the  6th  m  and  above.] 

A  cluster  8th  class  of  about  20  bright  stars  in  an  oblong  8'  1 ;  3'  br  

Chief  triangle  of  stars  9,  10,  11  m  of  an  oblong  irreg  cl   

A  bright  group  in  full  part  of  a  B  ;  not  rich  ;  irreg  oblong  cl ;  6'  1 ;  3  or  4'  br 

Chief  star  7' m,  of  a  v  L,  loose,  brilliant  cl  of  v  sc  stars  ;  1  of  7  m,  2  of 
8' m  ;  rest  9 ....  16  m.    Fills  more  than  field  ;  100 ....  150  stars. 

A  L  loose  cl  8th  class  of  L  and  S  stars,  full  20'  diam.  Has  in  it  about  20 
stars  above  1 1  m,  and  one  neat  double  star.  Place  that  of  a  star  8  m  in 
the  following  part. 

p  L  ;  F  ;  g  1  b  M  ;  in  a  field  of  about  60  stars  ;  one  of  which  =  9  m,  and 
some  others  also  of  less  magnitudes  are  involved. 

v  F  ;  vS;  R  ;  gbM;  at  least  60  st  in  field  

Middle  of  cluster  ;  not  v  rich  ;  irreg  R  ;  not  much  comp  ;  10'  diam.  Stars 
12 ....  15  m,  few  very  minute. 

A  p  rich  cl  of  about  60  stars,  12 ....  13  m  ;  irreg  R  ;  g  1  b  M  ;  8'  diam.  • . . 

vF;  R;  gbM;  ina  field  full  of  Milky  Way  stars  

vF;  R;  gbM;  in  a  field  of  50  or  60  stars  

A  double  star,  surrounded  with  very  evident  nebula  which  seems  to  belong 
to  both  stars. 

A  double  s): ,  or  a  He  and  a  nebula,  very  close  and  involving  the  star.  For 
pos  dist,  &c,  see  Catal  of  Double  Stars.  The  field  contains  about  70 
stars,  of  which  8  are  9' m.  I  cannot  be  quite  positive  that  the  neb  ex- 
tends beyond  the  large  star,  or  that  the  small  one  is  not  a  mere  condensa- 
tion of  it.    However,  I  remain  pretty  well  satisfied  of  its  investing  both. 

A  neb  attached  to  a  star  12  m,  but  involving  it  

A  double  star  (h  4083)  involved  in  p  B  nebula,  which  seems  to  belong  to 
both  stars ;  but  of  the  two  the  smaller  is  more  nebulous  ;  diam  50"  ;  in  a 
p  rich  patch  of  the  milky  way. 

Cluster  7th  class;  R;  p  rich;  insulated;  10'  diam;  stars  12  m,  nearly 
uniform. 

A  milky  way  cluster  7th  class  ;  irreg  fig  ;  pretty  much  compressed  in  middle. 
Stars  10. ...  13  m  ;  one  9  m. 

A  small  F  cluster  of  st  15  m  ;  3'  diam  ;  R  ;  gbM;  not  very  rich  

F ;  R  ;  gbM;  30"  

A  small  cometic  or  fan-shaped  wisp  of  nebula  attached  to  a  s|c  13  m;  there 
is  a  H«  7  ni  10  sec  foil ;  2'  north. 

B  ;  S  ;  p  s  b  M ;  E ;  between  2  stars  

p  B ;  m  E  ;  g  p  m  b  M  ;  80"  1 ;  20"  br  

B;  L  ;  v  m  E  in  pos  no°3  ;  p  s  1  b  M  ;  3'  1;  20*  br  

pF;  mE;  pmbM;  40"  1 ;  15"  br  

A  cluster  with  a  double  star  in  it  

A  double  star,  chief  of  a  cluster  8th  class  of  scattered  stars,  6'  diam ;  not 
very  rich  or  compressed. 


Sweep. 

771 
771 
53» 

676 
757 
757 


540 
661 
659 
526 

680 


771 

768 
678 

53i 
676 
687 
786 

54i 


809 
540 

77i 
53i 

678 
557 
675 

676 

559 
532 

558 
778 
682 


NEBULAE  AND  CLUSTERS  OF  STARS.  89 


No. 


3131 


3132 
3133 
3134 

3I3S 
3136 
3137 

3138 

3i39 
3140 
3 141 

3142 
3H3 
3i44 

3H5 

3146 

3 '47 
3148 

3H9 


Synon. 


VII.  63 

h.  516 


III.  49 
h.  521 


R  A.  1880.0. 
h.  m.  6.  d. 


A.  489 
or  A.  490 


I.  59 
h.  571 


8  29  22.0 


22.8 

8  30  12.4 
8  31  47.5 
8  32  53.5 

53-8 
8  33  10.9 
8  33  20.5 
8  36  47.6 

49-3 
8  37  1.3 

2-7 

8  37  35.6 
8  40  ± 
8  40  1.9 

8  40  5.6 
8  49  22.2 
8  49  32.4 

34-7 
8  54  27.9 


o  7.5 

3  25.6 

4  45-3 
47-4 

6  1.8 

2.9 


4-3 


N  P  D.  1830.0. 


130   4  54 


4  57 


4  55 

119  22  28 
124  9  55 
144  31  28 
31  36 
75    7  2 

135  37  39 

134  21  30 

20  15 

136  35  56 
35  48 

104  40  53 
143  21  -+- 
131  16  o 

138  10  1 
148  34  34 
114    1  31 
o  50 

135  13  57 


112  58  10 
104   7  53 

113  27  51 
30  o 

I31  44  5 
43  54 


44  42 


Description,  Remarks,  &c. 


A  H«  8  m  involved  in  a  p  B  R  neb,  not  concentric,  the  #  being  somewhat 
to  the  northward  of  the  centre,  and  the  nebula  not  being  quite  equally 
dense  on  all  sides,  though  most  condensed  in  the  neighbourhood  of  the 
star  ;  diameter  of  nebula  2^'.    (No  doubt)  PI.  VI.  fig  12. 

A  s(c  9  m  involved  in  neb  ;  3'  diam.  In  the  milky  way  with  multitudes  of 
equal  stars  all  round  the  neighbourhood,  none  of  which  are  so  affected. 
Sky  quite  pure,  not  the  slightest  nebulous  haze.  No  doubt.  The  nebula 
loses  itself  imperceptibly,  the  star  being  (though  excentric)  yet  in  the  most 
condensed  part. 

A  star  9  m  in  a  decided  and  perfectly  unequivocal  nebula.  It  is  not  the 
nebulous  haze,  as  other  stars  of  equal  and  larger  magnitudes  are  unaffected. 
Diameter  3'.  I  showed  it  to  Mr.  Maclear  and  another  gentleman  who 
saw  it  as  described. 

A  fine  L,  rich,  p  m  comp  cluster ;  irreg  E  ;  10'  1 ;  7'  br ;  stars  12  and  13  m 
nearly  equal. 

A  pretty  comp  cl  of  st ;  irreg  triangular  fig ;  much  more  comp  than  milky 
way  around  it ;  stars  13  m. 

p  B ;  S ;  R ;  has  3  or  4  v  S  st  close  to  it,  preceding,  which  give  it  an  elon- 
gated and  resolvable  appearance. 

p  F ;  S  ;  R ;  has  3  or  4  v  S  st  near  it,  preceding.  Observation  taken  by 
Mr.  Maclear. 

pB;  IE;  psmbM;  precedes  a  star  10  m  


Sweep. 


A  close  group  or  small  cluster  of  12  or  13  large  and  small  stars  j  place  of  a 
double  star,  the  chief  one. 

Cl  VII  class;  p  rich;  p  L;  12'  1 ;  8'  br;  fig  irreg;  rather  branching 
stars  1 1 ....  14  m,  not  comp  in  M. 

A  L,  rich  cl ;  irreg  oblong  ;  1 5  or  20'  long   

Cl  VI  class ;  irreg  R ;  gbM;  4' ;  resolved  into  distinct  stars  14  m  

Cl  irreg  R;  3' ;  not  m  comp  M  ;  stars  13  15  m  

v  F  ;  vS;  R;  b  M  ;  near  a  H<  15  m  

Cluster  VIII  class.    A  L,  poor,  loose  cl  of  stars,  10. ...  13  m   

A  pretty  rich,  irreg  R  cl ;  not  m  b  M  ;  st  12 . . . .  13  m;  place  that  of  the 
general  middle. 

A  cluster  8th  class,  not  rich,  nor  m  comp ;  8'  in  diam  ;  irreg  R;  stars  13  m 

eF;  S;  R;  pslbM;  difficult,  but  certain   

pB;  R;  vgpmbM;  borders  very  dilute  

F;  S;  R;  gpmbM;  20"   

eeF;  L;  vvmE;  an  extraordinary  long  narrow  ray  of  excessively  feeble 
light ;  pos  1 90  ±.  The  n  f  end  is  brighter  and  narrower  than  the  sp.  At 
least  20'  long,  extending  much  beyond  the  limits  of  the  field.  A  star  8  m, 
andone  8' m  near  it.    See  PI.  V.  fig.  12. 

e  F  ;  IE;  1  b  M  ;  rather  a  doubtful  object   

B ;  E  ;  p  s  m  b  M  ;  40"  1 ;  30"  br  

B  ;  p  L  ;  m  E  ;  nearly  in  parallel ;  psmbM  

B;  L;  mE;  pgmbM;  4'  1 ;  90"  br ;  pos  =  63°7   

O  Planetary  Nebula;  as  in  f  554;  observed  with  Mr.  Maclear  and 
another  gentleman. 

O  Planetary  Nebula  ;  p  F ;  exactly  R  ;  equal  to  a  star  9  m,  but  of  a 
dull  light.  At  first  I  was  inclined  to  think  it  double,  but  with  320  it  ex- 
hibited a  uniform  round  disc ;  nor  did  a  friend  to  whom  I  showed  it  see 
any  division.  Stars  to-night  perfectly  well  defined.  In  a  field  with  lead- 
ing stars,  of  which  a  diagram  was  made. 

p  B ;  R ;  6"  diam ;  equals  in  light  a  star  9' m  ;  a  very  careful  and  good 
observation. 

Viewed  past  meridian.  It  occurs  in  a  field  with  about  40  stars.  Diam  4" 
or  5"  at  the  utmost;  10"  is  too  large  certainly.  Very  like  that  of ./771, 
(h.  3101)  But  now  the  night  is  good  and  it  bears  magnifying.  With  320 
the  disc  is  dilated  into  a  dim  hazy  round  nebula ;  yet  there  is  a  peculiarity 
in  its  appearance  which  completely  separates  it  from  all  nebula;  of  the 
same  size.    A  very  remarkable  object. 


554 


529 


555 

53' 
54i 
552 
55' 
688 

527 
685 

542 

527 
553 
687 
440 
554 

680 
543 
559 
558 
553 


532 
687 

559 
532 

555 
554 


810 


772 


A  A 


90 


REDUCED  OBSERVATIONS  OF 


No. 

3150 
3*51 

3152 


Synon. 


3153 
3154 


3155 
3156 

3*57 
3158 

3IS9 
3160 

3161 

3 162 
3163 


II.  505 
h.  580 

A.  265 


III.  242 

A.  564 


R  A.  1830.0. 
h.  m.  s.  d. 


9  6  icrfc 
9    8  13.0 

9    8  24.8  : 

38.7 
41.0 


42.4 

9  8  43.0 
9    9  8.6 


9.4 


9  9  20.9 

9  10  20-t- 

9  II  18.9 

9  II  49.I 

9  II  51.I 

9  12  43.O 

9  '5  4-9-1 
50.9 

9  16  21.4 

9  16  33-3  ■ 


35.2 


37.6 
38.5 


N  P  D.  1830.0. 


IS7  14  32 
I05  35  48 

154    9  56 

9  56 
9  5« 


112  54  51 
I25  53  5i 


55  5 


116    7  20 

158  56  17 

158  38  22 

152  21  23 

127  18  7 

129  49  50 

112  25  51 

28  o 

140  22  44 

147  35  23 


35  21 


35  35 


35  1° 


Description,  Remarks,  &c. 


v  F;  v  S  ;  m  E  in  pos  1050  

pB;  mE;  psvmbM;  40"  1 , 


® ;  e  comp  pgvmbM;  up  to  a  perfect  blaze ;  diam  in  R  A  =  26\8  ; 
stars  16  m ;  equal.  R  A  doubtful;  the  mirror  being  in  a  spring  case 
(afterwards  disused). 

Superb  0  ;  diam  =  5' ;  v  m  comp  M  almost  to  a  nipple.  Stars  innumerable 
and  very  small;  13  ...  15  m. 

A  truly  beautiful  and  delicate  ®  ;  diam  in  R  A  =  45',  that  of  the  most  com- 
pressed part  15s;  g  v  b  M  ;  all  finely  resolved  into  perfectly  equal  stars 
like  the  finest  dust,  which  are  seen  with  the  left  eye  without  effort,  but  the 
right  requires  to  be  somewhat  strained  to  discern  them.  Runs  up  to  a 
blaze  in  the  centre. 

(B  >  4-'  or  5'  diam  1st  p  g,  then  p  s  b  M  ;  all  resolved  into  stars  16  m  and  a 
few  15  m.    A  neat  D  star  foil  dist  1  field 

F  ;  R,  or  v  1  E  ;  g  1  b  M  ;  25"  

A  very  curious  object  which  reminds  me  strongly  of  Messier's  No.  46  and 
IV.  39.  It  is  a  rich  cluster  of  the  VI  class  ;  stars  12. ...  14  m  ;  about 
8'  diameter  ;  g  p  m  b  M  ;  all  but  a  sort  of  vacuity,  in  which  is  situated  a 
p  B,  R,  neb  ;  40"  diam  ;  of  a  character  approaching  to  planetary,  having 
its  edges  shading  off  very  rapidly,  and  being  but  very  little  brighter  in  the 
middle. 

pB;  R;  vgvlbM  from  the  edge,  where  it  fades  off  very  suddenly  ;  be- 
ing all  but  a  planetary  nebula.  Situated  in  a  sort  of  vacancy  in  the  pre- 
ceding part  of  a  fine  rich  cl  of  st  1 1 . . . .  1 5  m,  which  nearly  fills  the  field. 
It  is  a  fellow  object  to  Messier's  46th,  with  its  enclosed  planetary  nebula, 
IV.  39.  PI.  V.  fig.  8. 

e  F  ;  attached  to  a  *  1 1  m  ;  somewhat  doubtful   

pF;  vS;  R;  glbM  

F ;  R ;  glbM;  40".    Nearly  on  merid  with  /3  argus  

F  ;  v  S  ;  between  two  st,  in  a  field  full  of  milky  way  stars.  No  doubt  of  the 
nature  of  the  object. 

v  F  ;  S  ;  R  ;  attached  to  a  star  12  m,  s  f   

0;  eF;  R;  vglbM;  resolved  into  v  S,  but  not  very  numerous  stars ; 
%\'  diam.    It  is  rather  a  cluster  of  the  6th  class  than  a  ®. 

B;  S;  R;  pgmbM;  the  borders  very  dilute   

pB;  S;  R;  vlbM;  15"  

Cluster  class  VIII.    Place  of  a  small  compact  knot  of  st  

O-  Planetary  Nebula.  R  A  doubtful,  being  far  below  the  f.  Pos  of 
adjacent  star  =  58°.8  ;  57°-3  :  mean  58°.o.  Set  microm  to  51. 1,  the 
measure  of  last  night,  and  carefully  examined.  It  cannot  pass  as  a  mea- 
sure, and  must  have  been  a  mistake  for  56. 1  or  61. 1 ;  measured  to-night 
with  the  utmost  care  ;  quite  calm. 

O-  Perfectly  sharp;  exactly  R;  not  the  least  hazy  or  mottled.  At  i£ 
diam  distant  from  the  edge  (or  taking  12"  for  the  diameter  of  neb  at  24" 
dist  from  centre)  there  is  a  star  at  pos  =  Si°.i  ;  well  examined  with  Mr. 
Maclear.  It  bears  320  well,  and  is  quite  sharp  and  uniform  with  that 
power.    R  A  imperfect  being  out  of  the  regular,/. 

O-  Beautifully  round  and  sharp  ;  just  like  a  small  planet  3"  or  4"  in  diam 
at  the  utmost.  Position  of  the  attendant  star  =  59°-3,  57.8  ;  mean  58.5  ; 
dist  2  j  diameters  from  centre.    Shown  to  Captain  Henning. 

O-  R  >  =  *  8  m ;  R ;  quite  uniform  in  light;  quite  sharply  terminated. 
Its  diameter  transits  over  a  wire  set  to  6o°  (30  from  parallel)  in  4  .03,  by 
a  mean  of  5  transits  ;  has  a  %  adjacent ;  pos  =  6o°.7  ;  dist  =  1  \  diam 
from  the  edge.  About  40  stars  in  the  field,  among  which  two  are  9  m. 
[This  would  give  16"  but  the  wire  was  much  too  thick.] 


NEBULjE  and  clusters  of  stars.  91 


No. 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


3l6+ 

3165 
3 166 

3167 
316S 


3169 

3170 
3171 


3172 
3*73 


3 '74 
3*75 
3176 


3177 
3178 


3179 


3180 


III.  597 


II.  556 


38.6 


38.8 


39.2 


9  J8  15-3 

9  18  46.3 
9  18  52.7 

54.8 
9  19  20.4. 
9  19  28.8 

31.8 


9  21  4.7.0 

9  22  57.6 
9  24  20.0 

55-5 

9  26  26+ 

9  26  35-9 
42.8 


9  27  2-5 
9  27  7.6 

9  27  56-7 


9  27  57-6 
9  28  48.4 


N  P  D.  1830.0. 


52.6 


9  29 


9  29  52.6 

S3-o 


34  55 


35  13 


35  4i 


123  21  55 

in    o  55 

117  17  23 

18  2 
114   4  o 

153    4  5i 

4  23 

5  6 


145  22  1 
22  57 
119  38  58 
142    9  -4- 

11  56 

110    6  + 
110  10  13 
9  54 

165  52  54 
105  38  52 
179  34  14 


142  41  26 

no  22  15 

22  34 

136  11  .. 


in  16  6 
17  40 


Description,  Remarks,  Sec. 


O-  The  finest  Planetary  Nebula  I  ever  remember  to  have  seen  for 
sharpness  of  termination ;  3"  diam  ;  exactly  R ;  no  more  haziness  about 
them  than  would  be  about  a  star  of  the  same  magnitude  to-night  (which  is 
a  favourable  one).  Light,  a  pale  white  =  H<  9' m.  Pos  of  companion 
s|c  =  59  8;  57.7;  58.4;  mean  58°.6  ;  >K  =  15  m.  A  very  remarkable 
object.  Showed  to  Stone,  who  distinctly  perceived  the  total  difference  of 
appearance  between  it  and  a  star  9' m  very  near  it.  A  second  companion 
sje  suspected  (at  about  half  the  distance  of  the  1st  by  diagram,  and  at  an 
estimated  position  of  3300  +)  among  multitudes  of  L  and  S  stars. 

0«  Diameter  8";  perfectly  uniform  in  light;  sharply  terminated,  just  like 
a  small  planet.  Position  of  attendants  star  =  6o°.7,  by  mean  of  2  mea- 
sures ;  dist  1  \  diam  ;  14th  mag. 

Quite  sharp  and  round  ;  8"  diam  ;  =  a  +  8  m  ;  pos  of  a  star  14  m  ;  dist 
1^  diam  from  edge  =  6o°.8,  by  a  mean  of  3  measures.  There  are  56  stars 
in  field  with  it,  of  which  the  largest  is  9' m. 

Observed  with  Mr.  Maclear,  April  2,  1834,  out  of  the  meridian.  Quite 
round,  well  defined,  and  about  3"  or  perhaps  4"  diam.  Much  better  seen 
(between  clouds)  than  last  night.  (/435O  The  small  star  is  still  i£  diam 
from  edge.  It  has  therefore  not  moved  perceptibly,  and  is  therefore  not  a 
planet. 

A  v  F,  S,  cluster,  class  VI ;  v  g  1  b  M  ;  resolved  so  as  to  see  the  stars  which 
are  15  m;  almost  to  be  called  a  v  F,  large  nebula. 

eeF;  50"  

p  F  ;  R  ;  s  m  b  M  ;  very  dilute  at  edges  ;  30"  

vF;  R;  gpmbM;  15"  

F  ;  S ;  R  ;  b  M  ;  15'   

F;  S;  R;  psbM;  15  20"  ;  has  3  stars  near,  prec   

F;  S;  R;  gpmbM;  20"   

F ;  S  ;  R ;  g  b  M;  near  a  bright  * •    (N.  B.— The  R  A  by  this  obs  comes 

out  i2\9  ;  but  the  mirror  having  been  put  by  inadvertence  into  a  case 

with  springs,  the  zeros  fluctuated,  and  the  observation  is  entitled  to  no 

weight,  the  collimation  having  been  neglected.) 

F;  pL;  R;  glbM;  80".   At  least  80  stars  in  field   

No  description   

F;  S;  vlE;  psbM;  15".    "Very  dilute  at  the  edges  

Cluster  of  loose  stars  ;  p  rich  ;  stars  n  ...  15  m ;  has  rather  a  vacancy  in 

the  middle  ;  fills  about  f  of  field. 
Cluster,  class  VII.;  p  rich,  L,  and  fine.    Stars  10...  13  m,  in  irregular 

lines  and  tracing.    The  chief  *  10  m,  taken  near  the  most  compressed 

part. 

e  F  ;  S  ;  R ;  the  preceding  of  two  

v  F  ;  p  L ;  IE;  the  following  of  two  

F  ;  IE;  glbM.  This  obs  makes  the  degree  of  N  P  D  109.  But  as  there 
can  be  no  doubt  of  the  identity  of  this  neb  with  my  Father's  III.  597,  his 
degree  (1 10)  is  preferred.    The  right  ascensions  in  this  sweep  are  bad. 

PF;pL;R;gbM;  45"   

p  B  ;  R;  20"  

Neb  Polarissima  Australis.  F ;  R  ;  glbM;  25".  Situated  nearly  half 
way  between  a  s(c  10  m  south  of  it,  and  a  small  triangle  of  st  1 1,  13,  13  m 
north.  Being  so  near  the  pole,  the  R  A  may  err  many  minutes  of 
time. 

A  pretty  rich  cluster,  8th  class ;  a  D  *  (one  of  the  chief)  taken  

pF;  R;  gpmbM;  40".  The  obs  makes  the  degree  109,  but  1 10  agrees 
with  my  Father's  place,  and  with  that  of/  561,  and  is  preferred. 

pB;  vS;  gmbM;  IE;  25"  1,  20"  br.    (R  A  not  good.)  

This  is  about  the  middle  of  an  enormous  cluster  of  a  degree  or  degree  and 
half  in  diameter,  very  rich  in  stars  of  all  magnitudes,  from  8  m  down- 
wards, which  merits  registry  as  a  sort  of  telescopic  Prsesape.  It  may 
perhaps  be  regarded  as  a  detached  portion  of  the  milky  way,  which  is 
here  very  much  broken  up. 

F;  S;  R;  gib  M;  20"  

F;  S;  R;  glbM;  2  or  3  small  stars  near  


Sweep. 


435 


764 


543 


787 

77° 
564 
771 

53* 
568 

773 
430 


55* 
784 
564 
439 

763 


770 
770 
561 

782 

675 
781 


763 
770 

56, 
776 


559 
53* 


92 


REDUCED  OBSERVATIONS  OF 


No. 

3181 
3182 

3184 

3185 
3186 
3187 
3188 


3189 
3190 

3191 

3192 
3193 
3194 


3i95 
3196 
3197 

3198 
3199 
3200 
3201 
3202 
3203 


3204 
3205 
3206 

3207 
3208 
3209 
3210 
321 1 
3212 
3213 
3214 
3215 
3216 
3217 
3218 


Svnon. 


A.  397 


III.  289 


V.  50 


II.  98 

III.  600 
III.  272 


III.  601 
III.  273 

II.  268 


R  A.  1830.0. 
h.  m.  8.  d. 


II.  293 


9  31  5-5 
9  3"  •• 

9  34  12.6 
9  35  42-3 

9  35  43-8 
9  37  37-2 
9  38  4.7 

9  38  *3-2 

14.6 

9  38  21.4 
9  38  51.4 

9  39  •• 

9  4i  34-6 
9  41  53.1 
9  43  2.4 

2.7 

9  43  45-° 
9  43  46-6 
9  44  i5-6 

9  45  13-8 

9  45  4°-8 

9  46  14.8 

9  46  20.1 

9  46  25-7 
9  46  53.7 

56-3 
9  47  0.9 
9  48  1 1.8 
9  49  21.5 

22.6 
9  49  41.7 
9  50  6.8 

9  5°  42-7 
9  51  20.4 

9  5'  23-7 
9  51  25-7 
9  51  46-3 
9  51  58.8 
9  52  14.0 
9  52  33-6 
9  52  37-5 
9  53  7-9 


N  P  D.  1830.0. 


74  18  5 
74  24  .. 

139  33  26 
133  58  11 

109  41  45 

107  36  14 

110  48  34 
120  24  26 

24  48 

J43  59  49 
119  39  48 

139  39  .. 

no  57  1 

108  23  19 
145  37  18 

37  28 
116  13  45 
72  31  34 
151  33  51 

107  50  39 

116  32  1 

72  45  38 

116  29  31 

107  50  19 

117  30  13 

30  9 

72  21  37 

163    9  50 

108  32  20 
32  19 

74  45  26 

107  21  55 
116    6  51 

119  33  18 

116  19  35 

108  42  24 
123  25  13 

117  30  17 
108  49  19 

120  44  19 
108  49  24 
120  51  3 


Description,  Remarks,  &c. 


v  F ;  R ;  20".    Another  suspected  6'  south,  nearly  on  the  same  meridian  . . 

Suspected  nebula.  (N.B. — These  suspicions  have  been  so  constantly 
verified  on  re-observation,  that  I  have  little  hesitation  in  registering  it 
as  an  object  in  the  catalogue.) 

A  small  p  comp  cluster  ;  irreg  fig  ;  4'  in  extent.    Not  rich  stars,  13  m  .... 

A  cluster  of  about  20  stars  1 1  m,  and  2  of  10' m,  forming  an  oblong  nearly 
in  parallel;  place  of  preceding  *  10' m. 

pB;  R;  bM;  r  

F  ;  R ;  g  b  M  ;  precedes  a  coarse  D  star   

v  F  ;  S  ;  has  a  %  2°  m  1'  following   

F ;  v  L ;  first  v  g,  then  v  s  m  b  M,  to  a  nucleus  (exactly  like  Halley's 
comet)  as  now  (Feb.  16,  1836)  seen  in  the  equatorial;  R;  diam  in 
R  A  =  24*.o.    Has  a  sfc  1 1  m,  s  p  just  at  the  edge. 

pB;  vL;  R;  v  s  1  b  M,  to  a  pretty  distinct  round  nucleus  4"  diam. 
Diam  of  nebula  =  15'  of  time.  The  nebulous  atmosphere  extremely 
dilute.    A  very  remarkable  object. 

Cluster  VIII.  class  ;  at  least  20  st  11  m  and  upwards,  and  many  smaller  . . 

F;  R;  30";  attached  or  contiguous  to  a  sfe  12  m ;  pos  =  3200  +  by 
estimation  from  diagram. 

A  small  irreg  cl  of  a  long  triangular  diverging  figure ;  contains  perhaps 
50  stars  12...  15  m.  Observed  for  A  397,  and  place  only  rough. 
Possibly  the  same  object  with  f  680,  No.  27,  which  see  above  (No.  3183). 

e  F ;  v  S  ;  R ;  north  of  a  H«  9  m  

F;  S;  R;  lb  M;  15"  

irreg  R  cl,  8'  diam,  of  50  or  60  st,  n  and  12  m.  In  the  milky  way,  but 
sufficiently  rich  and  distinct  to  be  registered  as  a  cluster. 

The  •}{■  B  2686,  in  the  midst  of  a  great  number  of  stars  n  and  12  m  

F ;  R ;  1  b  M  ;  30"   

®  ;  F ;  L  ;  R  ;  v  g  1  b  M  ;  2»' ;  resolved  with  left  eye   

The  chief  star  10  m,  of  a  cluster  class  VIII.  of  sc  st  10'  diam.    It  is  on  the 

borders  of  the  milky  way. 

v  F ;  R  ;  1  b  M  ;  30".    (R  A  correctly  reduced.)  

p  F  ;  R.    R  A  precarious  ;  a  hurried  observation  

v  F;  1  E;  gb  M;  25"  

p  F;  S;  R;  gb  M;  20"   

p  F  ;  L ;  R  ;  g  b  M  ;  50"   

pB;  S;  R;  vsmbM;  has  a  *  10  m  almost  contiguous ;  pos  from 

neb  =  203°.8. 

p  B  ;  R ;  25" ;  attached  to  a  s|e  12m  

e  e  F ;  R  ;  20"   

F  ;  L  ;  irreg  R  ;  g  1  b  M  ;  3' ;  many  v  S  stars  near  and  in  it   .... 

vF;  R;  glbM;  40"  

v  F  ;  E  ;  glbM;  60"  1 ;  50"  br   

v  v  F  ;  forms  an  appendage  to  a  *  !4  m  i  a  *  1 1  m  follows  

eF;  S;  R;  15*   

B  ;  R ;  g  m  b  M  ;  30"  

v  F ;  S  ;  R ;  close  to  a  double  star.    Requires  verifying  

v  F ;  S  ;  R ;  attached  to  a  s(c  13  m,  s  f  

v  F ;  v  S ;  R.    P  D  liable  to  some  uncertainty  

pB;  S;  R;  pmbM;  between  2  st  13  m   

p  F ;  R ;  60";  has  2  or  3  v  S  st  involved,  and  a  *  8  m  ;  2'  dist,  foil  

p  B  ;  p  S  ;  the  preceding  of  two  

F ;  L  ;  E  ;  v  g  v  1  b  M  ;  3'  1 ;  2'  br   

e  F  ;  R;  lbM;  follows  II  293.    (Place  somewhat  uncertain.)  

p  B;  R;  30";  gpmbM   


NEBULA  AND  CLUSTERS  OF  STARS. 


93 


Synon. 


3219 

3220 

3221 

3222 
3223 
3224 


3225 
3226 
3227 


3228 


3229 
3230 
3231 

3232 
3*33 


3234 
3235 
3236 

3*37 


I.  163 
h.  668 

A.  297 


R  A.  1830.0. 
h.  m.  s.d. 


N  P  D.  1830.0. 


9  54  39-z 
46.5: 

9  54  54-9 
60.8 

9  55  i7-5 
18.0 

9  56  41-7 
9  56  44.1 

9  56  54-9 


74.6 
91.8 


9  57  56-° 
9  58  36.8 
9  58  52.1 
55.6 
9  59  48.8 


51-7 


53.6 
55-9 

10  1 

10    1  8.8 
10    1  23.0 
23.9 
10    1  40.4 

10    4  6.7 


10  5  26.0 
10  6  46.8 
10  6  56.7 
57.0 
10    7  56.3 


143  58  19 

57  - 

120  51  32 
51  20 

115  20  45 
20  51 

"7  37  34 

96  54  13 
149  11  19 


21  33 
21  30 


123  23  55 
108  24  54 
119  5  42 
7  18 
129  36  45 


36  7 

36  33 
36  2 

158  33  •• 
118  13  37 
156  32  54 
32  39 
97  39  6 

120  47  15 


169  35  7 
116  50  51 
118  2  19 
2  3 
104  57  2 


Description,  Remarks,  &c. 


A  rather  remarkable  S  oval  cl  of  v  S  stars,  with  a  train  of  large  stars  running 
out  of  it,  s  p. 

A  small  close  clustering  knot  of  st  13  16  ra;  oval;  a  great  train  of  st 

12 ....  1 3  m  on  the  sp  side 

F;  S;  R;  gbM;  15'  

F;  S;  R;  lbM;  15'  

F ;  vL;  v  m  E ;  10'  1 ;  90'  br ;  place  of  a      12  m  in  or  near  the  centre 

v  F  ;  v  L  ;  12'  1 ;  2'  br ;  1  b  M  ;  pos  of  axis  82°.3-    See  PI.  V.  fig.  9. 

e  F ;  L  ;  3' ;  makes  an  obtuse  angled  triangle,  with  2  st  8  m  ;  one  nearly  on 

the  parallel,  the  other  nearly  north. 
vB;  L ;  v  m  E  ;  vsvmbM;  observed  among  clouds  


An  enormous  congeries  or  clustering  region  of  stars  2  or  3  fields  in  diameter, 
constituting  a  decided  cluster.  Stars  9. ...  14  m,  the  larger  magnitudes 
predominating.  There  must  be  many  hundreds.  The  place  taken  in  the 
centre  of  a  bright  equilateral  triangle. 

The  chief  >fc  9  m  of  a  v  L,  loose,  brilliant  cluster,  which  fills  many  fields  . . 

The  chief  jfc  8  m  of  a  v  L,  loose  cl  of  stars,  9 ....  13  m,  which  fills  many 
fields.  [As  both  this  and  the  last  observation  are  distinctly  written  and 
correctly  reduced,  no  doubt  they  belong  to  two  distinct  and,  nearly  equal 
stars  on  the  same  parallel.^ 

F  ;  R  ;  gbM;  40"  

F;  L;  R;  lb  M;  has  a  fine  double  ;)«  exactly  S  

p  F;  R;  vgb  M;  25"   

F ;  R ;  gbM;  20"  

O.  Planetary  Nebula,  with  a  H«  10  m  in  centre;  v  B;  very  well  de- 
fined, and  perfectly  equable  all  over  in  light,  there  being  no  condensation 
up  to  the  centre.  The  star  is  sharp  ;  the  nebula  velvety,  or  like  infinitely 
fine  dust ;  a  star  14  m  at  a  distance  rather  more  than  a  radius  of  neb  from 
edge  (by  diag);  has  its  position  from  centre  =  333°.8. 

Planetary  Nebula  ;  v  L ;  v  B ;  elliptic ;  has  in  it  a  s|«  9  m  somewhat 
excentric.  Its  light  is  exactly  equable,  i.  e.  not  increasing  towards  the 
middle;  yet  I  cannot  help  imagining  it  to  be  closely  dotted.  It  is  just 
like  a  star  out  of  focus  in  certain  states  of  the  mirror  and  atmosphere. 
Three  stars  near,  a  =  9' m;  b  =  9' m;  c  =  14  m.  A  very  extraordi- 
nary object. 

Well  seen,  as  described  in  f  554,  and  shown  to  Mr.  Maclear  and  another 
gentleman.  The  star  in  the  nebula  is  9  m,  very  sharp,  full,  and  distinct. 
Six  stars  9' m  in  the  field ;  one  companion  =  13  m. 

A  perfectly  well  defined  bright  elliptic  disc,  diam  in  R  A  =  4s.o ;  major 
axis  :  minor  :  :  5  :  4.  In  the  middle  is  a  sje  9  m,  which  is  quite  sharp, 
but  which  I  think  has  a  small  disc.  This  s|e  is  somewhat  excentrically 
placed.    See  PI.  VI.  fig.  9. 

B ;  R  ;  b  M ;  place  only  a  very  rude  approximation  

v  F ;  1  E  ;  25"   

p  B;  R;  gb  M;  40"   

p  B  ;  R ;  gbM;  40";  south  of  a  *  13  m   

F;vsbMtoaH«  16  m;  diam  1'  or  ij';  s  p  the  *  g  Sextantis,  which 
occasioned  its  being  taken  by  mistake  for  Halley's  comet,  and  the  conse- 
quent loss  of  that  comet. 

v  F ;  E ;  30";  has  a  H:  8'msp  

Looked  for  but  not  found  by  this.  However,  as  no  R  A  is  noted,  perhaps 
it  was  looked  for  too  late.  The  obs  of/ 5 35  is  positive,  and  correctly  re- 
duced. 

F  ;  IE;  v  1  b  M  ;  25";  has  a  *  15  m  in  it,  excentric  

e  F ;  S ;  R ;  precedes  2  B  st  (one  very  near  it)  

pB;  L;  mE;  gpmbM;  3'1   

B  ;  L ;  m  E  ;  g  v  1  b  M  ;  2'  1 ;  pos  50°-3  

pB;  pL;  gpmbM;  seen  through  haze   


535 
678 

549 
562 
771 
564 
687 


B  B 


94 


REDUCED  OBSERVATIONS  OF 


323S 


3239 


3240 


3*4-1 


3242 


3243 
3244 

3245 
3246 

3247 
3248 


3249 


Synon. 


A.  445 


A.  386 

IV.  10 

h.  710 


IV.  27 


R  A.  1830.0. 
h.  m.  s.  d. 


IO  10  38.0 
40.4 

10  10  38.4 


41.7 
42.9 
46.4 

10  10  41.9 

42.4 

10  n  4.2 


9.1 


IO   12  IX.O 


2O.5 


10  14  0.0 
10  14  7.4 
10  15  + 

10  15  53.5 

10  16  26.5 

28.9 

10  16  33.1 


33-7  = 

37-5 
38.0 

10  16  35.3 


N  P  D.  1830.0. 


J35  32  54 
33  24 

147    6  5 


4  3° 


115  51  20 


51  21 
170    1  46 


o  49 


151  49  56 


49  18 


123  23  59 
123  50  27 
140  52  ■+: 
71  59  1 

no  55  56 

55  5° 
107  46  55 


46  39 

46  48 
46  40 

121  36  25 


Description,  Remarks,  ice. 


(f)  ;  irreg  R;  gbM;  not  v  m  comp  ;  6';  res  into  st  13  15  m  

0  ;  irreg  R ;  7'  diam,  but  the  outliers  extend  to  at  least  10  or  12' ;  gpmbM, 
but  not  very  much  compressed ;  all  resolved  into  stars  13  ....  16  m. 

v  B ;  v  L ;  10'  1 ;  of  a  concave  or  crescent  form,  sharply  terminated 
inwards,  fading  away  outwards.  In  a  field  of  about  80  stars.  The 
place  is  that  of  a  He  13  m,  about  the  middle  of  the  crescent,  or  rather 
nearer  the  head.    (See  fig.  3,  PI.  IV.) 

p  B  ;  v  g  b  M  ;  of  a  falcated  or  semi-lunar  shape,  extending  over  f  of  the 
field.  The  place  is  that  of  a  double  star  in  its  vertex  or  southern 
extremity. 

Place  that  of  the  double  star  near  the  cusp  of  the  great  falcated  nebula, 
whose  extent  in  PD  is  =  1.3  rad  of  field  =  9'-75-  In  a  rich  field.  A 
clustering  group  follows. 

A  v  L  and  very  remarkable  nebula,  which  is  brighter  to  the  s  f  part,  and 
dies  off  to  the  n  p,  having  a  curved  form  and  forked  tail.  In  the  head  of 
it  is  a  double  star.  The  neb  is  p  B  ;  v  L  ;  fig.  irreg  ;  8'  1,  4'  br.  Among 
a  vast  number  of  milky  way  stars. 

pB;  S;  pmE;  bM;  25"  1.  This  obs  makes  the  minute  of  R  A  =  11, 
but/  562  makes  it  10,  which  is  preferred,  that  the  observation  may  not 
be  lost  in  future  by  looking  out  too  late. 

p  B  ;  E  ;  gbM;  25"  

Planetary  Nebula  ;  R,  or  v  1  E  ;  a  very  little  hazy  at  the  edges,  but 
still  pretty  well  defined  with  240.  Viewed  long  and  with  much  attention, 
being  a  very  remarkable  object.  I  am  positive  of  the  existence  of  two 
brighter  portions  near  the  edges.  (See  fig.  2,  PI.  VI.)  Companion  stars 
a  —  1 1  m,  pos  =  274°-7  ;  b  =  13  m,  pos  =  27 1°.5  ;  c  =  14  m,  204°.8. 
The  star  a  precedes  the  centre  14  sec,  which  is  also  the  diameter  in 
R  A  of  neb. 

O  !  P  B  ;  not  quite  uniform  in  its  light,  having  two  brighter  patches ;  1  E 
towards  a  ^  (a);  slightly  hazy  ;  diam  =  15  or  18"  (in  R  A  i3*.o  of 
time).  Pos  of  a  =  26517,  dist  =  0.7  diam  from  edge,  n  m;  of  c, 
pos  =  210.7,  dist  =  if  diam  from  edge.  [N.  B.  13'  in  time  —  33"-74 
in  arc] 

O  ;  Planetary  Nebula  ;  delicate,  exactly  round,  =  *  10  m  a  little 
dim  at  edges  ;  white  ;  with  320  considerably  hazy.  In  field  with  at  least 
150  stars. 

O  ;  perfectly  R ;  very  well  defined,  with  a  perfectly  uniform  light,  not  at 
all  mottled  ;  =  a  4c  10  m,  of  which  brightness  there  are  5  or  6  more  in 
the  field,  and  not  less  than  150  others  less  bright.  Examined  by  both 
Mr.  Maclear  and  myself  with  240,  which  shows  it  proportionally  magni- 
fied ;  quite  round  and  planetary ;  a  little  hazy  at  the  edges,  but  not  more 
so  than  is  due  to  the  decidedly  bad  definition  of  the  night,  and  the 
imperfect  figure  of  the  mirror,  which  has  been  injured  by  careless 
polishing  on  too  soft  a  polisher. 

pB;  vL;  vlE;  p  s  1  b  M,  to  a  centre ;  diam  2'   

vF;  R;  pgmbM;  40"   

A  group  of  9  L,  and  a  few  sc  small  stars   

A  star  9'  m,  affected  with  a  nebulosity,  chiefly  on  the  following  side. 
Imperfectly  seen  in  the  haze  of  a  S  E  drift. 

e  F ;  S  ;  R  ;  15"  ;  near  a  *  12  m  

e  F ;  S  ;  R ;  near  a  star   

Planetary  Nebula.    Viewed  past  merid  ;  place  from  Piazzis'  Catalogue. 

Somewhat  hazy,  with  a  slight  nebulous  atmosphere.    Colour  a  decided 

blue;  at  all  events  a  good  sky-blue.     Elliptic;  pos  of  axis  =  140°; 

diam  in  R  A  =  2\5.     Has  2  companion  stars  (a)  pos  =  i73°.o; 

(b)  pos  =  i37°.8. 

O  ;  of  a  decided  pale  blue  colour,  but  not  so  full  a  blue  as  the  planetary 
nebula  nh  42"'  1460  14' ;  oval ;  pos  of  the  longer  axis  =  135°  +  ;  3°'  1> 
25"  br;  uniform  and  v  B  ;  but  not  quite  sharp  at  the  edges. 

A  very  fine,  large  Planetary  Nebula,  25"  in  diam,  a  little  elliptic;  vB; 
uniform,  but  owing  to  a  hot  wind  too  ill  defined  for  detaUed  examination. 

O  ;  v  B  ;  decidedly  elliptic ;  a  little  dim  at  edges  ;  colour  very  decided 
pale  blue  ;  diam  in  R  A  =  35.o.  Pos  of  longer  axis  about  1 300 ;  pos  of 
the  nearer  of  two  companion  stars  =  172°.    (Plate  V.  fig.  5.) 

F  ;  p  m  E ;  g  1  b  M  ;  has  a^  nmnp   


NEBULiE  AND  CLUSTERS  OP  STARS. 


95 


Synon. 


325° 


3251 
3252 


3253 
3*54 

3255 
3256 

3257 


3*58 
3*59 


3260 
3261 
3262 

3263 


3264 

3265 
3266 


3267 
3268 


R  A.  1830.0. 
h.  m.  s.  d. 


10  18  32+ 


10  18  46.2 
10  19  + 
19  4.8 
6.2 
7.0 
9.0 

10  20  28.9 

10  20  35.3 
36.4 
10  21  7.2 

7-9 
12. 1 

10  21  12.9 
14.7 
18.6 
18.8 

10  21  26.4 
28.7 

3I.I 

32.0 
10  21  46.6 
10  21  48.7 

52.6 
10  21  51.6 
10  21  57.1 
10  22  13+ 

10  22  1 6— I— 

18+ 


10  22  20.1 


10  22  25.0 


10  23  11.9 
!S-3 

10  23  38.6 
10  24  6.0 

8.0 


N  P  D.  1830.0. 


146  61  30 

14-6  57  ± 
146  59  4 

124    5  32 
129    5  ± 
4  38 

4  20 

5  15 
4  24 

149  48  42 

133    1  43 

1  59 
124  47  32 

4-7  47 

46  ± 

124  43  47 

45  6 

43  0 

44  7 
124  43  7 

45  1 

42  40 

43  7 
133  47  3 
124  44  18 

45  o 

133  19  58 

>33  15  23 

124  29  + 

124  30  + 

30  + 


124  20  23 
21  37 

124  29  53 
32  + 

125  51  49 

52  33 

129  4  40 
129    4  16 

5  25 


Description,  Remarks,  &c. 


A  curious  object.    Stars  involved  in  evident  nebula, 
to  the  nearest  minute. 


R  A  only  observed 


A  decidedly  nebulous  group.  No  R  A,  and  P  D  very  rough,  being 
observed  5  or  6  fields  past  meridian. 

There  is  a  nebulous  appearance,  which  merits  re-examination.  Observed 
much  past  merid,  and  no  reliance  on  the  P  D. 

eF;  pLj  R;  vgvlbM;  60"   

pB;  R  ;  psbM;  30" j  has  a  *  1 3  m  n  f  

pB;  Rj  gpmbM;  25"  

p  B  ;  R  ;  g  b  M  ;  40".  Either  a  double  neb,  or  has  a  v  F  star  450  n  f . .  . . 
pB;  R;  gpmbM;  25"  

B ;  p  B  ;  R  or  v  1  E  ;  first  v  g,  then  p  s  b  M  ;  90"  or  2'  diam.  [N.B.— The 
nebula  has  evidently  been  seen  to  better  advantage  in  this  than  in  any  of 
the  foregoing  observations.] 

A  very  compressed  knot  or  cluster  of  milky  way  stars,  4'  in  diameter, 
somewhat  insulated  from  the  rest.    Stars  ...  15  m. 

p  B  ;  R  ;  S  ;  g  b  M  ;  20"   

B;R;gmbM;  25"  

e  F ;  v  S  ;  R.    The  first  of  a  group   

v  F ;  R  ;  psbM;  10"   

vF;  vS;  R;  sbM;  10".    The  preceding  of  a  group  

v  F ;  R ;  psbM;  12".    The  second  of  a  group  

F ;  S  ;  R ;  15"  

v  F ;  S  ;  R ;  s  b  M ;  12"  

F;  R;  pslbM   

e  F ;  IE;  1  b  M  ;  5".    The  third  of  a  group  

v  F ;  v  S  ;  R ;  near  a  star  12m  

e  F  ;  v  S  ;  R  ;  s  1  b  M  ;  6"  

v  F;  R;  p  sib  M   

F ;  S  ;  R ;  15";  entangled  among  2  or  3  st,  but  is  certainly  a  nebula  

F  ;  R  ;  p  s  1  b  M  ;  12".  The  4th  and  last  of  a  group.  (The  minute  by  this 
obs  is  22,  but  both  the  diagram  and  the  obs  of  f  541  prove  this  to  be  a 
mistake  for  21.) 

eF;  eS;  R;  lbM;  10".    The  4th  and  last  of  a  group   

eF;  S;  R  

F ;  m  E  in  pos  =  280°+  ;  psbM;  20"  

e  F  ;  v  S  ;  R.  By  a  diagram  made  out  of  meridian  in  which  4  nebulae  are 
delineated,  two  of  them  being  those  determined  in  f  446  Nos.  6  and  7. 

F  ;  S  ;  R.  By  diagram,  &c,  as  in  the  case  of  the  nebula  immediately  pre- 
ceding, to  which  this  is  contiguous. 

Place  concluded  from  those  of  the  nebula,  Nos.  6  and  7  of f  ^4&,  by  the  aid 
of  a  diagram  made  out  of  meridian,  in  which  also  4  nebulae  were  seen,  but 
of  which  only  3  are  identifiable  with  those  of  f  571 ;  the  small  nebula 
contiguous  to  and  preceding  this,  not  having  been  seen  owing  to  haze,  and 
a  5th  more  remote  and  brighter,  being  now  for  the  first  time  laid  down. 

F;  S  ;  R ;  b  M ;  15";  one  of  a  group  of  3  or  more  

F;  R;  20"  

Observed  also  in y  571  and  572  ;  which  see  above  

F ;  S ;  1  E  ;  b  M  ;  15";  one  of  a  group  of  3  or  more   

p  B  ;  p  m  E  ;  p  m  b  M,  as  per  diagram,  &c,  taken  out  of  meridian.  See 
Remarks  on  the  4  nebulae  immediately  preceding.    Seen  also  in  f  571. 

F;  IE;  psbM;  20"  

F;  L;  R;  pslbM;  60"  

Seen  past  merid ;  too  late  for  place  or  description  

F;  S;  has  a  H«  8  m,  n  p  

F  ;  S  ;  R  ;  spa  coarse  double  star  

F  ;  R ;  has  a  double  star  n  f  


Sweep. 


435 
784 
436 

54i 

540 

574 
555 
573 
810 

543 

686 
542 

54i 
448 

447 
448 

54i 
447 
572 
448 
54i 
447 
572 
686 
448 

54i 
542 

542 
57i 

57i 

572 


446 

572 

446 

572 

540 
574 
573 
555 
554 
555 


96 


REDUCED  OBSERVATIONS  OF 


No. 


3269 
3270 


Synon. 


III.  55 
h.  727 


A.  322 
A-  355 


R  A.  1830.0. 
h.  m.   s.  d. 


10  24  13.0 
10  25  33.6 

37.1 
38.6 
39.2 

10  25  35+ 
10  26  26.0 
10  27  35.1 

10  27  57.6 
10  27  59.9 
10  27  + 
10  28  14.0 
10  28  16.9 


10  28  22.9 
23.5 


N  P  D.  1880.0. 


24.6 
24.6 


123  58  52 
116  34  37 

35  26 

34  28 

35  20 
135  22  50 

124  25  17 
74  57  2 

121  57  48 
121  29  25 
147  19  - 
116  17  1 
116  43  22 


116  33  52 

32  28 

33  25 

34  31 


10  28  36.6     116  38  38 


V.7 


36.7 
35± 

10  28  45+ 

10  29  3.3 

5.2 

10  29  15.4 
10  29  33.4 
36.0 
36.5 


10  29  45.1 
48.8 
10  30  54.6 

10  31  49.3 
10  32  4.4 
10  32  18.9 
10  34  34.8 


39  0 
37:  31 

116  40  + 

1 16  44  25 


116  47  31 
116  42  47 

43  « 

44  3° 


130  45  o 

45  15 
147  44  30 

143  14  45 

125  9  56 

116  52  21 

74  r3  49 


Description,  Remarks,  &c. 


e  F;  E;  gib  M;  60"  1;  40"  br  

p  F.    The  first  of  a  group  scattered  over  more  than  one  field  

pB;  E;  gbM   

p  B ;  R  ;  gbM;  40"  

p  F;  S ;  R;  gbM;  15"   

p  F  ;  S  ;  R ;  gbM;  25",    R  A  coarsely  taken  by  an  auxiliary  star  

eF;  R;  15"  

pFj  S;  R  ;  g  p  m  b  M   

eF;  S;  R  

vF;  S;  R;  15"  

A  fine,  bright,  rich,  not  very  L  cluster.    (Equatorial  zone  review)  

v  F  ;  S  ;  R.    The  2nd  of  a  group  scattered  over  more  than  one  field  

e  e  F.  The  3rd  of  a  group.  [P  D  by  MS  38';  but  there  in  some  confusion 
in  the  entry,  the  figures  being  roughly  written  over,  and  no  doubt  being 
left  by  the  diagrams  that  the  most  visible  writing  is  5'  wrong,  and  that 
43  is  the  true  minute.'] 

The  4th  of  a  group  

One  of  a  group  ;  7  of  which  were  seen  and  laid  down  in  a  careful  diagram 
for  identification. 

F;  S;  R   

F  

A  double  nebula,  or  rather  two  distinct  nebulae  near  together.  By  diag,  both 
p  L,  R  pos  about  io°  n  p  or  s  f,  and  nearly  equal.  It  is  not  stated  which 
was  taken.    Presumed  to  have  been  the  preceding. 

The  preceding  neb  of  a  double  neb  ;  2  or  3  stars  also  near   

B  ;  L ;  double  ;  a  hurried  obs,  R  A  taken  only  to  the  nearest  minute,  and  a 
mistake  (rectified  in  the  reduction)  of  10'  committed  in  the  P  D. 

The  following  neb  of  a  double  one.  Place  deduced  from  that  of  the  preced- 
ing one  by  a  measurement  of  the  diagram. 

v  F  ;  p  m  E  ;  the  last  of  4  in  the  field  at  once  with  two  stars  6  m  near  them, 
one  above  and  one  below  them  (which  serves  to  identify  the  object  beyond 
doubt),  P  D  only  correct  to  the  nearest  minute. 

F ;  E  ;  g  b  M.  No  P  D  taken,  a  hurried  observation,  and  the  wire  mis- 
taken (rectified  in  reduction).  This  nebula  is  the  7th  of  the  group  in  fact, 
though  in  this  observation  called  the  "  5th  or  6th." 

The  8th  of  a  group  

p  F ;  S ;  R ;  b  M.    The  last  of  a  group  of  9  neb  

v  F ;  R.  [N.B. — This  numerous  and  very  interesting  group  has  been  made 
out  by  a  careful  collation  of  diagrams  made  in  f  564  and  689,  for  the 
purpose  of  identification,  from  which  it  appears  that  though  in  each  dia- 
gram only  7  were  seen  and  laid  down,  yet  there  are  in  reality  at  least  9 
in  the  whole  group.  Several  mistakes  of  reading  appear  to  have  been 
committed  in  the  hurry  of  observation  unavoidable  in  attempting  to  de- 
termine at  once  so  many  objects;  but,  on  the  whole,  the  group  appears 
to  be  satisfactorily  made  out.] 

F;  R;  glbM;  60"  

vF;  pL;  pmE;  gvlbM;  2'  

A  double  star  involved  in  nebula,  which  is  one  of  the  outliers  of  the  great 
nebula  about  n  Argus.  It  extends  to  a  ^  6.7  m  half  a  field  distant  south- 
wards, and  almost  as  far  north ;  p  B  ;  irreg  fig ;  fine  object. 

The  chief  s|c  (9  m)  of  a  poor  cluster  of  20  or  30  stars   

e  F  ;  v  S  ;  m  E  ;  appended  like  a  tail  to  a  :)<  15m  

vF;  pL;  IE;  glbM  

vF;  L;  R;vgvlbM;  3' or  4'  diam.  A  soft  globe  of  light,  resolvable 
with  the  left  eye. 


Sweep. 

447 
689 
562 
564 
563 
776 
572 
688 

678 
535 


NEBULAE  AND  CLUSTERS  OF  STARS. 


97 


No. 


Synon. 


R  A.  1830.0. 
h.   m.  s.d. 


NPD.  18S0.0. 


Description,  Remarks,  &c. 


Sweep. 


3*9! 

3292 

3293 
3294 
3295 

3296 


3297 

3298 
3299 


3300 
3301 

3302 

33°3 
3304 
3305 
3306 
3307 
3308 
3309 

3310 

3311 

3312 
33'3 
33H 


A.  309 


II.  100 
h.  804 


io  34  59-6 
61.3 
61.9 

64.3 
10  35  17.3 
17.9 
19.2 
23.4 
10  35  48.7 
50.7 
10  37  44.8 

10  38  24.8 
28.7 
28.8 

10  38  51+ 
59.8 
60.2 
73.8 


10  54  19. 1 

10  54  20.9 
10  55  21.5 
10  57  5.9 


125  28  11 

28  46 

27  7:: 

28  14 
125  28  21 

31  10 

28  59 

27  7:: 

125  28  45 

30  27 

132  49  18 

148  46  57 

47  4° 

47  21 J 

129    8  ± 

7  26 

8  18 

7  S 


10 

39  12.2 

113  32  11 

14.4 

32  10 

10 

40  8.3 

120  39  17 

10 

40  14.0 

114  16  40 

15.8 

15  31 

17-3 

16  22 

10 

44  =3-5 

72  19  59 

10 

44  32-8 

«34  '5  31 

44.6 

14  8 

10 

44  55-9 

122    1  27 

10 

44  58-i 

109  56  43 

10 

45  24-9 

110  52  41 

10 

47  3-i 

115  14  25 

10 

48  29.6 

103  23  47 

10 

50  51.6 

117  34  12 

10 

50  56.0 

135  39  46 

10 

51  1.9 

74  !5  2 

10 

52  58.7 

149  25  9 

148  56  10 

«°4  34  47 
107  52  2 
150  26  58 


Not  v  F  ;  R;  s  1  b  M  ;  15".    The  first  of  3   

B  ;  m  E  ;  a  nucleus  with  v  F  arms  nearly  in  merid   

p  F;  R   

pF;  S;  R;  v  s  m  b  M  to  a  H4  12m  

v  F ;  S  ;  1  b  M  ;  8".    The  2nd  of  3  

pB;  pL;  R;  psbM;  40"  

vF;  S;1E   

e  F;  R   

F  ;  v  S  ;  R ;  close  to  a  v  S  star ;  the  last  of  3   

v  F  ;  IE;  the  3rd  of  a  group  

F  ;  E  ;  g  b  M  ;  close  to  a  *  6.7  m.  The  minute  of  R  A  doubtful.  The 
written  record  makes  it  47  ;  but  as  this  is  impossible  from  the  context, 
37  is  assumed. 

The  s)«  n  Argus,  with  the  Great  Nebula  about  it,  of  which  see  the  mono- 
graph and  detailed  description. 

p  B  ;  R  ;  b  M.    Out  of  limit  of /.    Place  rough  

F ;  R ;  glbM;  30*   

vF;  S;  R;  gib  M;  15"   

v  F  ;  R  ;  glbM;  25".  [No  doubt  of  a  mistake  of  10  seconds  in  reading 
the  chronometer.'] 

F;  p  L;  R;  lb  M;  50"  

F  ;  p  L  ;  irreg  R  ;  glbM;  40" ;  C  

p  F  ;  S  ;  p  m  E  in  meridian  

F;  R;bM;  20"  

F ;  S ;  R.    Precedes  two  bright  stars  

p  F  ;  R ;  p  s  b  M.    Has  2  stars  10  and  1 1  m,  following  

e  F  ;  v  L  ;  v  g  v  1  b  M  ;  3'  or  4'  diam.  Has  a  bright  coarse  double  star 
(9  m)  s  P- 

The  chief  (9  m)  of  a  cluster  class  VIII.,  7'  diam  ;  not  rich  or  comp. 
Stars  10 ....  13  m. 

A  cluster  VIII.  class  ;  not  rich ;  irreg  fig  ;  7' j  st  9  .  .  .  13  m  

F  ;  S  ;  R ;  15".    Has  a  *  6.7  m  s  f  

vF;  L;  R;  vglbM;  r;  90"  

F;  S;  R  ;  b  M  ;  15"   

F;  R;  glbM;  20*   

e  e  F;  S  

p  F ;  S  ;  R  ;  b  M  ;  15".    Among  stars  

e  F ;  S  ;  R ;  gbM;  30"  

F;  L;  R;  gbM;  2J'  diam.  Has  a  *  11  m  6'  south,  and  a  little 
preceding. 

Place  of  a  small  double  star  in  the  following  part  of  a  loose,  rich,  pretty 
large  cluster  of  stars  13  m,  8'  or  10'  diameter ;  a  fine  object;  a  very  much 
condensed  milky  way  group. 

Three  very  close  stars,  10  m,  in  a  nearly  straight  line,  and  a  double  star 
north  of  them,  the  whole  involved  in  very  faint  nebula,  so  faint  as  to 
leave  some  doubt. 

pF;  S;  R;  glbM.    Has  a  star  14  m  near  

vF;  pL;  R;  vgvlbM  

Chief  star  of  a  pretty  rich  cluster,  class  VII  


448 

54i 
572 
446 
448 

54i 

446 
572 

541 

572 
686 

432 
435 
543 
540 
810 
574 
573 

559 
558 
444 
563 
562 


774 

686 

444 

560 

559 

563 
700 
452 

553 
688 

432 
435 

700 
560 
432 


C  C 


98 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R  A.  1830.0. 
h.  in.    s. d. 


3315 


A-  323 


3316 

3317 
3318 

3319 
3320 


3321 

3322 

3323 
3324 

3325 
3326 

3327 

3328 

3329 
3330 


III.  824 


333 1 

3332 
3333 


II.  269 


III.  529 


10  58  10.5 

59  16.8 
59  i9-° 


XPD.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 


10  58  48.7 
IO  58  51.2 

10  59  20.7 

11  I  54.5 

55-3 
11    2  31.3 
31.7 


11    2  36-r- 

44.6 
11    3  14.6 

11  3  16.5 
11    4  36.8 

11    4  38.4 
42.4 
11    4  454 

49.4 

11    4  57.9 

59.2 
11    4  59.9 

60.9 

11    5  3.2 

7.2 

11    5  14.2 
15.4 


11    5  34-5 


11  5  42.7 
11    6  20.7 


147  49  26 

45  18 
45  2° 


108  33  22 
108  37  37 
126  15  18 
126  37  33 

36  35 
126  37  23 

36  35 


126  32  33 

32  20 
i^5  55  47 

149  19  8 

150  27  12 

150  18  30 
18  7 

150  23  25 
23  2 

150  20  52 

20  46 
115  50  20 

49  52 
150  17  10 

16  44 
150  25  18 

26  IO 


IO3    IO  2 


149  52  33 
112  47  56 


A  glorious  cluster  of  immense  magnitude,  being  at  least  2  fields  in  extent 
everyway.  The  stars  are  8,  9,  10,  and  11  mag,  but  chiefly  10  m,  of 
which  there  must  be  at  least  200.  It  is  the  most  brilliant  object  of  the 
kind  I  have  ever  seen. 

Chief  *  of  a  v  L,  R,  loosely  sc  cl  of  st  8 . . . .  12  m,  which  fills  2  or  3  fields. 
A  fine  bright  object. 

The  chief  star  of  a  superb  cluster,  which  has  several  elegant  double  stars, 
and  many  orange-coloured  ones.  [N.B. — The  observations  are  correctly 
reduced,  but  owing  to  the  very  great  extent  of  the  cluster,  there  is  no 
reason  to  suppose  any  error  in  the  observation  of  f  543,  which  (as  no 
particular  star  is  mentioned)  belongs  probably  to  the  general  middle 
of  the  whole.] 

Viewed  with  Mr.  Maclear,  Feb.  26,  1835   

F ;  S;  R;  pslbM;  20".    The  preceding  of  2  

e  F  ;  S ;  R ;  vlbM;  15".    The  following  of  2  

e  e  F  ;  attached  to  a  v  S  star   

v  B  ;  R ;  p  g  m  b  M  ;  30".    The  first  of  a  group  of  3  

pB;  S;  R;  b  M  

p  B  ;  S  ;  R.    The  second  of  3  

F;  S;  R;  b  M.  On  the  same  parallel  with  No.  3319.  [N.B.— The 
chronometer  reading,  as  set  down  in  the  sweeping  book,  would  make  the 
minute  of  R  A  3,  instead  of  2  ;  but  the  context  of  the  immediately 
subsequent  observation  proves  this  reading  to  have  been  impossible,  and 
unquestionably  one  minute  too  late.] 

F  ;  R ;  near  3  bright  stars.  R  A  concluded  roughly,  from  an  estimated 
A  R  A,  with  574,  No.  12. 

e  F  ;  p  L  ;  involving  several  stars.    The  last  of  3  

e  F  ;  R ;  g  1  b  M  ;  20" ;  precedes  3  st  1 1  and  12  m,  nearly  on  the  same 
parallel. 

Middle  of  a  tolerably  rich  cluster,  class  VIII  

F  ;  oval.  The  first  of  a  group  of  6.  Place  by  collation  of  diagrams. 
PI.  IV.  fig.  10. 

F;  oval.    The  2nd  of  6.    Place  by  collation  of  diagrams   

R,  s  b  M,  by  diagram.    Place  by  collation,  &c.    PI.  IV.  fig.  10   

Fanshaped,  adhering  to  a  star.    The  3rd  of  6.    Place  by  direct  observation. 
A  *  12  m,  with  a  fan  nebula  attached.    Place  by  direct  obs.    PI.  IV. 
fig.  10. 

A  *  1 1  m  in  centre  of  a  round  nebula.  (The  4th  of  6.)  Place  by  direct 
observation. 

R  ;  has  a  *  in  middle.    Place  by  collation  of  diagrams.    PI.  IV.  fig.  10  . . 
v  B  ;  p  L  ;  p  m  E  ,  forms  equilateral  triangle  with  two  stars  8  and  8.9  m 
following,  distant  6'  or  7'. 

vB;  pL;   E;  vsvmbM 
PI.  IV.  fig.  10. 

by  collation  of  diagram.    The  5th  of  a 


60"  broad. 
F  ;  L  ;  oval ;  b  M 


has  an  elongated  nucleus ;  90"  long, 


group  of  6.  PI 
L,  b  M,  E  in  merid 


Place,  &c. 
IV.  fig.  10. 


Place,  &C.j  by  collation  of  diagram   

Place  by  collation  of  diagrams  ;  the  last 


S,  oval,  E  in  pos  160  +  by  diag, 
of  a  group  of  6.    PI.  IV.  fig.  10. 

eF;  oval.  Place  by  direct  observation.  [N.B. — This  close  and  very 
remarkable  group  not  admitting  direct  observation  of  all  the  individuals 
in  two  sweeps,  their  places  have  been  made  out  by  a  very  careful 
collation  and  independent  measurement  of  two  diagrams  made  in  sweeps 
432,  433,  for  that  express  purpose.  In  the  first  obs  only  5  were  noticed. 
In  the  other  a  6th  was  seen  and  laid  down.    See  fig.  10,  PI.  IV.] 

v  F  ;  R  ;  30" ;  v  1  b  M.  [N.B.— The  MS.  makes  the  degree  of  P  D  102  ; 
but  the  nebula  having  been  looked  for  and  found  by  the  working  list  as 
III.  529,  103  is  doubtless  the  correct  degree.] 

A  close,  p  rich,  comp,  oval  cluster  somewhat  insulated  

v  F  ;  R  ;  b  M  ;  much  diluted  at  the  borders  ;  30"   


NEBULA  AND  CLUSTERS  OF  STARS. 


99 


No. 


Synon. 


3334 


3335 
3336 

3337 

3338 

3339 
3340 


334i 
3342 

3343 

3344 
3345 

3346 

3347 
3348 


3349 
3350 

3351 
3352 

3353 
3354 

3355 

3356 

3357 
3358 


I.  241 
A.  617 


III.  530 
III.  531 


A.  481 


II.  159 
h.  891 

III.  532 


R  A.  1830.0. 
h.    m.  s.d. 


II.  562 


III.  935 


A.  zi 


h.  934 


II.  103 
h.  936 


11    7  50.3 


11  8  3.3 
11  9  31.3 
11  10  2.6 

11  10  21.6 
11  15  6.6 
»  IS  37-3 

45.4: 
11  16  51.7 

11  17  28.9 
32.9 

11  17  38.8 

11  19  38.3 
11  20  12.3 

11  21  25.1 
26.3 
27.4 

11  22  57.8 
58.9 

11  23  7.2 
8.6 


11  26  6.3 
11  27  8.4 
9-5 

11  27  30.5 
31.9 
11  27  53.6 

28  44.5 

11  30  7.6 
11  30  38.1 
38.3 
11  31  20.3 

11  31  23.8 

11  33  38.2 

11  37  49.2 


NPD.  1830.0. 


150  19  52 


122  54  7 
115    12  7 

121  52  57 

165  17  29 
102  53  40 
102  54  22 

54  55 
115  43  37 

132  18  o 
17  56 

72  11  40 

102  15  2 
149    1  10 

125  27  36 
26  56 
28  9 

103  17  52 
17  37 

119  15  32 
22  47 


103    9  12 
127     I  o 
o  18 

127      2  55 
2  43 
150   38  38 

40  28 

!39  45  54 
126  47  53 

47  45 
73  43  33 

73  42  33 

:o2  54  37 

145  25  48 


Description,  Remarks,  &c. 


Sweep. 


A  red  star  10  m,  the  centre  of  an  excessively  condensed  group  of  stars 
15  ....  18  m,  with  a  nebulosity  extending  over  2'  diameter. 

Viewed  the  neb  of  f  432,  No.  ax,  which  is  a  very  remarkable  object.  The 
centre,  when  examined  with  powers  240  and  320,  decidedly  not  a  star, 
and  the  nebula  about  it  all  resolved.  Perhaps  it  is  a  globular  cluster 
v  s  v  v  m  b  M. 

e  F;  R;  S;  gb  M;  15"  

F  ;  S  ;  R ;  g  b  M  ;  20"   

pBj  v  L  ;  oval ;  v  g  v  1  b  M  ;  r  ;  5'  1,  3'  br   

F  ;  p  m  E  ;  g  b  M  ;  50"  

F  ;  S  ;  R ;  g  b  M.    The  preceding  of  2  

p  F  ;  R  ;  20"  ;  has  3  st  10  m  near  it,  with  the  two  following  of  which  it 
makes  an  equilateral  triangle. 

pB;  IE;  psbM;  20" ;  the  following  of  2.    The  R  A  awkwardly  taken. 

F;  vL;  vglbM.  Several  S  stars  near,  and  one  =  7  m  nearly  south, 
at  6'  distance. 

Cluster  VIII.  class  ;  60  or  70  st  11 ....  13  m  in  a  comp  R  space,  10'  diam 

Not  very  rich,  but  a  good  cluster  ;  g  comp  M  ;  L  ;  R ;  very  sc  ;  almost 
fills  field ;  st  10  .  .  .  14  m. 

pB;  R;  pgmbM  

F ;  p  m  E  in  parallel  ;  g  p  m  b  M  ;  20"  

B  ;  p  L  ;  irr  R  ;  p  g  p  m  b  M  ;  90"  ;  r.  Almost  resolved.  It  is,  how- 
ever, by  no  means  a  mere  knot  of  the  milky  way. 

p  B ;  R ;  p  s  b  M  ;  15"   

B  ;  R  ;  p  s  m  b  M  ;  60"  

p  B  ;  R  ;  p  s  b  M  ;  20"  

pF;  S;  R;  vglbM;  15"  

p  B  ;  S;  R;  g  b  M  ;  15"   

p  F  ;  S  ;  m  E  ;  attached  like  a  wisp  to  a  H<  13  m  

p  B;  S;  m  E;  attached  to  a  [N.B.— The  observations  disagree 

much  in  P  D,  but  it  seems  probable  that  a  part  at  least  of  the  dis- 
cordance arises  from  the  star  having  been  taken  in  one  observation  and 
the  nebula  in  the  other.  Still  an  error  of  5'  in  one  or  other  reading 
must  have  been  committed.'] 

e  e  F  ;  R  ;  g  b  M  ;  difficult,  but  a  good  obs  

pB;  pL;  R;  glbM;  40"   

F;  IE;  gbM  

p  B ;  IE;  glbM;  40"  

v  F;  E  ;  g  v  1  b  M  

The  preceding  of  two  chief  stars  of  a  fine,  large,  loose,  R  cl  of  st  8  12  m; 

g  p  m  b  M  ;  fills  field ;  150  200  stars. 

A  very  fine  cl  class  VII.;  nearly  R;  8'  diam  ;  1  comp  M  stars  9  ....  15  m  ; 
place  that  of  an  orange  star  9.10  m  following  M. 

e  F  ;  R ;  20";  in  a  field  with  50  or  60  small  stars  

p  B  ;  R ;  v  s  b  M,  almost  to  a  star.    It  is  n  p  a  *  9  m  

B  ;  R ;  p  s  b  M  ;  precedes  (to  n)  a  He  9  m   

e  F  ;  R  ;  adjoining  to,  or  in  the  prolongation  of,  No.  4i,/688.  This  ob- 
servation sets  at  rest  the  doubt  in  my  former  catalogue,  and  shows  the 
erroneous  observation  to  have  been  that  of/419. 

v  F ;  IE;  gbM;  has  another  R  neb  at  its  extremity.  See  fig.  79  in  my 
Northern  Catalogue.  See  also  the  remark  above  (on  h  934)  as  to  the 
erroneous  R  A  of /419  in  that  catalogue. 

F;  IE;  pslbM;  40".  [N.B. — It  is  just  possible  that  by  a  double 
mistake  of  i™  in  R  A,  and  1°  in  P  D,  this  nebula  may  be  h  957.  Both 
observations  are  correctly  reduced.] 

v  F ;  IE;  has  two  stars  in  it   


432 
433 

572 
689 
444 

782 
687 
700 

687 


542 
774 


700 
435 

448 

54i 
446 
700 
687 
445 
444 


700 
573 
574 
573 
574 
43* 

434 

566 
574 
573 
688 


700 


437 


100 


REDUCED  OBSERVATIONS  OF 


No. 

3359 
3360 
3361 
3362 

3363 
3364 

3365 


Synon. 


3366 

3367 
3368 

3369 
337° 

337i 

337^ 
3373 
337+ 
3375 
3376 


III.  828 

I.  120 
h.  979 

II.  553 
h.  081 


II.  864 


I.  259 

III.  290 

A.  349 

I.  67 

II.  296 

III.  279 

III.  754 


It  A.  1830.0. 
h.  m.    s.  d. 


N  P  D.  1830.0. 


II  38  14.5 
15.0 
II  38  24.2 

II   39  21.5 

II  40  30.0 
33.I 
II  40  38.6 

11  41  5-3 


11  41  54.8 


55.8 
56.1 


56.9 
59.0:: 


11  42  26.6 
27-3 

11  43  44.8 

11  45  25.3 

11  46  + 

1 1  46  0.2 
1.2 

11  50  51.3 

11  52  18.6 

11  54  28.4 

11  55  33  5 

11  56  52.3 

11  57  12.0 


116  58  52 
58  16 
105  54  52 

100    o  21 

126  34  20 

34  23 
118  22  27 
137  19  23 


146  14  8 

14  19 
14  9 


H  3 
14  2 


117  54  42 
5i  27 

115  57  21 
109  37  29 
144  46  21 

103    1  28 
1  32 
108  19  24 

105  o  12 
152  14  12 
156  21  31 

"5  34  42 
103  35  27 


Description,  Remarks,  Ike. 


pB;  IE;  psbM   

PB;  S   

pB;  L ;  R;  vgpmbM;  r  (?)  j  90"  

p  B ;  R ;  pL;  45";  1"  g ;  then  psbM  

pF;  R;  or  IE;  gvlbM;  among  stars  

pB;  R;  orvlE;  vglbM;  35"   

pB;  R;  psmbM;  15"   

Place  of  a  D  sfc  in  a  v  L ;  not  v  comp  cl ;  class  VII.,  well  denned  and  in- 
sulated;  has  about  50  or  60  st  9....  12  m,  with  a  few  13....  14,  all 
loosely  sc ;  little  or  no  compression  in  M  ;  more  than  fills  field. 

A  fine,  large,  but  coarse  cl  class  VII. ;  stars  9,  10,  11  m;  two  double  stars 
are  in  it. 

Planetary  Nebula.  Perfectly  round  ;  very  planetary;  colour  fine  blue  ; 
a  very  little  ill  denned  at  the  edges ;  has  no  "  satellite  stars;"  very  like 
Uranus,  only  about  half  as  large  again  and  blue.    Diam  in  R  A  =  is-5. 

O  ;  diameter  8 . .  .  .  10";  perfectly  round  and  well  denned,  and  of  a  fine  blue 
colour. 

O;  a  perfect  planetary  disc  6"  diam;  quite  sharp,  with  not  the  least  hazi- 
ness. It  is  of  a  most  decided  independent  blue  colour  when  in  the  field 
by  itself,  and  with  no  lamp  light  and  no  bright  •)(..  About  10'  north  of  it 
is  an  orange  coloured  ^  8  m.  When  this  is  brought  into  view  the  blue 
colour  of  the  O  becomes  intense.  Shown  to  my  attendant,  John  Stone, 
who,  on  being  asked  what  colour,  said  at  once  "  blue." 

O  =  in  light  to  a  *  7  m  ;  diam  in  R  A  =  is.3  ;  viewed  with  all  the 
powers ;  very  beautiful ;  decidedly  blue. 

O  ;  colour  a  beautiful  rich  blue,  between  prussian  blue  and  verditter  green. 
The  light  is  fully  =  that  of  a  8  m  diameter  ;  2'.o  in  R  A ;  12*  by  care- 
ful estimation.  When  kept  steadily  at  rest  its  outline  is  sharp  and  clean, 
and  perhaps  a  very  little  elliptic.  A  feeble  lamp  light  gives  it  a  deep  in- 
digo contrasted  colour.  Do.  if  a  red  star  n  p.  about  10'  dist,  be  brought 
into  the  field  with  it.  My  attendant  saw  it  and  declared  propria  motu 
that  the  light  has  quite  a  green  cast  in  it.  About  90  stars  are  in  the  field, 
none  above  11  .  12  m,  and  only  one  of  that  magnitude  (meaning  when  the 
neb  is  central).  It  has  none  but  stars  16  m  near  it.  (R  A  possibly  not 
good  being  beyond  the  f). 

Feb.  26,  1835.  Viewed  with  Mr.  Maclear  after  f  551,  the  blue  planetary 
nebula.  Blue  colour  very  conspicuous.  Has  one  small  companion  cer- 
tain [pos  by  diagram  about  2900]  dist  =  a  full  diameter,  another  nearly 
certain  [at  about  half  the  distance  by  diagram,  and  pos  about  135°].  The 
field  is  full  of  stars.  Total  light  of  O  =  a  ~¥  6  or  6'  in.  A  very  little 
oval  in  pos,  about  1600  or  1650. 

p  B  ;  E  ;  m  b  M  ;  v  r  ;  20";  has  a  v  s  %  s  p  involved  

B;  pL;  IE;  glbM;  80"  1 ;  50"  br  ;  r ;  both  polar  distances  are  rightly 
reduced ;  one  may  have  been  5'  misread. 

v  F;  v  m  E  ;  2'  1;  15"  br;  pos  of  extension  =  59°-3  

F;  pL;  mE;  glbM;  60";  pos  236°.8  

Cluster  VI  class ;  p  rich ;  irreg  fig ;  R,  with  long  appendages,  g  p  m  b  M  ; 
9';  stars  13  m. 

vB;  R;  psmbM;  40";  forms  a  triangle  with  2  st  10.11  m   

B;  S;  R;  vgbM;  20'  

0;  F;  p  L;  R;  2';  resolved;  stars  barely  seen;  but  in  a  better  night  for 
definition  would  no  doubt  be  clearly  resolved  into  st  16  m. 

e  e  F ;  p  L ;  R ;  has  a  sjc  9  m  0.9  rad  of  field  dist ;  450  :t  n  f   

Cluster  VII  class  ;  loose  and  scattered,  but  pretty  rich  

v  F ;  R ;  40" ;  has  a  v  S  H=  in  centre ;  in  a  field  of  at  least  80  or  90  stars  .  . 

pB;  R;  gbM  

e  F ;  L  ;  p  m  E  ;  v  g  b  M.  The  direction  of  elongation  points  between 
two  stars  1 1  m  ;  very  near,  and  n  f  the  centre. 


Sweep. 


562 

700 

591 

573 
574 
452 
776 

553 
784 


NEBULA  AND  CLUSTERS  OF  STARS.  101 


No. 


3377 


3378 

3379 
3380 


3381 
3382 
3383 
3384 
3385 


3386 

3387 
3388 

3389 


3390 


3391 
3392 
3393 
3394 

3395 
3396 

3397 

3398 
3399 

3400 
3401 
3402 
34°3 


Synon. 


A.  291 


IL  865 

II.  866 

III.  533 
III.  534 


A.  292 


A.  67  ?  ? 


A.  300 


III.  764 


II.  771 


R  A.  1830.0. 


h. 

m. 

s.d. 

1 1 

57 

54.2 

150 

18  10 

56.2 

17  48 

56.8 

17  48 

57 

118 

5i  42 

57.6 

49  8 

11 

58 

1.8 

118 

52  2 

2.6 

49  18 

1 1 

58 

22.9 

129 

15  '7 

24.0 

15  18 

1 1 

58 

28.7 

103 

14  22 

12 

0 

9.0 

98 

5  11 

12 

3 

58-5 

103 

4  37 

12 

4 

39.8 

151  46  11 

12 

7 

30.7 

132 

22  33 

325 

22  36 

34.1 

23  0 

36.6 

22  45 

12 

8 

6.2 

144 

21  20 

'3 

17.8 

122 

31  54 

'+ 

46.4 

147 

10  30 

12 

58.5 

150 

55  38 

15 

16.3 

57  56 

15 

19. 1 

58  0 

12 

16 

LA. 

161 

43  ao 

8  n 
o.u 

42  32 

12 

16 

2I.O 

128 

48  13 

12 

J9 

6.S 

149 

9  8 

12 

*9 

31.8 

132 

19  8 

12 

20 

8.8 

119 

9  43 

12 

20 

22.7 

153 

5i  3 

12 

20 

26.7 

112 

13  25 

29.7 

14  0 

12 

23 

3-3 

129 

1  59 

23 

5-4 

2  43 

12 

23 

31.4 

96  36  43 

12 

26 

33.6 

128 

58  13 

34-3 

58  4 

12 

27 

0.6 

128 

29  53 

12 

28 

29.4 

132 

41  18 

12 

28 

41.6 

124 

34  7 

12 

28 

42.7 

129 

36  3 

NPD.  1830.0. 


Description,  Remarks,  &c. 


A  4=  10  m  in  centre  of  a  pretty  rich  close  cluster ;  5'  diam  ;  irreg  R ;  stars 
10.  ...13m. 

Middle  of  a  rich,  p  L,  irreg  R  cluster;  poor  VI.  or  rich  VII.  class  stars 
10. ...  14 ;  diam  5',  with  stragglers. 

Cluster  class  VII ;  pretty  rich  and  compact;  stars  10. ...  12  m,  and  nearly 
=  ;  diameter  5';  the  whole  field  is  in  a  state  of  wavy  fluctuation,  owing 
to  the  S  E  wind,  and  so  bad  that  each  star  is  dilated  into  a  large  puff  ball. 

The  first  of  a  double  nebula  (pos  11 1°.2,  by  mean  of  2  meas)  B ;  R ;  p  L  ; 
p  s  b  M  ;  r ;  25".    A  R  A  of  this  neb,  and  a  He  S  of  it,  =  2\o. 

p  F ;  R ;  g  b  M  ;  30";  r.    The  1st  of  a  double  neb,  pos  =  120.3  

The  2nd  of  a  double  neb  B;  R;  pL;  psbM;  r;  25"  

F ;  R  ;  g  b  M  ;  20";  r ;  the  2nd  of  a  double  neb  

F  ;  IE;  g  1  b  M  ;  under  a  curve  of  3  B  stars   

F ;  S ;  R ;  at  the  end  (or  forming  the  continuation  of  an  arc  of  3  stars  re- 
spectively, in  order  8,  9,  and  10  m.) 

F;  S;  R;  gb  M;  15"   

F;  vglbM;  pmEin  parallel ;  25"   

vF;  pL;  R;  vgbM;  60"  

Cluster  class  VI.  ;  v  F;  almost  nebulous   

pF;  pL;  IE;  vglbM;  50"  1  

p  F  ;  p  L  ;  p  m  E  ;  v  g  b  M  ;  2'  1,  45"  br   

p  B  ;  L  ;  p  m  E  ;  v  g  b  M  ;  2'  1,  1'  br  

F  ;  R  ;  g  1  b  M  ;  30"  

Cluster  class  VI.  F;  p  L;  irreg;  6';  resolved  into  st  13,  14,  15  m. 
Place  of  a  s|c  12  m,  chief  and  near  middle  of  cl. 

vF;  pL;  R;  vgvlbM;  90";  r  

A  p  rich  cl ;  not  m  comp  M  ;  stars  12. ...  14  m,  in  curved  branches.  A 
fine  double  star  follows. 

A  large  loose  cl  of  small  st  12 ....  14  m  ;  irreg  R  ;  not  v  rich  ;  1  comp  M ; 
diam  10'. 

Chief  sfc  10  m,  of  a  fine  rich  cl  which  fills  field  

Cluster  class  VI.  v  L  ;  v  B.  A  star  about  8.9  m  taken  ;  but  the  brightest 
part  of  the  cluster  is  about  4'  n  p.  Fills  field  ;  not  m  comp  M  ;  stars 
12 . .  13  m.  This  cluster  was  found  by  Mr.  Maclear  in  this  f  made  with 
him,  not  being  aware  at  the  time  of  its  having  been  before  seen  in  f  432. 

vF;  L;  vgbM;  6'  diam  ;  resolved  into  st  15  m  ;  rich  in  stars  ; 
a  delicate  and  faint  object ;  has  a  He  450  n  p,  (list  5'  from  centre.  Almost 
perfectly  insulated  in  a  very  large  space  almost  entirely  devoid  of  stars, 
being  the  smaller  and  southern  lacuna  below  the  great  "  coal  sack." 

cl,  class  VI.  Rich  ;  F  ;  L  ;  R  ;  vglbM;  8'  to  10'  diam  ;  stars  discrete, 
12,  13  ...  16  m  ;  insulated  ;  has  a      6  m  just  out  of  it,  n  p. 

pB;  S;  R;  pgvmbM  

cl  taken  for  A  300  ;  a  semi-elliptic  group  of  stars  11..12  m,  diameter  2'  . . 

eF;  L;  R;vgbM;  3'  diam  

e  e  F ;  v  S  ;  attached  to  a  afc  13  m.  (No  doubt  of  the  nebulous  character 
of  the  object. ) 

cl  VIII.  class  ;  poor  ;  scatt.    The  northern  of  2  st  8  m  taken  

p  B  ;  p  m  E  ;  s  p  m  b  M  ;  60"  1  

p  B  ;  E  ;  s  b  M  ;  pos  of  elongation  1300  

F ;  L  ;  R ;  vglbM;  90"   

e  F  ;  p  L  ;  R ;  vglbM;  40"  

vF;  L;  IE;  gvlbM;  2'  1  by  100"  br   

pF;  S;  R;  psmbMtoa  *  16m   

pB;  S;  R;  psmbMtoajfc  16  m   

F;  R;  or  1  E  ;  gib  M   

v  F  ;  S  ;  almost  exactly  south  of  a  #  10  m,  30"  dist   

vF;  L;  IE;  vglbM;  60"  1,  40"  br   

F  ;  p  m  E  ;  25"  1,  15"  br  ;  follows  2  stars   


Sweep. 


435 
432 

434 

452 

449 
452 

449 
810 

554 

700 
697 
700 
778 
458 

455 
456 
788 
784 

443 
435 

434 

432 
778 


567 


583 

458 
434 
686 
564 


690 
456 
458 
697 
458 
456 

574 
686 
572 
458 


D  D 


102 


REDUCED  OBSERVATIONS  OF 


No. 


3404 

34°5 
3406 
3407 

3408 
3409 
3410 

341 1 

3412 
3413 

34H 
34i5 
3416 

34i7 
3418 

3419 
3420 

3421 
3422 
3423 
3424 
342  5 

3426 

3427 
3428 
3429 
343° 
343i 
3432 

3433 
3434 
3435 


3436 


3437 


Synon. 


M.  68 


A.  272 


II.  772 
h.  1393 

II-  773 
h.  1394 


II.558 


A.  510  ? 

I.  129 
h.  1437 

III.  524 
h.  1438 

A.  511 


I.  133 


A.  301 


II.559 


K  A.  1830.0. 
h.  in.   s.  d. 


12  30  30.I 

12  31  46.2 
12  31  53.7 
12   32  29.3 

12  33  7.2 
12   33  26.4 

12  33  37-5 
12  33  38.4 

12  34  43.7 
12  35  3-5 

12  35  49.8 
12  36  + 
12  36  57.8 
12  37  14.2 
12  37  39.8 
12  37  58.1 
12  38  2.9 
12  38  6.8 
12  38  24.5 
12  38  24.9 
12  39  33.7 
12  40  12.5 

12  40  16.5 

12  40  36.9 
12  40  47.9 
12  42  52.3 
12  42  ± 
12  42  + 
12  42  57.0 

12  42  58.3 
12  43  27.3 
12  43  36.7 
37.1 


12  44  31.2 
33.6 

12  45  13.1 


NPD.  1830.0. 


115  48  50 

129  59  3 

130  2  8 

152     2  14 

I29  44  l6 

129  48  36 

96    6  16 

96  131 

130  48  53 

129  47  42 

99    9  0 

130  10  + 
130  47  3 

97  42  52 
130  40  3 
128  38  13 
100  42  42 
132  24  58 
130  37  33 

99  7  38 
130  22  38 

97  43  58 

100  28  43 

130  21  58 
130  26  23 
130  28  3 
130  10  + 
130  10  + 
99  3i  44 

130  8  53 

131  44  38 
149  25  28 

25  30 

25  36 


128  48  27 
48  3 


16  50+ 


Description,  Remarks,  &c. 


®  ;  irr  R  ;  g  b  M  ;  diam  in  R  A  =  12  ...  15  sec.  All  clearly  resolved 
into  stars  12  m;  very  loose  and  ragged  at  the  borders. 

e  F ;  L  ;  R ;  p  s  1  b  M.    The  first  of  2  

F;  L;  R;  vgbM;  r  (?).    The  following  of  2  

cl  class  VII.  Stars  11  ...  13  m  ;  about  6'  long  and  4'  br;  has  10  stars 
1 1  m,  and  some  20  or  30  smaller.  It  occurs  in  the  midst  of  the  black 
space  following  a  Cruris,  which  is  by  no  means  void  of  stars. 

eF;  vS;  R;  spa  star  at  the  edge.    The  first  of  2   

pF;  S;  R;  pslbM;  15".    The  following  of  2  

vF;  IE;  gib  M   

vF;  RorlE;  glbM   

pB;  S  ;  p  s  b  M  ;  12"   

v  F  ;  R  ;  b  M  ;  r.  Wind  violent.  [Right  reduced.  The  degree  of  P  D 
certainly  correct.'] 

e  F  ;  attached  like  a  wisp  toas|ei6m;asfc9in  precedes  

F;  R  ;  p  L;  gb  M  

eF;  S;  R;  vgbM.    [Right  reduced.    See  No.  3413.]   

v  F  ;  R  ;  glbM;  30"   

eF;  IE;  vgbM  

e  e  F  ;  p  L  ;  R  ;  60".    (No  doubt.)  

eF;  S  ;  has  one  or  two  small  st  entangled  in  it   

pF;  S;  R;  gbM;  15"   

eF;  S;  R;  vgbM;  60"  ;  n  f  a  small  star   

p  F  ;  E  ;  g  v  1  b  M  ;  45"  1  

pB;  L;  R;  gbM;  2'  resolvable   

vB;  R;  vsvmbM;  2^';  rto  left  eye   

p  B  ;  m  E  ;  v  1  b  M  ;  30'  1,  15"  br   

vF;  vS;  R;  psbM;  10"  

p  B  ;  R  ;  gbM;  30".    (More  nebulae  hereabouts.)   

F;  R;  gbM   

The  first  of  3  

The  second  of  3  

A  star  9  m,  with  a  strong  burr  about  of  very  small  extent ;  diam  10".  It 
is  the  best  specimen  of  the  class  of  "  stellar  nebulae"  that  I  remember  to 
have  seen.    A  star  s  f,  10  m,  dist  15';  has  no  burr. 

F  ;  L  ;  E  ;  gbM;  has  two  more  nebulse  preceding,  a  little  to  south  .... 

B  ;  R  ;  first  v  g,  then  v  s  b  M  ;  50*  

k  Crucis.    Place  of  the  largest,  central,  red  star   

The  same  red  star  taken.  Several  others  laid  down,  of  different  shades  of 
green. 

The  central  star  (extremely  red)  of  a  most  vivid  and  beautiful  cluster  of  from 
50  to  100  stars.  Among  the  larger  there  are  one  or  two  evidently 
greenish  ;  south  of  the  red  star  is  one  13  m,  also  red  ;  and  near  it  is 
one  12  m,  bluish.  (For  a  more  particular  description  of  this  beautiful 
cluster  of  variously  coloured  stars,  see  the  monograph  figure,  PI.  I.  fig.  2, 
and  the  accompanying  description.)  The  R  A  given  by  this  observation 
is  43  12.6,  an  error  induced  by  the  slider  of  the  eye-piece  not  having  been 
pushed  home  to  its  final  bearing. 

Viewed,  and  roughly  figured  for  future  reference   

B;  S;  IE;  psmbM;  25".    Wind  violent  

pB;  pL;  IE;  gmbM;  40"   

Viewed  in  its  place  by  working  list ;  p  F  ;  S  ;  R  ;  not  1st  class  

vF;  S;  R;  vlbM;  the  preceding  of  a  double  nebula   


NEBULA  AND  CLUSTERS  OF  STARS. 


103 


No. 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


3438 

3439 
344° 
3441 
3442 

3443 


3444 


3445 
3446 

3447 
3448 


3449 


345° 
3451 
345 1 
3453 
3454 

3455 

3456 

3457 
3458 
3459 

3460 

3461 
3462 

3463 


3464 
3465 


A.  164 


II.  549 
h.  1484 


A.  311 


II.  190 


II.  561 
A.  411 


12 

45 

14. 1 

98  16 

29 

12 

45 

35-7 

J37  49 

6 

12 

47 

2.3 

118  35 

13 

12 

47 

26.2 

130  52 

33 

12 

47 

26.3 

130  54 

3 

12 

47 

31.6 

154  1 

36 

33.0 

2 

1 

36.2 

2 

*5 

12 

47 

56.7 

159  56  50 

48 

25.1 

57 

25 

I.  130 


12 

47 

58.8 

97  35  5° 

12 

48 

26.8 

128  49  50 

12 

48 

29.0 

116  22  27 

12 

4S 

32.6 

135  19  21 

34.8 

20  23 

21  — 

12 

49 

49.8 

148  40  58 

68.0 

40  38 

12 

52 

6.6 

120    2  18 

12 

5* 

13.6 

120    0  18 

12 

5* 

28.2 

131  51  11 

12 

54 

9-5 

97    9  48 

12 

54 

34.1 

130  30  3 

12 

54 

59-8 

136  18  20 

12 

54 

59-8 

119  36  40 

61.3 

36  48 

12 

55 

15.4 

136  19  40 

J2 

55 

22.6 

99  25  58 

12 

55 

30.4 

138  22  24 

12 

55 

50.0 

132  41  3 

51. 1 

41  15 

12 

55 

54-9 

124  25  24 

12 

55 

58.! 

132  36  25 

59.1 

35  43 

12 

56 

38-5 

126  38  40 

39  •• 

12 

56 

48.2 

118  50  33 

12 

56 

58.1 

97    6  8 

vF;  Sj  R;  vlbM;  15";  has  a  *  sf;  the  following  of  2.  [N.B.— 
II.  559  is  not  noticed  as  double  in  Sir  W.  Herschel's  description.'] 

vF;  S;  R;  gib  M   

F  ;  R  ;  g  v  1  b  M  ;  40"   

e  F  ;  R  ;  g  b  M  ;  40".    The  preceding  of  2  

e  F  ;  R  ;  g  b  M  ;  30"  ;  90"  dist  from  the  foregoing  pos  =  i70°9   

Cluster;  R;  pS;  resolved;  irreg  ;  gbM;  3';  stars  13  .  . .  18  m. . . .  . . 

Class  VI.  ;  p  rich,  irreg  fig  ;  gbM;  3' ;  stars  v  S ;  comparatively  insu- 
lated ;  has  2  bright  stars  8.9  and  9.10  m. 

Cluster,  VII.  class  ;  5'  diam  ;  stars  10  ...  15  m.    The  foil  of  2  B  st  taken 

0;  B;  L;  R;  gbM;  stars  14  m,  and  one  7  m  n  p  the  centre  ;  a  fine 
object. 

0  ;  p  B  ;  L  ;  p  rich  ;  at  first  g,  then  v  s  p  m  b  M  ;  diam  of  the  bright 
part  3',  of  the  loose  stars  10' ;  stars  12 ....  16  m,  and  one  large  one  7  m, 
3'  or  4'  north  of  the  centre.  [N.B. — There  seems  to  have  been  some 
indecision  in  the  first  obs  whether  to  take  the  large  star  or  the  central 
portion  of  the  nebula.  I  presume  the  R  A  to  be  that  of  the  star,-  if  it 
be  not  that  in  one  or  other  obs,  the  moveable  wire  has  been  taken  for  the 
fixed."] 

B  ;  L ;  m  E  in  merid  ;  gpmbM;  3'1  

pF;  vS;  R;  sbMtoa  j|e  17  m;  pos  from  %   10  m  (distant  60") 

=  2500.3. 

F  ;  R  ;  gbM;  25"  

F  ;  m  E  ;  v  g  b  M  ;  90"  1,  25"  br  

B  ;  L  ;  m  E  ;  g  1  b  M  ;  2^'  or  3'  1,  1'  br  ;  pos  =  1570  ±  

F  ;  m  E  in  pos  147°  ;  vlb  M;  2'  1.  Taken  beyond  the  meridian,  and  out 
of  reach  in  R  A. 

A  very  poor  cluster  of  about  70  stars  11....  15  m,  very  loosely  scattered 
over  a  space  about  1 5'  long  and  8'  br. 

Cluster  VII.  p  rich  ;  L  ;  irr  R  ;  10' diam  ;  80  or  100  st,  10,  11,  12  m, 
with  a  stippling  of  much  smaller  ones. 

v  F  ;  R  ;  30"  ;  attached  to  a  star  ;  the  preceding  of  2  

v  F  ;  v  S  ;  R  ;  s  1  b  M.    The  following  of  2   

e  F  ;  precedes  3  or  4  st,  11 . .  12  m  

v  F  ;  R ;  g  1  b  M  ;  30"   

v  F  ;  R  ;  precedes  2  st  8.9  and  9  m  (with  which  it  makes  nearly  an  equila- 
teral triangle  by  diagram). 

e  e  F ;  S  ;  R ;  the  preceding  of  2  ;  a  H«  7  m,  just  at  the  northern  edge  of 
the  field. 

p  B;  R  ;  S  ;  b  M  ;  15";  has  a  H«  6  seconds  following   

P  F;  R  

F;  S;  R;  15".    The  following  of  2  

pF;  L;  R;  gpmbM;  60"   

B;  vL;  vmE;  vglbM.  Length  much  more  than  a  diameter  of  the 
field,  or  than  15'.  Its  light  extends  to  a  He  14  m  beyond  the  parallel  of 
B  4299.    Position  of  elongation  =  38°.7. 

B  ;  R ;  gpmbM;  60".    The  preceding  of  2  

p  B  ;  S  ;  R ;  b  M  ;  20"  

pL;  F;  R;  vglbM;  50"   

e  F  ;  S ;  R.  The  following  of  2  ;  barely  perceptible,  but  a  sure  obser- 
vation. 

e  F  ;  R  ;  p  s  1  b  M  ;  80"   

v  F  ;  p  S  ;  among  stars  ;  wind  furious   

Viewed  ;  a  diagram  made  representing  it  as  round,  with  three  small  stars,  one 
distant  about  1  semi-diameter  from  border  ;  pos  about  29  30;  another  dist 
f  diameter  ;  pos  =75°;  the  3rd  dist  i|  diam ;  pos  =  3000. 

F;  R;  gbM;  35"  

vB;  pL;  pmE;  psmbM;  90"  1  


104 


REDUCED  OBSERVATIONS  OF 


No. 

3466 

3467 
3468 
3469 
3470 

347i 
3472 

3473 


3474 

3475 

3476 
3477 
3478 

3479 
3480 

3481 
3482 

3483 
3484 

348S 

3486 
3487 

3488 

3489 
3490 

349 1 

3492 
3493 

3494 
3495 
3496 

3497 
3498 

3499 
3500 


Synou. 


I.  42 
h.  1540 


I.  138 


II.  566 


III.  117 

h.  1576 

II.  193 

h.  1577 

III.  118 

h.  1578 

II.  567 


III.  115 


R  A.  1880.0. 
ti.  m.    s.  d. 


i2  57  55-9 
55-9 
12  58  0.7 
12  58  56.0 

12  59  51.9 

13  o  12.6 
13  o  39.3 
13    o  49.1 


J3  3 


8.0 
8.2 
11. 1 
13    4  28.7 
31.8 

32-5 
13    6  4.0 


6  4.1 
6  18.5 

6  47.6 

7  8± 

8  47-7 
50.7 

8  53-2 

8  53± 

9  °-7 
13  10  31.0 
13  10  47.7 

47.8 
13  11  11. 3 
13  11  19.0 

21.3 
13  11  21.5 

27.3 
13  11  31.9 

13  11  33.9 

13  11  38.9 

13  12  22.9 
13  12  24.6 
25.3 
13  13  32-r- 
13  14  32.3 
13  14  39.5 

13  15  0.8 

'3  15  3-3 
4.8 

13  15  21.6 
22.5 
13  15  25.0 


N  P  D.  1830.0. 


117  18  41 
19  14 
112  46  5 
138  35  44 
1 17  44  18 
132  II  36 
III  38  30 
96  54  49 

132  12  6 

11  8 

11  10 

132    3  23 

3  25 

3  15 

152  30  51 

H9  9  35 
"3  4  55 
117  31  18 
117  26  + 

115  57  30 

56  59 
124  25  43 

124  31  58 
137    o  50 

116  30  47 
132  48  7 

48  55 
'3*  49  55 
132  49  12 

49  5 
132  50  7 

5°  35 
101  51  21 

101  46  18 

101  48  18 

125  44  40 
116  32  7 

32  7 

121  27  7 

121  27  7 

152  31  23 

101  24  3 

126  47  32 
48  10 

119  25  37 
25  20 
119  27  30 


Description,  Remarks,  &c. 


v  F  ;  v  L  ;  oval ;  v  g  1  b  M  ;  3'  1 ;  2'  br   

e  F  ;  v  L  ;  oval ;  vlbM;  3'  

F;pL;R;glbM;  60"  

B  ;  R;  g  m  b  M;  80"  

e  F  ;  R ;  30"  

v  F  ;  S ;  E  ;  possibly  a  small  group  of  stars,  but  I  think  it  is  nebulous  

p  F ;  R  ;  s  1  b  M  ;  35".    Among  stars  

pB;  R;  vgpmbM;  60"   

pB;  pS;  R;  gbM;  15";  in  a  curve  of  3  or  4  stars   

p  F  ;  S  ;  R.    The  middle  object  in  an  arc  of  stars   

B  ;  S  ;  R ;  pgbM;  12".    In  the  middle  of  an  arc  of  4  st   

p  B  ;  R ;  b  M  ;  40"  

pB;pL;  R;  gbM;  50"   

p  B ;  pL;  R;  gbM;  50";  has  a  *  7  m  ;  3°  n  f ;  dist  =  7%   

A  great  cluster,  or  a  surprisingly  rich  portion  of  the  milky  way.  It  con- 
tains 34  stars  11  m,  and  perhaps  150  or  200  more  of  less  magnitudes  in 
the  field. 

Cluster  VIII.  ;  oblong  ;  10'  by  7',  of  loose  sc  st  11  m  

F;  L;  R;  vgvlbM;  a  star  9m;!'  north  ;  precedes  10s  

p  F  ;  R ;  has  another  neb  n  f ;  i  R  A  =  201  + ;  A  P  D  =  5'  +  

The  following  of  2  

B;  pS;  R;  psbM;  12".    A  star  9  m  follows  io\5   

v  B  ;  R  ;  b  M  ;  has  *  10  m  n'  following  ;  30"  south  

e  F  ;  v  S  ;  R  ;  near  one  or  two  stars   

e  F  ;  v  S  ;  E.    (  ?  if  really  a  nebula)  

pB;  S;  R;  pslbM;  25"  

pB;  S;  pmE;  psbM;  has  a  %  7.8  m  following  

tF;  S;  R  

v  F ;  R  ;  20".    The  1st  of  a  group  of  4  

e  F  ;  R  ;  15".    The  2nd  of  a  group  of  4  

B  ;  p  L ;  R ;  60"  

p  F;  R;  30".    The  3rd  of  4   

F  ;  1  E.    The  last  of  group  ;  attached  to  the  preceding  one  

v  F  ;  R  ;  20".    The  last  of  4   

v  F  ;  S  ;  R.    The  1st  of  a  group  of  3  nebula;   

p  B  ;  S  ;  p  m  E.    The  2nd  of  a  group  of  3   

F ;  S ;  R.    The  3rd  of  a  group  of  3   

v  B  ;  R  ;  s  v  m  b  M  ;  50"   

vB;  pmE;  gmbM  

B;  R;  pL;  psmbMtoa  star  

e  e  F.    The  preceding  of  2   

F  ;  IE;  psbM.    The  following  of  2   

CI  class  VI.  ;  oval ;  4'  1 ;  3'  br  ;  stars  12 ....  16  m  ;  an  extremely  rich  clus- 
tering patch  in  the  milky  way,  which  is  here  superb. 

p  B  ;  S  ;  R  ;  or  1  E  ;  definition  bad  ;  doubted  at  first  if  it  really  was  a  ne- 
bula, but  remained  satisfied. 

B;  R;  psvmbM;  30";  r ;  probably  a  dimly  seen  ®   

p  B  ;  R ;  psbM;  20"  

e  F;  S;  IE   

vP;  S;  E  

v  F;  v  S  


NEBULA  AND  CLUSTERS  OF  STARS. 


105 


Xo. 


Synon. 


3501 


A.  482 


3502 
35°3 


3504 


A.  312  ? 


A.  440 


3S°5 
3506 

3507 

3508 

3S°9 
3510 

35" 


R  A.  1830.0. 
h.  m.  s.  d. 


13  15  28.7 


29.5 


3*-7 


33-i 


13  16  16.5 
13  16  20.2 

30.1 
13  16  36.0 


38.9 


13  16  44.9 

474 
13  18  9.3 


13  18  11. 2 
12.6 

13  18  23+ 

13  18  24.2 
13  18  28.5 
3 1.2 
13  19  38.0 


N  P  D.  1830.0. 


132    8  3 


7  30 


7  17 


118  56  48 

148    6  59 

7  39 

136  35  10 


35  38 


122  59  7 
60  6 
152  32  3 


118  40  28 
41  39 
118  45  ± 

1 18  44  28 
138    1  25 
1  19 
122  17  2 


Description,  Remarks,  &c. 


[A  nebula  consisting  of  two  lateral  portions,  and]  no  doubt  of  a  small 
streak  of  nebula  along  the  middle  of  the  slit  or  interval  between  them, 
having  a  star  at  its  extremity.  See  fig.  2,  PI.  IV.  Position  of  the  slit, 
124.7  ;  of  the  star,  with  another  near  the  nebula  and  south  of  it, 
332.3  ;  other  stars  also  laid  down  (see  description  of  the  figure).  A  most 
superb  calm  night ;  objects  admirably  defined.  Shown  to  a  bystander 
(J.  R.)  who  saw  it  as  figured  and  described. 

[Two  nebula;,  or  two  portions  of  one  separated  by  a  division  or  cut.]  The 
cut  is  broad  and  sharp.  The  two  nebulae  are  very  nearly  alike.  Perhaps 
the  slit  is  larger  towards  the  n  p  end,  where  there  is  a  star  between  them. 
There  is  certainly  a  very  feeble  trace  of  nebula,  an  island  as  it  were, 
running  from  this  star  between  the  sides  of  the  slit.  N.B.  No  "  moon- 
light effect"  seen  between  the  edges.  Night  very  fine.  Pos  of  the  slit, 
I20°.3-    The  place  taken  is  that  of  the  star  within  the  slit. 

A  figure  taken  (which  represents  the  internal  faint  nebula),  but  no 
description. 

A  most  wonderful  object ;  a  nebula  vB;  vL;  IE;  vgmbM,  of  an 
elliptic  figure,  cut  away  in  the  middle  by  a  perfectly  definite  straight  cut 
40"  broad  ;  pos  =  i20°.3 ;  dimensions  of  the  nebula,  5'  by  4'.  The 
internal  edges  have  a  gleaming  light  like  the  moonlight  touching  the 
outline  in  a  transparency. 

pB;  S;  E   

General  middle  of  cluster  VIII.  class,  p  B  ;  L  ;  irr  ;  sc  ;  30  or  40  stars 
11.12  m,  and  many  smaller  ;  pretty  well  insulated,  though  on  a  ground 
rich  in  v  small  stars. 

Cluster  VII.  class  ;  rather  a  fine  cluster  ;  rich,  but  loose  and  straggling. 
Fills  field.    Stars  1 1  and  12  m. 

0;  w  Centauri;  vvB;vvL;vvgmb  M;  all  clearly  resolved  into 
stars  of  two  magnitudes,  viz.,  13  and  15  ;  the  larger  lying  in  lines  and 
ridges  over  the  smaller.  Near  the  centre  are  two  distinct  darkish  spaces 
formed  by  a  deficiency  of  the  larger  stars  13  m  within,  and  an  excess 
without.  This  most  glorious  object  fills  the  whole  field  with  its  most 
condensed  part,  and  its  stragglers  extend  f  of  a  field  beyond  it  either  way. 
It  is  very  conspicuous  to  the  naked  eye  as  a  dim  cometic  looking  star, 
4  m  or  5  m. 

0  ;  a)  Centauri ;  diameter  full  20'.  It  much  more  than  fills  the  field. 
When  the  centre  is  on  the  edge  of  the  field,  the  outer  stars  extend  fully 
half  a  radius  beyond  the  middle  of  it.  The  stars  are  singularly  equal, 
and  distributed  with  the  most  exact  equality,  the  condensation  being  that 
of  a  sphere  equally  filled. — Looking  attentively,  I  retract  what  is  said 
about  the  equal  scattering  and  equal  sizes  of  the  stars.  There  are  two 
sizes  12  m  and  13  m,  without  greater  or  less,  and  the  larger  stars  form 
rings  like  lace-work  on  it.  One  of  these  rings,  15'  in  diam,  is  so  marked 
as  to  give  the  appearance  of  a  comparative  darkness  like  a  hole  in  the 
centre.  There  must  be  thousands  of  stars.  To  the  naked  eye  it  appears 
as  a  %  5  m  or  5.4,  rather  hazy.  There  is  a  ^  9  m  on  the  sp  border  of 
it,  about  4'  or  5'  south  of  centre,  and  several  8  m  are  scattered  far  away. 
My  attendant  (J.  S.)  called  up,  who  saw  the  hole  and  darkness,  and 
described  it  as  I  have  done  above.  On  further  attention  the  hole  is 
double,  or  an  oval  space  crossed  by  a  bridge  of  stars.  Position  of 
axis  =  1500.  Altogether  this  object  is  truly  astonishing.  (See  PI.  V. 
%•  7-) 

p  F;  R;  glbM;  25"   

eF;  S;  R;  g  b  M  ;  12"   

A  portion  of  the  milky  way  broken  up  into  clustering  masses  of  astonishing 
richness.  There  must  here  be  at  least  200  or  300  stars  in  the  field,  none 
greater  than  10  m. 

pF;  S  ;  R ;  b  M  ;  has  a  *  2'  fol ;  pos  by  diag  =  67°  

F;  S;  R;  pslbM;  15"  

The  preceding  of  a  double  nebulse ;  the  individuals  are  =  ;  R ;  v  F ;  S ; 
p  s  1  b  M 

p  F ;  S  ;  the  following  of  two  equal  neb  

p  F;  irr  R ;  or  triangular  ;  g  b  M;  r ;  40"  

pB;  IE;  glbM;  has  a  s|c  8  m  5'  dist ;  pos  sp   

pF;  L;  pmE;  vgbM;  r;  4'  1 ;  2'br;  with  left  eye  feebly  stippled 


E  E 


106 


REDUCED  OBSERVATIONS  OF 


No. 


3512 


3513 

35'4 

35i5 

3516 

3Si7 
3518 

3519 

3520 
3521 
3522 

3523 


35H 

3525 
3526 

3527 
3528 
3529 

3530 
353i 

3532 


Synon. 


A.  252  i 


III.  507 


A.  628 


II.  638 
A.  623 


A.  273 


R  A.  1880.0. 
h.  m.   s.  d. 


13  20  6.0 


6.8 

13   21    II. 2 
12.8 
13   21  37.I 


13  21  48.O 
50.6 
13  22  15.6 
13  23  I7.9 
13  23  30.4. 
13  25  28.3 

13  26  — 
13  26  I7.8 
13   27  2.3 

13  27  26.I 

27.9 


28.5 
30.I 

13   27  33.I 

33-7 
35-3 
36.4 

13  28  27.6 
31.3 

13  30  18.2 

13  30  37.2 
13  32  2.3 
13  32  37.5 

38.0 
13  32  53.1 

67.4 

!3  34  47-5 
54.2 

13  35  15-7 


N  P  D.  1830.0. 


150     3  21 


I  59 

117  16  38 
15  21 

r55    5  5i 


123  54  46 

54  * 
122  21  7 

97  53  56 

137  15  22 
122  36  22 

135  2  ± 
122  34  57 

138  57  44 

119    o  18 
o  16 


o  20 

o  8 

*3»  59  3 

59  2° 

58  30 

58  14 

134  58  15 

61  17 

120  46  22 

100  37  43 

119    3  18 

137  19  3 

18  2 

152    2  50 

2  26 

152    3  o 

2  16 

148  20  17 


Description,  Remarks,  &c. 


Place  of  a  double  star  in  centre  of  a  rich,  much  comp  but  v  F  cluster ; 
gb  M;  4' diam;  st  15  m;  a  remarkable  object.  [N.B.  By  a  singular 
coincidence  of  errors  the  R  A  of  this  obs  has  been  mistaken  1"',  and  the 
P  D  i°.  Both  are  corrected.  The  P  D  149°  could  not  have  been 
observed  in  f  596. 

A  small  but  very  rich  milky  way  cluster;  3 J'  1,  3'  br;  st  13....  16  m. 
Place  that  of  a  double  star. 

vF;  pL;  R ;  50" ;  has  a  *  7  m  11  f;  dist  =  10'  

v  F ;  pL;  IE;  avL  *  follows  12'  +  dist  

A  very  strange  object.  See  fig.  1,  PI.  VI.  A  nebula  of  oval  fig,  but 
having  a  central  and  brighter  axis  somewhat  curved,  and  terminating  in 
two  masses  brighter  than  the  rest ;  diam  about  90"  or  100".  It  involves 
3  stars,  one  of  which  with  320  is  double.  The  principal  $  is  10  m,  the 
others  e  S ;  a  multitude  of  other  stars  in  field. 

F;  pL;  R;  g  1  b  M  ;  45"  

F;  p  L;  IE;  vglbM;  50"   

p  B  ;  S  ;  R ;  first  g,  then  p  s  b  M ;  45"   

v  F;  S;  R;  gb  M;  15"   

F;  pL;  R;  vgbM;  50" ;  on  a  ground  faintly  stippled  with  minute  stars 

e  F  and  S ;  has  2  st  less  than  1  diam  of  neb,  distant  one  (by  diagram)  s  and 
one  p. 

v  F  ;  S ;  R ;  has  a  ^  near  lower  edge   

v  F  ;  S ;  R  ;  precedes  a      10  m,  dist  i|  diam  by  diag   

e  e  F  ;  IE;  30".  Requires  a  newly  polished  mirror,  and  a  night  such  as 
this  is  to  be  seen. 

185  Bode  Centauri.  E  ;  pos  of  axis  =  55°.i,  which  is  also  that  of  one  of 
the  2  stars  involved  in  it  =  10  m.    (See  fig.  5,  PI.  IV.) 

v  B;vL;  sbMtoa  centre  =  a  star  9  m,  diam  8",  of  a  resolvable  char- 
acter like  a  0,  surrounded  by  an  immensely  L,  extremely  dilute  almost 
equable  light  7'  or  8'  diam,  somewhat  oval,  and  passing  with  excessive 
suddenness  into  the  central  light. 

F;  vL;  E;  vsvmbMtoa  sharp  nucleus  (ill  seen,  owing  to  clouds)  . . 

v  L;  vB;  m  E,  vsvmbM  to  a  nucleus;  diam  in  R  A  =  17.5 
sec  =  3",  49"  in  arc ;  a  small  s)s  involved ;  pos  with  nucl  8o°  ■+-  by  a 
rough  diagram  made  at  the  time. 

vF;  pL;  IE;  glbM;  90"  1  

F;  pL;  R;  g  1  b  M  ;  40"  

F  ;  p  L  ;  oval ;  v  g  b  M  ;  60"  1 ;  50"  br   

F;  pL;  R;  vglbM;  40"  

e  F  ;  S  ;  attached  to  a  He  13  m.  (Certain)   

v  F ;  S;  R;  vglbM;  has  a  *  at  its  edge  

v  B  ;  m  E  ;  p  s  m  b  M  ;  2^'  1 ;  1'  br  

p  B ;  L  ;  p  m  E  ;  glbM;  2'  1;  if  br  

v  F ;  R  ;  v  1  b  M  ;  80"   

B  ;  R ;  vglbM;  45" ;  has  3  st  14  m  near  

B;  pL;  IE;  glbM;  r;  3V  small  st  near   

CI  class  VII.  ;  poor ;  L  ;  loose  irreg  fig  ;  fills  field  ;  st  12  m  

A  fine  rich  milky  way  group,  or  rather  outlying  cl  of  a  much  finer  cl  fol- 
lowing it. 

Cl  class  VII.  Small,  compact  irr  R  ;  1  *  8  m,  and  15  or  20  smaller  in  a 
knot.    No.  i,y  578,  is  an  outlier  of  it. 

A  brilliant,  compact,  milky  way  cl.  Rich ;  irreg  fig ;  g  b  M  ;  10';  stars  10, 
11,  12  m. 

Cl  class  VIII.    L ;  v  rich  ;  loosely  sc  ;  st  7.8  16  m ;  it  is  an  outlier  of 

the  milky  way,  but  very  rich  and  much  insulated. 


NEBULyE  and  clusters  of  stars.  107 


Synon. 


3533 


3534 


3535 
3536 
3537 


3538 
3539 
354° 

3541 


354* 
3543 

3544 
3545 


3546 
3547 

3548 


A.  388 


II.  306 
b.  167 1 


A.  282 
III.  923 


R  A.  1830.0. 
h.  ni.    s.  d. 


13  35  44-3 
45-4 

13  36  39.6 
42.6 

13  37  43.9 
13  37  59.0 
13  38  49.8 


13  38  57.5 

13  39  4o-5 

13  40  17.8 

13  40  18.3 


13  42  3.2 

13  43  H-5 
15. 1 
13  43  47.6 
13  45  50.2 

86.3 

13  46  15.4 
13  47  25.3 
26.3 
13  47  29.9 

32.6 


33-7 


34-i 


NPD.  1830.0. 


140  31  I 


153  50  16 

50  6 

119  32  8 

120  4  8 
149  35  39 


119  35  18 

119  38  18 

96  22  26 

140  21  33 


151    o  40 

117  38  23 
37  28 
137  39  36 

r59  33  5 

35  45 

119  29  58 

i33    5  58 

5  35 

129    8  53 

8  20 


8  49 


9  *3 


Description,  Remarks,  &c. 


(J) ;  B  ;  R  ;  vgbM;  resolved  ;  diam  2' ;  st  1 6  m  ;  a  B  st  7  m  in  field    . . 

0  ;  v  B  ;  g  m  b  M  ;  2^'  or  3'  diam  ;  resolved  into  st  15  m  ;  has  one  sfc 
12  m,  s  f ;  the  centre  near  the  edge.  It  is  in  the  field  with  B.  4618  a 
star  6  m. 

A  F,  oblong,  elliptic  cl  of  st  14  m  ;  g  1  b  M  ;  4'  1 ;  2J'  br   

A  S,  irreg  R,  very  compact  knot  of  M  way;  g  v  1  b  M  ;  stars  14  m;  a 
8  m  precedes. 

v  F  ;  R;vlbM;  follows  a  B  double  star  

p  F  ;  R ;  gbM;  20" ;  has  2  or  3  stars  close  to  it  

Cl  VII.  class  ;  much  more  than  fills  field  ;  a  very  L  and  rich  milky  way  cl, 
quite  insulated  on  the  prec,  n,  and  foil  sides,  and  nearly  so  to  the  S ; 
forming  a  kind  of  peninsular  projection,  but  much  richer  than  the  main 
body  of  the  milky  way. 

F;  R;  gbM;  30"  

F;  R;  gb  M;  30"  

F;  R;  psbMj  20"   

Planetary  Nebula.  A  very  singular  object.  At  first  I  thought  it  an  ill 
seen  double  star;  12.13  =  12.1301;  dist  2";  but  not  being  able  to 
get  it  into  focus  I  applied  320 ;  which  showed  it  as  a  hazy,  rather  elon- 
gated, planetary  nebulous  disc,  as  if  a  double  j|c  all  hut  obliterated.  It 
is  positively  not  a  star.  The  field  is  full  of  stars,  two  of  which  (Nos.  6 
and  7  in  the  figure),  are  equal  to  this  object  in  light,  but  320  shows 
them  both  quite  sharp.  It  is  a  difficult  object  to  find,  and  unless 
in  a  good  night  for  definition  (this  is  superb)  it  could  not  be  reco- 
vered. The  place  is  well  taken.  The  stars  in  the  neighbourhood  [laid 
down  in  a  diagram  made  at  the  time]  are  —  1  the  neb  ;  2  =  3=4  nearly 
equal,  and  14  m ;  5  =  15  m ;  6  =  7  12  m.  It  is  the  smallest  and  most 
difficult  planetary  nebula  I  have  ever  seen.  Fig.  15,  PI.  VI,  exhibits  its 
appearance  with  power  320.  [N.B. — By  this  figure  it  would  seem  rather 
to  belong  to  the  class  of  double  nebula?  or  double  stellar  nebula  of  the 
utmost  remoteness,  than  to  that  of  planetary  nebula,  properly  so  called.'] 

Cl  VII.  class  ;  14  stars  11  m,  and  30  or  40  smaller  in  a  round  space  8'  dia- 
meter.   The  general  middle  taken. 

B;  IE;  sbM;  20"  

pB;  R;  lbM;  20"   

v  F ;  v  S  ;  R ;  6" ;  has  a  *  8m;  3'  f  in  parallel  

Cl  VIII.  class ;  v  L,  loose  ;  straggling ;  stars  L  and  S  ;  fills  field.    The  star 

taken  is  a  double  one. 
Cl  VIII.  class;  irreg  fig;  8'  diam;  consists  of  about  a  dozen  stars  11  m, 

and  a  great  many  12,  13,  14  m. 

p  F ;  R  ;  g  1  b  M  ;  20";  exactly  in  M  between  2  st  10  m  

p  B;  v  S;  R;  gbM;  15"  

pF;  S;  R;  pgmbM;  in  a  group  of  small  st   

Place  hurried  and  imperfect.    Shown  to  Mr.  Maclear  and  friend.  AD* 

h  4636  involved  in  neb. 
Double  star  involved  in  neb.    See  fig.  10,  PI.  VI.    For  meas  of  the  D  star, 

see  Catal  of  those  objects.    Adjacent  stars  laid  down,  b  and  c  =  13  m  ; 

pos  of  1  =  28°.3  ;  a  =  9  m  ;  the  nebulosity  is  very  evident.    No.  3  has 

no  such  nebula ;  neb  at  least  2'  or  z^1  diam. 
A  close  double  star  in  a  v  L,  B,  luminous  atmosphere,  2'  diam.    The  *  a, 

which  is  quite  as  bright,  has  no  such  atmosphere.    The  atm  is  v  1  b  M. 

The  star  was  not  noticed  as  double  till  too  late  for  a  good  meas  after  I 

had  showed  the  object  to  my  attendant  J.  S.,  verified  with  240  and  320. 

A  furious  hot  north  wind,  but  the  definition  of  stars  excellent.    It  is  no 

illusion,  other  stars  are  sharp  and  brilliant,  and  have  not  the  least  nebulous 

appearance. 

Neb  seen  as  above.   Careful  obs  taken  of  the  stars  in  and  adjoining  it,  which 

see  in  the  Cat  of  D  stars, 
v  F ;  2'  diam  ;  a  *  9  m  following,  is  about  4'  dist,  is  unaffected  with  neb. 

Measures  taken.    See  Cat  of  D  st. 
Viewed  past  meridian,  seen  as  above,  and  a  diagram  made  and  measures 

taken  of  the  double  star,  which  see. 


Sweep. 

693 
566 

568 
581 

451 
564 
790 


564 
564 
697 

693 


578 

564 

45i 
464 
584 

598 

564 
686 
788 
461 

573 


460 


574 
718 
462 


108 


REDUCED  OBSERVATIONS  OF 


No. 


3549 


355° 
355i 
355^ 
3553 
3554 


3555 


3556 
3557 
3558 
3559 

3560 

35Sl 
3562 

3563 

35% 
3565 
3566 

3567 
3568 

35r>9 
3570 


3571 
3572 

3573 


Synon. 


A.  431 


III.  924 


A.  313 

III.  120 
h.  1798 

A.  302 


A.  469 
A.  342 


R  A.  1830.0. 
h.  m.    s.  d. 


13  48  39.O 
69.5 

13  50  50.6 
13  51  10.9 
13  51  26.5 
*3  53  1.7 
r3  53  37-6 
39.6 
40.8 
J3  56  5-9 

39.6 


41.7 

'3  57  17-5 
r3  59  55-2 
14  1  + 
14  1  15.3 
18.0 
14    *  3J-9 

14   2  40.9 
14   4  59.3 
59-5 
H    7  49-5 

14  10  40.2 
14  14  3.7 
14  14  9.8 

14  14  50.6 

14  15  26.1 
14  15  56.1 

14  17  9.0 
11.  5 

11.6 
14  19  49.8 
14  21  45.2 

45.8 
14  22  59.4 


N  P  D.  1830.0. 


60.9 


148  46  52 

44  27 

118    2  28 

i23    7  34 

122  14  32 
130  35  20 

123  9  26 
8  43 
8  47 

137  31  13 

30  9 


29  11 

119  11  48 

132  30  43 
122  50  ;+- 
135  16  43 

17  14 
119  51  13 

116  18  18 

137  18  36 
19  20 

35  5 
118  27  58 

"7  53  38 
*44    1  35 

167  37  48 

148  51  44 
102  24  12 

149  57  12 

57  25 

56  39 
118  59  23 

133  26  22 
26  27 

145  48  34 

49  3 


Description,  Remarks,  &c. 


CI  VI. ;  F;  rich;  highly  comp  ;  consists  of  p  L  and  e  S  st;  fig  oblong; 

10'  1 ;  7'  br;  place  that  of  chief  *  9  m. 
CI  VIII.  class;  8'  1;  5'  br ;  stars  12  and  13  m.    [N.B. — It  is  evident  that 

in  this  obs,  probably  from  defective  weather,  the  e  S  stars  of  this  cl  were 

not  seen.] 

v  F;  R;  gib  M;  25"  

v  F;  S;  R;  gb  M;  15*  

p  B  ;  pL;  R;  v  g  b  M  ;  90'  

e  F ;  E  between  2  v  S  st  a  little  s  f  

pB;  pL;  R;  gpmbM;  50"   

pB;pL;R;gbM;  50"   

pB;  R;  gmbM;  25"  

A  region  of  L,  B  st  8,  9 . . .  .&c.  m  ;  a  very  coarse  cluster.  Place  that  of  a 
brilliant  group,  one  of  which  is  a  double  star  class  III. 

A  region  of  L  stars  very  loosely  distributed,  but  which  yet  decidedly  form  a 
cluster.  Place  that  of  a  pretty  close  double  star  (4")  in  the  middle  of  a 
group  of  8.  The  cluster  is  30'  diameter,  and  is  divided  into  distinct 
groups.  [N.B. — The  two  double  stars  taken  in  this  and  the  foregoing 
observation  are  not  the  same.] 

Place  of  a  double  star  [the  same  as  that  of  f  695]  in  a  semi-elliptic  group 
forming  part  of  it,  but  insulated  in  a  large  scattered  cluster  or  tract  of 
bright  stars. 

pF;  S;  R;  pslbM;  15"  

pF;  vL;  R;  vgbM;  4'   

F ;  R ;  near  and  to  the  north  of  a  if.  8  m  

F;  S;  R;  psbM;  10"  

e  F  ;  R  ;  g  1  b  M  ;  20"   

p  B  ;  L  ;  R ;  g  b  M  ;  r.  Stars  barely  seen  in  the  nebula,  besides  several 
others  about  it. 

vF;  S;  R;  bM;  npa  star  

F  ;  S  ;  R ;  near  2  st  12  m  ;  a  small  D  s(j  foil  ;  5'   

pB;  S;  R;  psbM;  15"   

A  star  12  m,  perfectly  sharp  in  the  centre  of  a  very  dilute,  very  gradually 
fading  atmosphere,  p  m  E  ;  90"  1,  40"  br.  A  very  remarkable  specimen 
of  its  class. 

e  F ;  L  ;  2'  diam  ;  has  some  small  stars  involved  

pF;  E;  gvlbM;  25"  

A  poor,  coarse,  oblong  cluster,  which  is  the  most  condensed  part  of  a  rich 
region  of  stars  10  m.    Place  of  a  double      in  the  following  part. 

v  F ;  E  ;  g  b  M  ;  with  a  feeble  appearance  of  stars,  but  I  have  hardly  a 
doubt  of  its  being  a  nebula. 

A  small  close  group  of  large  and  small  stars,  forming  a  cluster   

F;  pL;  R  ;  gvlbM;  90"   

CIVIL  class;  irr  fig  ;  not  m  comp  M  ;  L;  10' diam.  There  are  perhaps 
100  stars,  11  and  11. 12  m  ;  with  a  good  sprinkling  of  12  and  13. 

Cl  VI.  v  rich  ;  irreg  R  ;  p  m  comp  M,  but  sc  at  borders  ;  15' ;  there  are 
3  st  10  m  ,  5  or  6  1 1  m  ;  the  rest  below  1 1  m. 

L,  p  rich,  irreg  cl  of  sc  st  8 . . . .  14  m  ;  fills  field   

e  F  ;  R  ;  20"  

pF;  L;  R;  vglbM;  has  many  stars  intermixed   

p  B  ;  L  ;  vgbM;  2'  ;  r,  or  with  stars   

Place  of  a  red  star,  the  chief  and  centre  of  a  fine  bright,  but  not  rich  cl,  of 
about  30  stars  9 ....  13  m.    This  red  or  high  yellow  star  is  8  m. 

Large,  p  brilliant,  coarse,  sc  cl  VII.  class,  which  more  than  fills  field  ; 
50  stars  more  or  less  9....  12  m;  chief  He  7  m>  yellow,  somewhat 
insulated,  taken  for  place  of  cluster. 


Sweep. 

790 
582 

564 
792 
701 

457 
792 
446 

572 
463 

695 


464 

564 
686 

792 
463 
464 
564 

453 
464 
463 
788 

45i 
564 

468 
587 

713 
702 

582 

578 

7'5 
564 

455 
454 
694 

577 


NEBULAE  AND  CLUSTERS  OF  STARS. 


109 


No. 


R  A.  1S30.0. 
h.  in .  s. d. 


N  P  D.  1830.0. 


Description,  Remarks,  Sec. 


Sweep. 


3574 

3575 
3576 

3577 
3578 


3579 
358o 
358i 
3582 

3583 

3584 
3585 
3586 
3587 

3588 

3589 

359° 

3591 

359* 

3593 
3594 


3595 
3596 

3597 

3598 

3599 


II.  196 

A-  333 

III.  508 
VI.  8  ? 


A.  356 


I.  71 


III.  736 


III.  116 

VI.  19 

III.  138 
III.  139 

III.  374 
h.  1918 


14  24  30.4 

33-3 
14  28  32.0 
14  30  19.9 

H  3*  4-5 
14  33  2.6 


5-6 


14  35  44.8 

14  36  49.7 

14  38  15.2 

14  41  38.5 

14  48  1.5 

14  48  52.6 
14  49  59.1 
14  51  32.3 
14  51  50.9 

54-3 
14  52  51.6 

H  53  7-9 

14  54  26.7 
28.1 
38.4 

14  56  19.8 
20.1 

14  56  48.8 

49.2 

15  4  23.9 
15    5  158 


19.5 

15  5  53-° 
15    7  39.1 

15    8  8.2 

iS    8  38.4 

39-7 
15  12  5.1 


135  1*  38 

12  20 
134  17  52 
"5  47  45 

146  49  o 
98  16  31 


16  8 


103  13  7 
143  48  29 

104  8  17 
Hi  57  53 

131  20  ■+: 

161  45  10 
141  14  12 
103  29  32 

96  46  6 
46  21 

143  40  12 

144  55  6 

162  12  12 
12  10 
11  33 

i54   o  55 
1  14 
125  40  9 

39  58 
103  37  27 

J35    0  51 


o  32 
99  26  18 

IIO  22  59 
113   2S  ± 

113   22  + 

26  40 
91   57  27 


v  F  ;  S  ;  IE;  between  2  stars  13  and  14  m,  forming  northern  side  of  a 
trapezium  of  4  stars  ;  one  of  the  others  is  S  in. 

vF;  E;  between  2  stars  (by  diagram),  and  has  a  large  star  s  p  

not  vF;  S;  vgbM;  25";  among  stars  

v  B  ;  p  L  ;  R ;  p  s  b  M  ;  1st  class  ;  20"  ;  r  ;  several  stars  near.  [N.B. — In 
the  R  A  the  wire  is  not  set  down.    The  1st  presumed.] 

Cluster  VII.  p  rich;  st  11....  13  m,  irreg  sc  10'  diam  ;  rather  more 
comp  M. 

F;  pL;  pmE;  gbM;  with  an  appearance  of  resolvability,  arising  as  I 
imagine  from  a  few  small  stars  accidentally  on  it,  as  I  hardly  think  it  can 
be  reckoned  a  cluster  in  the  sense  of  class  VI.  Re-examined  working 
list.  It  is  III.  508.  VI.  8  does  not  exist  in  the  space  assigned  to  it  in 
catalogue. 

F  ;  p  L  ;  gbM;  irreg  oval ;  r  ;  2^'  by  2'.  If  this  be  not  VI.  8,  there  is 
no  other  near  the  place.  [N.B. — It  does  not  agree  with  the  description  of 
that  cluster  in  my  Father's  catalogue,  which  states  it  to  be  8'  or  9'  in 
diam  ;  rich  ;  v  comp.  The  j|j  26  x  Virginis,  by  which  its  place  is  there 
determined,  is  a  mistake  for  577  of  Mayer's  catalogue.] 

vF;  E;  pslbM;  20"  

cl  VII.  class  ;  p  rich  ;  loose  ;  irreg  fig  ;  8' ;  st  10  and  n  m  

pB;  pmE;  gpmbM;  80"  

A  small  elongated  close  group  of  v  S  milky  way  st  3' 1,  ij'br;  so  close 
and  faint  as  to  approach  very  near  to  the  character  of  a  nebula. 

F ;  m  E.    In  field  with  and  npASC  1693  (k  Centauri).    Place  very  rude 

Viewed,  found  in  place,  and  seen,  as  described  in  f  456   

eF;  S;  R;  b  M;  15"   

a  p  L  cl  VII.  class;  coarse  ;  not  comp  ;  chief  D  %  taken  

vF;  S;  E  ;  g  1  b  M   

vB;  S;  psvmbM;  15";  almost  stellar  

pB;  R;  svmbM;  30" ;  hardly  bright  enough  for  a  first  class  nebula . . 

cl;  v  L  ;  coarse,  but  rich  and  fine  ;  diam  in  R  A  =  2  fields  in  PD  2| 
(30' and  45') ;  st  9,  10,  11,  12.    General  middle  taken. 

cl  VII.  class  ;  a  fine  L  cl  of  separate  stars  13  ...  14  m,  10'  diam;  not 
m  comp  M  ;  nearly  fills  field. 

pF;  pmE;  glbM;  35"  1,  20"  br.    In  a  field  full  of  st   

v  F;  IE;  glbM   

e  F  ;  pmE;  25"  

pB;  R;  vgvlbM;  60"  

pB;  R;  vgvlbM;  70"  

vF;  R;  vglbM;  20"  

eF;  E;  vlbM;  r;  15"  1   

B;  pmE;  psmbM;  involves  a  ^  14  m  to  northward  

O  ;  a  most  elegant  and  delicate  Planetary  Nebula.  Diam  in 
R  A  =  1  .35  by  many  observations.  Long  contemplated  with  180,  240, 
and  320.  The  disc  is  magnified  by  the  power  in  due  proportion.  It  is 
=  a  *  8.9  m  ;  perfectly  sharp,  not  the  slightest  haziness.  A  very  fine 
object.  It  has  no  "satellites."  My  attendant,  to  whom  I  showed  it, 
said  it  was  like  the  moon,  only  smaller,  and  not  in  the  least  like  a  star. 

O  ;  a  clear  round  planetary  white  disc  ;  at  most  4"  diam.  Has  two  stars 
14  m  near  ;  one  at  dist  90",  pos  108.8  ;  the  other  dist  120",  pos  6o°.2. 
See  fig.  8,  PI.  VI. 

pF;  L;  R;  vgbM;  3'  diam  

^  ;  p  F  ;  v  irr  R  ;  vgbM;  all  resolved  into  st  12  16  m  ;  diam  5' 

to  51'. 

p  B;  R;  p  g  b  M;  15".  (PD  "  tube  resting  on  gallery.)  [True 
P  D  =  1 1 3  29  40  probably.    See  the  next  nebula.] 

B  ;  R  ;  p  g  b  M  ;  20".    (Tube  resting  on  gallery.)  

p  F  ;  R  ;  gpmbM;  30"  

v  F  ;  IE;  gbM;  25"  1,  20"  br  


463 

695 
454 
453 

469 
697 


698 


702 
468 
702 
468 

456 

457 
569 
468 
702 
609 
697 
711 

694 

597 
598 

569 
581 
785 
792 
448 
702 
464 


695 

698 
722 

453 

453 
793 
6cS 


F  F 


110 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


3600 
3601 
3602 
3603 


3604 

3605 
3606 
3607 


3608 
3609 
3610 


361 1 


3612 

36l3 
3614 
3615 


3616 


A-  357 


A.  389 


II.  401 
h.  1926 


A.  552 


A-  343 


A.  334 


A.  304 


15  12  12.7 
15  12  17.2 
15  12  27.4 
15  14  43.8 

56.9 


81.8 

15  IS  45-7 

47.2 

15  20  46.4 

15  21  55.5 

15  23  9.6 

10.9 
15  47  37.9 

15  29  29.3 

15  33  22.0 


24.6 


3617 


15  34  55.8 
56.8 

IS  38  45-9 

15  38  58.9 
15  39  10.8 
15  42  5.3 
iz.o 

,5.6 

IS  49  !7-4 
18.4 

20.0 
21.2 
15  50  23.1 


102  28  12 

102  32  37 

96  44  32 

i43  56  5 

55  37 


53  47 

140   4  19 

4  20 
156  16  19 

92  14  35 
140    s  3 

5  * 
165   7  12 

119  59  46 

150  40  ss 


40  47 
39  S3 

127  13  15 
13  17 
H5  57  o 

103  13  32 
118  51  38 
146  56  16 

54  49 

55  14 

150   o  40 
o  41 

°  55 
o  45 
124    3  23 


B;  S;  R;  glbM;  15".    The  preceding  of  2   

F  ;  IE;  glbM;  25".    The  following  of  2  

e  F  ;  S  ;  p  s  b  M  ;  10°   

A  remarkable  cluster,  20'  diam  ;  R ;  very  discrete,  and  composed  of  small 
groups  of  2,  3,  4  stars,  chiefly  11,  12,  and  13  m,  sufficiently  insulated 
from  the  rest  of  the  pretty  rich  neighbourhood  to  be  considered  a  cluster. 

A  most  numerous  and  beautiful  milky  way  group  or  cluster  covering  a 
space  of  1  j  or  2  fields  diameter  (20'  or  30'),  entirely  composed  of  double 
and  triple  stars,  and  distinct  groups  of  4  or  5  nearly  of  a  size  (10  and 
11  m),  on  a  black  ground.    Perhaps  100  or  150  st  in  field. 

cl  VIII.  class.  The  field  uniformly  covered  with  insulated  stars  11  ...  14  m, 
forming  a  rich  cl  of  8th  class,  remarkable  for  the  total  darkness  of  the 
ground  and  absence  of  minute  stars.    Cl  much  more  than  fills  the  field. 

(J);  B;  L;  R;  gbM;  diam  in  R  A  =  16  sec.  Comes  up  to  a  B  blaze 
in  M.    Resolved  by  left  eye.    Stars  17  m. 

;  p  B  ;  fine  highly  condensed ;  vgbM;  3'  diam  ;  clearly  resolved. 
I  see  all  the  stars  (15m)  well. 

F  ;  S ;  among  a  crowd  of  milky  way  stars.  No  doubt  as  to  its  nebulous 
character.    All  that  is  starry  in  field  is  clearly  resolved. 

pB;  S;  R;  gbM;  18"   

Not  v  B  ;  S  ;  glbM;  90" ;  resolved  into  st  16  m,  with  one  of  12  m,  at 
or  a  little  beyond  the  s  p  edge. 

p  B  ;  R ;  v  g  b  M  ;  60"  ;  a  faint  "*  involved   

F;  pL;  R;  vgbM;  z'  

vF;  L;  R;  gbM;  r;  90"  

Planetary  Nebula.  Not  B  ;  p  F ;  S  ;  R ;  with  something  like  a  pro- 
tuberance, which  may  arise  from  an  accidental  star,  on  or  close  to  the 
edge.  Not  quite  sharp ;  a  little  furred  ;  light  not  quite  uniform  ;  an  odd 
sort  of  mottling  like  a  resolvable  light ;  taken  at  first  for  a  v  F  double 
%  out  of  focus;  12"  diam,  but  seen  with  240 ;  320  is  too  high  a  power 
for  it.    See  figure  7,  Plate  VI. 

O  ;  seen,  and  a  diagram  of  the  adjacent  stars  made,  but  the  stars  are  too 
dreadfully  ill  defined  to-night  to  state  any  particulars  further  than  that  it 
is  decidedly  not  a  star,  but  has  a  disc  8"  +  diam. 

O  ;  transit  just  missed ;  R  ;  5"  diam ;  about  equal  in  light  to  a  j|e  9m; 
of  a  feeble  intensity  of  light,  nearly  equable  ;  under  320  it  is  not  nebulous, 
but  indistinct  at  the  edges  ;  a  very  singular  kind  of  appearance — not 
"  mottled,"  not  "  curdled,"  but  yet  not  planetary.  In  a  field  with  about 
100  or  150  st. 

0;  vB;  R;  vgbM;  diam  in  R  A  io! ;  all  stars ;  a  *  10  m  follows 

centre  4'.o,  and  is  involved  ;  3  st  1 3  m  in  M. 
0  ;  fine  object ;  p  g  b  M  ;  diam  is'.o  ;  composed  of  distinct  st  13  . .  15  m ; 

one  sf?  10  m  is  eccentric,  and  3  of  13  m  in  centre  nearly, 
cl  VI.  class.    A  p  rich  1  cl ;  R;  1  comp  M  ;  12';  st  12  . . .  14  m  ;  nearly 

fills  field  ;  M  taken. 

e  F;  S  ;  R;  follows  avS  j)c  ;  25"   

v  F;  S;  R;  sb  M  

cl  VI.  or  VII.  class ;  p  m  comp  ;  irreg  fig  ;  5'  or  6'  diam  >  st  lz  16  m. 

cl;  S  ;  irreg  R  ;  gbM;  a  group,  or  rather  small  oval  p  m  comp  cl  of 

st  16  . . .  17  m.    A  few  =  15  m. 
A  milky  way  cl ;  but  so  densely  concentrated  as  to  merit  notice  as  a  fine 

cl  VI.  class ;  irreg  R  ;  gbM;  st  11  15  m.    [This  obs  makes  the 

minute  of  R  A  41.] 
L,  brill  cl  VII.  class;  fills  field;  not  rich;  st  8,  9,  10,  11  m,  with  smaller. 

Chief  H<  8  m  taken  ;  in  the  southern  part  of  cl. 
VII.;  loose;  sc  ;  brill;  stars  large;  much  more  than  fills  field;  46  st 

counted  above  12  m  ;  chief  sf;  7  m  taken. 

Chief  *  8  m  of  a  coarse,  p  L,  cl  of  st,  8  11m,  which  fills  the  field  

Chief  *  7  m  of  a  L,  oblong,  B,  sc  cl;  st  7  10  m   

F;  S;  R  ;  15";  g  p  m  b  M.    There  are  3  st  forming  a  triangle  about  6o°, 

n  p  the  neb. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


Ill 


No. 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 

cl ;  a  small,  compact,  knot  of  st  1 1 ....  14  m,  in  a  magnificently  full  field 
and  zone. 

The  chief  in  middle  of  a  most  superbly  rich  and  L  cl,  2c/  at  least  in 
diam,  as  it  much  more  than  fills  field  ;  not  m  comp  M ;  st  10. .  . .  12  m. 

Chief  D  star  of  a  superb  cl ;  15'  diam;  g  m  comp  M  ;  irreg  R;  stio..  ..15m. 

Place  of  a  neat  D  star  in  centre  of  a  superb  cl ;  very  L  and  rich  ;  composed 
of  equal  stars  12  m,  a  fine  object.    Much  more  than  fills  field. 

pF;  R ;  vgvlbM;  60";  with  left  eye  slightly  mottled,  but  not  resolved 

e  F;  E;  lbmj  25"  

cl  VIII.  class ;  L  ;  loose  ;  brill ;  irreg  fig  ;  fills  field ;  chief  H<  Y  rn  taken 

cl  VIII.;  L;  coarse;  B;  fills  field;  st  7,  8,  9,  10  m ;  sfc  7'  m  taken. 
N.B. — This  obs  makes  the  minute  of  R  A  5,  instead  of  4. 

0 ;  L;  F;  R;  vglbM;  all  resolved  into  st  15  18  m ;  4'  diam,  with 

stragglers.    A  delicate  and  beautiful  object. 

0 ;  pB;  L;  irrR;  gbM;  resolved  into  st  13  . .  . .  16  m  ;  rich  ;  p  comp  ; 
diam  5'  or  6'  by  estim  ;  50'  +  in  R  A.  A  fine  object.  [N.B. —  This  obs 
makes  the  minute  q/'R  A  7,  instead  of  6.] 

F  ;  L  ;  irr  R ;  v  g  b  M  ;  7'  or  8'  diam  ;  all  res  into  stars   

0;  vB;  R;  svvmbMtoa  blaze ;  diam  in  R  A  =  ios,5.  Stars  15  m, 
all  well  seen. 

0;  v  m  comp  M ;  p  s  v  m  b  M  ;  diam  i2s.o;  st  =  14  m ;  all  resolved. 
Fine  object. 

A  part  of  the  milky  way,  so  immensely  rich  as  to  be  one  vast  cluster  of 
clusters. 

cl ;  B  ;  L ;  loosely  sc ;  not  m  comp  M ;  fills  nearly  a  field ;  consists  of 
about  50  or  60  st  9  ....  1 1  m. 

Viewed ;  a  brilliant  cluster  class  VII.  ;  p  rich  L  ;  irreg  sc  ;  fills  field  ;  st  8, 
9,  10,  11  m. 

A  p  rich,  loose,  L  ;  roundish  cl  of  st  12 ....  14  m  ;  7'  diam  ;  not  m  comp  M 

VII.  class  ;  rich ;  L  ;  g  1  comp  M  ;  irreg  R ;  12';  st  13,  14,  15  m;  nearly 
fills  field. 

pB;  R;  pgbM;  r;  with  left  eye  I  can  barely  discern  a  few  of  the  stars 

B;  R;  p  gb  M;  r;  2'   

vB;  R;  p  L;  pgmbM;  z\.  Evidently  a  0,  but  3  v  B  and  near  full, 
and  I  cannot  see  the  individual  stars. 

B ;  R ;  p  s  b  M  ;  200";  r.  [R  A  by  this  obs  20\5,  but  the  eye-piece  has 
been  considerably  deranged  by  a  blow.] 

p  L  ;  oval ;  g  b  M  ;  resolved  

v  F  and  S  ;  is  pointed  to  by  2  small  stars  9  m  and  14  m  ;  the  sfc  9  m  is  the 
only  one  of  that  magnitude  within  6'. 

A  large  and  coarse  milky  way  cluster,  tolerably  insulated,  composed  of  large 
stars. 

pF;  R;  gpmbM;  45" ;  in  a  field  full  of  small  stars  

p  F  ;  IE;  g  1  b  M  ;  50"  1  

Neb  violently  suspected  immediately  preceding  a  double  star   

F;  S;  IE;  vglbM;  35";  certain  ;  follows  aD  *  

L  irreg  cl  of  loose  st  11  14  m,  which  fills  field ;  place  that  of  a  $  8  m 

in  preceding  part. 

Cluster  ;  place  of  a  H<  H  Normse  in  it  

0 ;  v  rich  ;  gpmbM;  diam  in  R  A  =  20'. o  ;  that  of  the  most  comp 
part  4s.  5  ;  stars  well  separated. 

Middle  of  a  small  group  of  p  B  stars   

Chief  H«  9  m  of  a  S  B  clustering  group  of  from  12  to  20  p  L  st,  with 
stragglers. 

vF;  eS;  R;  gbM;  10"   


Sweep. 


3618 
3619 


3620 
3621 
3622 


3623 


3624 

3625 
3626 

3627 
3628 


3629 
3630 

3632 

3633 

3634 
3635 

3636 
3637 

3638 
3639 


A.  359 
A.  360 


A.  326 


A.  68 


A.  514 


A.  412 


A.  536 


VI.  10 


A.  400 


VI.  40 


15  54  24.1 

H3  33 

24 

15  59  58.2 

143  46  31 

59-5 

45 

30 

45 

30 

16    1  47.0 

125  47 

53 

16   4  37.5 

123  48 

20 

16   4  46.1 

147  28 

0 

497 

28 

4 

16    6  29.7 

161  47 

39 

30.2 

47 

4 

38.3 

16    6  54.8 
55.0 
16  11  24.8 
16  13  58.4 


16  15  3.1 
10.6 

16  16  12.5 

13-9 
14.7 


16  16  53.3 
16  18  9.1 


47  12 
112  33  26 

32  27 

141  32  21 

130  15  46 


138  44  48 
45  36 

128  27  20 
27  10 
26  o 

26  25 

115  38  51 
162  52  58 


16 

J9 

3°-3 

142 

I4 

53 

16 

*9 

57.2 

150 

»3 

31 

61.8 

14  25 

16 

2 1 

IO± 

137 

44 

± 

16 

21 

27.7 

!37 

47 

*9 

16 

2 1 

35-7 

139 

23 

47 

16 

2 1 

59-9 

133 

40 

17 

16 

23 

2.5 

102 

40 

17 

16 

*3 

22.5 

J35 

15 

40 

31. 1 

IS 

4 

16 

23 

41.2 

'59 

1 

0 

599 
469 

696 
694 

79 1 
79 1 
575 
717 

598 

605 

606 
793 


468 

479 
456 

465 
693 

461 
460 
459 

462 

453 
606 

468 

596 

578 
463 
463 
693 

454 

702 

47i 
695 

579 


112 


REDUCED  OBSERVATIONS  OF 


No. 


Svnon. 


R  A.  1830.0. 
h.  in.  s. d. 


N  P  D.  1830.0. 

o        I  II 


Description,  Remarks,  &c. 


Sweep. 


3640 

3641 
3642 

3643 
3644 

3645 
3646 

3647 
3648 

3649 

3650 

3651 
3652 

3653 
3654 

3655 
3656 


Zi.413 


4>  483 


A.  413 


A.  442 


A.  364 


A.  454 


A.  499 
III.  584 

A.  520 


3657     A.  374  ? 


16  27  + 


16  28  18.0 
26.7 
16  28  37.8 

16  31  37.7 
16  33  42.9 
66.0 
16  34  52.8 

16  35  49.6 

60.5 

16  36  29.1 

16  37  9.4 

10.0 
12.3 

16  38  1.5 

7.6 

16  38  32.1 

16  39  46.8 
16  42  8.6 

16  43  13.5 

16  43  58.3 

61.8 

16  45  23.6 
24.5 

16  45  28.8 

30.2 
16  45  41.0 


138  40  + 


133  1  39 
1  27 

138  25  19 

137    8  13 

136  41  55 

42  15 

162  17  8 

143  26  23 

33  42 
148  41  24 

134  25  7 

24  50 
24  42 

148  54  27 
54  57 

!34  25  13 

130  55  24 

131  30  26 

in  52  37 
129  13  9 

12  15 

13  46 

134  29  57 
30  30 

135  38  56 

39  4° 
142  25  50 


The  brightest  part  of  a  v  L,  f,  diffused,  branching  nebula,  which  involves 
in  its  n  f  part  the  *  B  5789,  and  extends  into  the  cl  A  413,  which  it  in 
part  surrounds.  No  doubt  about  the  nebula,  which  in  the  brightest  part 
of  it  precedes  the  cluster  about  i"'  of  time.  The  following  stars  behind 
the  double  and  quite  free  of  nebula.  I  presume  the  neb  and 
cluster  to  be  unconnected. 

A  coarse  but  rich  cl  of  st  11 . .  12  m,  which  leaves  dark  lines  unoccupied, 
forming  sections.    (See  fig.  4,  PI.  V.) 

cl  VII.  p  rich;  irreg  R;  g  b  M;  10';  st  12...14  m;  a  straggling 
group. 

cl  VIII.  class;  consists  of  about  a  dozen  st  10..  11  m,  and  perhaps  as 
many  less,  with  stragglers,  which  fill  field.  In  its  p  part  is  a  fine  D  * 
(place  as  here  set  down),  and  yet  more  p  is  a  v  L,  faint  nebula,  in  which 
the  p  part  of  the  cl  is  involved. 

A  great  space  full  of  milky  way  stars,  so  thickly  sown  as  to  merit  being 
called  a  cluster. 

cl  moderately  comp  VIII.  class  ;  st  11  ...  n  m  ;  sfis  a  brilliant  knot  of 
st,  one  of  which  is  8  m,  and  the  others  9  m. 

A  singular  shaped  cl.  Irreg  R ;  comp  VII.  class,  set  as  it  were  in  a  nearly 
rectangular  frame  of  stars  detached  from  cluster.    See  fig  6,  PI.  V. 

eF;  pL;  vgvlbM;  2'  diam ;  quite  hopeless,  except  in  the  clearest 
and  finest  night,  and  with  the  mirror  bright. 

Found  in  the  place,  and  viewed.  It  is  very  visible,  and  the  P  D  is  right  per 
index. 

A  pretty  insulated  milky  way  cluster,  class  VII.  of  large  stars  ;  8'  diam  ; 
st  9  . . . .  12  m. 

Cluster,  class  VII.  ;  rich  ;  not  m  comp  M  ;  more  than  fills  field.  Stars 
1 1 ....  14  m,  but  chiefly  small. 

p  F  ;  R  ;  v  g  1  b  M  ;  has  a  yellow  jj:  5  m  preceding  it,  im  19s  +,  A  R  A, 
and  3'  or  4'  south. 

A  round  cl  of  st  13  m  ;  g  b  M  ;  4';  with  two  appendages  of  st,  n  and  s, 
making  together  a  long  cluster. 

p  rich ;  R ;  p  comp  M  ;  v  1  b  M  ;  4'  diam  ;  stars  discrete  12 ....  15  m  .... 

A  p  rich  cl  of  S  st,  11  m  and  under,  broken  up  into  2  or  3  groups  ;  fills 
§  of  field. 

0;  pB;  pL;  R;  gbM;  2^';  barely  resolvable   

pF;  L;  R;  glbM;  80"   

0  ;  viewed  in  place,  but  clouded  over  before  any  description  could  be 
made. 

A  v  L,  v  rich  cl ;  not  brilliant ;  not  materially  comp  M  ;  full  20'  diam  ; 
st  12 . .  13  m. 

A  star  5  m  in  a  great  cl,  or  an  immensely  rich  milky  way  patch  

A  fine  B,  L  cl ;  p  rich  ;  class  VII. ;  10';  st  10..  13  m.  Place  of  a  D  ^ 
5  m,  the  p  but  one  of  7  B  st  in  M. 


p  comp  : 
st  14  . . 


S  ;  2'  ;  rather  triangular  than  R ;  m  b  M  ;  resolved  into 
16  m. 


Cluster  VI.  class;  B;  L;  rich;  discrete;  12';  irreg  fig;  vlbM;  fine 
object ;  place  of  a  red  ^  ;m;  rest  11  m;  white. 

A  fine,  L,  rich  cl ;  class  VII. ;  st  9  12  m  ;  fills  field  ;  place  of  a  red 

i|c  8.9  m  in  centre. 

A  p  rich  brill  cl  of  st  10. . . .  12  m,  with  one  7.8  m  near  middle  

cl  VIII.  class  ;  coarse  ;  p  rich  ;  st  9 ....  12  m  

VII.  class;  p  rich;  loose  irreg  fig;  L  and  S  st,  9  15  m;  10'  1, 

7'  br. 

cl  VIII.  class  ;  loose  and  straggling  ;  place  that  of  a  D  He  in  central  more 
condensed  group ;  has  a  *  8  m  s  f ,  5'  dist,  and  another  7  m  more 
remote. 

The  chief  and  central  group  of  a  L  loose  cl,  whose  outlying  st  are  =  S  m, 
the  central  ones  =  12  m;  a  double  sfc  taken. 

A  small  triangular  cl,  2'  diam  ;  st  =  13  m  


693 


455 
454 
693 

463 
463 
695 
605 
606 
468 

599 

717 

463 

472 
454 

712 
582 
717 

455 

456 
479 

588 

461 

462 

456 

454 
472 

463 

464 
468 


NEBULAE  AND  CLUSTERS  OF  STARS. 


113 


riu. 

Synon* 

R  A.  1830.0. 

1\T  "D  Tl    1  fl^ft 
I\  r  1J.  ltsou. 

h. 

m. 

s.d. 

Of" 

3658 

16  48 

7- " 

126  51  0 

8.1 

50  IO 

3659 

M.  10 

16  48 

13.4 

93  48  35 

h.  1972 

3660 

A.  456 

16 

48 

22.0 

134  22  42 

27.9 

24  0 

3661 

M.  62 

l6 

50 

21.9 

119  50  48 

A.  627 

23.6 

50  42 

24.2 

50  18 

2  C  O 

5i  * 

26.6 

51  23 

3662 

A.  521 

16 

CO 
J 

21.0 

129  28  10 

23.2 

27  41 

3663 

M.  19 

16 

7-9 

116    0  51 

h.  1975 

9.8 

0  52 

3664 

A.  556 

16 

53 

14.3 

127  38  12 

3665 

VI.  1 1 

16 

54 

4.0 

114  30  57 

h.  1976 

3666 

TT  mr 
11.  195 

16 

54 

55-3 

1 12  27 

■3  667 

VI.  12 

16 

en 

35.6 

1 1 6  21 

h.  1977 

39.8 

3668 

«7 

I 

3-7 

152  36  49 

4-7 

36  35 

3669 

17 

3 

9.1 

148  58  5 

3670 

I.  147 

'7 

3 

45-7 

119  15  27 

46.4 

14  32 

3671 

I.45 

17 

5 

54.6 

117  56  12 

57-4 

56  17 

3672 

A.  522 

17 

6 

± 

129  15  + 

3673 

17 

6 

35-9 

132  41  33 

37-3 

4i  7 

3674 

17 

7 

0.4 

r54  49  3i 

3-3 

49  9 

Description,  Remarks,  &c. 


0 ;  eF;  vL;  vglbM;  4'  diam  ;  perceived  with  the  utmost  attention 
to  be  resolved  into  v  S  stars  20  m. 

VI.  class.  A  v  L  neb,  or  rather  v  F,  R  cl  VI.  class ;  vF;  irreg  R  ; 
vglbM;  4'. 

0  ;  fine,  L  ;  R  ;  B  ;  g  m  b  M  ;  diam  5' ;  with  stragglers,  several  of  which 
are  of  larger  sizes,  to  about  12'  diam  ;  all  resolved  into  st  11 ....  15  m, 
very  comp. 

A  superb,  v  L,  v  rich  cl,  which  fills  field ;  R  ;  vglbM;  st  11..12  m, 
thickly  sown  at  intervals  from  each  other  from  10"  to  20". 

v  L ;  v  rich  ;  fills  more  than  a  field ;  has  one  or  two  straggling  appendages 
p  and  s  ;  stars  11  and  12  m,  nearly  equal. 

0  ;  B;  L;  R;gmbM,  but  not  to  a  nucleus  ;  st  15  m  ;  v  fine  ;  diam  in 
R  A  =  i3*.o.    [Semi-diam — See  f  794.] 

0  ;  superb  ;  vB;  R;  psvmbM;  about  7'  diam  ;  all  resolved  into 
stars  15  m,  very  equal. 

0  ;  vB;  L;  R;  pgvmbM;  perfectly  resolved  with  left  eye,  hardly 
with  right.  The  most  condensed  part  is  a  perfect  blaze,  but  not  quite  in 
the  centre.  The  southern  part  runs  out  farther.  A  beautiful  object. 
(See  figure  13,  PI.  VI.)  Diam  =  13  . 5  in  R  A.  [No  doubt  semi- 
diameter.'} 

0;  vB;  L;R;  g  v  m  b  M,  to  a  blaze  ;  diam  in  R  A  =  27!.o  ; 
st  14. ...  16  m  ;  superb. 

B  ;  L  ;  R  or  1  E,  towards  the  n  f  side,  where  there  is  even  some  feeble 
appearance  of  another  centre  of  condensation  ;  p  s  b  M,  almost  to  a 
nipple  ;  st  15  m. 

cl ;  rich  ;  p  L  ;  brilliant ;  8' ;  st  irreg  sc  10  . . .  12  m  ;  place  of  a  D  s(;  in 
the  following  angle  of  a  triangular  condensed  group. 

A  p  rich  irreg  cl  of  nearly  =  st  10  m  ;  not  m  b  M  ;  7'  

0  ;  v  B  ;  R  ;  diam  10' ;  resolved  into  st  16  m   

Superb  0  ;  g  m  b  M,  but  not  to  a  nucleus  ;  diam  of  B  part  =  i2'.o,  of 
whole  cl  to  edge  =  iy\o  ;  resolved  into  st  14,  15,  16  m. 

A  p  rich,  L,  p  B,  cl  VII.  class,  of  loose  st  9,  10,  11  m,  which  fills  §  of 
field. 

0  ;  B  ;  R  ;  g  b  M  ;  diam  =  j\o  ;  resolved  into  st  16  m   

0  ;  irreg  R ;  gpm  comp  M  ;  3'  diam  ;  barely  resolved  into  st  16  .  .  .  18  m. 

0  ;  B  ;  R ;  psbM;  diam  j\o  ;  resolved  into  st  16  m   

0;  pB;  R;  psvmbM;  3^';  resolved  into  st  15  . .  16  m   

F;  RorlE;  vglbM;  diam  in  R  A  =  23s. ;  has  in  it  2  stars  and  a  3rd, 
with  2  or  3  more  outlying. 

F;  vL;  R;  vgvlbM;  3';  has  several  stars,  one  =  1 1  m ;  involved 
but  being  on  a  rich  ground  there  appears  no  connection. 

vF;  vS;  R;  glbM;  12"  

0  ;  B  ;  R;  g  b  M  ;  diam  in  R  A  =  6\o;  res  into  st  16  . .  .  17  m  

B  ;  R ;  at  first  s,  then  vglbM;  brighter  part  2'  diam  ;  but  there  is  a 
much  fainter  portion  which  extends  a  good  deal  further  ;  st  16  .  .  .  17  m. 

0;  pB;  S;  R;  pgvmbM;  2';  resolved  into  st  16 . .  17  m  

0;  B;  R;  gbM;  r;  90"  ;  has  2  small  st  very  near  

cl  VII.  class.    Rich  ;  pL;  R  ;  gbM;  st  12 . . . .  14  m  ;  not  a  0  

Coarse  B  cluster  VII.  mainly  included  within  an  equilateral  triangle  formed 
by  3  B  st  5  and  6  m.    The  n  f  of  these  taken. 

v  L  cl  VII.  class,  of  loose  st,  on  a  v  rich  ground  of  S  st.  The  chief  *  > 
6  m,  at  the  n  f  edge  taken. 

vF;  vS;  IE;  lbM;  15"  1,  12"  br  

v  F;  R  ;  gbM;  15"  

G  G 


114 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


3675 


3676 
3677 

3678 


3679 
3680 


M.  9 
h.  1979 


3681 
368a 

3683 

3684 


3685 
3686 

3687 


I.  46 


I.  48 
A.  225 


IV.  11 
h.  1981 


E  A.  1830.0. 
h.  m.  s.  d. 


17     7  17.4 


17  7  41.6 
17     9  12.4 

17     9  30.4 

32.2 

17  9  <M± 
17  10  35.8 

37.0 

37.6 

17  13  24.6 
17  13  29.2 

17  :3  38-5 

17  14  17.2 

19.5 
17  14  33.2 

17  14  33.1 
17  19  2.0 

17  21  0.7 


N  P  D.  1830.0. 


141  33  8 


33  40 


113  33  43 
108  20  55 

125   52  36 

S3  12 

123  58  ± 
128  17  42 


17  50 

116  10  50 
124    1  14 

107  38  30 

156  54  28 

53  37 
132  39  37 

119  49  47 
113  36  35 

122  27  15 


Description,  Remarks,  &c. 


Planetary  Nebula.  A  perfectly  uniform,  quite  round,  planetary  disc  ; 
like  a  star  out  of  focus.  A  very  little  uncertain  at  the  edges,  like  a  star 
on  a  dewy  unsettled  calm  night,  when  the  stars  look  large  without  being 
decidedly  ill  denned.  Diameter  =  5";  light  =  a  9.10  m.  There  is 
positively  no  bright  point  in  the  centre.  It  has  two  very  small  attendant 
stars,  one  14  m  ;  pos  from  centre  =  3 520. 3,  dist  from  edge  =  5  diam  ; 
the  other  also  14  m,  pos  96°.7  dist  from  edge  =  15  diam.  Occurs  in 
a  field  full  of  milky  way  stars.  [N.B. — Referring  to  the  description 
of  A  381,  I  see  no  ground  to  suppose  that  this  can  by  possibility 
have  been  the  object  intended  by  that  place  and  description.  At  all  events, 
the  remarkable  planetary  character  has  escaped  notice  by  the  author  of 
that  description.]    See  fig.  6,  PI.  VI. 

O  ;  delicate ;  F ;  v  S ;  diam  =  6"  or  7" ;  exactly  R ;  perfectly  uniform 
[as  respects  the  graduation  of  the  light  from  the  centre  to  the  edges] ,  but 
the  light  a  very  little  curdled.  Not  the  slightest  haziness,  but  like  a  star 
out  of  focus.  320  shows  rather  more  fur  at  the  edges  than  I  think  it 
would  to  a  planet  of  equal  size  and  light.  Its  light  is  =  a  s|e  10. 11  m. 
It  would  be  quite  useless  to  look  for  this  object  under  less  favourable  cir- 
cumstances— of  instrument  and  sky.  A  night  of  gloriously  perfect  defini- 
tion !  It  is  in  a  very  rich  place.  There  are  40  or  50  small  stars  in  field. 
Measures  of  the  two  companions  ;  1st  pos  =  35i°.o,  dist  =  1  diam  from 
edge,  sfc  =  14  m  ;  2nd  pos  =  9i0-4,  dist  =  f  diam,  #  =  13  m.  Showed 
it  to  my  attendant,  J.  S.,  who  saw  it  well. 

Viewed.  I  can  barely  discern  that  the  attendant  stars  are  as  in  f  599,  but 
it  is  so  faint  that  (the  stars  being  all  blotty  and  dreadfully  defined)  I  could 
not  be  sure  it  was  the  object,  till  too  late  to  take  its  R  A  and  P  D  on  the 
wires.  However,  it  was  just  in  the  middle  of  the  field  at  the  time  ex- 
pected, and  set  to  the  place  at  once. 

p  F  ;  R  ;  g  b  M  ;  r  ;  60".    No  doubt  it  is  a  0   

0 ;  B  ;  R ;  g  m  b  M  ;  4';  resolved  into  st  14  m  

p  B  ;  v  L  ;  v  irr  oval,  in  which,  though  excentric,  is  a  8  m,  whose  place 
is  that  taken.    One  side  of  the  neb  is  brighter  than  the  other. 

v  F ;  v  L ;  v  g  1  b  M  ;  5'  1 ;  4'  br  ;  out  of  M  is  a  *  8.9  or  9  m,  whose 
place  is  taken.  The  densest  part  of  the  nebula  follows  this  *  4s.  5  on  the 
same  parallel. 

The  whole  lower  end  of  the  zone  is  strongly  affected  with  nebulous  patches 
Annular  Nebula.    A  delicate,  e  F,  but  perfectly  well  defined  annulus 

15....  20"  diam.   The  field  crowded  with  st,  two  of  which  are  on  the  neb. 

(See  fig.  3,  PI.  VI.) 

A  beautiful  delicate  ring,  of  a  faint  ghost-like  appearance,  about  40"  diam  ; 
in  a  field  of  about  150  st,  11  and  12  m  and  under.  In  it  is  one  j|s  12  m 
very  conspic,  and  one  15  m  much  less  so.  Near  it  are  2  st  14  and  15  m, 
and  s  of  it  at  dist  60"  is  another. 

e  e  F  and  difficult  object ;  among  a  crowd  of  milky  way  stars.  My  attend- 
ant, J.  S.,  saw  the  darkness  in  the  centre  and  the  stars  as  described. 
[N.B. — Set  by  working  list  to  P  D  of  last  f,  and  entered  the  field  bisected 
by  the  horizontal  wire.] 

v  F ;  L  ;  R  ;  g  b  M  ;  2'  diam  ;  res  st  1 8  m   

F;  L;  E;  vglbM;  milky  nebulosity  ;  2'  1 ;  1^'  br  ;  close  to  and  almost 
involves  a  D  sjc . 

0 ;  vB;  R;  vgvmbM;  90" ;  resolved  into  stars  barely  discernible  with 
left  eye.    A  beautiful  softly  shaded  object. 

0 ;  B;  L;  R;  vgmbM;  diam  in  R  A  =  50' ;  diam  7'  or  8';  stars  all 
seen,  12. ...  16  m  with  outliers  extending  a  good  way. 

0  ;  irreg  R  ;  p  B  and  L  ;  g  b  M ;  4';  all  sharply  resolved  into  stars  14. .  17  m 

The  edge  of  the  milky  way  is  here  quite  sharp  and  definite,  forming  a  tele- 
scopic promontory  and  bays,  all  above  which  is  a  mass  of  stars,  and  all 
below  vacant  to  some  considerable  distance.    See  PI.  V.,  fig.  3. 

A  portion  of  the  milky  way  which  is  decidedly  nebulous,  and  by  no  means 
rich  in  L  stars.    The  nebula  is  in  patches  of  very  great  extent. 

Annular  Nebula.  Exactly  round  ;  p  F  ;  12"  diameter  ;  well  terminated, 
but  a  very  little  cottony  at  the  edge,  and  with  a  decided  darkness  in  the 
middle ;  =  a  *  10  m  at  the  most.  Few  stars  in  the  field  ;  a  beautiful 
specimen  of  the  planetary  annular  class  of  nebulas,  (fig.  4,  PI.  VI.). 

Cluster  VIII.  class ;  3'  or  4'  in  extent ;  a  bright  *  (=  B  6125)  taken  


Sweep. 


789 


599 


7H 


699 
791 
792 


794 
461 


718 
462 

453 

792 

699 

612 

709 
454 

478 

793 

794 


NEBULAE  AND  CLUSTERS  OF  STARS. 


115 


No. 


bynon. 


3688 


3689 


3690 


A.  457 


3691 
3692 


A.  366 


3693 
3694 

3695 
3696 
3697 

3698 

3699 
3700 

3701 

3702 


A.  568 

I.  44 
h.  1982 

M.  14 
h.  1983 


M.  6 


A.  612 


3703 
3704 


R  A.  1830.0. 
h.  m.  s.  d. 


17  22  43.1 

17  23  36.2 
36.6 
17  23  51.6 

52.O 


17  24  37.6 
38.7 

17  26  50.4 


5 1-9 


17  26  51.1 
17  27  2.8 

17  27  33+ 
17  27  59.9 
17  28  14.4 

!7-3 
17  28  41.0 

17  28  58.6 
17  29  31.9 

17  29  55.0 
17  32  4; 
17  33  6.2 
17-5 

17  34  31.4 


17  35  59.8 
'7  37  39- 


N  P  D.  1830.0. 


128  56  33 

122  26  31 
27  50 
134  36  26 

37  48 


159  39  42 
40  19 

H3  34  >5 
33  za 


124  53  31 
151  34  5i 

1 5 1  34  51 
126  49  53 
113  47  46 
47  49 
93    7  55 

122  5  52 
150  38  31 

175  23  48 
124  55  30 

122  14  33 
17  15 

123  36  35 


121  27  4 
125  22  + 


Description,  Remarks,  &c. 


A  star  9  m,  with  an  extremely  F  nebulous  wisp  or  tail,  extending  north- 
wards about  1'. 

A  star  9  m,  with  a  very  evident  e  F  nebulous  wisp  90"  1 ;  30"  br.  [The 
wisp  by  the  diagram  is  fan-shaped,  and  extends  in  the  n  p  direction  from 
the  star.    See  fig.  18,  PI.  VI.]. 

A  star  7  m  with  a  cl  of  st  12  m  assembled  about  it.  The  great  *  occupies 
the  centre.    A  very  remarkable  object. 

A  curious  cluster  consisting  of  one  L  jfc  6.7  m,  and  some  15  or  20  small 
ones  13  m  clustering  close  around  it. 

®  ;  v  B  ;  R  ;  first  p  g,  then  p  s  v  m  b  M  ;  4'  diam  ;  easily  resolved  with 
left  eye  into  st  17  m;  more  difficultly  with  right  eye  into  18  m  ;  exces- 
sively close  and  comp  ;  shading  off  insensibly  in  borders  into  the  general 
ground  of  the  heavens. 

fj) ;  v  B ;  R ;  at  first  p  g,  then  p  s  v  m  b  M  to  an  intense  almost  nuclear 
light.  The  right  eye  does  not  resolve  or  barely  makes  it  resolvable  ;  the 
left  resolves  it  completely  into  stars  17. .  .  .20  m.  A  superb  object  on  a 
rich  ground  of  milky  way. 

pF;  S;  R;  glbM;  20";  50  stars  in  field  

F;  S;  R;  glbM;  20";  has  a  13  m  s  p  (one  radius  of  neb  from  edge 
by  diagram.) 

(J)  ;  fine,  L  ;  B  ;  R  ;  g  b  M  ;  not  v  comp  ;  5'  diam,  but  stragglers  extend 
a  great  way.  In  M  is  a  more  comp  group  of  much  smaller  st.  The  stars 
at  circumference  are  larger  than  in  M  ;  at  n  f  border  is  a  D  sj: . 

Beautiful  (f) ;  L,  rich,  somewhat  coarse ;  10'  diam  taking  in  all  outliers ; 
rather  irreg  R ;  v  m  comp  M  where,  however,  the  st  are  v  S,  while 
every  where  else  they  are  13  m. 

Viewed  past  merid ;  a  fine,  L,  rich  cl ;  not  v  m  comp  stars  13  m.  In  the 
s  f  part  is  a  delicate  double  Hs  • 

Cluster  VIII. ;  small;  5';  place  of  chief  D  s|c  

e  F ;  S ;  R ;  almost  certain  it  is  not  a  small  D  % .  Definition  much  im- 
proved. It  is  certainly  a  nebula,  and,  with  long  attention,  I  see  another, 
still  fainter,  exactly  on  parallel,  and  30'  follows. 

e  e  F.    The  following  of  2   

Cl  class  VII.  p  rich  ;  pL;  irr  R  ;  8' ;  st  9  . . .  10  m  

pB;  R;  vgbM;  25";  asjs  13m  involved,  following  the  centre  

pB;  R;  vgbM;  2';  has  a  H<  1 1  m,  rather  following  the  middle  

A  most  beautiful  and  delicate  ®  ;  not  v  B,  but  of  the  finest  star-dust ;  all 
well  resolved,  especially  with  the  left  eye  ;  v  g  m  b  M  ;  diam  in 
R  A  =  15  sec;  excessively  rich.    All  the  stars  =  and  15  or  16  m. 

Chief  *  7  m  of  a  fine  L,  discrete  cl  of  st  10  11  m  ;  one  sjc  is  7  m, 

one  7.8.    Fills  field  ;  VIII.  class. 

e  F;  S  ;  R;  1  b  M  ;  15";  near  3  st  

Found  in  place,  and  seen  as  described  

pB;  R;  vgbM.    RA  rudely  taken,  and  may  be  very  erroneous. 

A  great  Nebulous  projection  of  the  milky  way  

Cl  class  VIII.  of  st  11  m  ;  fills  field  ;  not  rich  ;  stars  in  zig-zag  lines  .... 

Coarse,  rich,  v  L  cluster.  More  than  fills  field.  Stars  8 ....  12  m  ;  one  of 
8  m  taken. 

A  most  remarkable,  well  insulated,  semi-nebulous  milky  way  patch  of  a 
branching  rounded  fig. ,  within  the  limits  of  the  field,  quite  insulated  on 
the  p,  n,  and  f  side,  and  only  connected  on  the  S  side  by  a  narrow 
isthmus  with  a  branch  of  the  milky  way,  which  runs  meridionally  to  a 
great  extent.  It  forms  a  VI.  class  cluster  of  the  utmost  tenuity,  barely 
resolvable,  not  resolved.    See  fig.  1,  Plate  V. 

Small  cl  VIII.  class  ;  8'  diam  ;  has  20  or  30  st  10. .  . .  12  m,  nearly  insu- 
lated. 

A  very  decided,  tolerably  defined  semi-nebulous  mass  in  milky  way,  with 
abundance  of  v  S  st,  forming  altogether  a  telescopic  magellanic  cloud. 
It  fills  about  a  field,  and  has  branches  and  sinuses,  and  is  altogether  a 
very  remarkable  object. 


Sweep. 

718 
462 

791 
478 
463 

455 

597 
598 

468 
789 


79 1 
716 


716 
461 
453 

793 


478 

480 
481 

595 
791 

478 

794 

792 


478 
79 1 


116 


REDUCED  OBSERVATIONS  OF 


No. 


37°5 


3706 
3707 


3708 
3709 

3710 


3711 
3712 
3713 


3714 
3715 

3716 


3717 
3718 


3719 
3720 


3721 
3722 


A-  557 


A.  597  ? 
VI.  13 


m.  7 ; 


A.  460  ? 
A.  461 ? 


IV.  41 
h.  1991 


II.  199 
I.  49 


VII.  7 

M.  8 


E  A.  1830.0. 
Ii.  m.    s.  d. 


17  38  38.5 


40.2 

17  38  55± 
17  39  40.2 

50.0 

'7  4°  °zh 

17  40  ± 
17  4°  37± 

17  42  39.6 


17  42  41. 1 

17  43  o± 

17  43  8.3 
17  43  40.9 

17  44  28.8 

17  45  27.2 

17  46  40.0 

40.5 

17  47  19.5 
21. 1 

17  47  57-5 


17  49  20.0 
17  52  4.9 
6.6 


17  52  34.9 
35.8 
17  52  41.7 

41.9 

17  52  43.0 
17  53  25.1 
27.6 


53  3°  ' 


N  P  D.  1830.0. 


126  59  10 

59  ifi 

124  48  + 
120    9  45 

9  11 

118  42  + 

124  34 

125  20  -t- 

124  46  21 

45  4° 

112  16  46 

"9    5  ± 

!53  37  31 
120  23  22 

120  19  37 

156  24  18 

134  13  18 

13  37 

155  23  29 
23  47 

119  22  49 

114  38  4 

113  1  21 

1  32 


98  55  52 
56  58 
120    1  12 


117  53  " 
114  21  o 
21  4 

21  13 


Description,  Remarks,  &c. 


0 ;  v  B ;  R ;  v  g  b  M,  up  to  a  blaze.  In  field  with  y  Telescopii,  and 
nearly  on  the  same  parallel ;  with  left  eye  I  barely  see  it  resolved  into 
st  18  or  20  m.  The  whole  ground  of  the  heavens,  for  an  immense 
extent,  is  thickly  sown  with  such  st.    A  beautiful  object. 

0  ;  B ;  R ;  90" ;  v  g  b  M  ;  r  (barely  so)  ;  a  very  regularly  graduating 
neb  or  cl ;  in  field  with  y  Telescopii. 

A  v  fine  L,  rich  sc  cl  of  st  12. .  13  .  .m  ;  P  xvii.  254  

p  rich ;  irreg  R ;  st  13  m ;  a  cluster  with  a  great  black  cut  across  it ; 
6'  diam,  with  many  outliers. 

A  remarkable  cluster,  divided  into  two  by  a  broad  vacant  straight  band ; 
irreg  R  ;  8'  diam  ;  st  12  .  .  .  15  m.    See  fig.  5,  PI.  V. 

Here  begins  an  enormous  region  of  stars,  crowded  beyond  counting,  in  the 
milky  way. 

A  highly  condensed  nebulous  mass,  3'  diam,  or  an  irreg  R  neb  ;  p  m  b  M  ;  r. 

A  very  extensive  nebulous  clustering  mass  of  the  milky  way.  The  stars  of 
excessive  smallness,  and  infinite  in  number. 

A  brill  coarse  cl  VIII.  class,  of  about  60  st  7.8 . . . .  12  m,  which  fills  field. 
Irreg  fig.    A  *  8  m  taken. 

cl  VIII.  Very  fine  and  brilliant ;  stars  of  very  large  and  mixed  magnitudes. 
Fills  field. 

A  pretty  rich  insulated  milky  way  cluster  ;  place  of  a  coarse  double  s|;  in  it. 
The  milky  way  hereabouts  is  very  poor. 

Nebula.  No  description.  It  is  probably  only  a  nebulous  portion  of  the 
milky  way. 

F ;  S  ;  E  ;  b  M  ;  between  2  st  10  m  450  s  p  and  n  f  (diagram)  

An  extraordinary  B  nebulous  portion  of  the  milky  way,  on  a  black  ground 
v  L  ;  an  angle  taken  where  there  is  a  s|j  12  m.  [See  fig.  2,  PI.  V.,  copied 
from  a  diagram  made  at  the  time,  which  represents  this  remarkable  and 
instructive  object  as  marked  by  a  well  defined  contour.] 

The  milky  way  here  is  so  sharply  terminated,  that  the  southern  half  of  the 
field  has  few  stars,  while  the  northern  is  so  full  as  to  be  almost  nebulous. 

p  F  ;  S  ;  p  m  E,  in  direction  of  the  parallel ;  precedes  a  12  m,  which  is 
all  but  involved. 

A  distinctly  nebulous  insulated  group  ;  m  E  ;  2'  1 ;  90"  br  ;  many  stars  of 
considerable  size,  mixed. 

cl  v  rich  ;  irreg  R,  inclining  to  triangular  ;  v  g  1  b  M ;  4'  or  5'  diam  ;  with 
many  large  and  small  st  in  it.  Nebulous. 

v  F  ;  30" ;  involves  2  or  3  stars  

The  following  star  (14  m)  of  av  F  double  *  11  m  is  nebulous.  The  nebula 
is  excessively  faint,  but  I  am  sure  of  its  existence.  The  preceding  star 
is  free. 

The  southern  extremity  of  a  great  nebulous  promontory  of  the  milky  way, 
which  projects  into  the  field  as  the  Cape  of  Good  Hope,  on  a  map,  does 
into  the  southern  ocean. 

A  very  loose  but  very  rich  cluster,  which  fills  many  fields.    Stars  small . . 

The  triple  star  in  the  tririd  nebula   

One  of  the  most  remarkable  nebulae,  and  must  be  very  carefully  delineated. 
It  is  very  large,  and  has  many  outlying  portions  and  sinuses.  See  fig.  2, 
PI.  II. 

pB;  R;  gpmbM;  40"  

0  ;  F  ;  R  ;  p  s  b  M  ;  90" ;  r  ;  with  left  eye  I  discern  the  stars  in  it  .... 
0  ;  B;  R;  gvmbM;ina  nebuloid  portion  of  the  milky  way ;  resolved ; 
stars  16 . .  17  m. 

0  ;  p  B  ;  S  ;  R  ;  80" ;  resolved  into  st  16  m.  (See  the  remark  on  II.  200. 
R  A  17"  54'"-) 

A  pretty  compact  cl  class  VII.  of  st  9 ....  13  m ;  irreg  sc  diam  4'  

A  H«  6  m  (A  c  2074)  within  the  arch  of  the  great  nebula  MS  

A  noble  nebula ;  to  be  monographed.  The  star  taken  is  A  c  2074  =  9 
Sagittarii  7  m.  It  is  followed  by  a  great  cluster  VI.  13  of  which  with 
the  nebula  fills  many  fields. 

Superb  nebula.    The  star  A  taken.    See  PI.  I.  fig.  1   


NEBULiE  AND  CLUSTERS  OF  STARS. 


117 


3723 


3724 
3725 

3726 


3727 


3728 
3729 
3730 

3731 


3732 

3733 
3734 


3735 
3736 


3737 

3738 
3739 


3740 
374i 


II.  200 


A.  569 


A.  473 


VI.  12 


h.  ic 


VII.  30 
h.  1998 

II.  201 
A.  619 


A.  376 


VII.  31 
h.  2001 


VIII.  15 


R  A.  1830.0. 
h.    m.  s.d. 


17  53  54.2 
58.3 

17  54  ± 
17  54  14.4 
17. 1 

17  55  39.8 

41.0 

17  55  52.2 

17  56  50.7 
17  56  58.1 
17  58  52.5 

17  59  13. 1 

15.8 

16.6 
17  59  16.7 

17  59  34-4 

18  o  48.2 

48.6 

18    2  32.8 

18  2  35.1 
36.7 
36.8 

18    5  0.6 
0.9 

18  s  3.1 
18    5  34.1 

18    8  io± 

18    8  33.3 

18  8  52.4 
54.8 


N  P  D.  1830.0. 


120  2  58 
3  36 

126  18  ± 

114  19  II 

20  34 

133  44  31 

42  17 

153  47  3° 

166  36  50 

113  14  - 

115  56  23 

121  46  42 

46  29 

47  41 
117  32  38 

114  7  47 
123  54  15 

53  6 


in  39  27 

121  51  39 

50  52 

51  18 
51  30 

142  16  o 

15  14 

!53  51  44 

112  11  2 

121  59  55 

102  17  40 

153  17  42 

19  5 


Description,  Remarks,  &c. 


0;  p  B;  R;  g  b  M;  resolved  into  st  16..  17  m;  in  a  nebuloid  of  the 
milky  way. 

0  ;  B  ;  S  ;  R  ;  gib  M"  ;  resolved  into  st  16  m.  Both  this  and  I.  49  occur 
on  a  ground  so  astonishingly  rich  and  stippled  over  with  stars  17  m  indi- 
vidually discernible,  as  hardly  to  admit  a  pin's  point  between  the  stars, 
and  this  fills  more  than  the  whole  field  or  many  fields. 

A  large  milky  way  patch,  much  compressed,  one  portion  much  more  so ... . 

CI  L  and  B  ;  just  fills  field ;  a  D  *  taken.    This  cluster  follows  M  8   

A  B,  p  Rich,  irreg  R  cl ;  place  that  of  a  double  sfc  in  the  following  part  of 
the  cluster,  which  is  itself  involved  in  the  great  nebula  M  8. 

0 ;  B  ;  R  ;  g  b  M  ;  diam  in  R  A  =  6s.o ;  easily  resolvable.  The  left  eye 
resolves  it.    [Query  semi-diameter.] 

0;  B  ;  R ;  e  comp  ;  v  Fine ;  diameter  of  most  comp  part  =  ir.o  of  time 
inRA;  st  15  . .  16  m.  The  scattered  stars  extend  to  three  times  the 
diameter  and  die  away  very  gradually. 

e  e  e  F ;  vvvS;  R;  4".  This  is  the  smallest  nebula  I  recollect  to  have 
seen.  Its  light  is  not  greater  than  that  of  a  $z  14  m.  A  diagram  made 
for  security  of  finding  it  again.  See  fig.  16,  PI.  VI.  No.  1  =  10  m; 
2  =  3  =  12m;  4  =  13m;  5  =  6  =  7=i4m;8=i6m. 

v  F;  R;  gib  M;  15"  

The  middle  of  a  great  and  rich  cluster  in  the  milky  way   

0 ;  v  F  ;  a  little  oval ;  vglb  M;  barely  r ;  st  20  m ;  one  Hs  14  m;  diam 
in  R  A  =  7*.5. 

0  ;  p  B  ;  irreg  R ;  g  m  b  M  ;  composed  of  st  16  m,  on  a  milky  way  ground 
of  mixed  L  and  v  S  stars.  [P  D  by  obs  120,  but  this  is  an  obvious  mis- 
take, as  both  the  other  obs  make  it  121.] 

0;  pB;  R;  gbM;  80";  resolvable  or  resolved  in  a  field  very  full  of 
milky  way  stars. 

0  ;  not  vB;  R;  glbM;  2';  resolved.  The  stars  barely  discernible  . . 
Cl  VI.  An  oval  patch  comprised  within  limits  of  the  field,  barely  resolvable 

into  infinitely  minute  points,  but  which,  without  attention,  appears  as  a 

great  neb  1 5'  Ij  12'  br  ;  hardly  b  M. 

vF;  L;  oblong;  5'  1 ;  3'  br;  place  of  a  D  H«  involved;  6  other  st  near. 
Query,  if  involved. 

Planetary  Nebula  ;  1  elliptic  ;  hazy  at  borders  ;  seen  as  last  night.  [See 
next  obs.] 

A  L,  F,  oval,  Planetary  Nebula,  about  60"  1 ;  50"  br ;  or  55";  con- 
siderably hazy,  or  rather  indistinctly  terminated  at  the  borders,  but  not 
b  M  ;  a  star  6.7  m  precedes  it,  just  1  diameter  of  the  field  and  nearly  in 
the  parallel. 

Cluster  VIII.  class  ;  loose  ;  sc  ;  fills  field  ;  is  decidedly  richer  than  any  part 

of  the  milky  way  that  has  occurred  to-night. 

0;  pB;  L;  R;  glbM;  4'  diam  ;  resolved  into  st  1 5  m   

0;  vB;  L;  R;  gbM;  3';  resolved.    In  milky  way  

0;  pB;  R;  vglbM;  3^';  resolved  

Found  in  equatorial  in  a  zone  review  for  double  stars,  where  it  appeared  as 

a  F  R  neb  t'  diam.    July  16,  1836. 

0  ;  B  ;  R  ;  g  m  b  M  ;  entirely  resolved  into  st  16  m  ;  easily  seen  

0 ;  p  B  ;  R;  g  p  m  b  M  ;  25'  or  3'  diam  ;  easily  resolved  with  left  eye  into 

st  15  m. 

e  F  ;  S  ;  among  st.    A  *  6' m  s  p  10'  distant  

Oblong  cluster,  not  v  rich  nor  v  comp,  but  well  insulated;  st  13  m  ;  5'  1 ; 
4'  br. 

Milky  way  superb.  I  cannot  count  the  field,  but  by  estimating  the  number 
in  a  small  space,  there  can  hardly  be  less  than  1000  stars  in  it.  By  the 
best  judgment  I  can  form,  they  are  not  more  than  20"  asunder. 

A  poor  cl  class  VIII.  having  coarse  stragglers  to  a  great  distance.  The  chief 
s|e  7' m  taken. 

F;  S;  R;  p  gb  M;  15"  

eF;  S;  R;  orvlEjvlbM;  it  follows  a  H«  9  m  about  7  or  8s  of  time, 
and  is  about  3'  S  of  it. 


Sweep. 


794 
478 

792 
453 
474 

455 

454 

600 

607 
793 
453 

794 

619 

478 
723 

793 
792 

79 1 


478 
619 
794 

46  8 

789 

708 
793 

478 

617 

708 
600 


H  II 


lis 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R  A.  1830.0. 

N  P  D.  1830.0. 

h. 

m. 

s.  d. 

0 

18 

12 

44.2 

120 

25  32 

A7.0 

26  48 

47-3 

26  4 

18 

4.6 

114 

57  1 

18 

iS 

24.0 

113 

17  19 

18 

16 

20.2 

153 

23  18 

18 

17 

A.2.7 

102 

18 

20 

14.  I 

122 

27  CI 

16.3 

27  II 

_  f_  _ 
ID.7 

27  43 

18 

20 

254 

i«5 

35  57 

18 

21 

36.2 

113 

35  23 

18 

23 

22.8 

163 

24  7 

18 

■^4 

A  6 
4,u 

30  43 

iS 

24 

3I-S 

123 

6  40 

72.7 

C  47 

35.0 

6  43 

36.9 

6  1 

.... 

6  30 

jg 

26 

4.1 

114 

a  13 

4.6 

2  7 

18 

27 

27.1 

98 

21  19 

18 

29 

13.8 

152 

26  55 

14.0 

27  16 

18 

32 

5-7 

122 

26  46 

8.3 

26  35 

8.8 

26  54 

iS 

32 

9.9 

155 

21  25 

12.8 

20  26 

iS 

35 

53.8 

99 

33  39 

18 

37 

32.9 

H7 

29  36 

Descriplion,  Remarks,  &c. 


3742 


3743 


3744 


3745 
3746 

3747 


3748 

3749 

375° 
3751 

3752 


3753 


3754 
3755 
3756 

3757 

3758 
3759 


I.  50 


M.  28 
h.  2010 

II.  204  ? 


M.  69 
A.  613 


I.51: 


II.  205 
h.  2012 


A.  607 


M.  22 
h.  2015 


VIII.  12 


M.  70 
A.  614 


0  ;  vB;  R;  psvmbM;  diam  in  R  A  =  5*.o ;  all  clearly  resolved  into 
stars  barely  discernible. 

0;  B;  S;  R;  psmbM;  diam  6s  in  R  A ;  barely  resolved  so  as  to  be 
sure  it  consists  of  stars. 

0  ;  B  ;  R ;  at  first  g,  then  psvmbM;  3^'  or  4'  diameter  ;  clearly  re- 
solved into  st  16  m  ;  a  fine  object. 

0  ;  v  B  ;  R  ;  v  m  comp  ;  g  b  M,  but  not  to  a  nipple  ;  diam  in  R  A  =  i2'.o ; 
resolved  into  st  14. ...  16  m  ;  a  fine  object.  Occurs  in  the  milky  way,  of 
which  the  stars  here  are  barely  visible  and  immensely  numerous. 

p  B  ;  v  S  ;  4"  at  the  utmost  in  diameter ;  a  good  deal  furry  at  the  edges, 
and  ?  if  not  a  little  brighter  in  M.  It  is  not  a  "  Stellar  Nebula,"  but 
rather  a  link  between  a  O  ar>d  a  0  ;  is  probably  a  v  distant  and  highly 
comp  0  ;  has  a  *  9  m  ;'  dist,  s  f ;  night  superb  and  vision  perfect.  This 
is  one  of  the  smallest  if  not  the  very  smallest  nebulous  object  I  remember 
to  have  seen.    It  is  a  very  remarkable  object. 

pF;  S;  R;  gbM;  15"  

cl  VII.  class  ;  p  rich  ;  5' diam,  with  appendages,  st  12....  15  m.  Much 
richer  than  any  part  of  the  milky  way  seen  to-night. 

0  ;  B  ;  R ;  v  g  b  M  ;  resolved  into  st  14 . .  15  ;  diam  10s. o  in  R  A   

0  ;  p  B ;  R ;  3'  diam ;  st  14  . .  1 5  m  . .  

0;  vB;  R;gvmbM;  35';  all  clearly  resolved  into  stars  14  . .  16  m.  A 
blaze  of  stars. 

B  ;  S  ;  R ;  p  s  b  M  ;  diam  in  R  A  =  4'. 5  ;  barely  resolved;  a  very  delicate 
object;  doubtless  a  0. 

0;  pB;  R;  gpmbM;  2';  resolved  into  visible,  but  v  S  stars 
15  ...  16  m. 

vF;  IE;  glbM;  20"  

cl  VIII.  class  ;  a  small  well  insulated  group  of  a  roundish  figure,  5'  diam  ; 
st  12  .  .  .  13  m  ;  one  ^  9  m,  at  the  southern  edge. 

B  ;  p  m  E  in  parallel ;  g  m  b  M  ;  60"  1,  35"  br  ;  all  clearly  resolved  .... 

v  B  ;  S  ;  40" ;  res.  Among  close  st,  which  give  it  an  elongated  appear- 
ance, but  do  not  seem  to  belong  to  it. 

p  B  ;  S  ;  IE;  90"  1,  75"  br  ;  stars  15  m  

vB;  pL;  E;  gmbM;  resolved  into  st  rather  large  for  the  size  of  the 
neb.  It  is  much  like  an  oval  cluster  nebula,  of  which  there  are  plenty  in 
the  Nubecula  Major. 

Observed  July  16,  1836,  in  equatorial  zone  rev  ;  p  F ;  E  ;  1'  1  

0  ;  v  B  ;  v  L ;  v  m  comp  ;  v  g  v  m  b  M  ;  7'  diam.  The  stars  are  of  two 
magnitudes,  viz.,  15  . .  16  m,  and  12  m  ;  and  what  is  very  remarkable,  the 
largest  of  these  latter  are  visibly  reddish ;  one  in  particular,  the  largest  of 
all  (=  12. 1 1  m)  s  f  the  middle,  is  decidedly  a  ruddy  s):,  and  so  I  think 
are  all  the  other  large  ones. 

0  ;  fine;  v  rich;  v  m  comp  ;  g  m  b  M,  but  not  to  a  nucleus;  diam  in 
R  A  =  35s. 5  ;  consists  of  stars  of  two  sizes,  11  and  15,  with  none  inter- 
mediate, as  if  it  consisted  of  2  layers,  or  one  shell  over  another.  A  noble 
object.  [N.B.  —  Comparing  this  place  with  h  2015,  a  suspicion  of 
proper  motion  arises.'} 

A  cl  of  L  st.  It  is  the  commencement  of  the  bright  milky  way,  which  here 
comes  on  suddenly  in  its  main  body. 

p  F  ;  R  ;  p  s  b  M  ;  r  ;  25"  

Not  vF;  R;  psbM;  15...  20"   

0  ;  B ;  R ;  gmbM;  diam  in  R  A  =  7'.o  ;  resolved  into  st  14  ...  17  m. 

0  ;  B  ;  R  ;  gbM;  resolved  into  st  15  m   

Seen,  and  place  taken  ;  no  description.    [N.B. — This  is  no  doubt  M  70, 

though  the  P  D  of  that  object  is  stated  at  12 1°,  which  (all  the  above 

observations  agreeing)  must  be  the  wrong  degree. 

B ;  R;  psvmbM;  40";  has  a  :Jc  6.7  or  7  m,  5'  or  6'  n  p   

v  B  ;  R ;  first  v  g,  then  psmbM;  90";  a  s|t  6.7  m,  7' s  p  

cl  VII.  class;  p  rich;  irreg  R;  p  well  insulated;  not  much  comp  M; 

10'  diam ;  st  12  .  .  .  15  ;  one  9  m  taken. 

p  F ;  1  E  in  parallel ;  p  s  1  b  M  ;  40"  1,  30"  br  


NEBULAE  AND  CLUSTERS  OF  STARS. 


119 


No. 


Synon. 


3760 
3761 


3762 
3763 


3764 
3765 
3766 

3767 
3768 

3769 

3770 

3771 

3772 
3773 
3774 
3775 

3776 


3777 
3778 


3779 
3780 

3781 
3782 


1.47 

M.  54 
A.  624 


nr.  143 

h.  2022 


A-  573 


A.  262 


A.  295 


E  A.  1830.0. 
h.   m.  s.d. 


18  40  46.2 
18  41  33.6 

38.r 


50.9 

98  54 

10 

10.7 

120  41 

5 

10.7 

39 

39 

II. I 

40 

54 

39 

30 

24.0 

156  19 

17 

25.2 

19 

28 

49-7 

158  49 

27 

48 

58 

51.9 

112  54 

24 

8  46  16.8 
8  47  2.8 

8  48  .. 


49-5 

49.6 
49.9 

18  57  4.9 
18  58  13. 1 
14.8 

18  59  45.5 

19  1  53-3 

56.4 


N  P  D.  1830.0. 


153  21  38 
144    O  31 
I  I 


J47  59  1 
155    7  37 

144    9  48 


48 

4.1 

126 

5i 

0 

49 

I7.8 

r59 

9 

8 

50 

28.4 

152 

26 

1 

5° 

31. 1 

155  42 

5 

5° 

46.6 

155 

40 

35 

52 

22.4 

151 

36 

39 

24.3 

37 

6 

53 

34-5 

J54 

6 

22 

35.2 

6 

37 

54 

46.2 

152 

13- 

10 

55 

44.0 

150 

6 

48.6 

H 

16 

15  16 

14  21 

14  13 

147    18  9 

140  55  I 

53  27 

146  35  10 

140  55  9 

56  56 


Description,  Remarks,  &c. 


Neb.    No  description   

Fy  S;  IE;  18"   ,  ,  

F;  IE;  vgb  M;  80"  

vF;  vS;  R;  gbM;  12".  [This  P  D  was  read  off  =  1440  2'  38",  but 
being  already  2  fields  past  the  meridian,  this  will  require  a  large  swing 
correction,  which  will  bring  it  nearly  to  the  value  determined  in  the 
other  regular  observations.] 

0  ;  p  L ;  F ;  R,  rather  irreg ;  v  g  1  b  M  ;  6'  or  more  in  diam  ;  all  resolved. 
A  fine  object,  the  st  being  very  close  and  numerous. 

0  ;  B ;  R ;  g  m  b  M ;  diam  in  R  A  =  9";  clearly  resolved  with  left  eye . . 

0  ;  B  ;  p  L;  v  1  E  ;  gbM;  z\'  diam  ;  resolved  into  st  15  m,  with  a  few 
outliers  14  m. 

vvB;  R;  psvmbM,  to  a  large  nipple  ;  diam  2  J' ;  pos  of  a  %  13  m, 
almost  involved  =  1470  +. 

Obs  in  equatorial  zone  rev,  July  16,  1836,  on  a  neb.    B  ;  s  b  M  ;  90". .  . . 

v  F ;  R ;  g  1  b  M  ;  20";  a  j)e  9  m  5'  dist;  pos  =  2200  

e  F ;  g  1  b  M ;  20"   

vF;  L ;  R;  vgvlbM;  60" ;  R  A  ::  being  by  an  auxiliary  H<  

e  F  ;  R  ;  40" ;  too  late  for  R  A ;  same  neb  as  No.  603   

Close,  to  the  south  of,  i/2  Sagittarii ;  a  very  small  clustering  knot,  with 
perhaps  nebula.  A  doubtful  object.  I  see  3  or  4  of  the  st,  but  there  is 
also  a  nebulous  appearance. 

pF;  R;  p  s  b  M  ;  30"  ;  the  central  brightness  comes  almost  to  a  nucleus. 

pF;  S  ;  E ;  glbM;  15';  2  st  8  m  precede  ;  the  nearest  about  8'.  Both 
are  nearly  on  the  parallel,  or  a  little  south  of  the  neb,  by  diagram. 

e  F ;  p  L;  R.  The  R  A  not  observed,  but  the  observations  immediately 
preceding  and  following  being  48  "  and  53"',  it  is  probably  between  those 
limits. 

0;B;  L ;  R  or  v  1  E  ;  vgbM;  diam  5' ;  perfectly  resolved  into  st 
14. .  16  m,  with  stragglers  extending  to  8'  diam. 

vF;  S;  R ;  p  m  b  M  ;  10"  diam ;  spa  4:  7.8  m;  a  great  many  st  12  and 
13  m  in  field. 

eeF;  vglbM;  20"  ;  a  very  difficult  object  

vF;  R ;  glbM;  20"  ;  the  preceding  of  2  

e  F  ;  R;  glbM;  25";  the  following  of  2  

p  F ;  v  S ;  E  ;  psbM;  12"  1 ;  has  3  stars  preceding   

F ;  v  S ;  IE;  follows  2  st  14  m  

p  B ;  R ;  at  first  v  g,  then  s  v  m  b  M  ;  total  diam  2',  but  that  of  the 
B  part  =  15". 

B ;  R  ;  g  p  m  b  M  ;  60" ;  r   

e  F;  R;  glbM;  30"  

0;  B;  R;  p  rich;  p  s  m  b  M;  5';  stars  of  2  sizes,  viz.,  11. 12  and 

15  . .  16  ;  s  p  is  an  elegant  first  class  D  star. 
0;  B;  rich;  psmbM;  7'.    The  stars  are  of  2  magnitudes,  the  larger 

11  m,  run  out  in  lines  like  crooked  radii.    The  smaller,  16  m,  are  massed 

together  in  and  round  the  middle. 

0  ;  B  ;  L  ;  R  rather  irreg  ;  rich  ;  st  1 1 . . . .  1 6  m  ;  comes  up  to  a  blaze  in 
the  middle  ;  semid  in  R  A  =  25s ;  fine  ;  one  star  7.8  m  is  s  p  out  of  the 
cluster. 

0.    The  central  mass  consists  of  smaller  stars  than  the  outside  

0 ;  B ;  irreg  R ;  psvmbM;  all  resolved ;  st  11  15  m;  diam  5' ; 

has  a  s|s  7  m  4' s.  and  14s  prec. 

p  B  ;  R ;  gbM;  80"  

pB;  p  m  E  in  pos  630 ;  v  g  1  b  M  ;  60"  

e  F ;  p  m  E  in  parallel ;  glbM;  90"  1  [sic  in  MS.]  

p  B  ;  R  ;  20"  

e  F;  R;  p  L;  50"  

v  F;  irr  R ;  40"  


Sweep. 

708 
710 
789 
468 

591 

476 
477 

619 

603 
612 
603 
612 
793 


47i 

708 

468 


485 
614 


708 
708 
480 
481 
600 

708 
726 
726 

480 


47i 


716 

712 
789 
468 
710 
468 
789 


120 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


3783 
3784 
378s 
3786 

3787 
3788 
3789 


379° 


3791 


3792 
3793 


3794 

3795 
3796 

3797 
3798 


3799 
3800 

3801 
3802 
3803 

3804 


3805 
3806 
3807 
3808 

3809 
3810 
3811 


M.55 
A.  620 


A.  425 


R  A.  1830.0. 
h.  ra.    s.  d. 


19 


4  13-3 
4  25.8 
4  26.8 

4  45-6 

7  32.2 

8  49.0 

8  59.0 
61.3 
61.9 

9  47-5 
55-4 


19  12  2.5 
5-7 

19  16  21.0 
19  18  18.1 

20.3 

19  25  10.5 

11.9 
19  25  12.6 
19  25  16.0 

19  29  9.5 
9.9 

19  29  12.3 

14.5 

19  31  41.5 
!9  33  23-7 

19  46  52.7 

'9  47  3-4 
19  48  38.9 

19  49  6.2 
9.4 

'9  49  45-7 
19  50  4.8 
19  51  7.3 
19  52  17.5 
20.8 
19  53  6.2 
19  54  4.8 
19  54  50.7 

55-4 


X  P  D.  1880.0. 


150  47  14 
150  47  44 
150  49  24 
130  28  41 

154  II  30 
146  4  54 
150  13  41 

14  16 
13  41 

155  55  38 
56  47 
58  18  : 

145  17  2 

16  44 
129  13  10 

146  15  19 

J5  4 


161 


1  14 


1  25 
132  40  6 
128  55  20 


149 


2  36 
2  51 

121  21  6 

18  15 

145  44  « 
118  56  47 

r55  4i  27 

122  16  9 

137  32  12 

146  33  14 

3»  54 
130  40  12 

145  18  35 

J38  43  59 
144  50  29 

50  46 

146  51  56 
151  34  28 

138  50  40 

51  26 


Description,  Remarks,  &c. 


Sweep. 


v  F ;  R ;  IbM;  20".    The  1st  of  3   

eF;  15'.    The  2nd  of  3   

e  F  ;  20".    The  3  rd  of  3   

vF;  S;  R;  pslbM   

p  B  ;  R ;  psbM;  15"  

v  F ;  L ;  R  ;  vglbM;  90"  

vF;  R;  pslbM;  40"  

Not  v  F,  or  p  B  ;  R ;  psmbM;  30"  

tF;  R  ;  IbM;  20" ;  has  a  *  9  m  2'  south  

e  e  F  ;  S  ;  has  one  or  2  st  9  m,  5'  or  6'  dist  

e  e  F  ;  p  L  ;  among  small  stars   

Viewed  ;  e  e  F ;  but  it  is  a  nebula.  [No  R  A  observed,  and  the  P  D  not 
to  be  put  in  competition  with  those  of  regular  observations.] 

p  F ;  mE;  pslbM;  has  a  ^  near  s  p  end.  [N.B. — By  obs  the  minute 
of  R  A  is  13  ;  but  as  another  obs  makes  it  12,  the  earlier  minute  is 
preferred.] 

p  B  ;  p  m  E  ;  S  ;  follows  a  j|c  11  m  

eF;  R;  vgvlbM;  40"  

e  F ;  v  S  ;  IbM;  makes  a  lozenge  with  3  v  S  st  near  it  


e  F  ;  S  ;  R ;  within  [partly  within]  a  small  triangle  formed  by  3  st  11,  13, 
and  14  m. 

pB;pmE;gbto  one  end  (or  by  diagram  a  double  neb).  A  star  8  m 
follows  on  the  parallel. 

Not  v  F ;  IE;  g  b  M  ;  25"  

eF;  v  S  ;  appended  to  a  *  14  m  

eF;  R;  vgbM  

Well  looked  for,  but  only  a  small  star-group  found.    N.B. — Sky  murky  . . 

R ;  vgbM;  30" ;  haze  thickening  rapidly  

B  ;  m  E,  in  position  i69°.2  ;  p  s  b  M  ;  90"  

0;  pB;  vL;  R;  vglbM;  diam  in  R  A  3o'.o ;  all  resolved  into 
separate  st  13  ...  16  m  ;  not  so  comp  M  as  to  run  together  into  a  blaze 
or  nipple. 

(J) ;  a  fine  L,  R,  cluster ;  6'  diam  ;  all  clearly  resolved  into  st  ri,  12,  13  m; 
does  not  come  up  to  a  nipple. 

p  B  ;  p  m  E  ;  g  1  b  M  ;  40"  1,  30"  br  

e  F  ;  R  ;  v  1  b  M  ;  40"  ;  a  9  m  north  of  it,  at  6'  distance  has  what  may 
be  easily  taken  for  a  nebula  attached  to  it,  but  it  is  only  a  little  group  of 
v  S  st. 

eF;  R;  vS;  psbM;  has  :)t  1 1  m  90"  n  p,  and  one  8  m  6'  dist,  s  f . .  .  . 

pF;  R;  psbM;  15";  on  a  highly  stippled  or  dotted  ground  

e  F ;  IE;  g  1  b  M ;  30"  

v  F  ;  R ;  b  M ;  15" ;  found  and  viewed  by  the  place  of  7*467   

F  ;  L;  R;  v  g  1  b  M;  90";  forms  a  triangle  with  2  st  11  and  12  m, 
following  it. 

pF;  pL;  R;  vglbM;  80"  

p  B  ;  S  ;  R  ;  has  a  v  S  star  n  p  

v  F;  R;  b  M;  25"  

pF;  S;  RorvlE;  psbM;  15°  

vF;  S;  R;  glbM;  12"  

F ;  S ;  R,  or  1  E  ;  b  M   

Not  v  F ;  S;  R  

F;  R;  g  b  M;  40"  

B;  S;  IE;  pgmbM;  20"  

B  ;  S  ;  E  ;  g  p  m  b  M  ;  25".  If  a  misprint  of  420  12'  instead  of  410  12' 
be  presumed  in  Mr.  Dunlop's  catalogue,  this  object  is  identified  with  his 
No.  425. 


710 
488 
710 
729 
469 
716 
470 
726 
467 
729 


NEBULAE  AND  CLUSTERS  OF  STARS. 


121 


No. 

3812 
3813 
3814 

38lS 

3816 

3817 

3818 

3819 
3820 

3821 
3822 
3823 
3824 

3825 

3826 
3827 
3828 
3829 
3830 

3S31 
3832 


3833 
3834 


3835 
3836 

3837 
3838 

3839 
3840 

3841 
3842 
3843 


Synon. 


R  A.  1830.0. 
h.  m.    s.  d. 

N  P  D.  1830.0. 

O  IH 

19 

ss 

14.4 

I46  52 

17 

"9 

57 

9-7 

145 

16 

8 

»9 

57 

27.4 

138  51 

31 

3°-5 

51 

28 

57 

45.0 

138 

46 

16 

47-4 

46 

34 

19 

58 

48.5 

l6l 

17 

10 

5i-7 

16 

54 

20 

0 

13.7 

l6l 

22 

15 

15-7 

22 

25 

20 

0 

31.2 

l6l 

22 

5° 

32.2 

22 

0 

20 

1 

6.7 

136  39 

33 

20 

1 

24.9 

161 

22 

25 

•31. 1 
j 

22 

16 

20 

1 

56.5 

135 

1 

45 

20 

4 

20.1 

H3 

*7 

5* 

20 

5 

46.2 

144 

28 

23 

20 

6 

22.7 

135 

'9 

4 

24.2 

*9 

a5 

20 

8 

31.7 

138  46 

21 

34.4 

46 

22 

20 

1 1 

5I.O 

140 

57 

36 

20 

1 2 

48.  tL 

r34 

11 

20 
J 

20 

i« 

j 

•j  e.6 
j  j 

137 

34 

41 

20 

17 

J 

170 

34 

48 

20 

18 

A2. 1 

138 

2 

22 

20 

»9 

55-8 

134  46 

48 

20 

21 

8.1 

121 

23 

22 

8.7 

23 

21 

11.5 

23 

30 

12.7 

24 

O 

20 

23 

5.2 

164 

12 

54 

20 

23 

42.3 

122 

33 

0 

43-1 

32 

26 

43-7 

33 

23 

20 

a5 

43-4 

142 

40 

5i 

48.1 

41 

41 

20 

26 

8.9 

142 

44 

46 

'3-7 

43 

5i 

20 

27 

46.8 

144 

53 

54 

20 

28 

8.9 

159 

20 

30 

20 

30 

38.1 

123 

5 

10 

20 

30 

48.3 

143 

57 

35 

51. 1 

57 

44 

20 

37 

42.7 

128  36 

55 

20 

40 

7.8 

139 

24 

16 

20 

44 

56.7 

142 

30 

46 

58.: 

31 

25 

Description,  Remarks,  &c. 


Sweep. 


vFj  IE;  glbM;  20"  

eeF;  L;  pmE  

vB;  S ;  R ;  pgmbM;  20'   

vB;  R;  g  v  m  b  M  ;  30"  

F ;  p  m  E  in  parallel ;  g  b  M  ;  30"  1  

pF;  IE;  25"  

F ;  R ;  glbM;  30" ;  has  avS  ^  preceding ;  first  of  4   

F;  E;  40"  1;  has  a  s|j  9  m  10s.  5  preceding.  The  minute  of  R  A  altered 
from  59  to  58,  as  both  the  context  of  the  MS.  and  the  obs  of f  604  agree 
in  requiring. 

p  F ;  R ;  20" ;  a  v  S  almost  invisible  >k  s  f ;  2nd  of  4  

p  B;  S;  R;  r;  15"   

e  F  ;  e  S  ;  the  3d  of  a  group  of  4   

v  F;  v  S  ;  R  

F;  vS;  R;vgmbM;  10";  asjfjmsf  dist  5'  

pF;  S;  R;  r;  15";  the  last  of  4  

e  F  ;  v  S  ;  has  a  v  S      close  to  it  

vF;  L;  R;  glbM;  90"  

p  F ;  L  ;  p  m  E ;  glbM;  2'  1,  1'  br   

v  F ;  L  ;  IE;  2'  1,  90"  br   

F;  R;  vglb  M;  15"  


PB 
pF 
PF 


;  S;  R;  gb  M;  25"   

;  R;  s  v  m  b  M  to  a  ^  12  m;  20"  

;  R ;  g  b  M  ;  20"   

F;  R;  S;  glbM;  15"  among  stars   

F;  R;  p  s  b  M  ;  25*  :   

p  B  ;  p  L ;  g  b  M  ;  near  2  st  10  m   

p  B  ;  R  ;  p  s  m  b  M  ;  25"   

v  F ;  attached  to  a  sfc  12  m  s  f.    [N.B. — By  a  diagram  made  at  the  time 
the  star  is  s  p.] 

e  F ;  p.L;  R  ;  v  g  v  1  b  M  ;  40"   

p  B  ;  R ;  g  b  M  ;  has  2  or  3  st  very  near  it   

F ;  R  ;  g  b  M  ;  25" ;  between  2  stars  

F;  S;  IE;  bM;  15"  1,  12"  br  

p  B;  R;  p  gb  M;  25"   

F  ;  S  ;  R ;  glbM;  follows  a  hook  of  5  stars  

B  ;  m  E  ;  p  s  1  b  M  ;  2^'  1,  40"  br  

p  B  ;  p  m  E  ;  p  s  b  M  ;  80"  1,  20"  br  

B  ;  L ;  m  E,  in  position  6°.o  ;  psmbM;  3'1   

p  F ;  L ;  R  ;  glbM;  2' ;  the  preceding  of  2   

B  ;  p  L  ;  R  ;  g  b  M  ;  r ;  80"  

v  F;  R;  40"  

F;  R;  glbM;  30"  

p  B  ;  R ;  p  s  1  b  M  ;  60"  

p  F  ;  L ;  m  E  ;  v  g  b  M  ;  33'  1 ;  15'  br  ;  has  a  barely  perceptible  point  in 
the  middle. 

vF;  L;  R;  gbM;  on  a  faintly  stippled  ground   

e  F  ;  p  L ;  IE;  60"  1 ;  50"  br   

vF;  E;  lbM;  35"  1  

B ;  R ;  p  g  m  b  M  ;  25";  follows  4  st ;  of  which  1  is  9  m  

pB;  S;  IE;  gmbM;  18"  1   

e  F ;  S  ;  R ;  the  preceding  of  2   

vF;  pmE   


I  I 


469 
710 
467 
729 
467 
729 
604 
614 

614 
604 
604 
614 
463 
604 
614 
472 
6,5 
710 
463 
472 
467 
729 
615 
728 
463 
611 
463 

728 
619 
620 
476 
618 
606 
476 

477 
620 
468 
615 
468 
6,5 
710 
604 

495 
710 
615 
483 

497 
468 

498 


122 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R  A.  1830.0. 
h.  m.   s.  d. 

X  P  D.  1830.0. 
Ore 

20 

45  17-6 

134 

37 

14 

20 

45  36.1 

142 

30 

56 

37.6 

30 

55 

3  0  .u 

31 

3 

20 

4  12.0 

139 

J7 

!5 

17,3 

tfk 

1  u 

45 

20 

47  II.O 

146 

*3 

44 

12.0 

12 

43 

20 

51  49.4 

139 

42 

15 

52.8 

41 

40 

20 

52  7.8 

139 

47 

25 

20 

53 

J43 

*3 

5 

13.4 

*i 

20 

12 

A  A, 

TT 

20 

55  18.2 

i35 

29 

4 

22.0 

29 

25 

20 

56  15. 1 

137 

51 

49 

57  4-4 

T  C  A 

'54 

42 

53 

20 

17  0.2 

154 

12 

42 

20 

57  39-8 

139 

59 

18 

21 

0  2.1 

139 

58 

38 

21 

0  3.4 

158 

59 

12 

21 

3  36-1 

137 

54 

53 

37.6 

55 

15 

21 

4  5i-5 

139 

4- 

8 

53-5 

3 

57 

21 

7  20.6 

139 

16 

12 

25.8 

16 

25 

21 

14  1.6 

133 

I  I 

T  Q 

10 

21 

14  23.4 

150 

44 

55 

21 

14  57.1 

133 

8 

4 

21 

15  56.3 

139 

47 

5° 

21 

17  2.4 

143 

30 

59 

21 

19  29.4 

133 

49 

46 

30.7 

49 

26 

21 

19  40.7 

133 

54 

0 

41.4 

53 

26 

21 

20  56.7 

129 

2 1 

27 

22 

10 

21 

21  35.0 

134 

48 

44 

21 

22  II.O 

154 

39 

0 

13.9 

39 

7 

21 

23  50.1 

131 

34 

28 

50.2 

34 

22 

21 

24  28.8 

145 

18 

40 

Description,  Remarks,  &c. 


3844 
3845 


3846 
3847 

3848 

3849 
3850 

3851 

3852 
3853 
3854 
3855 

3856 

3857 
3858 

3859 
3860 

3861 
3862 
3863 
3864 
3865 
3866 

3867 

3868 

3869 
3870 

3871 
3872 


A.  263 


eF;  S;  R;  45"   

F j  L ;  1  E  ;  g  1  b  M  ;  90"  1 ;  the  following  of  2   

v  F;  pL;  IE;  vgbM  

F  ;  R  ;  g  1  b  M  ;  20"   

F;  S;  R ;  gpmbM;  has  a  v  B  $  1'  prec   

pB;  S;  IE;  gbM;  among  B  stars   

A  %  10  m,  to  which  is  attached  or  almost  so,  by  its  extremity  an  e  F,  v  s 
nebulous  ray ;  v  m  E  in  merid  15"  1;  4"  br  ;  night  superb,  and  without 
this  condition  it  were  useless  to  look  for  this  object. 

eeF;  vS;  R;  Sofa  small  ^  13  m,  10"  dist  

p  F;  p  L;  R;  g  1  b  M   

F;  S;  R;  smbM;  15"   

e  F  ;  R ;  1  b  M  ;  has  n  *  11  m  60"  foil  on  parallel  

pB;  vS;  R;  pslbM;  12"   

pB;  S;  R;  psmbM;  15"  

pBj  S;  R;psbM;  15";  among  stars  

A  nebulous  looking  but  doubtful  object  following  a  s(s  10  m.  My  eye  is  too 
much  fatigued  to  be  able  to  decide  on  its  nature. 

F;  E;  vgvlbM;  60"  1 ;  30"  br ;  near  a  *   

p  F;  S  ;  R  ;  b  M ;  has  2  st  12  m  north  

p  B  ;  IE;  p  g  b  M  ;  30"  1  

pF;  R;  psbM;  25";  has  a  ^  7-8  m  10'  prec,  exactly  in  the  parallel . . 

eeF;  S ;  R ;  on  a  delicately  and  uniformly  stippled  ground ;  a  bright 
triple      6'  or  7' s  f  nearly  points  to  it. 

B ;  R;  gpmbM;  35"  

vF;  R;  gib  M;  25"   

F;  pL;  R;  glbM;  90"  

B ;  L  ;  p  m  E  ;  gbM;  2'  1 ;  90"  br   

B  ;  S  ;  E ;  has  a  >)c  10  m  3'  n  f  

B;  pmE;  psmbM;  40"  1 ;  has  a  He  nmsf  

B  ;  R  ;  p  g  m  b  M  ;  60". . . ,  

v  B ;  p  S  ;  p  m  E  ;  p  s  v  m  b  M  ;  25"  1,  1 5"  br  

e  F  ;  v  S  ;  R  ;  the  preceding  of  2  

B;  IE;  gpmbM;  90"  1,  40"  br   

v  F  ;  S  ;  R ;  the  following  of  2   

eeF;  v  S  ;  R  ;  10" ;  the  feeblest  object  imaginable  

eF;  v  m  E,  in  pos  =  90°.8  ;  v  g  b  M  ;  80'  1 ;  has  a  *  s  

F ;  L  ;  v  1  E  ;  vglb  M;  2'  br  ;  the  preceding  of  2   

F  ;  p  L  ;  IE;  g  v  1  b  M  ;  60°  

v  F  ;  just  seen  ;  R  A  deduced  roughly  from  that  of  the  preceding  nebula  . . 

F ;  S ;  R  ;  vglbM;  30"  ;  the  following  of  2   

p  F  ;  S  ;  R  ;  p  s  b  M  ;  15'   

v  F ;  v  S  ;  R  ;  15".    Too  late  for  R  A  

B  ;  R  ;  p  s  b  M ;  30"  

p  B  ;  p  L ;  R ;  gbM;  60"   

F  ;  L  ;  R  or  1  E  ;  v  g  p  m  b  M;  60";  r ;  with  long  attention  it  appears 
mottled.    Perhaps  A  263,  with  3"'  correction  in  R  A. 

pF;  S;  R;  gbM;  15"   

v  F;  R;  20"  

p  B  ;  L;  v  m  E  in  pos  i27°.i ;  first  g,  then  p  s  1  b  M  to  a  v  feeble 
nucleus  ;  4'  1,  40"  br ;  has  a  j|e  1 1  m  preceding. 


NEBULAE  AND  CLUSTERS  OF  STARS. 


123 


No. 


Synon. 


3873 


3874 
387S 

3876 

3877 

3878 

3879 

3880 
3881 
3882 

3883 

3884 

3885 
3886 

3887 
3888 


3889 
3890 
3891 

3892 
3893 


3894 

389S 
3896 


3897 
3898 
3899 

3900 


M.  30 
h.  2128 


K  A.  1830.0. 
h.  m.   s.  d. 


21  25 


21  27  57.4 
21   27  57.4 
80.8 
21   28  54.I 

21   29  27.4 

31.6  : 

21  30  45.5 

21  30  55.7 

21  31  26.0 
21  31  42.8 
21  31  59.8 

21  34  33.2 
33-7 
21  34  57.2 

59-4 
21  35  13.7 
21  36  1.5 
21  36  42.0 
21  36  42.6 

44-4 
46.2 

21  36  45.0 
21  38  3.4 
21  39  33.3 
34.2 
21  40  21.7 
21  40  24.8 


21  41  34.7 
38.2 
21  42  16.0 
21  43  43.5 
47-7 
49.3: 
ai  44  5.2 
21  44  45.4 
21  44  59.1 
62.9 
21  45  9.5 
12.6 


N  P  D.  1830.0. 


127  32 


154  40  3 
172  18  14 

17  36 
165  52  29 

133   I7  56 

18  46 

113  56  38 
143  28  34 

135  33  42 
125  13  1 

124  56  4 
56  36 

139  12  28 
11  50 

139  7  58 
8  o 
137  17  49 
161  6  57 
151  29  32 
141  21  14 

20  32 

21  22 

151  23  27 

125  13  58 
125  40  11 

39  48 
147  20  25 
146  21  53 


139  2  47 
2  50 

138  40  47 
141  28  24 
27  37 
26  45 
120  5  o 
119  49  54 

140  19  16 
19  15 

125  37  12 
36  20 


Description,  Remarks,  &c. 


eF;  p  L ;  vgbM;  2';  place  considerably  uncertain,  having  been  found 
when  much  past  the  meridian  in  searching  in  vain  for  A  561.  This  neb  is 
much  too  faint  to  have  been  seen  with  9  inches  aperture  \to  say 
nothing  of  the  difference  of  place,  for  mine  cannot  be  so  much  in  error 
as  would  reconcile  them].  It  precedes  a  6  m  nearly  in  the  parallel, 
about  40  seconds  of  time. 

v  F  ;  S  ;  R ;  12" ;  has  a  v  S  double  41  n  f ,  near  

F  ;  p  L  ;  R  ;  v  g  v  1  b  M  ;  50"  

F;  pL;  vglbM;  has  a  H«  1 3  m  on  it  

p  F ;  R  ;  first  v  g,  then  p  s  b  M  ;  in  a  field  with  many  large  stars,  and 
strongly  stippled. 

B;  S;  R;  psmbM;  15";  (fog)  

B;lE;gpmbM.  [RA  obtained  by  calculating  from  A  P  D  and 
observed  position,  with  a  star  near  it,  and  therefore  not  to  be  considered 
as  exact.] 

(J) ;  B ;  IE;  bM;  4'  1,  3'  br ;  all  resolved  into  st  16  m,  besides  a  few 
12  m.    Two  lines  of  rather  larger  stars  run  out  n  f. 

eF;  IE;  vglbM;  30" ;  makes  an  obtuse  angled  triangle,  with  2  st 
9  and  10  m  to  n. 

vF;  pL;  R;  vglbM;  2'  diam   

e  F  ;  v  S  ;  among  stars   

v  F;  S;  R;  b  M  

p  F  ;  too  late  for  transit   

vF;  R;  S;  glbM;  the  preceding  of  2   

p  F;  R;  gb  M;  15"  

p  F  ;  S  ;  R ;  glbM;  the  following  of  2  

v  F;  R;  g  b  M;  15"  

Not  v  F  ;  S ;  R  ;  g  b  M  ;  20"   

p  B  ;  R  ;  v  g  b  M  ;  20'';  a  star  9  m  follows,  8'  dist   

eF;  pL;  R ;  60"  ;  the  preceding  of  2   

e  F  ;  IE;  glbM;  70"  1,  60"  br  

B ;  L ;  p  m  E  ;  v  g  b  M  ;  2'  1,  80"  br  

vF;  pmE;  vglbM.  (N.B. — Mirror  begins  to  show  signs  of  a  want 
of  light.) 

p  B;  p  L;  IE;  gbM;  40"  1,  35  br ;  the  following  of  2  

p  B  ;  R  ;  glbM;  20"   

p  B  ;  R  ;  b  M  ;  20";  a  ^  14  m  precedes  just  out  of  neb   

p  B  ;  L  ;  v  g  b  M  ;  has  5  st  8  m  in  field  surrounding  it   

pF;  R;  gbM;  35"   

F;  L  ;  R  ;  first  g,  then  p  s  1  b  M.  [N.B. — It  is  not  improbable  that  this 
and  the  nebula  immediately  preceding  f  499  are  identical,  one  or 
other  being  mistaken  i°  in  P  D.  Still,  as  both  observations  are  clearly 
■written  in  MS.,  and,  as  the  difference  of  P  D  even  then  is  rather  con- 
siderable, (i'  28")  I  have  thought  it  necessary  to  enter  them  separately '.] 

B  ;  R  ;  g  m  b  M  ;  39"  

vB;  pL;  R;  smbmto  nucleus ;  45"   

B  ;  R  ;  p  g  b  M  ;  20";  within  a  triangle  of  3  st  13  m  

eF;  mE;  vgbM;  rather  wedge-formed ;  ?  if  not  binuclear  

F;  IE;  vglbM;  40"  

F;  pL;  IE;  vgbM;  r  

e  e  F;  v  S;  10";  barely  perceptible;  sky  perfectly  clear  

e  F ;  S ;  E  ;  or  has  aneF  #  near  

pB;  S;  R;  gbM;  15"   

pB;  S;  IE;  psmbM;  20"  

B  ;  p  L ;  glbM;  more  nebulas  hereabouts  

B ;  p  L ;  irreg  R ;  glbM;  r ;  60"  


727 

795 
796 
627 


728 


474 


490 
493 
49  2 
493 
497 
49  6 
497 

49  6 
490 
616 
613 
468 
498 
730 

613 

493 
492 

493 
499 
500 


497 
496 

497 
468 

730 

498 
620 

49S 
497 
496 
492 
493 


124 


REDUCED  OBSERVATIONS  OF 


No. 
3901 

3902 

39°3 
3904 

3905 
3906 
3907 

3908 
3909 
3910 

3911 


Synon. 


3912 

3913 
39H 

39J5 


3916 


39»7 


R  A.  1830.0. 
h.  m.    s.  d. 


21  49  5.5 


21  49  2I.9 
23.6 
29.I 

21    50  Z.I 

21   50  53.8 

544 
56.7 
21  50  55.2 

21  51  11. 2 


21  52 


21  52 


21  52 


21  52 


2.9 
8.3 
4.8 

5-i 
8.8 
9.1 
6.6 
6.8 

7-4 
10.1 
9.2 


NPD.  1830.0. 


10.4 
21  52  II. 6 

12.6 


12.9 

48  8 

13.6 

46  49 

15.0 

49  0 

15.8 

48  24 

21   52  l8.8 

126  37  20 

21  54  4.1 
21  54  8.6 
9-5 

21  54  51.9 
52.9 
55-9 
57-5  = 

21  55  47.5 

49-3 
21  56  11. 2 


134    6  59 


122  41  43 
41  52 
41  23 

134  12  4 

142  34  1 
33  7 
33  42 

115  26  51 

138  30  20 

154  5i  47 
51  52 
122  40  13 

41  21 

42  24 
40  54 

122  46  51 

46  53 

47  18 
45  49 

122  49  4 


48  3 
122  47  41 

48  34 


Description,  Remarks,  &c. 


155  27  47 
155    7  5* 
8  12 

140  56  37 

56  43 
56  32 
56  33 

155  3i  27 
31  53 
140  49  30 


F;  L;  m  E ;  vgbM;  (Fog)   

Viewed ;  pF;  pL;  IE;  glbM;  50";  readily  found  in  place  by/489, 
but  place  not  re-taken. 

p  F  ;  1  E ;  g  1  b  M ;  40"  

tF;  pL;  R;  gbM;  40"   

vF;  pL;  IE;  vgbM;  50"  1,  40"  br  

pB;  S;  R;  psmbM;  15"   

Viewed  ;  readily  found  by  place  of  7*489  ;  B;  IE;  vsvmbMto  nucleus 

p  F;  S;  R;  pslbM;  15"  

pB;  S;  R;  psbM;  20"   

p  B  ;  R ;  p  s  b  M  ;  20"  

F ;  R  ;  v  g  1  b  M  ;  45"  ;  has  a  s|«  10  m,  90"  dist  from  centre,  following 
in  parallel. 

e  F  ;  S  ;  R  ;  difficult  to  distinguish  from  a  ^  15m;  has  a  %  8  m,  dist 
4'  n  p  nearly  in  parallel,  and  another  1 1  m,  60"  n  f. 

F;  RorlE;  vgbM;  40"   

p  F ;  IE;  gbM;  25"  long   

p  B ;  p  L ;  g  b  M.    [The  first  of  a  group  0/4.]    See  Jig.  1 1,  PI.  IV.  . . 

pB;  E   

pB;  R;  40"   

F;  pL;  IE;  gbM  

B;  v  S;  R;  s  b  M  to  a  *.    [The  2nd  0/4.]  

B;  S;  R;  sbM  

pFj  R  

pB;S   

In  f  49  3  this  was  taken  for  a  v  F  star,  but  I  now  perceive  it  plainly  to  be  a 
small  faint  round  nebula.  {Place  deduced  front  that  of  the  larger  neb, 
to  vhich  it  is  attached  (Aro.  4  of  the  group),  by  a  careful  measurement 
of  the  diagram  made  at  the  time,  taking  for  the  unit  of  measure  the 
line  joining  the  centres  of  the  2nd  and  \th  neb.} 

p  F  ;  S  ;  attached  to  a  larger,  following  it.    [77(e  yd  0/4.]  

vB;  pL;  sbMtoa  star ;  has  a  very  faint  star  s  p.  {The  last  of  a 
group  0/4.] 

B ;  R ;  m  E,  or  rather  distinctly  binuclear,  or  a  double  nebula.  Pos  of 
the  smaller  about  2500.  Much  brighter  and  better  seen  than  last  night. 
Not  a  doubt  about  the  nature  of  the  appendage. 

B  ;  p  S ;  R ;  double  

B;  R;  gp  mb  M;  40"  

B;  pL;  R;  smbM;  place  roughly  derived  from  that  of  the  2nd  of  the 
group  as  observed. 

B  ;  R;  p  g  b  M  ;  40".    [See  fig.  11,  PI.  IV.  for  this  group.]   

eF;  S;  R;  2'  n  of  a  *  8  m;  a  double  star  10  =  ion  follows  nearly  on 
the  parallel  of  the  neb,  and  pointing  directly  to  it.  A  sure  observation  ; 
but  except  in  the  finest  nights  this  neb  will  not  be  seen. 

vF;  S;  IE;  vgbM;  20"  

pB;  S;  R;  gpmbM;  20"   

pB;  S;  R;  psbM;  20"   

B ;  R  ;  g  m  b  M  ;  20"  ;  has  a  He  12  m  60"  foil  

pB;  R;  pslbM;  20" ;  position  of  a  ^  14  m  from  neb  =  ioi0-7  .... 

p  B  ;  R  ;  25";  among  small  stars  

vB;  S;  R;  smbM;  15";  among  many  stars.  The  R  Ascensions  of 
this  f  uncertain  to  4  or  5  seconds,  owing  to  unexplained  fluctuations  of 
the  zeros. 

vF;  vS;  R;  pslbM;  follows  a  *  n  m,  3'  

v  F  ;  S  ;  R ;  3,  but  a  good  observation  

pF;  S;  R;  smbM;  15"   


NEBULAE  AND  CLUSTERS  OF  STARS.  125 


No. 


Synon. 


K  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 


3918 

3919 
3920 

3921 

3922 

3923 
3924 
3925 
3926 

3927 
3928 


3929 
3930 


393 1 
3932 

3933 
393+ 
3935 
3936 

3937 
3938 

3939 


394° 

394i 
3942 


III.  458 


21  56  40.3 
41.0 
45-9 

21  56  49.5 
21  56  57.0 


21  56  54.3 

54-5 
58.0 

21  57  3-3 

21  57  41. 1 

21  58  35.1 

21  59  7.0 

21  59  25.5 


31.2 
34.2 
27.6 
29.2 
29.5 

33-5 
33.6 
19.1 
21.4 
22.9 
23.7 
5-5 


5  16.0 


22    9  27.3 
22  i  1  17.0 
22  13  24.6 
22  13  27.9 
22  13  42.5 
22  14  36.9 
37.2 
22  15  58.7 
60.5 
64.6 

22  16  30.9 
31.9 
32.0 
36.3 

22  16  55.0 

22  17  21.2 
25.1 


122  4  o 
4  25 
4  9 

148  15  11 
122    o  30 


121  58  23 

59  16 
57  3° 
121  52  13 

119  52  39 
137  59  20 
159  29  32 

118  38  27 

155  40  42 

41  4 

121  22  53 
23  34 
23  22 
22  45 

116  59  27 

120  12  59 
13  13 

12  6 

13  19 
136  41  23 
136  41  8 

145  57  5° 
115  31  43 

119  12  27 
119  48  15 

123  12  33 

124  32  58 

33  9 

122  3  26 

2  26 

2  33 

3  ± 
122    o  13 

o  36 


151 


o  34 
2  o 


126    o  34 
o  15 


p  F  ;  R  ;  g  b  M.    PD  roughly  deduced  from  No.  1 5  of  this  /  

v  F  ;  a  large  star  follows   

v  F.  [This  is  the  first  of  a  group  of  3,  No.  2  of  which,  however,  is  so 
faint  as  to  have  escaped  obs  in  sweeps  494  and  620.] 

pB;  IE:  glbM;  aj'  1,  ij' br  

Found  in  place  ;  p  B  ;  L  ;  E  ;  first  g,  then  p  s  1  b  M  ;  3'  1,  2'  br  

eF;  S  ;  star  like;  the  znd  of  a  group  of  3.  [N.B. — It  precedes  the 
■$rd  2  beats  of  the  chronom  —  ■  V.o.  The  R  A  here  set  down,  it  must 
be  noticed,  is  comparable  only  with  that  single  value  of  the  R  A  of  the 
others,  which  results  from  f 619.] 

p  F ;  R  ;  g  b  M.    [The  last  of  a  group  of-}.]  

p  F  ;  the  following  nebula  ;  a  large  star  follows   

F  ;  R;  g  b  M  ;  the  3rd  of  3  ;  follows  the  2nd  is.o  

pB;  L;  IE;  gb  M;  80".  [As  this  nebula  might  be  seen  in  the  same 
field  with  all  those  of  the  group  of  3  observed  in  sweeps  494,  619,  620, 
it  properly  belongs  to  that  group  of  which  it  forms  the  \th  and  last.'] 

v  F  ;  v  S  ;  R ;  almost  uniformly  bright  

v  B  ;  R ;  g  b  M  ;  45"  

PF;  R;  gbM;  25"  

A  v  S  cluster  or  resolvable  nebula  ;  irreg  R ;  lb  M;  2'  diam  ;  has  2  or  3 
st  larger  than  the  rest. 

pB;  R;  p  s  b  M  ;  near  2  stars  

eF;  S;  J  d   

F ;  R ;  gbM;  has  2  st  14  m  near,  one  almost  involved  

vF;  S;  R;  2vSst  near  

F;  R;  gbM   ,  

p  F ;  IE;  gbM;  either  r,  or  has  loose  stars  

p  F;  S;  IE;  b  M;  15"  1,  12"  br  

F ;  pL;  R ;  gbM;  80"   

p  F;  L;  R;  glbM;  r   

v  F;  IE;  glbM;  50  or  60"  1  

eF;  pL;  R;  vglbM;  50"  

p  B  ;  vS;  p  m  E  ;  p  s  b  M  ;  1 5"  1,  8"  br.    The  preceding  of  2   

F ;  v  S  ;  R  ;  10".  The  following  of  2.  A  star  8  m  follows  nearly  on  the 
parallel,  and  another  to  the  north. 

e  e  F  ;  R;  rather  a  doubtful  object  

Not  v  F;  S  ;  R;  b  M;  30"  

v  F ;  S  ;  R  or  E,  as  if  it  had  a  feeble  neb  s  p  ;  glbM;  15"   

eF;  pL;  R;  vglbM;  40"  

eF;  S;  R;  lbM   

B ;  IE;  gbM;  50" ;  has  a  bright  triple  *  sp  

p  B  ;  R ;  p  g  b  M  ;  40"  ;  a  large  triple  sp  

vF;  S;  R.    [The  preceding  of  a.]  

p  F;  S  ;  IE  

v  F;  irreg  R,  or  1  E  ;  40  or  50"  

F  ;  R;  g  1  b  M.    Rough  place   

pF;  pL;  IE;  glbM.    [The  following  0/2.]   

v  F;  S;  R  

p  F;  S;  R  

v  F  ;  IE;  30"  

eeF;  IE;  vgvlbM;  very  difficult,  but  a  certain  observation.  It  is 
n  p  the  first  of  3  stars  10.11  m. 

vF;  pL;  R;  vgvlbM;  30"  

vF;  S;  R;  gbM;  15"   


494 
620 
619 

470 

735 
619 


494 
620 
619 
494 

495 

49  6 
616 

475 

602 
727 
494 
495 
620 
619 

475 
620 

494 
619 

495 
490 
490 

499 
474 
475 
495 
494 
493 
492 

494 
620 
619 
494 
494 
495 
620 
619 
726 

492 
486 


K  K 


126 


REDUCED  OBSERVATIONS  OF 


Synon. 


3943 

3944 
3945 

3946 


3947 
3948 

3949 


395° 


395i 
3952 

39S3 
3954 
3955 
3956 

3957 
3958 

3959 
3960 


3961 
3962 

3963 


3964 

3965 

3966 

3967 
3968 

3969 


II.  469 


A.  255  ? 


A.  51S 


R  A.  1830.0. 


h. 

m. 

s.d. 

22 

>9 

10.5 

115 

43 

27 

10.7 

43 

29 

22 

27.8 

126 

>9 

29 

22 

21 

14.3 

128 

42 

10 

25.8  : 

38 

52 

22 

21 

38.8 

128 

41 

20 

46± 

37 

+ 

22 

23 

46.4 

131 

49 

6 

22 

23 

47-9 

118 

7 

17 

22 

26 

22.4 

116 

55 

10 

22.4. 

c  1 

55 

32 

22 

28 

0.2 

128 

6 

0 

4.2 

7 

0 

6.5 

5 

7 

22 

2S 

29.5 

157 

21 

34 

22 

33 

42.8 

128 

45 

5° 

22 

2A 

6.1 

150 

43 

22 

34 

50.3 

120 

56 

27 

22 

35 

46.2 

130 

14 

0 

22 

40 

40.8 

127 

44 

45 

22 

43 

57.0 

136 

15 

8 

22 

+4 

4.1.3 

130 

*3 

2 

22 

44 

52.0 

154 

36 

2 

45 

I9.3 

I  30 

34 

•7 

21. 1 

11 

Co 

22 

46 

2.0 

133 

33 

22 

22 

46 

38.8 

155 

55 

57 

44.0 

56 

0 

22 

46 

57-3 

127 

56 

10 

62.2 

56 

40 

63.3 

55 

2 

22 

47 

17.9 

128 

16 

15 

19.2 

15 

10 

23.9 

13 

55 

15 

2 

22 

47 

38.1 

"31 

58 

53 

39.1 

58 

26 

22 

52 

32.0 

130 

58 

57 

22 

52 

35.0 

130 

29 

23 

22 

53 

12.9 

131 

44 

'9 

14.8 

44 

53 

22 

54 

27.9 

141 

1 

5° 

N  P  D.  1830.0. 


Description,  Remarks,  &c. 


p  B  ;  irr  R ;  25"  ;  involves  a  double  s)e  (13  m  +  14  m)  

F;  E;  b  M;  r;  binuclear,  pos  62°.3.  Rather  an  equivocal  object, 
whether  nebulous  or  a  group,  but  I  incline  to  regard  it  as  a  nebula. 

v  F  ;  R  ;  g  1  b  M  ;  20"   

e  F ;  S ;  R.    The  preceding  of  z   

e  e  F  ;  perceived  with  the  utmost  difficulty,  and  taken  at  leaving  the  field. 
[Place  very  uncertain.] 

e  F;  S;  R.    The  following  of 2   

Required  very  long  attention  to  see  (mirror  growing  dim).  [Place  very 
rude,  by  estimations  from  the  preceding  nebula,  which  is  itself  ill  deter- 
mined in  this y.] 

F ;  p  L  ;  p  m  E  ;  about  pos  of  750  with  parallel ;  z\'  long  

v  F  ;  S  ;  IE;  follows  a  ^  n  m  in  the  parallel   

p  B  ;  L  ;  m  E  in  merid  ;  v  1  b  M  ;  4'  1,  2'  br  ;  D   

B  ;  tL;  m  E  in  merid  ;  g  v  1  b  M  ;  4'  1,  1 J  br  

B  ;  L ;  m  E  in  merid  ;  3'  1,  i'  br ;  cloud  prevented  transit  being  observed . . 

pF;  R ;  g  b  M  ;  20"  

e  F;  S;  v  1  E  

e  e  F  ;  barely,  but  certainly  seen.  [N.B. — The  obs  makes  the  R  A 
zt)m  6^.5,  and  as  the  P  D  fails  of  a  perfect  agreement,  it  is  not  impos- 
sible that  this  mag  be  a  different  nebula.'] 

p  B  ;  m  E  in  parallel ;  g  b  M  ;  50"  1,  20"  br   

e  e  F  ;  v  S  ;  R  ;  a  double  star  follows  about  401  on  the  parallel  

F;  S;R;bM;  15"  

F  ;  p  L  ;  v  m  E  in  merid  ;  vgvlbM  

F ;  IE;  g  1  b  M  ;  30"  1  

e  F ;  v  S  ;  R ;  appended  (s  f  45°,  dist  30")  to  a  *  12  m;  place  taken  that 
of  the  star. 

p  F ;  IE;  g  1  b  M.    Query  if  it  have  not  a  v  S  sfc  involved  

v  F  ;  S  ;  R  ;  15".  [The  minute  altered  from  45  to  44  of  R  A,  as  required 
by  the  context  of  the  observations.] 

p  B  ;  R;  v  g  1  b  M  ;  40"  

A  long  p  B  ray,  4'  long,  psvmbM;  elongated  in  pos  44°.7   

B  ;  p  L ;  v  m  E  in  pos  4i°9  ;  pgmbM;  3'  1,  20"  br  ;  has  a  *  1 1  m, 
2'  dist,  pos  from  nucleus  i2°.9. 

e  F  ;  v  L ;  3'  diam  at  least ;  it  is  s  p  a  $  7  m,  8'  dist  

p  F  ;  R  ;  g  p  m  b  M  ;  20"  

B  ;  R  ;  g  p  m  b  M  ;  r  ;  40"  

p  B;  v  L;  R;  orvlE;  vgbM;  4'  diam  ;  with  left  eye  r,  hardly  re- 
solved P  D  bad.    A  fine  object. 

B;  vL;  R;  orvlE;  vglbM;  5'   

vF;  vL;  R;  vglbM;  3'   

B;  L;  R;  gpmbM,  2';  r  with  right  eye ;  with  left,  barely  resolved  in 
the  centre. 

B  ;  L  ;  R  ;  g  b  M  ;  2r>'  or  3'   

p  F ;  p  L  ;  v  1  E  ;  v  g  1  b  M  ;  50"  1   

v  F ;  (mirror  dim)  

v  F;  IE;  45*  

F;  vL;  R;  vgmbM;  3'  diam  

F  ;  L ;  m  E  ;  vglbM;  pos  of  elongation  33°.8  ;  4'  1 ;  1'  br  ;  loses  itself 
imperceptibly. 

e  F;  v  L;  v  1  b  M  ;  6'  1;  3'  br  

v  F ;  v  m  E,  in  pos  5°  ± ;  100"  1   

p  B  ;  S  ;  v  m  E ;  has  a  sjc  11  ra  preceding  its  extremity  

e  F  ;  R  ;  g  1  b  M  ;  60"  ;  has  a  *  1 1  m  n  p  3'  dist   


NEBULAE  AND  CLUSTERS  OF  STARS. 


127 


Synon. 


B  A.  1830.0. 
h.  in.  s. d. 


NPD.  1830.0. 


Description,  Remarks,  &c. 


II.  2  ? 
h.  2211 


A.  475 
A.  476  ? 

II.  236 

h.  2226 

A.  477 

I.  104 
h.  2228 


A.  347  ? 


22  55  36.3 

38.4 
22  56  35.4 


22  57  41.2 

44.1 
44.6 

23  o  14.6 

15.2 
23    2  56.2 


134    o  59 

1  44 
127  11  44 


127  11  50 

10  7 

11  35 

i34  19  55 
20  40 
118  27  8 


*3 

5 

19.9 

134 

3i 

36 

*3 

6 

9-7 

129 

27 

22 

28 

+ 

*3 

6 

44.8 

'33 

31 

17 

23 

8 

59.8 

133 

2 

47 

23 

9 

14. 1 

95 

34  56 

23 

9 

29.5 

133 

9 

42 

a3 

9 

57.0 

133 

10 

57 

23 

10 

16.2 

99 

*5 

24 

23 

1 1 

33.6 

153 

3 

22 

23 

12 

36.4 

172 

50 

10 

23 

12 

39-7 

133 

24 

34 

44-5 

24 

53 

23 

12 

38.2 

158 

36 

z 

39-9 

35 

18 

23 

*3 

27.0 

120 

12 

32 

23 

H 

3 1.0 

120 

18 

43 

23 

15 

33-3 

148 

43 

30 

34-4 

43 

5i 

23 

15 

54.0 

148 

49 

5i 

23 

16 

24.4 

158 

57 

32 

32.5 

58 

0 

23 

16 

57.0 

148 

44 

50 

a3 

17 

8.7 

156 

12 

42 

23 

17 

10.0 

130 

9 

36 

10 

+ 

23 

x9 

18.9 

150 

38  56 

23 

23 

7.8 

'45 

2 

17 

23 

*3 

39-9 

142 

37 

47 

40.5 

38 

28 

23 

*5 

3-7 

,56 

20 

34 

p  F;  S;  R;  12";  makes  an  obtuse-angled  triangle,  with  2  st  7  m  at  some 
distance. 

e  F  ;  R  ;  20";  makes  a  triangle  with  2  st  7  m   

p  B  ;  S  ;  R ;  g  b  M  ;  attached  to,  or  not  much  separated  from,  a  s(:  8  m 
just  S  of  neb,  60"  dist.  [N.B. — The  description  of  this  neb  and  the  next 
agree  so  irell  that  it  seems  highly  probable  they  are  the  same,  this  being 
1"  too  early  in  R  A.  Nevertheless,  on  that  supposition,  there  is  still  a 
rather  unusual  discordance  of  places,  and  as  the  minute  is  quite  distinctly 
written  in  the  original  observations,  I  have  preferred  leaving  the  question 
of  iden  tify  open.] 

Not  v  F ;  S  ;  R  ;  appended  to,  and  very  nearly  n  of,  a  ^:  9  m,  the  preced- 
ing of  2  st,  neb  90"  from  . 

F ;  R ;  g  1  b  M  ;  pos  2°.i  from  a  s(s  10  m  30"  dist   

F  ;  S  ;  R ;  just  n  of  a  $  9  m  

F;  pL;  IE;  glbM;  near  2  st  

B;  L;  IE;  v  g  m  b  M,  to  a  ^  13m   

B;  R;  psvmbM;  60".  [The  degree  (118)  of P  D  is  distinctly  written 
and  rightly  reduced.  Still,  supposing  119  to  be  the  correct  reading,  the 
place  agrees  so  well  with  II.  2,  that  it  is  very  likely  that  nebula  with  a 
mistaken  degree.] 

pB;  S;  IE;  pgmbM  

pF;  S;  R;  or  IE;  vgvlbM;  attached  toa  ^  10  m  in  parallel  

e  e  F ;  close  to  a  Hs   

B  ;  S ;  m  E,  nearly  in  the  parallel ;  v  s  b  M  to  a  13m   

pB;  L ;  pmE;  gbM  

p  B  ;  R ;  gbM;  20"   

pB;  pmE;  gbM;  90";  the  preceding  of  2  

F;  pmE;  gbM;  j';  [the  following  of  2]  

F  ;  p  L  ;  pmE;  2'  1 ;  ij'  br  

e  F  ;  e  S  :  rather  a  doubtful  object ;  situated  among  5  small  stars  

vF;  pL;  R;  vlbM;  90" ;  2  or  3  st  near  it  

p  B  ;  S  ;  R  ;  p  s  b  M  ;  20"  

vF;  R;  glbM;  20"  

pF;  v  S  ;  pmEin  parallel ;  psbM  

vF;  R;  or  IE;  gbM;  15"  

e  F  ;  S ;  R  ;  s  b  M  ;  rather  a  doubtful  object   

v  F;  S;  R;  glbM;  15"  

F  ;  R  ;  gbM;  35"  

p  B  ;  R  ;  glbM;  40";  the  preceding  of  2   

e  F  ;  S  ;  R ;  the  following  and  fainter  of  2  

e  F,  and  feeble,  if  a  neb  ;  pslbM;  vS;  R;  10".  It  follows  a  large  %  • 
Re-examined — it  is  a  nebula. 

e  F;  R  ;  S  ;  15"  follows  a  star  10  m  on  parallel  22s. 5  

e  F;  R   

eF;  L;  R;  vgvlbM;  100";  a  difficult  object   

Double  nebula  ;  individuals  equal ;  e  F ;  R  ;  b  M  ;  20";  follows  a  line  of  4 
st  1 1  and  12  m  somewhat  oblique  to  meridian. 

A  double  neb  ;  both  e  F  ;  S  ;  R ;  follows  an  oblique  line  of  4  stars  10  and 
1 1  m. 

B;  S;  IE;  vsvmbMtoa  #  iim  

pF;  L;  R;  vglbM;  2'  

p  B  ;  S  ;  R ;  20";  precedes  a  *  8  m  37*   

B;  S;  E;  p  sb  M   

e  e  F;  p  L;  40";  very  difficult,  but  certain   


128 


REDUCED  OBSERVATIONS  OF 


No. 


Synon. 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Description,  Remarks,  &c. 


Sweep. 


3999 

4000 
4.001 
4002 
4003 


4004 

4005 

4006 
4007 
4008 
4009 
4010 
401 1 

4012 
4013 
4014 


4015 


III.  190 


23  26  0.6 
6.3 

23  27  20.4 
23  32  59.5 
23  33  7.5 
23  35  59.1 
60.0 
60.2 
23  36  54.5 
56.! 
23  39  1.1 
2.3 

23  41  59.6 
23  49  5.9 
23  49  12.8 
23  50  11. 1 
23  54  10.5 

23  55  56  7 
68.5 
23  56  35.2 
23  57  45-2 
23  59  4-J-7 

41.8 
41.9 
23  59  55.8 
57-i 


146  56  56    !  v  B ;  p  m  E  ;  s  m  b  M  ;  30"  1;  has  a  $  9  m  23'. 5  p,  10"  n   

57    2    I  P  B  ;  1  E ;  first  g,  then  p  s  1  b  M  follows  a  %  8  m  nearly  in  parallel  

128  52  59      p  B  ;  oval;  orpmEjvgbM;  3'   

156  55    o      e  F;  S;  R;  the  p  of  2  ;  pos  from  the  other  =  2100   

156  54  20      e  F;  S;  R;  25";  the  following  and  largest  of  2   

133  52    o      pB;S;R;pgmbM;  25"  

5126      pB;  R;  TSTmbMtoat  14m;  50"  

50  55      B;  S;  IE;  vsmbMtoa  small  round  almost  stellar  nucleus  

120  27  23      F;S;R;glbM;  has  a      12  m  1'  dist  following   

26  46      e  F;  S;  R;  has  a  very  small  :js  following  it  

121  27    7      B;  L;  R;  psbM;  2'  diam  

28  23      B;  Lj  R;  psmbM;  90"  diam   

131  41  *3    I  B;  R;  g  b  M ;  90"  

1344543  !eF;vS;R;lbM  

134  39  48    |vF;vS;R;lbM;  follows  3  st  12,  13,  and  14  ni   

146  24  18    :  pB;  S;  R;  gmbM;  25"   

125  11  40      vF;  S;  R;  among  S  stars  

153    048    j  v  F;  v  S;  R;  gb  M;  12"  

o  40      F;  S;  R;  gb  M;  15"   

134  11  32      eeF;vS;nfa  star  7.8  m  distant  3'   

94  39  5°    i  F  j  R ;  first  v  g,  then  p  s  b  M  ;  has  2  st  9  m  s  f  

120  51  33  eeF;  L;  mE;  requires  the  utmost  attention  to  perceive  though  the  sky 
is  perfectly  pure. 

5°  53    j  v  F  ;  m  E  ;  v  g  v  1  b  M   

51  13    !  vF;  pL;  vmE;  gvlbM;  2'  long  

124  49  17      F ;  p  L ;  R  ;  b  M ;  40"   

48  36      Not  vF;  L;  IE;  glbM;  60"   


504 
735 
737 
508 
508 
639 
728 
489 
494 
495 
495 
494 
737 
489 
489 
732 

493 
736 
726 
489 

739 
620 

495 
494 
635 
493 


APPENDIX. 

Places  and  Descriptions  of  Eight  Nebulae  discovered  by  the  late  Sir  William  Herschel, 

but  not  published  in  his  Catalogues. 
The  Places  are  brought  up  to  1830  by  the  precessions  of  the  determining  Stars. 


Synon. 


III.  982 

in.  983 
11. 908 

IV.  79 

11. 909 

in.  979 
in.  980 
in.  981 


R  A.  1830.0. 
li.  m.   s.  (1. 


8  28  16.2 

8  29  18.2 

8  38  58.2 

9  41  18.0 
9  47  9  ° 


10  10  17.2 


N  P  D.  1830.0. 


16  29  31 

16  35  31 

19  5  31 

19  25  55 

17  3  55 

q  16  c 


Description,  Remarks,  &c. 


Stellar  "|  Two.    The  preceding  is  within  1'  of  a  small  star  which  follows  it,  and 
I     which  is  free  from  the  burr  which  affects  the  Stellar.    III.  983  follows 
v  F;  S  J     24  Bode  Ursae  (Groomb  1457)  3"'  19',  and  is  2°  30'  north  of  that 
J      III.  982  is  6'  n  of  the  other.    Discovered  Sept.  30,  1802. 

p  B  ;  p  L ;  easily  resolvable.  I  believe  I  see  some  of  the  stars  ;  figure  irreg ;  fol- 
lows 24  Bo.  Ursae  (G.  1457)  6"'  59%  and  is  o°  9'  north  of  it.  Discovered  Sept. 
30,  1802. 

A  v  B,  beautiful,  ray  of  light,  about  8'  long,  2'  or  3'  broad ;  brightest  in  the  mid- 
dle of  all  its  lengths.  Follows  27  Ursse  (G.  1563)  14"'  12s,  and  is  2°  27'  south  of 
that  star.    Discovered  Sept.  30,  1802. 

F,  p  L,  R;  the  last  of  3,  the  others  are  II.  333  and  334.  Follows  27  Ursre 
(G.  1563)  20"'  3%  and  is  o°  5'  south  of  it.    Discovered  Sept.  30,  1802. 

Stellar  ~l  Three  in  a  line,  1'  distant  from  each  other.  The  place  is  that  of  the  last, 
v  F  ;  S  >  which  precedes  191  Bode  Camelopardali  (G.  1643)  7"  44-,  and  iso0  38' 
vF;  S)     south  of  it.    Discovered  Sept.  26,  1802. 


129 


SYNOPTIC  TABLE  OE  THE  DATES  OE  THE  SWEEPS  REFERRED  TO  IN  MY 
CATALOGUES  OF  NEBULA,  DOUBLE  STARS,  &c. 


Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

1823 

1827 

July 

Feb. 

Sept. 

Nov 

77 

7 

125 

18 

177 

T  r 

'5 

227 

19  bis 

40 

7° 

r5 

126 

r9 

178 

16 

228 

1825 

41 

4 

79 

16 

ivj.cll  in 

179 

'7 

Dec. 

April 

42 

5 

go 

18 

127 

5 

l80 

18 

229 

16 

IO 

8 1 

21 

128 

I  0  I 

1 8  bis 

2 

3 

1 1 

I023 

82 

23 

129 

9 

,0. 

1 82 

1  2  t-pr 

1 0  cer 

1530 

May 

ivxay 

83 

25 

130 

1 1 

Oct. 

Jan. 

4 

9 

43 

Q 
0 

°4 

20 

131 

1 1  bis 

.0. 
I83 

1 

250 

5 

2 1 

44 

29 

^5 

29 

132 

12 

184 

4 

reo. 

Aug. 

0  uiy 

00 

30 

J33 

12  bis 

.0. 
1X5 

g 

231 

9 

(L 
U 

20 

45 

I 

Aug. 

'34 

12  ter 

186 

9 

232 

10 

4° 

2 

8-7 
°7 

20 

J35 

J3 

I87 

10 

233 

1 1 

7 

4 

Aug. 

88 

2 1 

I3& 

r4 

188 

234 

J9 

8 

7 

47 

5 

89 

22 

137 

16 

189 

28 

235 

20 

9 

9 

48 

r 
O 

90 

24 

!38 

17 

I90 

29 

March 

Oct. 

oept. 

91 

25 

139 

*9 

23b 

1 

4 

IO 

4 

49 

10 

92 

20 

140 

20 

1829 

237 

1 1 

Oct. 

April 

May 

238 

*5 

7 

12 

11 

1827 

93 

12 

141 

7 

I9I 

2 

239 

16 

r3 

12 

J  an . 

94 

!3 

142 

9 

I92 

4 

24O 

r4 

13 

5° 

21 

95 

ID 

!43 

10 

July 

24I 

20 

'5 

!7 

51 

22 

96 

"  ' 
l8 

144 

"3 

193 

2 1 

242 

23 

52 

*3 

97 

H5 

I94 

23 

243 

24 

98 

22 

I4O 

15 

!95 

27 

244 

25 

1620 

99 

147 

16 

196 

29 

245 

25  bis 

Feb. 

1821 

JNov. 

143 

16  bis 

197 

31 

246 

26 

ID 

*3 

May 

100 

1 1 

May 

Aug. 

247 

29 

March 

53 

29 

101 

12 

149 

1 

198 

1 

April 

17 

3 

54 

30 

102 

16 

150 

199 

5 

248 

12 

18 

103 

151 

6 

200 

6 

249 

!3 

4 

17 

J9 

10 

1827 

104 

17  bis 

152 

8 

201 

8 

250 

17 

20 

11 

Jan. 

105 

i53 

9 

202 

20 

251 

J9 

21 

12 

55 

26 

io53 

22 

154 

11 

203 

21 

252 

20 

22 

13 

56 

27 

106 

22  bis 

155 

12 

204 

25 

253 

24 

April 

Feb. 

107 

23 

156 

!3 

205 

29 

254 

25 

23 

1 

57 

17 

108 

24 

i57 

14 

Sept. 

255 

26 

24 

3 

58 

!9 

109 

24  bis 

July 

206 

2 

256 

27 

May 

59 

24 

Dec. 

158 

5 

207 

8 

May 

*s 

6 

60 

25 

1 10 

16 

J59 

6 

208 

12 

257 

>3 

26 

7 

March 

III 

16  bis 

160 

9 

209 

H 

258 

15 

27 

8 

61 

23 

1 12 

17 

161 

!3 

210 

19 

259 

16 

28 

9 

62 

24 

113 

20 

162 

15 

211 

24 

260 

18 

June 

63 

25 

114 

23 

163 

'9 

212 

25 

261 

22 

29 

30 

64 

26 

"5 

24 

164 

19  bis 

213 

29 

262 

24 

July 

65 

30 

116 

25 

,65 

20 

214 

30 

263 

25 

30 

1 

66 

31 

117 

27 

Aug. 

Oct. 

June 

31 

7 

67 

April 

166 

17 

215 

5 

264 

20 

32 

9 

2 

167 

18 

216 

5  bis 

July 

33 

24 

68 

'9 

1828 

168 

r9 

218 

9 

265 

1 1 

34 

3i 

69 

19  bis 

Jan. 

169 

ao 

219 

27 

266 

12 

Aug. 

70 

23 

118 

8 

170 

21 

220 

28 

267 

13 

35 

1 

71 

24 

119 

>3 

Sept. 

221 

3° 

268 

14 

36 

2 

72 

27 

120 

18 

171 

2 

Nov. 

269 

15 

37 

5 

73 

28 

121 

19 

172 

5 

222 

7 

270 

16 

Dec. 

74 

29 

122 

19  bis 

173 

7? 

223 

16 

271 

21 

38 

28 

July 

123 

Feb. 

i74 

1 1 

224 

17 

272 

22 

39 

1  3° 

75 

2 

175 

12 

225 

18 

273 

26 

76 

6 

124 

•7 

176 

12  bis 

226 

'9 

274 

27 

*  Nos.  43  ....  49  are  Sweeps  made  in  1823  which  had  been  mislaid,  having  been  written  on  loose  paper,  and  not 
found  until  after  No.  42.  As  a  renumbering  of  the  intermediate  Sweeps  would  have  created  confusion,  it  was  thought 
better  to  carry  on  the  numbers  in  regular  succession. 

L  L 


130 


SYNOPTIC  TABLE  OF  THE  DATES  OF  THE  SWEEPS 


Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

July 

April 

reb. 

June 

1835 

June 

275 

28 

337 

3 

399 

3 

r  _ 
402 

29 

Jan. 

594 

1 

276 

29 

338 

4 

400 

no  such  f 

July 

528 

1 

595 

2 

Aug. 

339 

5 

401 

7 

463 

1 

529 

2 

596 

16 

277 

10 

34° 

6 

402 

26 

464 

2 

530 

20 

597 

17 

278 

J3 

341 

9 

403 

465 

5 

531 

22 

598 

18 

279 

15 

342 

10 

March 

466 

6 

532 

23 

599 

J9 

280 

do. 

343 

'3 

404 

8 

467 

7 

533 

24 

600 

20 

281 

16 

344 

14 

405 

21 

468 

8 

534 

27 

601 

21 

282 

19 

May 

406 

25 

469 

9 

535 

28 

602 

22 

283 

23 

345 

j 

407 

28 

470 

10 

536 

29 

603 

23 

Sept. 

346 

2 

408 

29 

47' 

12 

537 

do. 

604 

27 

284 

7 

347 

4 

409 

do. 

472 

27 

538 

30 

605 

28 

285 

8 

348 

5 

410 

30 

473 

28 

539 

31 

606 

29 

286 

10 

349 

6 

April 

474 

29 

Feb. 

607 

30 

287 

1 1 

350 

do. 

411 

2 

475 

30 

540 

1 

July 

288 

12 

351 

8 

412 

3 

47  6 

3i 

54i 

2 

608 

»5 

289 

J3 

352 

9 

413 

4 

Aug. 

542 

3 

609 

16 

290 

do. 

353 

do. 

414 

5 

477 

1 

543 

4 

610 

20 

291 

H 

354 

11 

415 

17 

478 

3 

544 

17 

611 

21 

292 

do. 

355 

12 

416 

*9 

479 

4 

545 

20 

612 

22 

293 

16 

356 

14 

417 

20 

480 

7 

546 

21 

613 

do. 

294 

17 

357 

16 

418 

21 

481 

8 

547 

22 

614 

23 

295 

18 

July 

419 

23 

482 

12 

548 

23 

615 

24 

296 

20 

358 

30 

420 

25 

483 

24 

549 

24 

616 

do. 

297 

21 

359 

31 

421 

26 

484 

30 

550 

25 

617 

28 

298 

22 

Aug. 

422 

28 

485 

31 

551 

26 

Aug. 

299 

23 

360 

3 

423 

29 

Sept. 

552 

27 

618 

14 

300 

24 

361 

4 

May 

486 

1 

March 

619 

!5 

301 

25 

362 

5 

424 

1 

487 

3 

553 

1 

620 

18 

302 

do. 

363 

6 

425 

18 

488 

4 

554 

2 

Sept. 

Oct. 

364 

8 

426 

'9 

489 

5 

555 

3 

621 

14 

303 

5 

365 

10 

427 

22 

490 

6 

556 

4 

622 

18 

304 

9 

366 

1 1 

428 

23 

49 1 

21 

557 

•  • 

623 

'9 

305 

10 

367 

12 

492 

23 

558 

20 

624 

do. 

306 

»♦ 

368 

14 

1834 

493 

25 

559 

21 

625 

no  such/ 

307 

15 

Sept. 

March 

494 

27 

560 

22 

626 

21 

308 

16 

369 

3 

429 

5 

495 

28- 

561 

23 

627 

22 

Dec. 

370 

do. 

430 

8 

496 

30 

562 

24 

628 

do. 

309 

13 

371 

6 

43 1 

»3 

Oct. 

563 

26 

629 

24 

310 

'4 

372 

9 

432 

14 

497 

2 

564 

30 

630 

do. 

3ii 

16 

373 

10 

433 

16 

498 

3 

565 

no  such  f 

631 

27 

312 

18 

Oct. 

434 

3« 

499 

4 

566 

31 

632 

no  such  f 

3»3 

do. 

*2  7  A. 

A 
T 

April 

500 

c 
5 

567 

April 

Oct. 

3H 

20 

375 

5 

435 

1 

501 

6 

1 

633 

17 

376 

43  6 

502 

23 

568 

634 

18 

3 

3 

1831 

377 

28 

437 

4 

503 

27 

569 

4 

635 

J9 

Jan. 

378 

29 

438 

6 

504 

28 

57° 

7 

636 
637 

22 

3i5 

6 

379 

31 

439 

10 

5°5 

3° 

57i 

18 

23 

316 

6  bis 

Nov. 

440 

1 1 

506 

31 

572 

20 

638 

do. 

317 

7 

380 

2 

441 

do. 

Nov. 

573 

21 

639 

24 

318 

8 

3«i 

3 

442 

13 

507 

1 

574 

22 

Nov. 

319 

1 1 

382 

4 

443 

28 

508 

2 

575 

do. 

640 

10 

Feb. 

383 

7 

444 

29 

509 

3 

576 

23 

641 

11 

320 

2 

384 

8 

445 

30 

510 

4 

577 

do. 

642 

13 

321 

385 

9 

May 

511 

6 

578 

24 

643 

H 

322 

5 

386 

28 

446 

1 

512 

*3 

579 

25 

644 

18 

323 

9 

Dec. 

447 

2 

5»3 

24 

May 

645 

!9 

324 

10 

387 

9 

448 

3 

5i4 

26 

580 

1 

646 

20 

325 

12 

388 

10 

449 

5 

5i5 

30 

581 

2 

647 

21 

326 

389 

23 

450 

6 

Dec. 

582 

3 

648 

22 

327 

16 

390 

31 

45i 

8 

516 

1 

583 

16 

Dec. 

328 

'7 

452 

10 

5i7 

584 

17 

649 

8 

2 

March 

1832 

453 

13 

518 

3 

585 

18 

650 

9 

329 

7 

Jan. 

June 

5J9 

4 

586 

'9 

651 

10 

330 

8 

39 1 

3 

454 

1 

520 

5 

587 

23 

652 

1 1 

331 

1 1 

392 

4 

455 

3 

521 

6 

588 

24 

653 

13 

332 

»3 

393 

23 

456 

5 

522 

23 

589 

25 

654 

14 

333 

'4 

394 

24 

457 

523 

59° 

26 

655 

15 

334 

17 

395 

25 

458 

8 

524 

26 

591 

27 

656 

do. 

335 

18 

396 

27 

459 

24 

525 

27 

592 

29 

657 

16 

April 

397 

do. 

460 

26 

526 

28 

593 

31 

658 

20 

336 

1 

398 

29 

461 

28 

527 

29 

659 

24 

IN  THE  CATALOGUES  OF  NEBULA. 


131 


Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Sweep. 

Date. 

Dec. 

March 

July 

Oct. 

Jan. 

June 

660 

25 

685 

14 

711 

3 

738 

4 

762 

5 

789 

6 

661 

26 

686 

15 

712 

5 

739 

5 

763 

do. 

790 
791 

7 

687 

16 

713 

6 

740 

9 

764 

do. 

do. 

9 

1836 

688 

18 

714 

741 

12 

765 

25 

792 

8 

Jan. 

689 
y 

22 

715 

7 

742 

13 

766 

27 

793 

27 

662 

8 

600 
y 

25 

716 

do. 

Nov. 

767 

28 

794 

663 

9 

April 

717 

9 

743 

1 

768 

3 1 

sept. 

664 

10 

60  1 

7 

5 

718 

10 

744 

4 

Feb. 

7Q1; 

21 

665 

1 1 

602 

7 

7 

719 

12 

745 

5 

769 

1 

706 

23 

666 

17 

y  j 

15 

720 

13 

746 

8 

770 

do. 

7Q7 

/  j  1 

24 

667 

18 

604. 

721 

do. 

747 

11 

771 

5 

708 

1  J 

do. 

668 

*9 

695 

20 

722 

14 

748 

do. 

772 

7 

799 

*5 

669 

20 

May 

723 

15 

749 

12 

773 

9 

800 

26 

670 

22 

696 

1 1 

724 

do. 

750 

do. 

774 

28 

Nov. 

671 

23 

697 
698 

12 

725 

16 

751 

do. 

March 

801 

28 

Feb. 

18 

Aug. 

Dec. 

775 

2 

802 

29 

672 

8 

699 

do. 

726 

1 1 

752 

4 

776 

3 

803 

30 

673 

9 

700 

r9 

727 

31 

753 

5 

777 

7 

Dec. 

674 

11 

June 

Sept. 

754 

do. 

778 

8 

804 

X 

675 

12 

701 

3 

728 

2 

755 

8 

779 

13 

805 

3 

676 

14 

702 

5 

729 

5 

756 

9 

780 

28 

806 

23 

677 

IS 

703 

6 

730 

do. 

757 

11 

781 

29 

807 

24 

678 

16 

704 

7 

731 

6 

758 

26 

782 

3i 

808 

25 

679 

17 

705 

do. 

732 

1 1 

759 

30 

April 

680 

18 

706 

do. 

733 

12 

783 

1838 

1 

March 

707 

do. 

734 

IS 

1837 

784 

5 

Jan. 

681 

7 

708 

8 

Oct. 

Jan. 

785 

do. 

809 

22 

682 

8 

709 

9 

735 

2 

760 

2 

786 

6 

810 

683 
684 

10 

710 

do. 

736 
737 

3 
4 

761 
761^ 

3 
4 

787 
788 

7 
do. 

132 


LIST  OF  FIGURED  NEBULA  REFERRED  TO  IN  THE  CATALOGUE. 


R  A.  1830. 

NPD.1830. 

No.  in 

Plate. 

Fig. 

Synonyms,  ice. 

E  A.  1830. 

NPD.1830. 

No.  in 

Plate. 

Fig. 

Synonyms,  dec. 

Catal. 

Catal. 

h.  m.  s. 

0 

/ 

h. 

m. 

s. 

0 

130 

IO 

2315 

TV 
1  V  . 

Q 

A.  507. 

5 

41 

J59 

5° 

2950 

TTT 
111. 

4 

(jroup  in  the  Nubecula 

O    ID  20 

163 

2 

2322 

IT  T 
111. 

1 

47  Toucani  (Bo.). 

2951 

Major. 

0  21  ^8 

124 

12 

2327 

VT 

V  1. 

l9 

A.  590  ? 

2952 

O  ^.6  §2, 

125 

37 

2359 

V 
V  . 

10 

A.  530. 

2953 

°  53  l9 

163 

0 

2370 

IV. 

r 
0 

A.  25. 

2954 

1 V  . 

2  26  48 

129 

47 

2487 

VI. 

'4 

A.  519  ?  ? 

7 

9 

40 

102 

55 

3°75 

4 

v  - 
V.  21. 

3  16  58 

1 12 

a 

2534 

VI. 

17 

IV.  77. 

Q 

5 

29 

22 

130 

5 

3131 

VT 
V  1. 

12 

3  27  9 

126 

43 

2552 

IV. 

I 

Nova. 

5 

54 

25 

J35 

'4 

3r45 

V . 

12 

4    5  31 

I23 

r9 

202  I 

V. 

1 1 

A.  600. 

9 

9 

9 

125 

54 

3J54 

V . 

0 
5 

A.  564. 

4  56  52 

I5t) 

43 

27O9 

III. 

3 

Group  in  Nubecula 

9 

55 

'7 

rl5 

2 1 

3221 

"17* 

V . 

9 

27 10 

Major. 

9 

59 

52 

I29 

3b 

3225 

V  1. 

9 

27  1 1 

10 

1 0 

42 

'47 

0 
5 

3239 

TV 
1  V  . 

3 

27 1 6 

10 

1 1 

7 

170 

1 

3241 

VT 
V  1. 

2 

580 

1 59 

11 

2775 

VI. 

1 1 

Nova. 

10 

16 

30 

107 

47 

3248 

VT 
V  1. 

5 

TV 

iv.  27. 

5  J4  29 

'59 

33 

2802 

III. 

6 

Group  in  Nubecula 

10 

27 

145 

47 

3295 

TY 

t]  Argus. 

2503 

Major. 

1 1 

4 

54 

150 

22 

3324 

TV 

x  V . 

10 

2o04 

3325 

25O5 

3326 

28o8 

3327 

- 

5  22  36 

28lO 

3329 

158 

4 

284O 

III. 

2 

Group  in  Nubecula 

333° 

--  0  _}  -. 

Major. 

12 

43 

36 

149 

26 

3435 

I 

2 

2843 

»3 

15 

31 

132 

8 

3501 

TV 
IV. 

2 

A     a  9 1 
_i  .  4°2. 

2844 

I  1 

16 

■37 

116 

35°4 

"IT* 

V . 

7 

to  Centauri. 

2845 

!3 

21 

37 

155 

6 

35M- 

VI. 

1 

A.  252. 

5  26  56 

95 

30 

VIII. 

9  Orionis. 

J3 

27 

28 

119 

0 

3523 

IV. 

5 

185  Centauri  (Bode). 

C   27  O 

94 

57 

II. 

3 

f  I  In (inic 

J3 

40 

18 

140 

22 

1  CA.  T 

VI. 

T  c 
*  J 

5  27  9 

160 

1 

2859 

IV. 

7 

Group  in  the  Nubecula 

!3 

47 

34 

129 

9 

3548 

VI. 

10 

2864 

Major. 

15 

5 

18 

135 

1 

3594 

VI. 

8 

2865 

15 

33 

23 

150 

41 

3610 

VI. 

7 

2872 

16 

2S 

22 

J33 

2 

3641 

V. 

4 

2875 

16 

33 

54 

136 

42 

3644 

V. 

6 

2876 

16 

5° 

24 

119 

5i 

3661 

VI. 

13 

M.  62. 

5  27  45 

158 

58 

2866 

VI. 

20 

Group  in  the  Nubecula 

17 

7 

«9 

141 

33 

3675 

VI. 

6 

2867 

Major. 

17 

10 

37 

128 

18 

3680 

VI. 

3 

2868 

17 

14 

33 

132 

40 

3684i 

V. 

3 

Milky  Way. 

2869 

17 

!9 

2 

113 

37 

3686 

VI. 

4 

IV.  11. 

5  35  55 

157 

41 

2910 

III. 

5 

A  220  and  group  in  the 

r7 

22 

43 

128 

57 

3688 
37°22 

VI. 

18 

Milky  Way. 

2913 

Nubecula  Major. 

17 

34 

31 

123 

37 

V. 

1 

2916 

17 

39 

45 

120 

9 

3707 

V. 

5 

VI.  13. 

2918 

17 

43 

41 

120 

23 

37i3i 

V. 

2 

Milky  Way. 

5  39  7 

160 

'7 

2923 

IV. 

9 

Group  in  the  Nubecula 

17 

5* 

6 

113 

1 

3718 

II. 

2 

IV.  41,  and  V.  1,  2,  3. 

2925 

Major. 

17 

53 

28 

114 

21 

3722 

I. 

1 

M.  8. 

2933 

17 

55 

52 

153 

47 

3727 

VI. 

16 

M.  17. 

2935 

18 

10 

49 

106 

■4 

11. 

1 

2936 

21 

52 

10 

122 

46 

3908 

IV. 

11 

2938 

3909 

2939 

39IO 

5  39  53 

'59 

11 

2941 

II. 

4 

30  Doradus  (Bode). 

3911 

5  4i  •• 

'59 

5° 

2948 
2949 

III. 

4 

Group  in  the  Nubecula 
Major. 

OF  THE 


LAW  OF  DISTRIBUTION 

OF 

NEBULA  AND   CLUSTERS   OF  STARS 

OVER 

THE  SURFACE  OP  THE  HEAVENS. 


(91)  The  distribution  of  nebulae  and  clusters  over  that  portion  of  the  heavens  visible  in 
our  latitudes  is  extremely  unequal.  A  mere  inspection  of  my  Northern  Catalogue  will  suffice 
to  show,  that  an  immense  and  evidently  systematic  inecpiality  exists  among  the  numbers  of 
them  which  occur  in  each  successive  hour  of  right  ascension.  This  is  an  induction  "per 
enumeration  simplicem" — a  mere  matter  of  statistics;  and  its  results  are  not  a  little  remarkable. 
The  following  table  exhibits  a  synoptic  view  of  the  numbers  in  question  : — 


NUMBERS  OF  NEBULAE,  &c,  IN  EACH  HOUR  OF  R  A  IN  MY  NORTHERN  CATALOGUE. 


Hour  of 
R  A. 

No.  of 
Neb. 

Hour  of 
R  A. 

No.  of 
Neb. 

Hour  of 
R  A. 

No.  of 
Neb. 

Hour  of 
R  A. 

No.  of 
Neb. 

Hour  of 
R  A. 

No.  of 
Neb. 

Hour  of 
R  A. 

No.  of 
Neb. 

h  h 

h  h 

h  li 

h  h 

h  h 

h  h 

o  to  I 

89 

4  to  s 

36 

8  to  9 

72 

12   to  13 

44 1 

16  to  17 

32 

20  to  21 

36 

i  ,,  a 

109 

5  ,-,  6 

3* 

9  11  10 

109 

13  ..  H 

214 

17  „  18 

18 

21  ,,  22 

45 

*  „  3 

89 

6  „  7 

56 

10  ,,  11 

'54 

14  ..  '5 

153 

18  ,,  19 

34  ' 

22  ,,  23 

60 

3  „  4 

24 

7  „  8 

55 

11  ,,  12 

271 

15  ,,  16 

42 

19    ,,  20 

37 

23  0 

98 

(92)  It  is  evident  from  this  that  the  great  mass  of  the  nebulae  in  that  part  of  the 
heavens  visible  in  our  latitudes,  is  accumulated  upon  the  six  hours  of  R  A  between  9h  and  15h ; 
on  both  sides  of  which  the  falling  off  is  rapid,  and  after  15h  very  sudden ;  while  within  the  6 
hours  in  question  the  condensation  increases  to  a  very  marked  maximum  between  the  hours 
12  and  13.  Another  maximum,  but  very  much  less  marked,  occurs  between  the  hours  1  and  2, 
and  is  also  gradually  shaded  off  on  the  preceding  side,  and  more  suddenly  on  the  following. 

(93)  The  true  import  of  this  rough  and  simply  statistical  view  of  the  subject  is  not  seen, 
however,  till  we  come  to  project  the  places  of  the  individual  objects  on  a  chart  or  globe,  so  as 
to  obtain  a  distinct  view  of  their  mode  of  grouping,  and  a  measure  of  their  actual  degree  of 
condensation  at  each  point.    For  this  purpose  the  usual  projections  of  the  sphere  are  ill 

M  M 


134 


OF  THE  LAW  OF  DISTRIBUTION 


adapted.  In  the  orthographic  projection,  the  projected  representations  of  the  equatorial  zones 
are  contracted  into  infinitely  narrow  annuli,  while  those  of  the  polar  ones  preserve  their 
natural  magnitude.  In  the  stereographic  projection,  on  the  contrary,  the  equatorial  areas  are 
unduly  dilated  as  compared  with  the  polar.  For  our  purpose  a  projection  is  required  which 
shall  represent  equal  areas  on  the  sphere  by  equal  ones  on  the  projection.  The  following 
construction  will  satisfy  this  condition. 

(94)  Supposing  r  to  be  the  radius  of  the  sphere,  take 

R  =  r  .  V% 

and  with  R  for  a  radius  describe  a  circle.  This  will  be  the  projection  of  one  hemisphere,  and 
its  area  will  be  equal  to  the  surface  of  the  hemisphere.  Now,  to  divide  this  circle  into  annuli 
corresponding  to  zones  of  equal  polar  distance  on  the  sphere,  so  that  the  area  of  each  annulus 
shall  be  equal  to  that  of  the  spherical  zone  of  which  it  is  the  projection,  we  have  only  to 
calculate  a  series  of  radii  according  to  the  formula 

p  =  R  .  S?P  .2.o ;  or  p  =  2  r  .  sin  \  0  ; 

"  sin  4a°  *        r  2  > 

and  with  these  radii  describe  circles  about  the  common  centre,  then  will  each  circle  be  the 
projection  of  a  parallel  of  6°  polar  distance.  To  execute  this  projection  in  fact,  however,  no 
calculation  at  all  is  needed,  for  since  the  radius  of  the  sphere  is  of  no  consequence,  we  have 
only  to  take  out,  upon  any  scale  we  please,  the  successive  values  of  sin  30',  sin  1°,  sin  1°  30', 
and  so  on  to  sin  45°  from  a  table  of  natural  sines  and  these  will  be  the  radii  of  circles 
corresponding  in  our  projection  to  the  successive  polar  distances  1°,  2°,  3°,  .  .  .  .  90°. 

(95)  On  this  principle,  having  constructed  charts  representing  the  northern  and  southern 
hemispheres,  divided  into  zones  of  3°  in  breadth  in  polar  distance,  and  into  hours  of  R  A 
(subdividing  each  of  the  latter  into  quarters),  I  laid  down  the  nebulae  in  each  from  the  joint 
contents  of  both  catalogues,  so  as  to  obtain  a  coup  cTceuil  of  their  distribution  over  the  whole 
heavens.  This,  and  not  the  construction  of  regular  charts  for  publication,  being  the  object  in 
view,  it  was  not  considered  necessary  to  project  each  individual  nebula  in  its  precise  place — 
but  only  to  lay  down,  in  each  rectangular  space  of  3°  of  P  D,  and  15m  of  R  A,  the  true 
number  of  nebulae  which  had  been  found  to  exist  in  that  area,  distributing  them  therein 
uniformly,  and  denoting  each  by  a  round  and  sufficiently  conspicuous  dot.  The  numbers  of 
such  dots  found  to  occur  in  the  several  hours  of  R  A  (which  will  suffice  for  our  immediate 
purpose)  are  expressed  in  PI.  X,  figs.  1,  2,  which  may  be  taken  as  a  synoptic  view  of  the 
distribution  of  the  nebulae  in  both  hemispheres  as  it  results  from  my  own  observations.* 
The  following  are  the  principal  conclusions  which  may  be  drawn  from  this  operation. 

(96)  1st,  The  distribution  of  the  nebulae  is  not,  like  that  of  the  milky  way,  in  a  zone  or 
band  encircling  the  heavens,  or  if  such  a  zone  can  be  at  all  traced  out,  it  is  with  so  many 
interruptions,  and  so  faintly  marked  out  through  by  far  the  greater  part  of  its  circumference, 
that  its  existence  as  such  can  be  hardly  more  than  suspected. 

(97)  2dly,  One-third  of  the  whole  nebulous  contents  of  the  heavens  are  congregated  in  a 

*  There  are  between  300  and  400  nebulae  of  my  Father's  Catalogue  still  unobserved  by  me,  and  which  are  not 
included  in  this  induction.  However,  they  are  for  the  most  part  very  faint  objects,  and  I  have  satisfied  myself 
that  they  would  have  little  or  no  effect  in  modifying  its  conclusions  had  they  been  admitted. 


OF  NEBULuE  AND  CLUSTERS  OF  STARS. 


135 


broad  irregular  patch  occupying  about  one-eighth  of  the  whole  surface  of  the  sphere ;  chiefly 
(indeed  almost  entirely)  situated  in  the  northern  hemisphere,  and  occupying  the  constellations 
Leo,  Leo  minor,  the  body,  tail,  and  hind  legs  of  Ursa  major,  the  nose  of  the  Camelopard,  and 
the  point  of  the  tail  of  Draco,  Canis  venatici,  Coma,  the  preceding  leg  of  Bootis,  and  the  head, 
wings,  and  shoulder  of  Virgo.    This,  for  distinction,  I  shall  call  the  nebulous  region  of  Virgo. 

(98)  3dly,  Within  this  area  there  are  several  local  centres  of  accumulation,  where  the 
nebulse  are  exceedingly  crowded,  viz.  1st,  from  59°  to  62°  of  N  P  D  in  the  13th  hour  of  R  A 
between  the  northern  part  of  Coma  and  the  fore  legs  of  Chara,  as  also  (in  the  same  hour) 
from  72°  to  78°  NPD,  between  the  palm  branch  and  the  northern  wing  of  Virgo,  and  again, 
in  the  same  hour,  from  80°  to  87°  NPDin  the  northern  wing  and  breast  of  Virgo.  North- 
ward the  nebulous  area  terminates  almost  abruptly  with  a  very  rich  patch  between  the  nose  of 
the  Camelopard  and  the  tail  of  Draco.  The  line  of  greatest  condensation  connecting  these 
most  condensed  patches  is  irregular  and  wavy,  without  appearance  of  reference  to  anyone 
particular  centre,  and  the  shading  off,  though  patchy,  is  on  the  whole  gradual. 

(99)  The  southern  portion  of  this  great  nebulous  region  extends  but  little  (at  least  with 
any  marked  intensity)  beyond  the  equator,  though  it  may  perhaps  be  considered  as  prolonged 
by  one  or  two  pretty  rich  patches  in  the  13th  and  14th  hours  of  R  A,  as  far  as  the  141st  degree 
of  N  P  D,  where,  at  all  events,  it  is  abruptly  terminated.  These  patches  occupy  the  point  of 
the  southern  wing  of  Virgo,  and  the  region  about  the  tail  of  Hydra  and  head  of  Centaurus. 

(100)  The  lesser  nebulous  region  in  the  northern  hemisphere  extending  in  R  A  from  about 
22h  to  2h,  and  in  P  D  from  50°  or  60°  NPDto  the  equator  (beyond  which  it  also  projects 
considerably  into  the  southern  hemisphere),  is  much  less  concentrated,  and  has  none  of  those 
densely  congregating  groups  or  centres  of  accumulation  which  form  so  distinct  a  feature  in  the 
other.  Confining  ourselves  at  present  to  its  development  in  the  northern  hemisphere,  it 
occupies  the  chest  and  wing  of  Pegasus  and  the  southern  Fish,  the  area  included  by  the 
connecting  band  of  the  Fishes,  the  northern  Fish,  and  nearly  the  whole  of  Andromeda.  This 
I  shall  call  the  nebulous  region  of  Pisces. 

(101)  Between  these  principal  masses  an  almost  total  disconnection  exists  throughout  all 
the  region  from  16h  to  19h  on  the  one  hand,  and  from  3h  to  6h  on  the  other,  from  the  pole  down 
to  the  equator,  for  the  few  nebulse  sporadically  scattered  over  this  great  area  are  quite 
insufficient  to  convey  any  idea  of  junction,  though  perhaps  a  thread  of  connection  may  be 
traced  across  the  head  and  sword  of  Perseus  through  Camelopardalus,  with  the  dense  mass  of 
nebulse  which  forms  the  northern  limit  of  the  nebulous  region  of  Virgo.  This  barren  region 
includes  the  constellations  Aries,  Taurus,  the  head  and  upper  part  of  the  body  of  Orion, 
Auriga,  Perseus,  Camelopardalus,  Draco,  Hercules,  the  northern  parts  of  Serpentarius,  the 
tail  of  Serpens,  that  of  Aquila,  and  the  whole  of  Lyra. 

(102)  Sporadic  nebulas,  increasing  in  frequency  with  the  increase  of  R  A  from  the  6th 
hour,  over  Canis  minor,  Gemini,  Lynx,  and  Cancer,  lead  gradually,  but  without  any  other 
prevalent  feature  in  their  distribution,  to  the  region  of  Virgo,  and  complete  our  survey  of 
the  northern  hemisphere. 

(103)  In  the  southern  a  much  greater  uniformity  of  distribution  prevails.  If  we  except 
the  two  Nubecula;  (which  are  full  of  nebulas,  and  the  greater  of  which  is  even  richer  in  objects 
of  that  class  than  the  densest  portion  of  the  northern  group),  the  general  character  of  this 


136 


OF  THE  LAW  OF  DISTRIBUTION 


hemisphere  is  that  of  alternating  patches  of  nebulae,  and  vacuities  of  greater  or  less  extent, 
some  of  the  latter,  however,  being  very  extensive.  In  one  of  these  vacuities  in  which  compa- 
ratively few  nebula?  occur  the  south  pole  is  situated,  having  one  nebula,  however,  within  half  a 
degree  of  it  (as  the  north  pole  has  also  one  within  five  or  six  minutes).  This  barren  region 
extends  nearly  15°  on  all  sides  of  the  pole,  and  immediately  on  its  borders  occurs  the 
smaller  nubecula. 

(104)  This  nubecula  is  insulated  from  communication  with  other  nebulous  patches.  The 
case  is  otherwise  with  the  larger  nubecula  which  stands  in  connexion  with,  and  in  termination 
of,  something  approaching  to  a  zone  or  band  of  connected  patches  of  nebulae  which  extends 
along  the  back  of  Dorado,  through  the  following  portion  of  Horologium  across  Eridanus  and 
the  following  portion  of  Fornax,  over  the  paws  and  body  of  Cetus  to  the  equator,  where  it 
unites  with  the  nebulous  region  of  Pisces,  the  nebulae  growing  decidedly  more  frequent  as  we 
approach  that  constellation. 

(105)  One  of  the  most  remarkable  features  in  the  southern  nebulous  system  is  the 
extraordinary  display  of  fine  resolved  and  resolvable  globular  clusters  which  occurs  between 
16h  45m  and  19h  in  R  A  in  the  region  occupied  by  Corona  Australis,  the  body  and  head  of 
Sagittarius,  the  tail  of  Scorpio,  with  part  of  Telescopium  and  Ara.  Here,  in  a  circular  space  of 
18°  in  radius,  we  find  collected  no  less  than  thirty  of  these  beautiful  and  exquisite  objects 
(Nos.  3658,  3661,  3663,  3665,  3666,  3667,  3670,  3671,  3677,  3683,  3690,3692,  3698,  3705, 
3720,  3723,  3726,  3730,  3731,  3736,  3737,  3742,  3743,  3747,  3748,  3749,  3753,  3756,  3763, 
3770).  This  is  certainly  something  beyond  a  mere  accidental  coincidence.  Are  we  to 
suppose  that  in  this  direction  the  visual  ray  encounters  some  branch  of  the  general  nebulous 
system  nearer  to  us  than  the  rest.  Or  are  we  to  connect  it  with  the  very  peculiar  structure  of 
the  Milky  Way  in  this  particular  part  of  its  course,  which  is  here  unlike  in  its  constitution  to 
any  other  portion  of  that  zone,  and  which  passes  diametrically  across  the  circular  area  in 
question.  It  can  scarcely  be  doubted  on  reading  the  descriptions  of  TsTos.  3690,  3720,  3723, 
that  some  at  least  of  these  objects  belong  to  and  form  a  part  of  the  Milky  Way. 

(106)  The  general  conclusion  which  may  be  drawn  from  this  survey,  however,  is,  that  the 
nehulous  system  is  distinct  from  the  sidereal,  though  involving,  and  perhaps,  to  a  certain  extent, 
intermixed  with  the  latter.  The  great  nebulous  constellation  in  the  northern  hemisphere 
which  I  have  called  the  region  of  Virgo,  being  regarded  as  the  main  body  of  this  system, 
and  subtending  at  our  point  of  view  an  angle  of  80°  or  90°,  it  is  evident  that,  supposing  its 
form  to  approach  to  the  spherical,  our  distance  from  its  centre  must  be  considerably  less  than 
its  own  diameter,  so  that  our  system  may  very  well  be  regarded  as  placed  somewhat  beyond 
the  borders  of  its  denser  portion,  yet  involved  among  its  outlying  members,  or  forming  an 
element  of  some  one  of  its  protuberances  or  branches  of  which  the  individuals  are  the  sporadic 
nebulae  confusedly  scattered  over  the  general  surface  of  the  heavens,  and  of  which  the 
prolongation  in  a  direction  tending  towards  the  constellation  Pisces  may  give  rise  to  the 
apparently  denser  grouping  of  the  nebulae  in  that  region. 

(107)  It  must  not  be  left  out  of  consideration,  and  has  been  distinctly  remarked  by  Sir 
Wm.  Herschel  as  an  element  of  whatever  speculation  a  closer  attention  to  this  subject  and  a 
more  perfect  classification  of  nebulous  objects  may  lead  us  to  indulge  in,  that  the  most  con- 
densed portion,  and  what  may  fairly  be  regarded  as  the  principal  nucleus,  of  the  region  of 


OF  NEBULAE  AND  CLUSTERS  OF  STARS.  137 

Virgo  is  situated  almost  precisely  in  one  pole  of  the  Milky  Way.  Taking  that  great 
circle  as  a  horizon,  the  whole  of  that  stratum  forms,  as  it  were,  a  canopy  occupying  the 
zenith,  and  descending  thence  to  a  considerable  distance  on  all  sides,  but  chiefly  on  that 
towards  which  the  North  Pole  lies.  The  phenomena  on  the  other  side  of  the  Milky  Way, 
though  much  less  characteristic,  are  not  altogether  dissimilar,  the  nebulous  region  of  Pisces 
and  Cetus  standing,  on  the  whole,  in  pretty  nearly  the  same  relation  to  that  circle,  the 
most  condensed  part  of  that  stratum  being  elevated  at  an  altitude  of  between  60°  and  70° 
above  its  plane.  If  we  leave  out  of  view  in  this  estimate  the  band  of  clusters  of  the  VII. 
and  VIII.  classes  which  accompany  the  Milky  Way,  and  a  great  many  (probably  the  whole) 
of  which  are  to  be  looked  upon  rather  as  part  and  parcel  of  that  sidereal  zone,  than  as  properly 
belonging  to  the  nebulous  system ;  this  division  of  the  nebulse  into  two  chief  strata,  separated 
(apparently)  from  each  other  by  the  Galaxy,  will  become  much  more  distinct  and  striking. 
Indeed,  there  are  few  features  more  remarkable  in  the  constitution  of  the  Milky  Way  itself 
than  the  comparative  rarity  of  nebulse  of  the  1st,  2nd,  and  3rd  classes  within  its  limits.  I  do  not 
mean  simply  comparatively  with  the  immense  number  of  stars,  but  with  the  area.  The  only  parts 
which  are  exceptions  to  this  rule  are  the  portion  of  its  course  where  it  traverses  the  mass  of 
globular  clusters  already  mentioned,  Art.  (105),  and  that  where  it  passes  through  the  Cross 
and  Centaur,  where  it  encounters  a  faint  prolongation  of  the  nebulous  region  of  Virgo.  In 
any  point  of  view  which  has  hitherto  occurred  to  me,  the  nubeculae  must  be  considered  as 
exceptional.    Their  constitution  is  cpiite  peculiar,  and  will  be  separately  considered. 


OF  THE  CLASSIFICATION  OF  NEBULiE. 

(108)  The  distinction  between  nebulse  and  clusters  of  stars,  must  depend  on  two  very 
different  considerations ;  viz.,  1st,  on  the  power  of  our  instrument  to  distinguish  the  very 
minute  individuals  of  which  a  resolvable  cluster,  or  one  entirely  composed  of  stars,  may 
consist ;  and,  2ndly,  on  the  idea  we  attach  to  the  word  "  nebulous,"  that  is  to  say,  on  the 
distinction  which  we  conceive  to  exist  between  objects  physically  nebulous,  and  objects  only 
optically  so.  An  object  really  composed  of  discrete  stars,  will  appear  nebulous,  or  be  optically 
nebulous  when  it  consists  of  stars  so  small,  or  so  close,  or  both,  as  either  to  be  separately 
indiscernible  by  the  light  of  the  telescope,  or  incapable  of  being  duly  separated  from  each  other 
by  its  defining  and  magnifying  powers.  Under  different  degrees  of  instrumental  imperfection  in 
these  two  respects,  such  an  object  may  offer  any  variety  of  appearance,  from  a  mere  vaporous 
and  barely  discernible  patch  of  light  to  a  brilliant  surface  of  mottled,  or  even  of  sensibly 
uniform  illumination.  The  great  nebula  in  Andromeda,  for  example,  may  be,  and  not 
improbably  is,  optically  nebulous,  owing  to  the  smallness  of  its  constituent  stars,  while  the 
interior  portion  of  those  resolved  clusters  in  which  the  stars  are  described  as  "  running  together 
into  a  blaze,"  or  to  "  have  a  nucleus  of  a  higher  degree  of  condensation"  in  the  centre,  are  so, 
owing  to  their  closeness. 

(109)  As  respects  the  idea  conveyed  by  the  word  nebula,  it  seems  not  easy  to  draw  any 
distinct  and  serviceable  line  of  demarkation  between  objects  optically  and  physically  (i.  e.,  appa- 
rently and  really)  nebulous.  We  have  no  knowledge  of  any  natural  limit,  in  either  direction,  to 

N  N 


138 


OF  THE  CLASSIFICATION 


the  real  size  and  lustre  of  those  self-luminous  bodies  we  call  stars.  Masses  of  luminous  matter, 
as  large  as  mountains  or  planets,  if  congregated  by  millions  at  the  vast  distance  of  a  nebula, 
would  affect  our  sight  armed  with  any  conceivable  amount  of  telescopic  power  we  can  hope 
to  attain,  individually,  no  more  than  the  undistinguishable  particles  of  a  cloud  of  dust  on  a 
sunny  day,  or  than  the  constituent  aqueous  spherules  of  an  actual  cloud  or  fog,  from  which  the 
term  in  question  derives  its  origin.  It  is  between  discrete  and  concrete  forms  of  matter  only 
than  any  true  physical  line  can  be  drawn  between  a  multitude  of  distinctly  separated  bodies, 
whether  greater  or  less,  constituting  a  system,  and  continuous,  solid,  liquid,  or  gaseous  matter 
constituting  a  whole,  or  individual.  No  one  has  yet  considered,  or  is  likely,  I  presume,  to 
consider,  a  nebula  as  a  solid  or  liquid  body  (in  our  sense  of  the  words)  variously  luminous  in 
its  different  parts.  The  gaseous,  or  (to  speak  more  properly)  the  cloudy  form  of  matter  has 
rather  suggested  itself  to  the  imagination  of  those  who  have  speculated  on  this  subject  (for  we 
must  bear  in  mind  that  a  cloud  is  not  a  gas,  but  a  mixture  of  gasiform  with  solid  or  fluid  matter, 
or  both,  in  a  state  of  extreme  subdivision).  It  is  certainly  conceivable  that  a  continuous  tran- 
sparent liquid  or  gaseous  medium  may  be  luminous  throughout  its  whole  substance ;  but  it 
will  be  found,  I  apprehend,  on  a  careful  examination  of  every  case  apparently  in  point,  that 
nature  furnishes  no  example  of  such  a  thing  within  the  limit  of  direct  experience.  Ignited 
liquids  (as  glass,  for  example,  or  melted  nitre,  &c.)  are  demonstrably  only  superficially 
luminous.  Were  it  otherwise,  their  apparent  intensity  of  illumination  would  be  proportional 
to  the  depth  of  melted  matter,  which  is  not  the  case.  Air,  however  intensely  heated  (if 
perfectly  free  from  dust),  gives  out  no  light.  Even  flames  are  more  than  surmised  to  owe  their 
light  to  solid  or  fluid  molecules  existing  in  them  as  such,  and  in  a  state  of  ignition.  The  flame 
of  mixed  oxygen  and  hydrogen  can  hardly  be  doubted  to  owe  what  little  light  it  possesses  to 
intermixed  impurities,  and  in  the  flames  of  carbonaceous  matters,  and  others  where  metals  or 
phosphorus  are  burned  and  fixed  oxides  generated,  the  intensity  of  the  light  bears  an  evident 
proportion  to  the  fixity  of  the  ignited  molecules,  on  whose  surfaces  it  may  be  presumed  to 
originate  by  some  unknown  electric  or  other  process. 

(110)  Waving,  however,  the  question  as  to  the  constitution  of  flame  (which  I  suppose  no 
one  will  be  disposed  to  contend  for  as  the  material  of  a  nebula),  there  is  no  want  of  examples  of 
luminous  bodies  floating  in,  or  intermingled  with,  non-luminous  transparent  media.  The 
luminous  appearance  of  the  sea,  which  is  due  to  organized  beings,  sometimes  of  large  dimen- 
sions, is  a  familiar  instance.  On  the  solar  envelope,  too,  of  whose  fluid  nature  there  can  be 
no  doubt,  we  clearly  perceive  by  our  telescopes  an  intermixture  (without  blending  or  mutual 
dilution)  of  two  distinct  substances  or  states  of  matter;  the  one  luminous,  the  other  not  so, 
and  the  phenomena  of  the  spots  and  pores  tend  directly  to  the  conclusion  that  the  non- 
luminous  portions  are  gaseous,  however  they  may  leave  the  nature  of  the  luminous  doubtful, 
and  suggest  the  idea  of  radiant  matter  floating  in  a  non-radiant  medium,  and  having  a  ten- 
dency to  segregate  itself  by  subsidence,  after  the  manner  of  snow  in  air,  or  precipitates  in  a 
liquid  of  slightly  inferior  density. 

(111)  Between  a  cloud  or  mist,  and  a  shower,  there  is  no  real  distinction,  but  that  in  the 
latter  the  globules  are  large  enough  to  overcome  the  resistance  of  the  medium  in  which  they 
exist,  and  acquire  a  greater  or  less  velocity  of  descent.*    If  water  were  nearly  of  the  same 

*  "Waving  the  question  as  to  the  supposed  vesicular  state  of  water  in  clouds  and  mists. 


OF  NEBULAE  AND  CLUSTERS  OF  STARS. 


139 


specific  gravity  as  air,  it  might  be  scattered  through  our  atmosphere  in  large  globes,  with  no 
more  tendency  to  fall  in  rain  than  at  present  in  a  cloud,  as  we  see  in  immiscible  liquids  of 
nearly  the  same  specific  gravity  shaken  together.  Now  there  is  nothing  to  prevent  our 
generalizing  the  notion  of  a  luminous  cloud,  and  suppose  the  possibility  of  masses  of  luminous 
matter — of  whatever  density  or  variety,  of  whatever  bulk  or  minuteness — forming  a  connected 
system,  and  prevented  from  collapse  or  from  mutual  interference,  by  the  resistance  of  a  trans- 
parent and  non-luminous  medium,  which  shall  serve  them  as  a  common  vehicle,  and  perform 
other  useful  cosmical  offices  to  them.  Such  an  idea,  as  a  matter  of  pure  speculation,  has  even 
something  inviting  in  it,  as  rendering  in  some  degree  conceivable  the  solution  of  a  problem 
otherwise  almost  inapproachable, — I  mean  that  of  the  stability  of  a  cluster  of  stars  in  the 
state  of  apparent  condensation  in  which  we  see  so  many  of  those  wonderful  systems.  The 
dynamical  equilibrium  (if  I  may  use  such  a  phrase  to  express  internal  mobility  of  parts,  accom- 
panied with  a  conservation  of  outward  form  and  regular  condensation  towards  a  centre)  of  a 
globular,  elliptic,  or  other  cluster  of  totally  disconnected  stars,  acted  on  only  by  central  forces, 
cannot  certainly  be  denied  as  an  abstract  possibility ;  nay,  under  one  very  peculiar  condition 
(that  of  a  uniform  distribution  of  stars  in  a  sphere)  we  perceive  it  to  be  so,  and  that  such 
equilibrium  must  subsist.  But  beyond  this  case  we  cannot  reason  distinctly ;  and  it  certainly 
becomes  exceedingly  difficult  to  conceive  the  conditions  of  conservation  of  such  a  system  as 
that  of  w  Centauri,  or  47  Toucani,  &c,  without  admitting  repulsive  forces  on  the  one  hand,  or 
an  interposed  medium  on  the  other,  to  keep  the  stars  asunder. 

(112)  Such  a  mixed  system  might  admit  of  a  statical  instead  of  a  dynamical  equilibrium, 
the  interposed  medium  serving  to  propagate  pressure  and  give  unity  to  rotation,  so  as  to  bring 
its  movements  and  figure  under  the  Newtonian  laws  of  rotatory  equilibrium.  Nay,  if  we 
choose  to  give  the  reins  awhile  to  speculation,  and  admit  the  gradual  absorption  of  such  a  fluid, 
it  is  far  from  inconceivable  that  a  system  of  orbitual  movements  might  become  established 
among  its  members ;  at  first  entirely,  but  gradually  less  and  less  under  the  conservative  control 
of  its  resistance  and  impulse,  as  they  approached  in  their  forms,  magnitudes,  and  other  elements, 
to  a  final  state,  in  which  the  absorption  of  the  medium  should  be  total,  and  the  system  dynami- 
cally stable,  under  conditions  of  adjustment,  such  as,  in  an  infinitely  simpler  form  of  enuncia- 
tion, preserve  the  stability  of  our  planetary  system. 

(113)  But  such  a  medium  is  purely  hypothetical.  We  see,  after  all,  only  the  luminous 
portions  of  a  nebula,  and  can  have  no  other  knowledge  of  their  aggregation  or  segregation 
than  what  our  telescopes  afford  us.  The  distinction  between  nebulae  properly  so  called,  and 
those  which  we  are  to  consider  as  certainly  or  very  probably  clusters  of  stars,  resting,  as  it  must 
do,  on  the  merely  temporary  and  conventional  ground  of  the  capacity  or  incapacity  of  our 
telescopes,  wholly  or  partially  to  resolve  them,  can  never  become  a  permanent  ground  of 
classification,  since  every  new  improvement  in  the  powers  of  the  telescope  will  cause  more  and 
more  nebulae  to  pass  into  the  class  of  clusters. 

(114)  Nevertheless,  granting  it  to  be  impracticable  to  draw  any  clear  line  of  separation 
between  nebulas  and  clusters,  yet  their  degree  of  resolvability,  connected  as  it  is  with  the  abso- 
lute brightness  of  their  constituent  stars,  and  their  distance  from  us,  must  always  form  an 
important  character  in  their  description,  and  is  fully  as  much  entitled  to  be  received  as  an 
element  in  their  classification  as  their  total  brightness,  or  degree  of  condensation  about  a 
centre,  &c.     It  has  already  been  remarked,  Art.  (44),  as  the  result  of  a  very  extensive 


140 


OF  THE  CLASSIFICATION 


induction,  that  the  normal  form  of  what  may  be  called  Regular  Nebulae  is  the  Elliptic,  admit- 
ting every  degree  of  ellipticity,  from  the  spherical  to  the  linear  form  ;  every  law  of  condensa- 
tion, from  the  circumference  to  the  centre  of  the  apparent  outline,  from  a  uniform  disc  to  a 
star-like  centre,  surrounded  with  faint  and  gradually  fading  nebulosity;  every  grade  of  bright- 
ness, from  an  object  like  w  Centauri  distinctly  visible  to  the  naked  eye,  to  the  feeblest  third-class 
nebula,  barely  discernible  with  the  best  telescopes  ;  and  every  shade  of  resolvability,  from 
stars  distinctly  numerable  even  in  the  middle,  to  a  total  absence  of  any  suspicion  of  stars 
indicated  by  the  slightest  mottling  of  surface.  Another  feature,  common  to  all  nebulae  of  this 
class,  is  the  diminution  observable  in  the  ellipticity  of  their  strata  from  without  inwards,  so  as 
to  approach  to  a  spherical  nucleus,  however  elongated  their  extreme  elliptic  outline. 

(115)  When  sensible  objects  possess  no  qualities  but  such  as  are  common  to  them  all,  and 
differ  only  in  the  greater  or  less  degree  in  which  those  qualities  are  present  in  them,  the  only 
classification  they  admit  is  evidently  a  classificatio  per  gradus — one  grounded  on  the  measured 
or  estimated  intensities  with  which  those  several  qualities  co-exist  in  the  same  individual. 
Classes  (or  rather  subclasses)  founded  on  such  gradations  are  purely  arbitrary,  and  admit  of  no 
natural  lines  of  demarcation.  If  minerals,  for  example,  differed  from  each  other  only  in 
respect  of  hardness,  transparency,  and  specific  gravity,  it  would  be  a  question  of  pure  conve- 
nience, how  many  degrees  of  these  qualities  we  might  choose  to  regard  as  distinct  from  each 
other,  and  consequently  how  many  classes  we  could  form  by  their  combination,  in  the  absence 
of  exact  numerical  statement,  which,  when  attainable  in  each  particular,  goes  to  abolish  the 
idea  of  sub-classes  altogether,  by  assigning  to  each  individual  its  precise  place  in  the  more 
general  class.  As  regards  the  division  of  our  great  class  of  Regular  nebulae  into  sub-classes, 
it  will  amply  suffice  to  recognize  in  each  character  five  degrees — two  extreme,  and  three  medial. 
Pursuant  to  this  idea  I  would,  therefore,  propose  the  following  system  of  numerical  sub- 
classification  and  nomenclature : — 


SUB-CLASSIFICATION  OF  REGULAR  NEBULAE.    CLASS  I. 


Sub-class 
in  respect 
of 

Magnitude. 

Brightness. 

Roundnesj. 

Condensation. 

Resolvability. 

1 

Great. 

Lucid. 

Circular. 

Stellate. 

Discrete. 

2 

Large. 

Bright. 

Round. 

Nuclear. 

Resolvable. 

3 

Middle-sized. 

Faint. 

Oval. 

Concentrate. 

Granulate. 

4 

Small. 

Dim. 

Elongate. 

Graduating. 

Mottled. 

5 

Minute. 

Obscure. 

Linear. 

Discoid. 

Milky. 

(116)  As  regards  concentration,  a  nebula  may  have  a  double  class,  since  the  law  of  con- 
densation may  be  infinitely  varied,  so  as  to  render,  for  example,  such  combinations  as  Discoid- 
nuclear,  mottled-stellate,  &cc,  not  incompatible.  In  fact,  the  heavens  furnish  many  such  instances. 
Comparatively  speaking,  however,  they  are  rare,  and,  for  the  purposes  of  general  classification, 
to  serve  for  the  formation  of  a  catalogue  of  nebulae,  such  as  I  hope  to  see  one  day  constructed, 
the  distinctive  character  in  respect  of  concentration  may  always  be  satisfactorily  indicated  by  a 
single  epithet  or  number,  leaving  the  few  remarkable  cases  to  be  specially  noticed. 

(117)  The  utility  of  the  system  thus  proposed,  in  affording  in  very  small  compass  a  good 


OF  NEBULAE  AND  CLUSTERS  OF  STARS. 


141 


deal  of  information  respecting  the  physical  (or  optical)  characters  of  a  nebula,  in  thus  rendering 
possible  a  general  descriptive  catalogue  of  convenient  magnitude  for  reference,  will,  I  am 
disposed  to  think,  be  found  considerable.  It  is  not  necessary,  to  this  end,  to  write  or  print 
the  words  at  length,  or  even  to  arrange  the  numbers  separately  into  columns.  Such  a  com- 
bination as  I.  22435,  when  once  the  system  is  familiar,  is  quite  as  distinct  as  if  each  figure  were 
placed  in  a  separate  column  with  appropriate  heading,  and,  after  a  little  practice,  cpiite  as  intel- 
ligible as  if  for  each  number  its  appropriate  word  were  written.  Thus  the  above-mentioned 
combination  reads  as  follows  : — A  nebula  of  the  1st  class  (i.e.  regular),  large,  bright,  elongate, 
concentrate,  milky,  a  description  which  readily  recalls  to  the  imagination  such  an  object  as  is 
represented  in  our  figure  19,  PI.  VI.,  while  (to  express  our  meaning  by  a  few  more  instances) 
the  combinations — 

I.  32155— or  Middle-sized,  Bright,  Round,  Discoid,  Milky. 

I.  11242 — Great,  Lucid,  Round,  Graduating,  Resolvable. 

I.  11325— Great,  Lucid,  Oval,  Nuclear,  Milky- 
will  satisfactorily  express  such  objects  as  are  represented  respectively  in  PI.  V.  fig.  8,  of  this 
volume,  fig.  88  of  my  northern  catalogue,  and  PI.  IV.  fig.  5  of  this,  or  185  Centauri.  In  such  a 
system  of  abbreviation,  o,  or  zero,  in  any  place,  might  indicate  the  absence  of  information  as  to 
the  appropriate  particular. 

(118)  In  this  sub-classification,  which  is  founded  solely  on  the  optical  aspect  of  the  nebulae, 
without  reference  to  any  notions  we  may  entertain  of  their  intimate  nature,  both  globular  clus- 
ters and  planetary  nebulae  are  included,  the  essential  characters  of  the  former  being  roundness 
and  resolvability  in  their  higher  or  highest  degrees,  and  that  of  the  latter  a  simply  discoid  round 
or  slightly  oval  appearance,  with  or  without  a  stellar  nucleus.  Nevertheless,  these  bodies,  in 
their  best  characterized  state,  are  so  remarkable,  that,  without  prejudice  to  their  being  duly 
included  in  the  general  classification,  it  will  be  well  to  retain  for  them  these  distinctive  names, 
and  to  mark  them  for  attention  by  special  characters,  such  as  ©  and  Q,  which  in  a  catalogued 
arrangement  may  be  appended  to,  or  substituted  for,  the  Roman  numeral  I.  expressive  of  their 
class.    Thus,  ®  22232  and  O  33355  would  be  read,  respectively — 

A  globular  cluster,  Large,  Bright,  Round,  Concentrate,  Resolvable,  and 
A  planetary  nebula,  Middle-sized,  Faint,  Oval,  Discoid,  Mottled. 

I  should  observe  that  in  this  nomenclature  the  term  resolvable  is  to  be  understood  in  a 
somewhat  stronger  sense  than  it  was  originally  used  by  Sir  W.  Herschel,  and  hitherto  by 
myself — that  is  to  say,  not  as  implying  merely  a  suspicion  of  consisting  of  stars,  but  that  sort 
of  partial  resolution  which  leaves  no  room  for  doubt  as  to  the  object  consisting  of  stars,  though 
they  are  not  seen  so  well  insulated  from  each  other  as  is  implied  in  the  term  Discrete. 

(119)  Annular  nebulae  belong,  no  doubt,  to  the  general  class  of  regular  or  symmetrical 
nebulae,  and  in  the  full  generality  of  the  expression  of  the  law  of  condensation,  which  of  course 
admits  of  an  internal  vacuity,  it  would  suffice  to  add  a  sixth  number  and  word  (6,  Annular)  to 
our  column  headed  Condensation ;  and  the  occurrence  of  the  number  6,  or,  for  distinction's  sake, 
a  capital  A  in  the  numerical  exponent  of  the  sub-class,  would  sufficiently  mark  the  character  of 
such  an  object.  As  there  are  so  few  objects  of  this  kind  known,  it  is  hardly  worth  while  to 
make  a  class  apart  for  them,  but  in  such  an  arrangement  as  I  am  now  proposing,  the  word 

o  o 


142 


OF  THE  CLASSIFICATION 


Annular  at  full  length  might  conveniently,  on  that  very  account,  be  substituted  for  the  whole 
numerical  combination  in  question — {thus,  I.  Annular).  In  this  view  they  would  be  considered 
as  a  sub-class  apart,  and  this  distinction  at  least  they  merit,  if,  as  is  most  probable,  their 
physical  structure  be  that  of  hollow,  elliptic,  or  spherical  shells  of  stars,  as  I  have  already 
before  suggested,  Art.  (53). 

(120)  Double  Nebula,  like  double  stars,  may  be  either  optically  or  physically  double ;  but 
as  we  are  here  deprived,  at  least  at  present,  of  the  criterion  of  orbitual  motion,  I  should  feel 
disposed  to  include  under  this  head  those  cases  only  in  which  two  nebulae  of  the  regular  kind 
are  so  near  each  other  as  to  mix  their  nebulosities,  or  to  be,  as  it  were,  included  one  in  another, 
or  if  disjoined,  yet  so  close,  or  otherwise  so  related  in  appearance,  as  very  strongly  to  suggest 
the  notion  of  a  real  vicinity  in  space,  and  therefore  of  probable  physical  connection.  In  the 
very  remarkable  case  of  M.  62,  which  is  a  double  globular  cluster,  or  one  such  cluster  with 
another  included  within  it  (Fig.  13,  PI.  VI.  of  this  volume),  and  in  the  cases  of  the  nebulae 
represented  in  figs.  68,  69,  70,  and  71  of  my  northern  catalogue,  it  seems  impossible  to  doubt 
such  physical  connection.  As,  however,  no  instance  has  yet  occurred  in  which  the  individuals 
of  such  a  pair  do  not  each  belong  to  the  regular  (i.e.  elliptic  or  spherical)  class,  it  does  not 
appear  necessary  to  erect  a  separate  class  for  them,  but  rather  to  regard  them,  as  we  have  done 
with  the  annular  nebulae,  as  a  peculiar  (though  very  interesting)  sub-class  of  regular  nebulae,  to 
be  specially  designated  in  the  few  cases  where  their  closeness  is  such  as  to  prevent  their  being 
separately  entered  in  a  catalogue,  which  may  be  done  by  the  letter  D  affixed  to  the  numeral 
expression  of  the  sub-class  of  the  principal  individual,  or  by  special  description  in  a  note. 

(121)  We  come  now  to  consider  the  next  great  division  of  our  nebulous  system 
II.  Irregular  Nebulce,  in  which  class  may  be  comprehended  all  which,  to  a  want  of  complete 
and  in  most  instances  even  of  partial  resolvability  by  the  power  of  the  20-feet  reflector,  unite 
such  a  deviation  from  the  circular  or  elliptic  form,  or  such  a  want  of  symmetry  (with  that 
form)  as  precludes  their  being  placed  in  class  I.,  or  that  of  Regular  Nebulae.  This  second  class 
comprises  many  of  the  most  remarkable  and  interesting  objects  in  the  heavens,  as  well  as  the 
most  extensive  in  respect  of  the  area  they  occupy.  Such,  for  instance,  as  the  great  nebulae  about 
6  Orionis,  ??  Argus,  c  Orionis,  and  k  Cygni,  as  well  as  those  smaller  but  still  very  extensive 
and  most  singular  objects,  IV.  41,  8  Messier,  17  Messier,  30  Doradus,  &c. ;  the  partially 
symmetrical  forms  M.  51,  M.  27,  and  M.  64,  &c. ;  and  a  variety  of  others. 

(122)  To  subdivide  this  class  would  almost  be  to  create  as  many  sub-classes  as 
individuals,  such  is  the  capricious  variety  of  their  forms  and  general  aspect.  In  consequence 
I  shall  not  attempt  it,  but  content  myself  with  specifying  as  matter  of  nomenclature,  a  few 
terms  which  express  characteristic  features  in  their  appearance,  accompanying  each  with  one  or 
more  examples. 

1.  Sub-regular  nebulae,  or  those  which  possess  a  certain  degree  of  symmetry,  and  an 
evidently  systematic  structure.  Such  are  M.  51,  M.  27,  M.  64,  figured  in  figs.  25,  26,  27, 
of  my  Northern  Catalogue,  and  PI.  IV.  fig.  1,  PI.  VI.  figs.  1  and  2,  of  this  volume. 

2.  Compact;  such  as  V.  21,  (PI.  4,  fig.  4)  M.  78  =h.  368  (fig.  36,  Northern  Catalogue)  &c. 

3.  Branching;  as  0  Orionis;  V.  14,  and  15;  (figs.  33  and  34  of  Northern  Catalogue);  c 
Orionis  (PI.  II.  fig.  3,  of  this  volume). 

4.  Convoluted;  as  M.  17,  Plate  II.  fig.  1. 


OF  NEBULiE  AND  CLUSTERS  OF  STARS. 


143 


5.  Cellular;  30  Doradiis;  M.  8;  h.  2093  (fig.  82,  N.  Cat.)  shown  by  Mason  to  be 
connected  with  and  to  form  a  part  of  V.  14.  As  the  annular  form  may  be  conceived  to 
originate  in  a  spherical  or  ellipsoidal  envelope,  enclosing  a  hollow  space  of  similar  form  within 
it,  so  may  also  this  kind  of  appearance  in  a  nebula  be  conceived  to  originate  in  an  actual 
cellular  structure  of  the  nebulous  mass,  or  in  convoluted  and  mutually  intersecting  sheets  or 
folds  of  a  nebulous  stratum  variously  penetrated  by  the  visual  ray. 

6.  Fissured ;  IV.  41,  PL  II.  fig.  2,  h.  3501  (PL  IV.  fig.  2). 

7.  Cometic;  PL  VI.  figs.  17,  18,  &c. 

(123)  In  a  synoptic  catalogue  of  nebulae  it  would  hardly  be  necessary  to  indicate  in 
addition  to  the  class  II.  to  which  they  belong,  any  other  particulars  than  those  which  refer  to 
magnitude  and  brightness,  for  which  the  two  first  columns  of  the  synoptic  view  of  the 
sub-classes  of  class  I.  furnish  sufficient  means.  Thus  II.  1.1,  will  indicate  a  great  and 
brilliant  irregular  nebula — II.  3.3,  a  middle-sized  (common-sized)  and  faint  one.  As  nebulae 
of  this  class  will  necessarily  be  objects  of  especial  interest  to  every  observer,  it  will  answer 
every  purpose  in  the  synoptic  catalogue  which  indicates  their  places,  to  give  him  some  notice 
of  this  kind  that  he  may  be  enabled  to  judge  how  far  the  magnifying  power  and  light  of  his 
telescope  may  be  expected  to  show  him  its  peculiarities — or  whether  he  may  expect  to  see  it 
at  all. 

(124)  The  third  principal  class  or  subdivision  of  these  objects  is  that  of  Irregular  Clusters. 
This  class  will  comprehend  all  the  clusters  designated  by  Sir  W.  Herschel  as  of  the  VII.  and  VIII. 
classes,  and  such  of  those  of  his  VI.  class  as  are  irregular  in  their  form,  and  canuot  be  referred 
to  the  class  of  Globular  Clusters.  It  will  suffice  to  divide  them  into  three  sub-classes  III.  1, 
III.  2,  and  III.  3,  according  to  their  general  impression  on  the  eye,  without  descending  into 
minutiae  of  detail  which  admit  of  infinite  variety,  according  as  we  regard  their  richness  in  stars, 
the  magnitudes  of  their  constituent  stars,  their  size,  general  form,  or  degree  of  concentration 
towards  one  or  more  centres.  III.  1,  in  this  view  will  indicate  a  rich,  brilliant,  and  conspicuous 
cluster;  III.  3,  a  poor  and  inconsiderable  one;  and  III.  2,  such  a  one  as  cannot  properly  be 
characterized  in  either  of  these  forms  of  expression.  This  is  quite  sub-division  enough  for 
every  useful  purpose. 


OF  THE  TWO  NUBECULA  OR  MAGELLANIC  CLOUDS. 

(125)  The  general  appearance  of  these  objects  to  the  naked  eye  in  a  clear  night  and  in  the 
absence  of  the  moon  (whose  light  completely  effaces  the  lesser  and  almost  also  the  larger 
of  them),  is  that  of  pretty  conspicuous  nebulous  patches  of  about  the  same  intensity  with  some 
of  the  brighter  portions  of  the  milky  way.  That  such  is  their  aspect  as  regards  their 
impression  on  the  unassisted  eye  of  others  as  well  as  my  own,  is  evident  from  what  is  said  of 
them  by  Lacaille  (Acad.  Sci.  1775,  p.  195)  and  by  M.  Riimker  (Preliminary  Catalogue,  &c. 
Hamburgh,  1832,  p.  17).  Whether  their  figures  in  Phil.  Trans.  1828,  i.,  which  are  stated  to 
have  been  engraved  from  "  very  correct  drawings,"  are  eye-drafts  or  telescopic  representations, 
their  author  has  not  informed  us.    If  the  latter,  I  am  unable  to  reconcile  them  with  my  OAvn 


144 


OF  THE  TWO  NUBECULA. 


observations  as  regards  the  greater  part  of  their  details.  If  the  former,  they  certainly  tend  to 
convey  such  a  conception  of  their  appearance  as  must  inevitably  create  a  sentiment  of 
disappointment  in  the  mind  of  any  one  (as  I  confess  it  did  in  mine)  who,  having  his 
imagination  excited  by  representations  so  striking  and  extraordinary,  is  presented  for  the  first 
time  with  a  view  of  the  real  objects.  I  consider,  therefore,  that  it  will  not  be  irrelevant  to  lay 
before  the  reader  such  representations  as  I  have  been  able  to  make  of  them,  entirely  icithout 
telescopic  aid,  when  seated  at  a  table  in  the  open  air,  in  the  absence  of  the  moon,  and  with  no 
more  light  than  absolutely  necessary  for  executing  a  drawing  at  all.  See  Plate  IX.  figs.  1  and 
2.  They  are  copied  from  one  of  my  working  charts  (pricked  off,  as  to  the  positions  of  the 
more  conspicuous  stars  from  Bode's  Atlas,)  and  on  the  same  scale  as  the  originals.  It  will 
not  fail  to  be  noticed  that  the  situations  occupied  by  both  nubeculae  with  respect  to  the 
surrounding  stars,  especially  by  the  nubecula  minor,  is  very  different  from  what  is  represented 
in  Bode's,  and  in  many  other  charts  and  globes  in  common  use.  I  ought  to  add  that  all  my 
own  attempts  to  delineate  other  than  very  small  portions  of  the  nubecula  major  from  the 
telescope,  have  been  completely  baffled  by  the  overwhelming  complexity  of  its  details.  The 
lesser  cloud  is  less  complex — but  for  that  very  reason  less  interesting. 

Of  the  Nubecula  Minor. 

(126)  The  Nubecula  Minor  is  situated  between  the  parallels  of  162°  and  165°  N  P  D, 
and  between  the  meridians  of  0h  28m  and  lh  15m  RA.  It  is  of  a  generally  round  form  to  the 
unaided  eye,  nor  can  any  very  material  deviation  of  its  centre  of  brightness  from  its  centre  of 
figure  be  noticed.  As  seen  in  the  telescope,  however,  the  most  conspicuous  and  resolvable 
region  appears  to  lie  somewhere  about  0h  45m  30s  R  A,  and  164°  16'  N  P  D,  which  is 
somewhat  to  the  south  of  its  middle.  It  is  preceded  at  a  few  minutes  distance  in  R  A,  by 
the  magnificent  globular  cluster  47  Toucani  (Bode),  but  is  completely  cut  off  from  all 
connection  with  it ;  and  with  this  exception,  its  situation  is  in  one  of  the  most  barren  regions 
of  the  heavens.  I  cannot  better  describe  its  general  insulation  than  in  the  words  of  a 
memorandum  in  the  Gage-book  sweep  745.  "  The  access  to  the  Nubecula  Minor  on  all  sides 
is  through  a  desert."  Neither  with  the  naked  eye  nor  with  a  telescope  is  any  connexion  to  be 
traced  either  with  the  greater  nubecula  or  with  the  milky  way.  In  order  to  convey  a  better 
idea  as  well  of  this  kind  of  insulation  as  of  the  general  character  of  the  nubecula  itself,  I  shall 
here  bring  into  one  view  such  incidental  notes  respecting  these  points  as  I  find  scattered  up 
and  down  in  the  journals  of  my  sweeps,  and  of  the  accompanying  gages,  noted  in  the  intervals 
of  actual  observation. 

(127)  Zones  including  or  passing  through  the  Nubecula. 

Sweep  441.— (Sub  Polo)— Zone  162°  ....  165°. 
"  Oh.  30m.  R  A  164°  27'  P  D.    The  edge  of  the  smaller  cloud  comes  on  as  a  mere  nebula. 
"  Oh.  40m.  53-6s.— 164°  24'  7"  (a  nebula).    In  the  edge  of  the  cloud,  vision  bad,  objects  faint  and  much 
light  cut  off  by  tree  tops,  but  the  cloud  is  not  resolved,  and  seems  a  very  mysterious  object." 

Sweep  482.— Zone  162°  ....  165°.    August  12,  1834. 
"23h.  19m.    Began.    The  ground  of  the  sky  very  decidedly  but  not  very  richly  dotted  rather  than 
'  stippled'  with  faint  stars  *.    Stars  of  9,  10,  11,  12  magnitudes  are  sparingly  scattered  over  it." 


*  For  this  phenomenon  see  more  hereafter. 


OF  THE  TWO  NUBECULA. 


145 


"  Oh.  2m.  The  lesser  nubecula  is  now  approaching,  but  I  discern  no  indications  in  the  field  throughout 
the  zone  which  should  lead  to  expect  any  remarkable  object.  On  the  contrary,  the  stippled  or  dotted 
appearance  mentioned  at  23h.  19m.  is  gone  and  the  ground  is  black." 

"Oh.  13m.  6-5s.  163°  5'  55".  There  is  now  a  great  increase  of  st.  13m.  in  the  field.  On  further  examina- 
tion they  appear  to  be  the  outliers  of  the  great  globular  cluster"  (47  Touc.)   This  cluster  "  is 

completely  insulated.  After  it  has  passed,  the  ground  of  the  sky  is  completely  black  throughout  the 
whole  breadth  of  the  sweep." 

"  Oh.  29m.  7'3s.    The  field  begins  to  show  more  stars  and  to  be  alive." 

"Oh.  37m.  5-ls.  We  are  now  in  the  cloud.  The  field  begins  to  be  full  of  a  faint  light,  perfectly  irresolv- 
able." 

"  Oh.  46m.  3-7s.  164°  19'  23".  I  should  consider  about  this  place  to  be  the  body  of  the  cloud  which  is  here 
fairly  resolved  into  excessively  minute  stars,  which,  however,  are  certainly  seen  with  the  left  eye." 

"  lh.  9m.  50-2s.  Re-examined  by  the  side  motion  the  whole  cloud  in  detail  and  in  general.  The  main 
body  is  resolved,  but  barely.  I  see  the  stars  with  the  left  eye.  It  is  not  like  the  stippled  ground  of 
the  sky.  The  borders  fade  away  quite  insensibly  and  are  less  or  not  at  all  resolved.  The  body  of  the 
cloud  does  not  congregate  much  into  knots,  and  altogether  it  is  no  way  a  striking  object,  apart  from  the 
nebula  and  clusters."    "  N.B.  Mirror  a  good  deal  tarnished — at  least  a  fourth  of  its  light." 

Sweep  625.— Zone  162  ... .  165.    September  21,  1835. 

"Oh.  39m.  Ills.  164°  0'  52".    Here  commences  a  very  starry  region." 

"  Oh.  44m.  55  0s.  164°  13'  22".  This  seems  to  be  the  body  of  the  cloud.  It  is  a  fine  rich  large  cluster  of 
very  small  stars  12  . . . .  18  mag.  which  fills  more  than  many  fields,  and  is  broken  into  many  knots, 
groups  and  straggling  branches,  but  the  whole  (i.  e.  the  whole  of  this  clustering  part)  is  clearly  re- 
solved. 

"  lh.  2m.  42  3s.  163°  15'  56".    Neb.,  &c.    The  field  rich  with  st.  11  ....  15  m." 
"  lh.  15m.    The  cloud  is  past,  and  the  zone  is  as  free  of  stars  as  before  it  came  on." 

Sweep  738.— Zone  162  165.    October  4,  1836. 

"  Oh.  37m.  8-9s.  164°  22'  18"  (a  neb.  taken).    This  is  in  the  light  part  of  the  cloud. 
"  Oh.  40m.  13-0s.  164°  2'  8".    The  field  here  has  light  in  it  and  many  stars. 

"  Oh.  41m.  43-9s.  164°  12'  28"  (a  cluster  taken).  It  is  the  preceding  knot  of  the  resolvable  portion  of  the 
body  of  the  Nubec.  Min.,  which  fills  the  subsequent  field  and  consists  of  irregularly  clustered  stars  12 
....  16  ....  20  m." 

"  Oh.  49m.  162°  4'  18".    A  field  almost  black.    This  is  decidedly  above  (north  of)  the  cloud." 

Sweep  745.— Zone  162  165.    November  5,  1836. 

"  Oh.  33m.  5Ms.  164°  20'  54"  (a  nebula  taken).    The  field  is  full  of  the  nebulous  light  of  the  Nubecula." 

"  Oh.  43m.  19s.  164°  31'  47".    Lower  limit  of  the  light  of  the  Nubecula." 

"  Oh.  47m.  21s.  163°  7'  16".    Upper  limit,  but  here  it  is  starry,  at  the  other  limit  nebulous. 

"  lh.  13m.  164°  15'.    This  seems  to  be  about  the  end  of  the  small  cloud.    The  field  has  15  or  20  stars  in 

it  11  15  m.    Above  and  below,  it  is  almost  vacant." 

"  2h.  0m.    Here,  after  a  region  of  utter  barrenness,  commences  a  somewhat  brighter  region.    N.B. — The 

access  to  the  Nub.  Minor,  on  all  sides,  is  through  a  desert  (Gage  Bk.  /'  745)." 
"  2h.  42m.    A  miserably  poor  and  barren  region." 
"  3h.  30m.    Most  dreary  since  the  small  nubecula  (Gage  Bk.)." 

"  3h.  40.  Swept  assiduously  since  2h.  30m.,  but  it  is  a  barren  and  utterly  uninteresting  region,  having  few 
stars  and  neither  nebula  nor  double  stars." 

(128)  Sweeps  above  and  below  the  Nubecula  Minor. 

Sweep  616.— Zone  159  162.    July  24,  1835. 

"22h.  50m.  23°  30'.    The  latter  part  of  this  zone  most  oppressively  desolate.    N.B.— Admirably  well 


146 


OF  THE  TWO  NUBECULA. 


swept."  (Gage  Bk.)  The  average  of  the  gages  during  this  interval  was  8  stars  per  field  of  all  magni- 
tudes. 

Sweep  509.— Same  zone.    November  3,  1834. 

"  lh.  9m.  59°  9'.    The  lower  part  of  the  sweep  (i.  e.  at  162°  NPD)  contains  a  good  deal  of  loose  light,  and 
is  evidently  the  border  of  the  Nubecula  Minor,  but  there  are  not  many  stars,  and  the  light  is  perfectly 
irresolvable  and  not  congregated  into  knots  or  distinct  nebulse.'' 
"  lh.  28m.    All  this  part  of  the  sweep  is  singularly  barren  of  stars,  scarcely  any"  exist,  "  say  on  an  average 
2  or  3  in  a  field  of  all  magnitudes  from  10  to  16." 

It  is  perhaps  worthy  of  notice  that  the  fine  Globular  Cluster  A  62,  which  occurs  in  this  zone  at 
Oh.  57m.  161°  46'  is  situated  beyond  the  limits  of  the  Nubecula,  like  47  Touc,  to  which,  though 
much  inferior  in  brilliancy,  it  is  yet  a  not  unworthy  fellow. 

Sweep  622.— Zone  165  ....  168°  NPD.    September  18,  1835. 
"23h.  0m.  0°  22'.    Gages  averaging  13  stars  in  the  field  of  all  magnitudes  from  8-9  downwards,"  (Gage 
Bk.) 

"  Oh.  22m.    No  sign  of  the  cloud."    (Gage  Bk.) 

"  Oh.  25m.  22*2s.    Looking  well  out  for  symptoms  of  the  lesser  cloud  but  I  perceive  none." 

"  lh.  0m.    No  symptoms  of  the  cloud  unless  perhaps  a  very  feeble  light  in  the  field  at  the  upper  edge  of 

the  zone."    (164°  56')  (Gage  Bk.)    Average  of  Gages  since  0  22  =  13  stars  per  field. 
"  lh.  10m.    A  most  dull  and  uninteresting  sweep."    (Gage  Bk.) 

"  lh.  32m.  127s.  Swept  steadily  from  0-50 — sky  10,  but  nothing  of  the  slightest  interest.  Very  few  stars 
above  10  m.,  and  all  single."  Average  of  Gages,  per  Gage  Book,  from  lh.  0m.  to  4h.  0m.,  12  stars  per 
field. 

(129)  There  are  37  objects  entitled  to  entry  in  the  Catalogue,  as  nebulae,  or  clusters,  within 
the  area  of  the  Nubecula  Minor. 

Of  the  Nubecula  Major. 

(130)  The  Nubecula  Major  is  situated  between  the  parallels  of  156°  and  162°  NPD, 
and  the  meridians  of  4h  40m  and  6h  0m  in  R  A.  Its  brightest,  and  for  the  most  part, 
unresolved  portion  (which  has  been  pitched  on  several  times  in  sweeping  as  "  the  main  body 
of  the  cloud")  is  situated  in  5h  20m  R  A  and  159°  40'  NPD,  but  the  whole  region  between 
5"  10m  and  5h  30m  in  R  A,  and  from  158°  50'  to  160°  10'  in  N  P  D,  is  almost  equally  entitled 
to  be  so  called.  The  brightest  and  richest  region  of  resolved  and  clustering  stars  is  situated 
about  5"  30m  R  A,  157°  0'NPD. 

(131)  The  Nubecula  Major,  like  the  Minor,  consists  partly  of  large  tracts  and  ill-defined 
patches  of  irresolvable  nebula,  and  of  nebulosity  in  every  stage  of  resolution,  up  to  perfectly 
resolved  stars  like  the  Milky  Way,  as  also  of  regular  and  irregular  nebulas  properly  so  called, 
of  globular  clusters  in  every  stage  of  resolvability,  and  of  clustering  groups  sufficiently 
insulated  and  condensed  to  come  under  the  designation  of  "  clusters  of  stars,"  in  the  sense  in 
which  that  expression  is  always  to  be  understood  in  reading  my  Father's  and  my  own  catalogues. 
In  the  number  and  variety  of  these  objects,  and  in  general  complexity  of  structure,  it  far  sur- 
passes the  Lesser  Nubecula ;  some  idea  of  which  may  be  formed  by  comparing  the  numbers 
of  registered  nebula;  and  clusters  in  each.  For  while,  within  the  limits  assigned  above  to  the 
latter,  the  number  of  such  nebulae  and  clusters  amounts  only  to  37,  and  taking  in  six  outliers, 
which  may  be  regarded  as  forming  part  of  its  system,  at  most  to  43,  (a  very  remarkable  con- 
centration of  such  objects  already,  within  an  area  not  much  exceeding  ten  square  degrees), — the 


OF  THE  TWO  NUBECULA. 


147 


former  within  an  area  of  about  42  square  degrees,  allows  us  to  enumerate  no  fewer  than  278 
(without  reckoning  between  50  and  60  outliers,  immediately  adjacent,  and  which  may  very 
fairly  be  regarded  as  appendages  of  the  nebulous  system  of  the  Nubecula  Major)  making  an 
average  of  about  to  the  square  degree,  which  very  far  exceeds  anything  that  is  to  be 
met  with  in  any  other  region  of  the  heavens.  Even  the  most  crowded  parts  of  the  stratum  of 
Virgo,  in  the  wing  of  that  constellation,  or  in  Coma  Berenices,  offer  nothing  approaching  to 
it.  It  is  evident  from  this,  and  from  the  intermixture  of  stars  and  unresolved  nebulosity  which 
probably  might  be  resolved  with  a  higher  optical  power,  that  the  nubeculae  are  to  be 
regarded  as  systems  sui  generis,  and  which  have  no  analogues  in  our  hemisphere. 

(132)  To  the  naked  eye,  as  shown  in  Fig.  2.  PI.  VII.,  the  greater  nubecula  exhibits  the 
appearance  of  an  axis  of  light  (very  ill-defined  indeed,  and  by  no  means  strongly  distinguished 
from  the  general  mass)  which  seems  to  open  out  at  its  extremities  into  somewhat  oval  sweeps, 
recalling,  in  some  faint  degree,  the  appearance  of  that  extraordinary  object  Mess.  27.  It  would 
be  strange,  indeed,  but  not  beyond  the  analogies  of  other  wonderful  disclosures  effected  by 
optical  improvements,  if  instruments  yet  to  be  created,  or  even  possibly  those  already  in  pro- 
gress, should  one  day  analyse  this  last  mentioned  object  into  subordinate  groups  and  systems 
of,  perhaps,  equal  complexity.  In  the  nubecula  itself,  there  is  a  nebula  (h.  2878)  which,  as 
will  be  seen  in  the  description  and  remarks  annexed  to  its  observation  in  the  Catalogue,  has 
given  rise  to  a  similar  train  of  speculation. 

(133)  The  only  object  which  stands  at  all  conspicuously  distinguished  from  the  general 
misty  illumination  of  the  greater  nubecula  (at  least  to  my  eye),  is  the  great  looped  Nebula 
30  Doradus  of  Bode,  which,  however,  is  merely  to  be  perceived  as  a  small  indistinct  patch, 
evidently  not  a  star,  and  that  only  in  fine  nights.  Of  this  object,  an  ample  description  has  been 
already  given,  to  which  I  shall  here  only  add,  that  it  is  unique  even  in  the  system  to  which  it 
belongs,  there  being  no  other  object  in  either  nubecula  to  which  it  bears  the  least  resemblance. 
Of  the  very  peculiar  character  of  several  other  of  the  nebulous  constituents  of  the  nubecula 
when  viewed  in  the  20  feet  reflector,  sufficient  specimens  have  been  given  in  figures  2 — 6, 
PI.  III.,  figs.  7,  9,  Plate  IV.,  and  figs.  11,  20,  Plate  VI. 

(134)  The  immediate  neighbourhood  of  the  Nubecula  Major,  is  somewhat  less  barren  of 
stars  than  that  of  the  Minor,  but  it  is  by  no  means  rich,  nor  does  any  branch  of  the  Milky 
Way  whatever  form  any  certain  and  conspicuous  junction  with,  or  include  it;  though  on  very 
clear  nights  I  have  sometimes  fancied  a  feeble  extension  of  the  nearer  portion  of  the  Milky 
Way  in  Argo  (where  it  is  not  above  15°  or  20°  distinct)  in  the  direction  of  the  nubecula.  On 
the  whole,  however,  I  do  not  consider  this  appearance  as  more  than  would  be  accounted  for  by 
the  general  increase  of  the  number  of  small  stars  which,  in  almost  every  part  of  the  course  of 
the  Milky  Way,  accompany  its  borders,  and,  in  a  telescope,  announce  its  approach.  I  have 
encountered  nothing  that  I  could  set  down  as  diffused  nebulosity  anywhere  in  the  neighbourhood 
of  either  nubecula. 

(135)  I  have  already  stated  that  the  excessive  complexity  of  detail  in  this  object  baffled 
every  attempt  to  delineate  the  whole  or  any  large  portions  of  it  by  the  aid  of  the  telescope.  It 
was  my  wish  to  have  done  this,  so  as  to  present  a  correct  and  magnified  drawing  of  it,  and  to 
this  end  I  took  roughly,  with  the  equatorial,  the  place  of  every  star  visible  in  that  instrument 
down  to  the  10th  magnitude,  in  both  Nubeculae,  with  a  view  to  the  formation  of  charts  precise 


148 


OF  THE  TWO  NUBECULA. 


enough,  and  sufficiently  detailed  to  serve  as  the  groundwork  of  such  drawings  of  both  objects. 
This,  in  itself,  was  no  trifling  operation,  when  conducted,  as  it  was,  in  such  a  manner  as  I  shall 
describe,  so  as  to  secure  the  observation  of  every  visible  object,  without  the  possible  escape  of 
any  (except  by  the  intervention  of  unperceived  cloud).  It  was,  however,  executed  in  a  series 
of  34  zones,  observed  (as  regards  the  Nubecula  Major)  between  Nov.  2,  1836,  and  March  26, 
1837.  The  series  for  the  Nubecula  Minor  (as  less  interesting)  were  deferred,  and  were  not 
completed  till  December,  1837.  The  results  of  these  observations,  reduced  by  clock  and  index 
errors  obtained  from  stars  occurring  in  the  zones,  are  contained  in  two  Catalogues,  hereto 
subjoined ;  and  in  order  to  render  them  as  complete  as  I  have  the  means  of  doing,  all  the 
objects  observed  in  the  20  feet  have  been  also  inserted  which  fall  within  the  limits  prescribed 
for  each.  By  far  the  greater  part  of  the  nebulae  and  clusters  are  in  this  predicament,  the 
power  of  a  5-inch  achromatic  object-glass  being  inadequate  to  render  visible  more  than  a  few 
of  the  brighter  and  more  conspicuous  among  them.  But  the  drawings  proved  beyond  my 
unassisted  power  to  execute,  and  I  was  obliged,  though  with  regret,  to  rest  content  with  having, 
at  least  so  far,  roughed  out  the  groundwork  of  them,  and  prepared  the  way  for  the  more  suc- 
cessful operations  of  some  other  astronomer,  to  whom  I  earnestly  recommend  the  completion 
of  a  work  at  once  so  interesting  in  its  performance,  and  instructive  in  its  result. 

(136)  The  process  of  zone  observation,  followed  with  the  equatorial,  is  applicable  to  the 
complete  mapping  down  of  any  given  region  of  the  heavens,  and  is  as  follows : — The  index  error 
of  the  declination  circle  being  ascertained,  clamps  are  screwed  on  the  limb  of  that  circle,  so  as 
to  allow  the  telescope  a  motion  of  only  a  single  degree  on  the  meridian,  viz.,  from  one  whole 
degree  in  polar  distance  to  the  next,  allowing  1'  of  overlapping  on  either  side,  which  is  ample 
when  the  polar  axis  is  in  good  adjustment.  The  combined  error  of  clock  and  hour  circle  being 
also  ascertained,  the  instrument  is  set  to  a  given  right  ascension  (that  fixed  upon  for  the  com- 
mencement of  the  area  to  be  mapped — allowing  also  a  minute  of  time  antecedent,  as  margin), 
and  the  observation  commences  by  sweeping  with  the  telescope  on  the  declination  circle,  up 
and  down  from  clamp  to  clamp  with  a  very  faintly  illuminated  field,  just  sufficient  to  allow  the 
cross  wires  to  be  seen,  which  of  course,  for  this  purpose,  must  be  placed  parallel  and  perpendi- 
cular to  the  medium.  This  sweeping  movement  is  carried  on  by  hand,  slowly  and  steadily, 
without  moving  the  right  ascension  handle,  until  an  object  is  seen,  when  the  sweeping  motion  is 
arrested,  the  object  brought  to  bisection  on  the  horizontal  wire,  and  the  transit  taken  over  the 
vertical.  The  circles  are  then  read  off",  and  the  observation  registered.  By  this  time  the 
object  will  have  advanced  in  the  field  beyond  the  meridian  wire.  It  is  then  to  be  brought  back 
precisely  to  that  wire  by  moving  the  right  ascension  handle,  and  the  loss  of  time  being  thus 
recovered,  the  sweeping  recommences  from  the  very  same  point  of  R  A,  until  another  object 
comes  within  the  range  of  observation.  In  this  way  of  operating,  by  following  the  heavens  in 
their  diurnal  movement,  it  is  evidently  impossible  that  any  object  within  the  optical  power  of 
the  instrument  can  escape  being  observed,  if  the  attention  be  kept  sufficiently  alert,  and  no 
clouds  intervene.  I  can  scarcely  flatter  myself  that  literally  every  star  down  to  the  10th  magni- 
tude which  exists  in  the  areas  so  observed  of  the  nubecula^  will  be  found  in  these  Catalogues  ; 
but  I  feel  assured  that  the  number  which  have  escaped  of  that  and  larger  magnitudes  must  be 
very  small.  It  was  not  considered  necessary  to  go  over  the  work  twice.  Independent  of  the 
value  of  time  under  all  the  circumstances,  the  sweeping  position,  at  considerable  altitudes,  with  any 


OF  THE  TWO  NUBECULA. 


149 


instrument  but  a  reflector  is  so  excessively  painful  (and  indeed  so  permanently  injurious  to  the  muscles 
of  the  back  and  neck),  that  it  is  scarcely  endurable  beyond  an  hour  at  a  time,  for  which  reason 
alone  I  felt  little  inclination  to  repeat  it. 

(137)  The  places  of  the  objects  in  the  Catalogues  annexed,  as  has  been  said,  are  rough. 
Their  accuracy  amply  suffices,  however,  for  the  intended  purpose.  In  polar  distance  there  can 
hardly  be  more  than  1'  error,  that  being  the  limit  of  exactness  in  reading  the  declination 
circle.  In  R  A,  I  presume  also  that  an  error  of  12  sec.  of  time  (corresponding  at  this  polar 
distance  to  about  1'  of  space)  may  occasionally  occur  from  a  similar  cause  as  respects  the  hour 
circle  reading,  which,  as  well  as  the  declination  circle,  being  intended  only  for  setting  the 
instrument,  and  not  for  any  nice  determination  of  places,  admitted  of  no  greater  precision. 
Comparing  the  places  of  such  stars  as  have  occurred  in  several  zones,  I  find  no  instance  of 
a  greater  discordance  in  the  equatorial  places  between  the  extreme  determinations  and  the  mean 
of  all  in  A  R,  in  the  Catalogue  of  the  greater  nubeculae,  and  only  one  in  N  P  D  even  in  the 
case  of  nebulae,  which,  from  their  faintness  in  the  equatorial,  admit  of  less  certain  observation. 
In  the  Catalogue  of  the  nubecula  minor,  being  materially  nearer  to  the  pole,  the  discordances 
in  R  A  are  apparently,  but  not  really,  greater,  and  in  P  D  there  is  only  one  star  (No.  189, 
Cat.),  and  no  nebula  which  exceeds  the  limit  assigned. 

(138)  In  this  respect,  however,  the  observations  are  suffered  to  speak  for  themselves,  since 
in  these  Catalogues,  as  well  as  in  those  of  the  nebulae  and  double  stars,  each  individual  result 
of  observation  has  been  set  down  without  taking  means,  and  none  have  been  rejected  for  dis- 
cordance. The  nebulae  observed  in  the  sweeps  are  also  inserted  for  the  sake  of  comparison,  as 
well  as  to  complete  the  nebulous  part  of  the  Catalogue.  The  stars  observed  in  the  sweeps 
have  been  added  for  a  similar  reason,  and  for  the  sake  of  comparison  with  the  Brisbane  Cata- 
logue. The  Catalogues  are  by  this  somewhat  extended  in  bulk,  it  is  true,  but  on  the  whole  they 
present  in  this  form  a  fairer  picture  of  the  work  done. 

(139)  In  the  following  catalogues,  the  first  column  contains  the  general  number,  for  each  ; 
the  second  the  object,  star  (S)  Nebula  (N.),  Globular  Cluster  ((§)  or  cluster  of  stars  (C). 
Column  3  contains  the  magnitude  of  the  star  as  estimated  at  the  time  of  observation  rejecting 
quarter  magnitudes,  or  the  degree  of  brightness  of  the  nebulae,  expressed  by  the  Roman 
numerals,  as  in  my  Father's  classes  I.  II.  III.  or  otherwise,  following  the  nomenclature  and 
notation  of  his  Catalogues.  The  fourth  column  contains  the  right  ascension,  and  the  fifth  the 
polar  distance  reduced  to  1830.0.  Lastly,  column  6,  contains  the  number  of  the  zone  in 
which  the  object  has  been  observed  or  the  indication  of  its  being  inserted  from  a  20-feet  sweep, 
characterized  by  the  letter  f  in  italics.  Identifications  of  stars  with  stars  in  the  Brisbane 
Catalogue,  and  other  remarks  are  placed  at  the  end  of  the  Catalogues,  and  referred  to  by  the 
general  numbers.  In  the  Catalogue  of  the  Nubecula  Minor,  it  will  be  noticed  that  some  of 
the  zone  observations  have  extended  beyond  the  limits  of  R  A  fixed  on,  both  ways  as  the 
boundary  of  the  Nubecula.  The  stars  so  observed  are  retained  for  the  sake  of  any  possible 
occasion  which  may  arise  hereafter  of  referring  to  them.  In  this  Nubecula,  it  ought  to  be 
mentioned  (or  at  least  in  the  area  proposed  to  be  mapped),  a  small  portion  (between  the 
parallels  of  164°  and  165°,  and  from  R  A  0h  45m  to  lh  16m)  by  some  inadvertence  escaped 
being  included  in  the  equatorial  zones. 

(140)  Several  stars  of  the  Brisbane  Catalogue,  which  (supposing  their  places  in  that 

Q  Q 


150 


OF  THE  TWO  NUBECULA. 


Catalogue  to  be  correct)  have  not  been  encountered  in  the  zone  observations,  are  inserted  into 
the  appended  Catalogues  by  bringing  up  their  places  to  1830.  Six  such  cases  occur  in  the 
Nubecula  Minor  (see  Nos.  29,  70,  123,  131,  136,  155).  Of  these  Nos.  29  and  70  (B  28  and 
S3)  seem  to  be  merely  duplicates  of  other  stars  of  that  Catalogue,  which  I  have  found  in  their 
places,  originating  in  misreadings  or  errors  of  reduction  therein  committed.  Nos.  123  and 
131  (B  120  and  126)  occur  in  the  unobserved  space  alluded  to  in  the  last  article.  In  the 
case  of  No.  136  (B  129),  it  appears  to  be  the  star  No.  133,  with  lm  error  in  R  A.  No.  155 
(B  150,  or  151,  for  these  are  one  star)  was  missed  by  a  want  of  exact  overlapping  in  R  A  in 
zones  4  and  34.  In  the  Catalogue  of  the  Nubecula  Major,  I  have  no  reason  to  suppose  that 
any  of  the  Brisbane  stars  which  really  exist  have  escaped  observation.  Several  cases  of 
duplicates  and  probable  misreadings  or  errors  of  reduction  in  the  Brisbane  Catalogue  indeed 
occur,  but  they  are  not  such  as  to  leave  any  doubt  as  to  the  identity  of  the  stars. 


FIRST  APPROXIMATION  TOWARDS  A  CATALOGUE  OF  OBJECTS 

IN  THE 

MAGELLANIC  CLOUDS, 

AS  OBSERVED  WITH  THE  SEVEN-EEET  EQUATORIAL 

AND  THE 

TWENTY-EEET  REFLECTOR. 


CONTAINING  THE  PLACES  FOE,  1830.0 

OP 

919  STARS,  NEBULiE,  AND  CLUSTERS  IN  THE  GREATER 

AND  OF 

244  IN  THE  LESSER  NUBECULA. 

INTENDED  AS 

PREPARATORY  TO  THE  CONSTRUCTION  OF  CHARTS  OF  THE  NUBECULA  AND  TO 
THE  FUTURE  EXECUTION  OF  DRAWINGS  OF  THEM  IN  DETAIL. 


153 


STARS,  NEBULA,  AND  CLUSTERS,  IN  THE  NUBECULA  MINOR. 


No.  for 

Obj. 

Mag. 

R  A.  1880.0. 

N  P  D.  1830.0. 

Zone. 

No.  for 

Mag. 

R  A.  1830.0. 

NPD.  1830.0. 

Zone. 

Refe- 

Refe- 

Obj. 

rence. 

h. 

m.  s. 

0      /  // 

rence. 

h.   m.  s. 

0     1  11 

I 

S 

IO 

0 

0  32 

163  25  54 

7 

51 

s 

10 

0  24  3 

163    6  24 

7 

2 

S 

9' 

Q 

1  3/ 

162    4  II 

8 

9' 

0  IO 

6  28 

4 

9' 

49 

4  54 

7 

52 

S 

9' 

0  24  59 

163    7  16 

1 

3 

S 

9 

O 

I  7$ 

162  54  41 

8 

53 

N 

III. 

0  25  48 

164    3  8 

/ 

4 

s 

IO 

O 

I  39 

162  32  41 

8 

54 

S 

6 

0  26  9 

162  12  14 

/ 

5 

s 

IO 

O 

I  AC 

1  4i 

162  31  41 

8 

7 

1 1 

11  50 

2 

6 

s 

7' 

O 

164  10  54 

7 

7 

15 

12  46 

1 

6 

0  14 

10  20 

/ 

55 

s 

10 

0  27  36 

163  28  58 

+ 

7 

s 

IO 

0 

3  0 

163  33  24 

7 

56 

s 

9' 

0  28  0 

163  47  28 

4 

IO 

32  54 

7 

57 

s 

9' 

0  28  41 

162  28  46 

1 

8 

s 

9' 

0 

163  11  34 

7 

58 

s 

9' 
9' 
8' 

0  28  49 

164  49  32 

6 

9 

s 

IO 

0 

1     T  T 

l64    5  54 

7 

51 

49  5 

/ 

IO 

s 

9 

0 

3  J7 

163  13  34 

7 

59 

s 

0  28  50 

164    9  55 

/ 

1 1 

s 

9 

0 

7    A  A 

162  54  56 

8 

8' 

57 

9  28 

4 

12 

s 

10 

0 

4  32 

164    1  54 

7 

s 

8' 

58 

9  32 

6 

13 

s 

8' 

0 

C  A 

5  4 

162  28  41 

8 

60 

N 

III. 

0  29  8 

164    6  25 

/ 

'4 

s 

9 

0 

5  7 

162  25  1 

8 

61 

s 

9 

0  29  27 

163  46  48 

4 

15 

s 

10 

0 

5  29 

162  22  41 

8 

62 

s 

10 

0  30  36 

162  37  46 

1 

16 

s 

9' 

0 

6  39 

162  14  41 

8 

63 

s 

9' 

0  30  45 

162  47  46 

1 

17 

s 

9 

6  58 

163    7  41 

8 

64 

s 

9' 

0  30  54 

162  35  16 

1 

9' 
9' 

07 

7  54 

7 

65 

s 

8 

0  31  37 

164  53  2 

6 

18 

s 

0 

7  31 

162  40  41 

8 

s 

8 

41 

53  5° 

/ 

19 

s 

8' 

0 

7  3s 

162  21  41 

8 

66 

s 

8 

0  31  38 

164  58  43 

/ 

20 

s 

8 

5!  1 
0  1 

162  11  41 

8 

67 

s 

i 

0  31  58 

164   4  14 

/ 

21 

s 

9' 

9  21 

162  51  41 

8 

60 

4  32 

6 

22 

s 

10 

9  44 

162  56  41 

8 

7 

61 

4  28 

4 

23 

s 

IO 

9  58 

162  11  11 

8 

68 

s 

Q 

0  32  8 

163  12  58 

/ 

24 

s 

9 

10  6 

162  49  11 

8 

s 

8 

14 

12  48 

4 

25 

s 

9 

° 

10  23 

162  15  41 

8 

69 

s 

9 

0  32  47 

162    2  50 

2 

26 

s 

8' 

10  47 

162  19  41 

8 

s 

q 

54 

3  46 

1 

27 

s 

10 

11  44 

167  c  7  24. 

70 

s 

0  32  54 

164  13  17 

28 

s 

9' 

12  2 

163  45  54 

7 

71 

s 

9' 
8' 

0  32  54 

162  33  46 

1 

29 

s 

7 
8' 

12  44.4 

163     0  21 

72 

s 

0  33  27 

164  40  32 

6 

30 

s 

° 

12  52 

162  c.4  41 

8 

73 

s 

8 

0  33  42 

164  53  21 

6 

31 

s 

9 

12  57 

162    7  1 

8 

74 

N 

II. 

0  33  52 

164  19  47 

/ 

32 

s 

8' 

14  46 

167  c8  KA. 

J    J  JT 

7 

7? 

N 

III. 

0  33  55 

164  23  56 

/ 

33 

s 

10 

16  9 

163     l6  54 

7 

76 

s 

9 

0  34  14 

162  33  46 

1 

34 

s 

9 

16  15 

163    12  24 

7 

77 

N 

II. 

0  34  40 

164  17  IO 

/ 

35 

s 

IO 

0 

16  19.3 

163      2  0 

/ 

78 

S 

10 

0  34  52 

164    3  28 

4 

36 

© 

0 

l6  24. 

163      2  II 

8 

10 

53 

3  8 

/ 

24 

O  54 

7 

79 

s 

IO 

0  34  57 

165    1  32 

6 

8 

VI. 

26 

1  35 

/ 

80 

s 

9' 

0  35  7 

165    6  12 

6 

26 

1  5 

2 

81 

s 

9' 

0  35  33 

164  36  32 

6 

29 

1  5 

2 

82 

N 

III. 

0  37  5 

164  31  32 

/ 

1  46 

1 

83 

N 

II. 

0  37  IO 

164  22  IO 

/ 

37 

s 

1 1 

0 

16  35 

163    3  24 

7 

84 

S 

9 

0  37  13 

164  39  22 

6 

38 

s 

9 

0 

16  36 

162  56  46 

1 

85 

s 

IO 

0  37  38 

163  14  48 

4 

9 

37 

56  20 

2 

86 

s 

8 

0  37  52 

162    6  46 

1 

39 

s 

1 1 

0 

17  19 

163    2  54 

7 

s 

8 

53 

6  20 

2 

40 

s 

9 

0 

17  22 

163  33  24 

7 

s 

9 

55 

6  8 

/ 

41 

N 

II. 

0 

19  4 

162  28  23 

/ 

87 

s 

9 

0  37  58 

164  45  32 

6 

42 

s 

9 

0 

19  22 

162    9  16 

1 

88 

s 

10 

0  38  2 

163  11  38 

4 

I 

22 

1 1  50 

2 

89 

s 

10 

0  38  12 

164  25  32 

6 

43 

s 

0 

20  7 

162  50  20 

2 

90 

s 

9' 

0  38  20 

164  44  32 

6 

44 

s 

8 

0 

20  12 

162  48  46 

1 

91 

s 

IO 

0  38  37 

164    9  32 

6 

8' 
9' 

'3 

162  51  20 

2 

92 

N 

II. 

0  39  6 

164  18  28 

/ 

45 

s 

0 

20  17 

163    4  46 

1 

93 

N 

II. 

0  39  IO 

164   0  53 

/ 

46 

10 

40 

4  28 

4 

94 

N 

11. 

0  39  38 

164  26  36 

/ 

s 

10 

0 

20  22 

163    6  24 

7 

95 

s 

9 

0  39  45 

164  24  38 

/ 

47 

s 

IO 

0 

20  31 

162    7  50 

2 

10 

5° 

24  2 

6 

48 

s 

9' 

0 

22  25 

164  42  32 

6 

96 

s 

9,' 

0  39  49 

162  42  46 

1 

49 

s 

0 

23  2 

164    1  24 

7 

97 

s 

9 

0  40  5 

163  31  58 

4 

20 

1  52 

6 

98 

N 

II. 

0  40  17 

164    1  51 

/ 

I 

25 

1  28 

4 

99 

s 

10 

0  4°  53 

163  46  28 

4 

5° 

s 

0 

23  54 

165    6  32 

6 

100 

N 

III. 

0  40  58 

164  24  55 

f  \ 

R  R 


154 


STARS,  NEBULAE,  AND  CLUSTERS, 


No.  for 

R  A.  1830.0. 

N  P  D.  1830.0. 

No.  for 

Obj . 

R  A.  1830.0. 

N  P  D.  1830.0. 

Zone. 

Refe- 

Obj. 

Mag. 

one. 

Refe- 

Mag. 

rence 

.   m.  s. 

0      /  // 

rence. 

i.    m.  s. 

a      1  11 

IOI 

Cl 

0  41  44 

164   12  28 

/ 

*59 

s 

IO 

1     3  4 

163  49  45 

34 

1 02 

N 

III. 

0  42  16 

164  27  52 

/ 

160 

N 

1    3  6 

163  48  15 

34 

103 

S 

10 

0  42  49 

164  29  32 

6 

N 

i. 

IO 

47  37 

/ 

104 

s 

IO 

0  42  53 

164   l6  32 

6 

161 

S 

8' 

1    3  11 

162  44  42 

2 

105 

s 

9 

0  43  26 

163     4  l6 

1 

9, 
8' 

*3 

44  47 

/ 

s 

9 

40 

3  28 

4 

28 

45  45 

34 

106 

s 

9 

0  43  20 

164  24  57 

r 

162 

N 

III. 

1    3  32 

162  40  32 

s 

9 

27 

24  32 

6 

163 

S 

10 

1    3  40 

163  47  45 

34 

107 

s 

9' 

0  43  51 

162  27  46 

1 

164 

S 

10 

1    3  42 

163  56  45 

34 

108 

s 

10 

0  43  57 

164   2  32 

6 

165 

s 

9' 
9 

1    3  49 

163  32  45 

34 

109 

s 

9' 

0  44  14 

164  31  32 

6 

166 

53 

32  45 

34 

1 10 

s 

10 

0  44  29 

164  24  32 

6 

S 

10 

1    3  51 

163  27  45 

34 

1 1 1 

s 

7' 

0  44  29 

162    5  20 

2 

167 

s 

10 

1    4  2 

164   6  45 

34 

7' 

0  44  29 

5  ifi 

1 

168 

s 

IO 

1    4  16 

163    6  45 

34 

7 

0  44  33 

4  5° 

2 

169 

s 

IO 

1    5  2 

163  38  45 

34 

I  12 

s 

10 

0  44  39 

164  24  2 

6 

170 

s 

IO 

1    5  2 

162  57  45 

34 

113 

N 

III. 

0  45  13 

164   4  37 

/ 

171 

s 

/ 

1    5  3 

163  51  45 

34 

114 

s 

10 

0  45  17 

164  57  2 

6 

8 

4 

52  16 

/ 

"5 

s 

9' 

0  45  17 

162  47  20 

2 

172 

s 

9' 

1    6  2 

163  56  45 

34 

116 

S 

10 

0  45  18 

163  36  28 

4 

!73 

s 

10 

1    6  9 

164   5  45 

34 

117 

Cl 

VI. 

0  45  3° 

164  16  22 

/ 

174 

s 

9 
9' 

1    6  12 

163   4  42 

2 

118 

s 

9" 

0  45  46 

162  42  50 

2 

12 

5  45 

34 

119 

N 

II. 

0  46  12 

164  18  17 

f 

9 

H 

5  45 

34 

IZO 

N 

III. 

0  47  12 

164  18  46 

/ 

175 

s 

10 

1    6  45 

163  10  45 

34 

121 

N 

II. 

0  47  19 

163    7  10 

/ 

176 

s 

10 

1    7  1 

163  22  45 

34 

N 

29 

7  20 

2 

177 

s 

IO 

1    7  47 

162  31  45 

34 

122 

S 

10 

0  47  44 

163    4  50 

2 

9' 

52 

31  42 

2 

123 

s 

7 

°  47  55 

164  47  35 

178 

s 

9 

1  7=57 

162  33  45 

34 

I24 

S 

ro 

0  48  8 

162  51  20 

2 

179 

s 

IO 

1  7:59 

162  29  45 

34 

125 

N 

III. 

0  48  12 

163    9  48 

/ 

180 

s 

IO 

1    8  27 

163  22  45 

34 

126 

s 

10 

0  48  21 

162  48  20 

2 

181 

s 

9' 

1    8  45 

162  36  42 

2 

10 

22 

20 

2 

9 

53 

35  45 

34 

127 

s 

10 

0  48  54 

163    3  20 

2 

182 

N 

II. 

1    9  0 

164  11  40 

/ 

128 

s 

6 

0  49  12 

165  13  43 

183 

s 

IO 

1    9  21 

164    6  45 

34 

129 

s 

9' 

0  50  23 

164  2  58 

4 

184 

s 

9' 

1    9  41 

163  38  45 

34 

130 

N 

I. 

0  50  24 

163  23  58 

4 

185 

N 

1    9  44 

162  28  12 

2 

25 

23  21 

/ 

N 

ii. 

47 

26  46 

f 

131 

s 

7' 

0  50  32 

ifi4  44  59 

186 

N 

11. 

1    9  59 

164  12  14 

/ 

132 

s 

10 

0  50  59 

163  54  58 

4- 

187 

s 

9' 

I   IO  2 

164  10  45 

34 

J33 

s 

8' 

0  51  7 

163  59  28 

4 

188 

N 

11. 

1  10  53 

164  14  8 

/ 

134 

S 

10 

0  52  10 

162  11  20 

2 

189 

S 

IO 

1  12  45 

162  30  12 

2 

135 

N 

III. 

0  52  16 

165  22  12 

/ 

IO 

12  52 

162  27  45 

34 

136 

S 

7 

0  52  30 

163  59  14 

190 

s 

IO 

1  13  0 

162  50  45 

34 

137 

N 

0  53  15 

163    5  12 

2 

191 

s 

8' 

1  13  11 

164  11  45 

34 

N 

16 

6  28 

4 

192 

s 

9 

1  !3  37 

163  36  45 

34 

Cl 

VI. 

'9 

5  54 

/ 

193 

s 

8' 

1  *3  53 

162    0  42 

2 

138 

s 

10 

0  53  20 

162  33  42 

4 

8' 

59 

0  15 

34 

139 

s 

8 

0  55  14 

163  36  28 

4 

8 

61 

0  43 

/ 

7 

'4 

37  3 

/ 

194 

1  14  0 

164  15  .. 

/ 

140 

s 

8 

0  55  44 

162  28  42 

2 

195 

s 

10 

1  14  47 

164    5  45 

34 

8 

54 

27  28 

/ 

196 

s 

9 
8' 

1  14  56 

162  41  12 

2 

141 

s 

10 

0  56  12 

163    7  48 

4 

58 

40  45 

34 

142 

N 

III. 

0  56  28 

162  32  15 

/ 

197 

s 

9' 

1  14  58 

162  44  12 

2 

"43 

s 

9' 

0  57  20 

162  59  42 

2 

9 

63 

43  45 

34 

9 

29 

60  18 

/ 

198 

s 

10 

1  15  11 

163  26  45 

34 

144 

I. 

0  57  27 

161  45  41 

/ 

199 

s 

10 

1  15  18 

163  22  45 

34 

145 

s 

10 

0  57  28 

163  27  28 

4 

200 

s 

8 

1  15  40 

ifi3  37  45 

34 

146 

s 

9 

0  57  47 

163  15  48 

4 

8 

42 

38  36 

/ 

H7 

N 

0  57  56 

162  57  42 

2 

201 

s 

9 

1  '5  53 

ifi3  34  45 

34 

Cl 

VI. 

57 

58  9 

f 

202 

s 

9 

1  16  40 

162  39  57 

33 

148 

N 

II. 

0  58  30 

163  44  4 

/ 

203 

s 

8' 

1  16  40 

ifi3  55  57 

33 

30 

44  28 

4 

204 

s 

10 

1  16  47 

163  10  45 

34 

149 

S 

10 

0  58  30 

163  40  28 

4 

205 

s 

10 

1  16  47 

ifi3    5  45 
163  52  57 

34 

150 

S 

9 

0  58  47 

163  10  12 

206 

s 

9' 

1  16  48 

33 

151 

S 

10 

0  59  12 

162  23  12 

2 

207 

s 

IO 

1  16  49 

163    8  45 

34 

152 

S 

10 

0  59  16 

162  47  12 

208 

s 

9 
9' 
9 

1  16  5, 

162  38  42 

2 

i53 

S 

8 

0  59  34 

162  38  42 

2 

209 

s 

1  17  0 

163  26  57 

33 

7 

35 

38  58 

/ 

2 10 

s 

1  17  24 

162  28  57 

33 

'54 

N 

III. 

0  59  48 

162  54  18 

/ 

211 

s 

10 

1  18  2 

163  21  57 

33 

iS5 

S 

7 

0  59  57 

163  27  35 

* 

212 

s 

IO 

1  18  4 

162  20  57 

33 

156 

s 

9' 

1    0  57 

162  12  42 

2 

2I3 

s 

IO 

1  18  5 

162    6  57 

33 

157 

N 

III. 

1    2  29 

162  40  11 

f 

214 

s 

IO 

1  18  17 

162  26  57 

33 

SS| 

N 

II. 

1    2  43 

163  16  1 

215 

s 

9' 

1  18  47 

163  19  27 

33 

IN  THE  NUBECULA  MINOR. 


155 


No.  for 

Obj. 

Mag. 

RA.  1830.0. 

NPD.  1830.0. 

Zone. 

No.  for 

Obj. 

Mag. 

RA.  1830.0. 

NPD.  1830.0. 

Zone. 

Refe- 

Refe- 

rence. 

0  / 

n 

rence. 

h. 

0  / 

a 

, 

21 

O 

9; 
9' 

I  19 

12 

162  S3 

57 

33 

22 
27 

c 
0 

9 

1 

24 

5 

164  9 

57 

33 

17 

53 

42 

c 

0 

9 
c' 
0 

6 

9 

27 

33 

217 

e 

0 

9 

I  19 

26 

162  23 

57 

33 

-7  ->  8 

Q 

O 

I 

24 

30 

162  48 

57 

33 

9 

27 

24 

42 

2 

s 

I 

30 

48 

57 

33 

218 

s 

g 

I  19 

31 

163  12 

57 

5  i 

22Q 

s 

y 

1 

25 

r3 

l63  4 

57 

Si 

8 

36 

12 

37 

f 

230 

s 

10 

I 

25 

37 

163  50 

57 

33 

219 

s 

9 

I  19 

31 

162  23 

57 

33 

231 

s 

9' 

I 

25 

39 

163  52 

57 

33 

9 

37 

24 

42 

2 

232 

N 

I. 

1 

a5 

45 

164  25 

56 

/ 

220 

s 

10 

I  19 

49 

162  46 

57 

33 

233 

s 

8 

I 

26 

36 

164  1 

57 

33 

221 

s 

9 

I  20 

39 

162  56 

42 

2 

234 

s 

10 

I 

26 

40 

163  56 

57 

33 

9 

43 

56 

57 

33 

235 

s 

10 

I 

26 

57 

163  54 

27 

33 

8 

45 

56 

18 

/ 

236 

s 

10 

I 

27 

30 

163  38 

57 

33 

222 

s 

10 

I  20 

5° 

163  21 

27 

33 

237 

s 

1 

27 

54 

162  18 

57 

33 

223 

s 

9' 

I  21 

18 

162  5 

57 

33 

238 

s 

I 

28 

55 

162  45 

57 

33 

9 

24 

5 

57 

33 

239 

s 

9 

I 

30 

54 

163  10 

27 

33 

224 

s 

10 

I  21 

57 

163  38 

57 

33 

240 

s 

9 

I 

31 

44 

163  12 

57 

33 

9 

69 

38 

8 

./' 

241 

s 

9 

I 

32 

3 

163  36 

57 

33 

225 

s 

8 

I  23 

5 

162  34 

12 

2 

242 

s 

9 

I 

32 

17 

163  41 

57 

33 

8 

17 

35 

22 

/ 

243 

s 

10 

I 

35 

3 

163  33 

57 

33 

7 

34 

33 

57 

33 

244 

s 

9 

1 

35 

37 

164  0 

57 

33 

226 

s 

8' 

I  23 

15 

163  38 

27 

33 

NOTES  ON  THE  FOREGOING  CATALOGUE. 


No. 

6 
29 

30 
34 
35 
36 

37 
38 
39 
40 

44 

45 
5i 
54 
57 

59 
61 

65 
67 
7° 

72 
73 


81 
84 
86 

87 
90 

97 
105 
106 
1 10 
1 11 
112 
117 

123 
128 


5'  error  in  P  D  in  the  Brisbane  catal. 


is  B.  6. 

B.  28.    Not  observed  by  me.    I  presume  it  to 

be  B.  29,  with  5'  error  in  P  D. 
B.  29. 

B.  36  =  B.  37. 
The  D  #  in  ®  47  Touc. 
B.  38  =47  Touc. 
The  preceding  of  two. 
B.  41. 

The  following  of  two. 
B.  42. 
B.  48. 
B.  50. 
B.  60. 
B.  66. 
B.  73- 
B.  74- 

B.  75  =  B.  76. 

Has  a  st  10  m  south  about  2'  distant. 
B.  80.    Has  a  star  10  m  750  s  p,  distant  about  3'. 
B.  83.    Not  observed  by  me.    Is  most  probably 
B.  80,  with  i'"  error  in  R  A,  and  10'  in  N  P  D. 
B.  88  =  B.  90.    1"  error  in  R  A,  in  B,  or  in 

my  obs. 
B.  85.    Place  from  B. 
but  place  not  taken, 
apparent. 
B.  91. 
B.  98. 
B.  101. 
B.  102. 
B.  104. 
105. 
1 11. 
110. 


Seen  by  me  in  zone  6, 
for  some  reason  not 


The  R  A  in  the  Brisbane  cat  has  39" 


B. 
B. 
B. 

The  preceding  of  2. 
B.  112. 

The  following  of  2. 

The  middle  of  the  great  resolved  cluster  of  the 
Nubecula  Minor. 

B.  120.    Not  observed  by  me. 

B.  123.  Not  observed  in  the  zones,  being  be- 
yond their  limit  ;  but  is  the  most  conspicuous 
star  (5.6  m)  to  the  naked  eye  close  to  the 
Nubecula. 


No.  Note. 

130  B.  124.    The  zone  observed  gives  49"'  R  A,  but 
•     4  coinciding  observations  in  sweeps  make  it  50. 

131  B.  126.    Not  observed  by  me. 

136  B.  129.    Do.   But  I  presume  this  to  be  identical 

with  No.  133,  with  1"  error  of  R  A  in  the 
Brisbane  catal. 

137  B.  131. 

139  B.  139. 

140  B.  140. 

143  B.  143.    5'  error  in  the  P  D  of  the  Brisbane 

catal. 

144  B.  142. 
150  B.  146. 
153    B.  148. 

155    B.  150=  151.    Not  observed  by  me.    There  is 

certainly  no  such  double  star  in  this  place. 
161    B.  164. 
164    B.  161  ? 

171  B.  169. 

172  B.  170. 

178  The  minute  of  R  A  should  perhaps  be  6. 

179  Do. 

189    No  doubt  the  same  star,  with  a  mis-reading  in 
P  D  in  one  or  other  observation. 

192  B.  184. 

193  B.  185. 

194  The  Nubecula  Minor  terminates  at  this  place, 

as  observed  in  the  20-feet.  One  minute  fur- 
ther in  R  A,  it  is  completely  past. 

196  B.  189. 

197  B.  191. 
200    B.  194. 

202  B.  198. 

203  B.  200. 
208    B.  198. 

217  B.  206. 

218  B.  207. 

219  On  parallel  of  B.  206. 

224  B.  211. 

225  B.  213. 

230  The  preceding  of  2. 

231  The  following. 

234  The  preceding  of  2. 

235  The  following  of  2. 


156 


STARS,  NEBULiE,  AND  CLUSTERS,  LN  THE  NUBECULA  MAJOR. 


No.  for 

Obj. 

Mag. 

R  A.  1830.0. 

N  P  D 

1830.0. 

No  for 

Obj. 

Mag. 

R  A.  1830.0. 

N  P  D 

1830.0. 

Zone. 

Refe- 

Zone. 

Refe- 

rence. 

h.   m.  s. 

0 

/ 

» 

rence. 

h. 

m. 

s. 

0 

/ 

» 

I 

S 

9 

4  41  7 

156 

12 

54 

12 

5° 

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9 

4 

47 

58 

156 

45 

54 

13 

2 

S 

8 

4  41  20 

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12 

55 

f 

51 

s 

8 

4 

48 

27 

161 

24 

55 

16 

7' 

21 

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32 

52 

N 

4 

48 

33 

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3=> 

20 

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3 

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8 

4  4i  58 

161 

48 

25 

16 

53 

S 

9 

4 

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4 

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s 

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4  42  2 

158 

55 

16 

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ID 

3 

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8 

5 

55 

53 

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54 

s 

10' 

4 

39 

157 

5 

15 

32 

5 

N 

4  42  13 

156 

7 

25 

/ 

55 

N 

4 

48 

41 

159 

40 

IO 

/ 

6 

s 

8' 

4  42  36 

156 

5° 

36 

/ 

56 

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10' 

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157 

3 

15 

32 

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49 

54 

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s 

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157 

8 

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32 

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s 

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s 

9 

4 

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156 

51 

54 

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4  42  43 

160 

31 

13 

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59 

N 

4 

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30 

31 

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4  42  46 

160 

30 

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60 

s 

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4 

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25 

13 

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4 

157 

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4  43  12 

156 

40 

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3 

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4  43  47 

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68 

s 

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161 

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N 

III. 

4  44  ± 

160 

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69 

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4 

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4  44  26 

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4 

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/ 

IN  THE  NUBECULA  MAJOR. 


157 


No.  for 

Mag. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Zone 

No.  for 

Obj. 

Mag. 

R  A.  1830.0. 

NPD.  1830.0. 

one. 

Refe- 

Refe- 

rence. 

h    m  s 

0      /  // 

h. 

m.  s. 

0      /  * 

99 

f  11 

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p 
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130 

XT 

JN 

TT 
11. 

4  58  0 

159  50  15 

9 

193 

s 

5 

5 

4  56 

161  32  46 

f 

N 

1 

48  44 

p 

f 

0 

59 

32  55 

ID 

131 

XT 

JN 

I. 

4  58  12 

157  29  47 

f 

I94 

s 

IO 

c 

J 

C  I 

j 

156  56  54 

J3 

132 

s 

9 

4  58  18 

159    6  45 

9 

!95 

s 

7' 

c 

J 

c  1 

162    5  55 

16 

I33 

N 

4  58  20 

156  40  41 

/ 

196 

N 

III. 

e 

j 

<;  7 

156  27  20 

/ 

J34 

S 

10' 

4  58  22 

1S9  54  15 

9 

J97 

CI 

II. 

5 

c  IO 

j 

160  34  17 

/ 

'35 

s 

9 

4  58  24 

161    3  43: 

15 

198 

s 

9 

c 

D 

1  IO 

159  59  J5 

9 

13b 

8 

28 

2  25 

16 

10 

IO 

59  J3 

15 

5s 

9' 

4  58  34 

156  26  54 

13 

199 

N 

C 
J 

<  12 

159  10  15 

9 

*37 

C» 
3 

9 

4  58  35 

159  14  15 

9 

200 

N 

II. 

c 

J 

<;  28 

158  16  37 

f 

I3X 

XT 

JN 

III. 

4  58  36 

160  41  7 

f 

201 

N 

II. 

5 

C  2Q 

159  36  43 

/ 

139 

XT 

JN 

I. 

4  58  39 

156  14  16 

/ 

202 

S 

7' 

e 

j 

158  19  IO 

5 

140 

a 
S 

9' 

4  5'8  39 

156  58  24 

J3 

s 

8 

39 

18  27 

f 

141 

10 

4  58  42 

157  19  33 

12 

203 

8 

5 

5  4° 

159    8  15 

9 

142 

c 

6' 

4  58  48 

161    9  55 

16 

•• 

8 

44 

8  5 

5 

J43 

10' 

4  58  49 

J59  55  15 

9 

204 

s 

10 

5 

5  45 

161  37  55 

16 

144 

N 

T 
1. 

4  58  55 

159  38  56 

/ 

205 

N 

II. 

5 

5  4*> 

!59  34  7 

/ 

IN 
IN 

59 

39  J5 

9 

206 

s 

9' 

5 

t  n 

j  j 

160  53  43 

15 

59 

38  15 

9 

207 

s 

9 

5 

5  55 

159  24  45 

9 

H5 

Q 

c 

O 

N 

IO 

4  59  5 

161  51  55 

16 

208 

s 

8 

5 

5  59 

156  n  24 

!3 

9 

4  59  21 

159  19  15 

9 

209 

s 

9 

S 

6  7 

159  56  15 

9 

147 

I. 

4  59  2' 

159    6  15 

9 

210 

N 

5 

6  14 

159  39  15 

9 

148 

N 

4  59  24 

J57  59  4° 

J 

XT 

IN 

T 
1 . 

16 

37  35 

p 
J 

149 

S 

8' 
VII. 

4  59  38 

160  24  13 

15 

21 1 

N 

I. 

5 

6  15 

159  26  17 

f 

150. 

c 

4  59  47 

!56    5  15 

/ 

212 

N 

III. 

5 

6  17 

160  57  27 

f 

151 

s 

9 

502 

156  14  54 

213 

S 

9' 

5 

6  20 

160  48  43 

15 

15a 

s 

10 

5    0  29 

1S&  34  54 

13 

214 

N 

S 

6  21 

158  51  1 

/ 

i53 

s 

8 

III. 

S    0  36 

158  49  19 

5 

215 

S 

9 

S 

6  28 

158    7  35 

5 

i54 

N 

5    0  36 

160  24  25 

/ 

216 

N 

5 

6  36 

160  56  43 

15 

155 

N 
S 

II. 

5    0  49 

1S9  47  57 

/ 

N 

43 

56  16 

/ 

,56 

9 

5    1  1 

159    8  15 

9 

217 

S 

8 

5 

6  38 

158  37  4 

5 

i57 

N 

II. 

5    1  13 

160     2  12 

/ 

c 

VII. 

40 

39  48 

/ 

158 

S 

s 

9' 

5    1  25 

'57  4°  33 

12 

218 

s 

10 

5 

6  43 

160  25  43 

'5 

159 
160 
161 
162 

8' 

5    1  33 

159  35  15 

9 

219 

s 

10 

S 

6  43 

160  32  43 

15 

s 

10 

5    1  34 

161    6  25 

16 

220 

c 

VI. 

S 

6  43 

160  56  16 

/ 

s 

10 

5    1  44 

160  42  13 

15 

221 

N 

II. 

5 

6  47 

158  50  57 

/ 

N 

II. 

5    1  47 

159  51  0 

/ 

222 

s 

10 

5 

7  6 

160    6  43 

15 

163 

s 

10 

5    1  53 

160  42  13 

15 

223 

N 

II. 

5 

7:13 

161  58  28 

/ 

s  s 


158  STARS,  NEBULAE,  AND  CLUSTERS 


No.  for 
Refe- 
rence. 

Obj. 

Mag. 

R  A.  1830.0. 
h.  m.  s. 

N  P  D.  1830.0. 
0      /  * 

Zone. 

No.  for 
Refe- 
rence. 

Obj. 

Mag. 

R  A.  1830.0. 
h.  m.  s. 

N  P  D.  1830.0. 
0     t  11 

Zone. 

224. 

N 

III. 

5 

7  '■i 

'37 

-9 

Si 

/ 

6 

5° 

22 

33 

12 

225 

N 

II. 

5 

T  IO 

T  C*7 

J3/ 

if. 

1  3 

/ 

5' 

59 

22 

55 

21 

226 

S 

10 

c 
3 

7  43 

l6l 

fi 

33 

16 

5 

59 

23 

39 

17 

227 

S 

8' 

5 

7  4-6 

54 

43 

15 

5' 

fir 

°5 

23 

J3 

15 

8 

C2 

t  + 

y 

17 

275 

S 

9' 

5 

1  i 

49 

157  46 

3 

12 

228 

s 

10 

c 
3 

7  4-6 

l6o 

13 

A  1 

4-3 

15 

276 

c 

VII. 

5 

'4 

1 

J57  34 

7 

/ 

229 

N 

II. 

5 

7  4° 

157 

40 

/ 

277 

s 

8 

5 

J4 

5 

I58  12 

49 

5 

230 

s 

8 

5 

7  3" 

J59 

J5 

9 

278 

c 

5 

9 

J57  3s 

4° 

/ 

231 

s 

9 

3 

1 60 

43 

15 

279 

N 

I. 

r 

3 

J4 

1  j 

'59  J7 

30 

/ 

9 

61 

18 

39 

17 

280 

c 

5 

!4 

J57  31 

23 

/ 

CI 

9 

68 

33 

/ 

281 

N 

3 

1A 

159  31 

*5 

9 

232 

s 

10 

3 

8  1 

161 

[6 

35 

16 

N 

II. 

20 

30 

12 

/ 

233 

N 

I. 

5 

0  7 

x59 

/ 

282 

N 

II. 

5 

'4 

23 

J59  33 

55 

/ 

234 

s 

9' 

c 

8  10 

1 60 

T  n 
J  9 

39 

17 

283 

N 

I. 

3 

'4 

29 

1 59  33 

/ 

9' 

T  1 

1  3 

161 

*9 

43 

15 

284 

N 

III. 

5 

'4 

32 

J59  34 

1 

— 

235 

c 

£ 

3 

8  29 

24 

g 

/ 

285 

s 

9' 

5 

'4 

45 

159  11 

'5 

9 

236 

s 

9' 

5 

8  52 

t  rft 
150 

24 

54 

13 

286 

N 

III. 

5 

'4 

4° 

160  39 

52 

/ 

237 

s 

10 

S 

P.  re 

5  55 

'57 

23 

3 

12 

287 

s 

9; 

5 

'4 

49 

'59  45 

J5 

9 

238 

s 

9' 

5 

9  3 

158 

41 

31 

5 

9' 

5° 

43 

T  9 
I  O 

IO 

239 

N 

III. 

5 

9  18 

156 

3° 

5° 

/ 

288 

s 

10 

5 

x4 

52 

159  32 

J5 

9 

240 

s 

7 

5 

9  22 

Jul 

2  3 

55 

16 

289 

N 

5 

'4 

52 

'59  33 

46 

— 

241 

s 

10 

5 

9  27 

ID  I 

24 

25 

16 

290 

s 

10 

5 

'4 

53 

J59  31 

O 

— 

242 

N 

I. 

5 

9  35 

158 

57 

59 

/ 

10 

°5 

30 

IO 

N 

35 

59 

0 

5 

291 

s 

10 

5 

'4 

57 

159  27 

48 

IO 

243 

S 

10 

5 

9  35 

20 

55 

16 

292 

s 

10 

5 

'4 

59 

'59  43 

t  SI 

IO 

244 

N 

II. 

5 

9  +*> 

J57 

59 

10 

/ 

293 

s 

10 

5 

J5 

% 

IDI  18 

25 

16 

245 

S 

8 

5 

9  51 

I5D 

37 

24 

13 

2  94 

s 

10 

5 

J5 

IO 

159  22 

16 

IO 

8' 

52 

37 

rft 

5° 

/ 

295 

s 

7' 

5 

J5 

1 1 

IDI  14 

25 

16 

246 

N 

5 

10  7 

*59 

5 

J5 

9 

296 

N 

II. 

5 

J5 

J3 

I50  18 

51 

N 

I. 

12 

3 

23 

/ 

297 

N 

5 

*5 

ID 

159  29 

0 

— 

247 

N 

5 

*59 

2 

25 

5 

298 

s 

10 

5 

1 5 

20 

'59  44 

T  9 

15 

IO 

248 

CI 

18 

2 

49 

/ 

299 

s 

10 

5 

J5 

33 

1 59  43 

4-3 

10 

S 

9 

3 

10  24 

J59 

23 

J5 

9 

300 

s 

10 

5 

J5 

39 

159  23 

1 0 

IO 

249 

N 

S 

1 0  24 

*59 

20 

J5 

9 

301 

N 

III. 

5 

1 5 

42 

156  20 

41 

/ 

N 

I. 

32 

20 

9 

/ 

302 

N 

III. 

5 

IS 

52 

156  30 

1 1 

/ 

250 

S 

7' 

5 

I O  42 

J59 

55 

39 

17 

3°3 

s 

10 

5 

]5 

53 

156  44 

54 

13 

8 

45 

ft  £L 

5  6 

*5 

9 

3°4 

s 

10 

5 

]5 

57 

159  22 

IO 

8 

5° 

55 

J7 

/ 

305 

s 

9 

5 

•5 

5° 

Tftn  St 

9 

17 

251 

N 

5 

10  46 

*59 

u 

x5 

9 

D3 

Q 

8 

12 

/ 

N 

I. 

47 

5 

53 

/ 

306 

N 

II. 

5 

J5 

5s 

'59  9 

2 1 

/ 

N 

55 

0 

53 

5 

307 

s 

9' 

5 

1 0 

0 

159  2 

J5 

9 

252 

S 

9 

5 

11  11 

S3 

54 

13 

9' 

22 

0 

Id 

IO 

253 

S 

9 

5 

11  27 

6 

1  ft 

9 

17 

308 

s 

9 

5 

j  0 

10 

J57  J4 

27 

5 

254 

N 

II. 

5 

11  31 

158 

57 

45 

/ 

3°9 

s 

9 

5 

1  0 

IO 

J59  49 

1 0 

IO 

255 

S 

8' 

5 

1 1  32 

J59 

30 

*5 

9 

310 

s 

8 

5 

I  ft 

1  0 

J7 

160  46 

9 

J7 

256 

S 

9' 

5 

11  47 

I  60 

40 

9 

17 

311 

s 

9' 

5 

T  ft 

I  0 

32 

160  27 

39 

17 

257 

S 

10 

5 

1 1  50 

I  60 

23 

9 

17 

312 

s 

8 

5 

I  0 

45 

161  41 

55 

16 

258 

S 

10 

5 

11  58 

ID  I 

35 

55 

16 

313 

s 

9 

5 

J7 

4 

»57  43 

33 

12 

259 

N 

III. 

5 

12  3 

I56 

20 

5° 

/ 

3H 

N 

II. 

5 

*7 

5 

»59  37 

48 

IO 

260 

N 

III. 

5 

12  23 

IDO 

59 

2 

/ 

N 

IO 

38 

35 

/ 

261 

N 

I. 

5 

12  28 

158 

55 

27 

f 

3i5 

N 

II. 

5 

17 

6 

157  30 

29 

/ 

262 

S 

9 

5 

12  36 

i57 

46 

1 

/ 

316 

s 

10 

5 

17 

13 

160  13 

39 

17 

263 

s 

8 

5 

12  43 

159 

44 

*7 

/ 

317 

s 

9' 

5 

J7 

17 

159  29 

18 

IO 

8 

44 

4S 

15 

9 

318 

s 

9' 

5 

17 

21 

158  21 

45 

5 

8 

49 

45 

48 

10 

319 

s 

10 

5 

17 

34 

158  19 

39 

5 

264 

s 

9' 

5 

12  48 

,58 

9 

51 

5 

320 

s 

7' 

5 

17 

43 

160  38 

39 

17 

265 

N 

II. 

5 

13  0 

i57 

49 

18 

/ 

321 

N 

III. 

5 

17 

47 

157  37 

1 1 

/ 

266 

s 

10 

5 

13  1 

156 

24 

54 

!3 

322 

O 
& 

IO 

5 

17 

47 

159  2 

48 

IO 

267 

s 

10 

5 

13  10 

160 

38 

9 

17 

323 

s 

9' 

5 

17 

48 

158  18 

7 

5 

268 

s 

nt 

5 

13  15 

i57 

54 

33 

12 

324 

s 

IO 

5 

17 

49 

159  57 

18 

IO 

269 

N 

5 

13  16 

158 

57 

40 

/ 

325 

s 

9 

5 

17 

52 

159  13 

18 

IO 

270 

s 

10 

s 

13  19 

161 

21 

55 

16 

326 

N 

II. 

5 

iS 

4 

158  2 

57 

/ 

271 

s 

9' 

5 

13  21 

160 

34 

39 

17 

327 

N 

II. 

5 

iS 

6 

159  49 

35 

/ 

272 

N 

III. 

5 

13  25 

156 

29 

6 

/ 

328 

S 

9' 

5 

iS 

8 

158  39 

5 

5 

273 

s 

IO 

5 

13  29 

156 

3i 

54 

13 

8' 

12 

38 

32 

19 

274 

s 

6 

5 

13  44 

i57 

23 

3 

12 

329 

s 

10 

5 

18 

159  5fi 

18 

IO 

5' 

48 

22 

55 

22 

33° 

N 

I. 

5 

18 

156  47 

5° 

/ 

49 

23 

2 

19 

331 

s 

9 

5 

18 

17 

159  45 

18 

IO 

f 

5° 

22 

54 

13 

332 

c 

7 

5 

18 

17 

158  45 

56 

/ 

5' 

55 

23 

4 

28 

s 

8' 

25 

46 

34 

5 

55 

22 

35 

14 

s 

8 

33 

46 

2 

'9 

c 

5' 

55 

22 

33 

/ 

333 

s 

10 

5 

18 

32 

156  58 

54 

13 

IN  THE  NUBECULA  MAJOR. 


159 


No.  for 
Refe- 
rence. 

Obj. 

Mag. 

R  A.  1830.0. 
h.  m.  s. 

N  P  D.  1830.0. 
0     /  // 

Zone. 

No.  for 
rence. 

Obj. 

Mag. 

R  A.  1830.0. 
h.  m.  s. 

N  P  D.  1830.0. 
0  to 

Zone. 

334 

N 

5 

18 

33 

>59 

30 

18 

IO 

396 

s 

8' 

5 

22  45 

158  13  32 

19 

N 

1. 

35 

3° 

29 

/ 

397 

s 

IO 

5 

22  46 

159  36  14 

1 1 

335 

S 

10 

s 

iS 

43 

159 

56 

18 

IO 

398 

N 

5 

22  48 

158    8  0 

/ 

336 

S 

q 
y 

s 

18 

47 

158 

31 

2 

5 

N 

III. 

5° 

8  2 

19 

y 

58 

31 

32 

19 

399 

N 

5 

22  50 

158    3  27 

337 

s 

10 

5 

18 

48 

158 

41 

32 

19 

400 

S 

9' 

5 

22  51 

I<7  20  33 

J  1       J    J  J 

12 

338 

s 

8 

5 

18 

5i 

160 

25 

39 

17 

401 

S 

9' 

5 

22  54 

161  42  55 

16 

339 

s 

0 

5 

iS 

52 

158 

3S 

30 

5 

402 

N 

III. 

5 

22  54 

156  32  IO 

/ 

8' 

52 

38 

2 

19 

403 

S 

10' 

5 

22  57 

158    1  32 

19 

34° 

s 

10 

5 

19 

10 

160 

0 

18 

IO 

404 

N 

II. 

5 

22  57 

157  20  24 

/ 

34i 

s 

10 

5 

*9 

11 

158 

38 

2 

19 

405 

N 

II. 

5 

23  2 

160   6  17 

/ 

342 

s 

10 

5 

'9 

14 

161 

6 

55 

16 

406 

S 

10 

5 

23  3 

156  34  35 

J4 

343 

N 

II. 

5 

*9 

14 

156 

55 

5i 

/ 

407 

s 

7' 

5 

23  J3 

160    1  19 

25 

344 

s 

9' 

5 

'9 

17 

156 

9 

54 

13 

408 

s 

10 

5 

23  22 

160   6  58 

18 

345 

CI 

VII. 

5 

19 

23 

J59 

23 

18 

/ 

409 

s 

10 

5 

23  38 

ICQ  <C  44 

J  7     J  J  TT 

1 1 

s 

9 

31 

23 

18 

IO 

410 

s 

9' 

5 

23  41 

160  43  28 

18 

346 

N 

43 

:3 

18 

IO 

411 

s 

8' 

5 

23  41 

158  13  32 

19 

s 

10 

5 

'9 

23 

159 

54 

18 

IO 

412 

s 

IO 

5 

23  43 

158    2  32 

19 

347 

s 

10 

5 

19 

23 

158 

1 2 

32 

19 

413 

s 

9' 

5 

23  46 

158  59  2 

19 

348 

s 

10 

5 

'9 

3i 

159 

20 

18 

IO 

414 

s 

IO 

5 

23  56 

156  32  5 

14 

349 

s 

9 

5 

J9 

34 

J59 

25 

18 

IO 

415 

N 

II. 

5 

24  12 

160  18  24 

/ 

35° 

N 

III. 

5 

l9 

37 

156 

58 

8 

f 

416 

s 

10' 

5 

24  15 

160  23  58 

18 

351 

s 

0' 

y 

5 

!9 

38 

158 

45 

32 

IQ 

y 

4-17 

T  / 

N 

III. 

5 

24  47 

156  36  16 

r 

J 

352 

s 

8' 

5 

J9 

41 

156 

36 

54 

j 

4l8 
1 

s 

7 

5 

24  51 

161  TO  <  c 

16 

8' 

52 

156 

36 

5 

14 

4IQ 

s 

IO 

5 

24  52 

1^6    KQ   3  C 

ij     jy  .ij 

14 

353 

s 

7' 

5 

*9 

42 

'3 

54 

13 

420 

s 

9' 

5 

24  59 

159  38  44 

I  I 

7' 

51 

12 

35 

14 

421 

N 

II. 

5 

25  7 

ic6  32  I 

J  J 

f 

354 

s 

9 

5 

'9 

43 

159 

31 

18 

IO 

422 

s 

9 

5 

25  11 

158    I  ■J'? 

12 

355 

s 

10 

5 

J9 

43 

156 

25 

24 

13 

8 

14 

2  32 

IQ 

y 

356 

N 

5 

*9 

48 

159 

43 

18 

IO 

42  3 

s 

8 

5 

25  16 

1^6   24  3C 

14 

357 

s 

q' 
y 

5 

*9 

49 

158 

2 

2 

19 

c 

39 

24  36 

f 

J 

358 

N 

1. 

5 

J9 

53 

J59 

34 

33 

/ 

424 

s 

10 

5 

25  23 

160  15  58 

l8 

N 

55 

156 

35 

18 

IO 

42C 

s 

10' 

5 

25  33 

IC8  43  12 

IQ 

*y 

359 

S 

9' 

5 

J9 

51 

46 

54 

13 

426 

s 

7 

5 

25  37 

158    8  32 

10 

360 

s 

q 
y 

5 

*9 

57 

158 

44 

32 

IQ 

y 

427 

s 

10 

5 

25  41 

l6l    1 7 

16 

361 

s 

8 

5 

'9 

57 

161 

42 

25 

16 

s 

10 

5 

25  51 

1C7  cc  3-1 

J  /    JJ    J  J 

12 

362 

s 

10 

5 

'9 

58 

158 

35 

32 

10 

y 

A2Q 

N 

II. 

5 

25  56 

I c8    17  2 

j      j  / 

r 

J 

363 

N 

III. 

5 

20 

1 

161 

25 

29 

r 

J 

A.'XO 

TJ 

s 

8 
I. 

5 

26  0 

i c6  1 c  c 

IA 

T 

364 

s 

9' 

5 

20 

1 

158 

55 

32 

IQ 

y 

A.1 1 

N 

5 

26  4 

i  <;6  4-1  0 

J        TT  v 

f 

J 

365 

N 

III. 

5 

20 

5 

T59 

10 

0 

f 
j 

N 

8 

IA 

T 

366 

s 

IO 

5 

20 

10 

158 

3 

2 

TO 

xy 

tj^ 

N 

I. 

5 

26  7 

l6o     2  ^3 

f 
J 

367 

c 

VI. 

5 

20 

16 

i57 

2 

4i 

f 

A  "3  1 

s 

IO 

5 

26  23 

T  CO    2*3  A/1 
*  J  tt- 

I  I 

368 

s 

10 

5 

20 

18 

!57 

iS 

3 

12 

A?  A 
TJT 

s 

IO 

5 

26  24 

1 J /    Tu    J  i 

1 2 

■360 

j  y 

N 

5 

20 

25 

*59 

48 

18 

IO 

A.1  C 
<tlj 

N 

II. 

5 

26  28 

ic8  c8  1 t 
1  j 0  j  5l 

f 
J 

370 

s 

10 

5 

20 

33 

T59 

48 

18 

IO 

tJu 

N 

5 

26  30 

T  C7     1"7  11 

xj/  j 1  5$ 

371 

N 

II. 

5 

20 

32 

156 

56 

28 

f 

J 

c 

26  35 

18  CO 

f 

J 

372 

s 

10 

5 

20 

36 

158 

7 

32 

IO 

Ly 

t3  / 

s 

IO 

5 

26  34 

l6l    17  CC 

l6 

373 

N 

III. 

5 

20 

5° 

159 

56 

52 

f 
j 

Ai8 
t3° 

s 

IO 

5 

26  47 

ICQ   20  11 

1jy  -^y  T*t 

I  j 

374 

N 

VIII. 

5 

21 

7 

J59 

38 

18 

IO 

A"2Q 

H-jy 

s 

IO 

5 

26  50 

ICO    11  AA. 

*jy  j x  it 

I  j 

375 

C 

5 

21 

19 

156 

1 

58 

f 

A  AC) 
TT 

s 

9' 

y 

5 

26  51 

ICQ   AC  IA 
XJ7    TJ  xf 

1 1 

376 

s 

10 

5 

21 

27 

J59 

11 

18 

IO 

9 

64 

TJ     J  J 

20 

377 

s 

8 

5 

21 

33 

158 

8 

2 

10 

y 

A  A  T 
TT 

s 

10 

5 

26  55 

IC7  C7 

J  /     J  I  JJ 

I  2 

378 

s 

11 

5 

21 

35 

J59 

38 

18 

IO 

A  A  7, 

TT 

N 

II. 

5 

27  3 

ICQ   c8  CO 

xjy  )° 

f 

379 

s 

9 

5 

21 

51 

158 

31 

32 

IQ 

y 

N 

5 

t8  aa 

I  I 

380 

N 

II. 

5 

2 1 

55 

!59 

4i 

32 

f 

443 

s 

10' 

5 

27  7 

I  CO    12  AA 

j  y  tt 

I  I 

381 

s 

1 1 

5 

21 

57 

159 

38 

18 

IO 

AAA 
11  1 

s 

10' 

5 

27  11 

ICQ    12  IA 

jy  t 

I  j 

382 

s 

9' 

5 

21 

58 

J59 

25 

18 

IO 

s.s 

10 

18 

13  33 

20 

383 

s 

8' 

5 

22 

2 

160 

54 

39 

17 

445 

N 

III. 

5 

27  7 

160  4  19 

/ 

384 

N 

8' 

11 

53 

58 

18 

446 

N 

III. 

5 

27  10 

158  58  34 

/ 

5 

22 

8 

158 

5 

J3 

/ 

447 

S 

IO 

5 

27  13 

158  14  32 

19 

385 

s 

9' 

5 

22 

13 

161 

55 

55 

16 

448 

N 

III. 

5 

27  27 

158  56  52 

/ 

386 

N 

11. 

5 

22 

13 

156 

iS 

7 

/ 

449 

N 

II. 

5 

27  36 

158  57  3 

/ 

387 

N 

I. 

5 

22 

16 

*59 

38 

40 

/ 

450 

S 

IO 

5 

27  41 

158  58  32 

'9 

388 
389 

S 

8 

5 

22 

27 

161 

7 

25 

16 

CI 

* 

47 

57  34 

/ 

N 

5 

22 

27 

158 

4 

31 

45i 

N 

5 

27  43 

J57  34  33 

12 

390 

S 

10 

5 

22 

27 

i59 

37 

48 

IO 

CI 

48 

35  34 

/ 

10 

28 

36 

44 

1 1 

452 

N 

5 

27  45 

158  58  .. 

/ 

10 

33 

37 

14 

II 

453 

S 

6 

5 

27  46 

158  45  32 

19 

391 

s 

10 

5 

22 

28 

161 

37 

55 

16 

54 

45  19 

/ 

392 

N 

II. 

5 

22 

31 

158 

6 

58 

/ 

54 

45  33 

20 

393 

S 

10 

5 

22 

40 

159 

37 

44 

1 1 

S 

6 

59 

44  59 

21 

394 

s 

10 

5 

22 

40 

159 

35 

44 

1 1 

454 

IO 

5 

27  49 

*59  35  33 

20 

395 

s 

9' 

5 

22 

4i 

158 

46 

32 

19 

455 

s 

1 1 

5 

27  49 

158  58  42 

'9 

160 


STARS,  NEBULJS,  AND  CLUSTERS 


No.  for 

No.  for 

Obj. 

Refe- 

Obj. 

Mag. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Zone. 

Refe- 

Mag. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Zone. 

rence. 

h.  m.  s. 

0      /  // 

rence. 

h.  m.  s. 

0 

/  a 

a  rA 

45° 

XT 
IN 

5  27  5° 

159  13  44 

1 1 

5°5 

XT 

JN 

5  31  20 

157 

4  25 

22 

XJ 
JN 

At 
01 

13  33 

20 

rt 
l> 

28 

5  23 

J 

4S7 

0 
S 

10 

5  27  57 

158  37  32 

19 

5O0 

XT 

IN 

30 

4  3 

12 

458 

N 

III. 

5  28  3 

J59  59  4 

/ 

s 

9' 

5  31  31 

160 

23  28 

18 

459 

S 

9 

S  28  7 

157  44  3 

12 

507 

s 

9 

5  31  35 

159 

54  33 

20 

9 

*3 

43  33 

12 

9 

8 

41 

54  33 

20 

400 

8 

17 

42  25 

22 

508 

0 

5  31  37 

160 

5  58 

18 

XT 

IN 

5  28  9 

159  58  44 

1 1 

509 

XT 

IN 

8' 

5  31  39 

!59 

52  33 

20 

XT 

IN 

*  A 
ID 

58  44 

1 1 

510 

s 

5  31  39 

156 

48  5 

14 

401 

XT 

II. 

l8 

59  49 

/ 

511 

s 

9' 

5  3i  44 

158 

13  52 

19 

0 

9' 

5  28  1 1 

161    6  25 

16 

512 

s 

IO 

5  31  45 

159 

27  33 

20 

A  £> " 

4.02 

0 

9 

5  28  12 

156  40  5 

14 

5J3 

a 

IO 

5  31  49 

159 

15  43 

20 

A  A* 
4D3 

1M 
IN 

TIT 
1X1. 

5  28  19 

159  S8  59 

r 
J 

5H 

9' 

5  31  55 

156 

28  5 

14 

a  a  a 

4.64 

0 

8 

5  28  19 

160  12  28 

18 

5J5 

s 

9r 

5  32  0 

159 

10  33 

20 

8 

24 

11  55 

r 
J 

f  T  A 

51b 

10' 

7 

10  33 

20 

A  A  r- 

4b5 

0 
0 

8 

52821 

158  11  32 

J9 

s 

IO 

5  32  5 

157 

34  25 

22 

A  AA 
4"0 

it 

I. 

5  28  32 

156  21  35 

14 

5r7 

IO 

5  32  6 

156 

0  35 

14 

A  A.T 

4°  7 

N 

33 

21  41 

/ 

518 

s 

IO 

5  32  9 

159 

40  33 

20 

10 

5  28  42 

159  34  33 

20 

IO 

14 

40  3 

20 

.AO 

405 

XT 

JN 

5  28  44 

159  16  44 

1 1 

5J9 

N 

TT 

11. 

5  32  11 

!59 

16  33 

20 

i~  i 

5° 

15  33 

20 

N 

12 

18  7 

J 

A  A~ 

469 

52 

15  35 

/ 

520 

s 

9 

5  32  12 

160 

18  28 

18 

5  28  45 

159    7  44 

1 1 

521 

s 

9 

5  32  24 

157 

55  33 

12 

c 

5i 

7  12 

/ 

9 

29 

55  25 

22 

470 

0 

10 

5  28  47 

157  59  33 

12 

9 
8' 

34 

55  25 

22 

8' 

53 

60  32 

19 

522 

s 

5  32  24 

160 

56  8 

18 

471 

S 

9 

5  28  47 

160  52  28 

18 

8 
II. 

25 

55  55 

16 

472 

S 

10 

5  28  55 

159  20  44 

11 

523 

N 

5  32  39 

160 

57  12 

i» 
J 

473 

S 

8 

5  29  7 

156  48  35 

14 

524 

s 

^ 

5  32  45 

157 

11  25 

22 

474 

s 

8 

5  29  13 

156  45  5 

14 

9 

49 

11  25 

22 

475 

XT 

JN 

I. 

5  29  15 

160    6  19 

/ 

525 

N 

T 
1. 

5  32  45 

157 

38  13 

/ 

476 

/ 1 

5  29  17 

157  33  42 

/ 

526 

S 

IO 

5  32  47 

158 

38  29 

21 

477 

0 

7 

5  29  20 

156  33  56 

/ 

527 

s 

9 

5  32  48 

156 

29  5 

14 

478 

XT 
JN 

7' 

23 

33  5 

14 

528 

s 

9 

5  32  52 

157 

47  25 

22 

II. 

5  29  22 

160  52  15 

/ 

c 

VI. 

53 

48  36 

f 

479 

0 

9 

5  29  24 

158  IO  2 

19 

529 

s 

8 

5  33  2 

161 

2  41 

23 

4-50 

XT 

JN 

5  29  27 

159  16  44 

11 

7 

3 

3  25 

_  A 
ID 

c* 

Vll. 

34 

16  22 

/ 

53° 

CI 

T7TT 
V  11. 

5  33  5 

»59 

22  38 

J 

IO 

39 

15  33 

20 

53i 

s 

IO 

5  33  10 

161 

32  11 

23 

QaJS  I 

0 

IO 

5  29  29 

160  39  20 

18 

532 

s 

IO 

5  33  11 

161 

20  11 

23 

452 

IO 

5  29  30 

159    2  44 

11 

533 

N 

TT 
11. 

5  33  15 

160 

4  17 

J 

483 

c 

IO 

5  29  34 

158  56  32 

19 

534 

s 

9' 

5  33  15 

159 

16  33 

20 

484 

S 

9 

5  29  34 

160    5  14 

11 

535 

N 

5  33  33 

160 

16  28 

l8 

485 

0 

10 

5  29  37 

i56    9  5 

14 

N 

T 
1. 

45 

16  3 

J 

450 

55 

8 

5  29  5° 

161  20  55 

16 

536 

N 

5  33  36 

161 

11  11 

23 

A  o„ 
487 

0 

10 

5  29  55 

160    3  28 

18 

N 

TT 
11. 

41 

11  30 

J 

488 

CI 

II. 

5  30  2 

158  52  15 

/ 

537 

N 

II. 

5  33  37 

157 

49  26 

J 

489 

XT 

IN 

5  3°  J5 

161  59  55 

/ 

538 

N 

II. 

5  33  42 

157 

36  25 

22 

49O 

s 

9 

5  30  26 

157  51  25 

22 

N 

53 

34  7 

f 

9, 

30 

50  33 

12 

539 

S 

9 

5  33  43 

»59 

20  33 

20 

491 

s 

9 

5  30  26 

156  42  35 

14 

540 

s 

 / 

IO 

5  33  58 

158 

22  29 

21 

492 

XT 

IN 

* 

5  30  26 

157    0  3 

12 

54i 

s 

IO 

5  34  2 

160 

39  58 

IS 

N 

I. 

27 

0  31 

/ 

542 

s 

9' 

5  34  9 

157 

7  25 

22 

N 

29 

1  5 

14 

543 

s 

IO 

5  34  14 

158 

40  29 

21 

493 

s 

8 

5  30  28 

161  13  55 

16 

IO 

17 

40  59 

21 

494 

s 

5  3°  32 

158  60  32 

19 

544 

s 

9' 

5  34  26 

157 

26  55 

22 

\ 

34 

59  33 

20 

545 

s 

9' 

5  34  29 

»57 

20  25 

22 

ty  j 

s 

9 

5  3°  39 

158  22  32 

19 

546 

8' 

158 

3  29 

2  I 

496 

s 

8 

5  3°  4i 

161    2  55 

16 

547 

s 

5  34  38 

157 

6  25 

22 

497 

s 

9 

5  3°  44 

156  40  5 

H 

548 

s 

%• 

5  34  44 

160 

47  28 

18 

498 

s 

9' 

5  3°  47 

158    3  32 

19 

549 

s 

IO 

5  34  44 

157 

23  25 

22 

499 

N 

II. 

5  3°  49 

156  35  25 

/ 

55° 

s 

IO 

5  34  49 

157 

4  25 

22 

N 

54 

35  35 

14 

55i 

s 

8' 
VI. 

5  34  56 

157 

0  25 

22 

500 

S 

10 

5  3°  53 

*59  34  33 

20 

CI 

65 

0  20 

/ 

501 

N 

I. 

5  3°  54 

157  24  33 

12 

552 

s 

IO 

5  34  56 

157 

14  25 

22 

N 

58 

24  35 

/ 

553 

s 

IO 

5  34  58 

157 

3  25 

22 

N 

58 

24  55 

22 

554 

s 

IO 

5  35  6 

157 

27  25 

22 

502 

S 

9 

5  31  11 

158  13  32 

19 

555 

s 

10' 

5  35  i° 

158 

6  29 

21 

9 

!9 

13  29 

21 

556 

s 

IO 

5  35  11 

156 

59  55 

22 

5°3 

s 

10 

5  31  12 

158    6  32 

19 

557 

s 

IO 

5  35  11 

157 

27  5 

22 

504 

•  s 

6' 

5  31  15 

160  55  55 

16 

558 

s 

IO 

5  35  15 

158 

20  9 

21 

8 

19 

56  28 

18 

559 

s 

IO 

5  35  17 

157 

7  25 

22 

IN  THE  NUBECULA  MAJOR. 


161 


No.  for 

No  for 

Refe- 

Obj. 

Mag. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Zone. 

Refe- 

Obj. 

Mag. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Zone. 

rence. 

h.  m.  s. 

0     /  0 

rence. 

h.  m.  s. 

0  la 

560 

N 

I. 

5  35  *7 

161  48  30 

/ 

623 

S 

8 

5  37  55 

!58  57  33 

20 

561 

S 

8' 

5  35  20 

157  34  25 

22 

624 

— 

10 

59 

57  29 

21 

562 

S 

10 

5  35  24 

159  53  33 

20 

s 

7' 

5  37  59 

161  46  11 

23 

563 

CI 

VI. 

5  35  24 

i56    7  55 

/ 

625 

s 

10' 

5  38  3 

J59  35  33 

20 

564 

N 

II. 

5  35  25 

157  39  48 

/ 

626 

s 

10' 

5  38  3 

161  12  11 

23 

565 

S 

10 

5  35  27 

158  20  29 

21 

627 

N 

II. 

5  38  8 

157  31  6 

/ 

566 

s 

10' 

5  35  27 

159  20  33 

20 

628 

c 

VI. 

5  38  9 

159  29  IO 

567 

s 

7' 

5  35  28 

158  18  29 

21 

629 

N 

V. 

5  38  20 

159  53  IO 

568 

N 

III. 

5  35  39 

160    3  32 

/ 

630 

S 

10 

5  38  20 

160  23  28 

18 

569 

s 

10 

5  35  39 

160  34  58 

18 

63 1 

s 

10 

5  38  2i 

158    4  29 

21 

570 

s 

10 

5  35  42 

160  31  58 

18 

632 

s 

9 
8' 

5  38  26 

158  30  29 

21 

571 

N 

L 

5  35  45 

157  40  51 

/ 

633 

s 

5  38  26 

158  48  29 

21 

N 

46 

40  25 

22 

6  34 

s 

10 

5  38  26 

160  49  48 

18 

57* 

S 

10 

5  35  51 

158  51  29 

21 

635 

N 

II. 

5  38  27 

161    6  20 

/ 

573 

s 

10 

5  35  52 

158  25  29 

21 

636 

CI 

VI. 

5  38  29 

J59  3°  57 

/ 

574 

CI 

VI. 

5  35  54 

156  59  46 

/ 

637 

N 

I. 

5  38  38 

160  15  28 

18 

575 

N 

5  35  55 

161    5  41 

22 

638 

N 

43 

15  21 

/ 

N 

I. 

58 

6  27 

/ 

N 

II. 

5  38  41 

160  46  13 

/ 

576 

N 

I. 

5  35  58 

157  41  24 

/ 

639 

N 

II. 

5  38  44 

160  21  38 

/ 

577 

S 

10 

5  36  2 

157    9  25 

22 

640 

N 

III. 

5  38  46 

160  13  24 

/ 

578 

s 

8 

5  36  2 

159  34  33 

20 

641 

S 

8' 

5  38  48 

157  16  25 

22 

579 

CI 

1 1 

5  36  2 

J59  53  33 

20 

642 

N 

5  38  56 

159  x5  33 

20 

580 

s 

10' 

5  36  4 

157  45  25 

22 

643 

S 

9 

5  38  56 

158  30  59 

21 

58i 

s 

9' 

5  36  5 

157  59  25 

22 

644 

N 

III. 

5  38  59 

156  57  46 

/ 

582 

s 

9 

22 

60  29 

21 

645 

S 

9 

5  39  4 

158  50  29 

21 

s 

10 

5  36  7 

156  57  25 

22 

646 

S 

10 

5  39  J4 

159  12  3 

20 

583 

N 

III. 

5  36  10 

160  :  9  42 

/ 

647 

s 

1 1 

5  39  25 

158  55  29 

21 

584 

s 

8' 

5  36  11 

156  24  5 

14 

648 

N 

5  39  28 

160  20  28 

18 

585 

s 

10 

5  36  J3 

i57    9  55 

22 

N 

I. 

30 

19  22 

/ 

586 

s 

10 

5  36  16 

156  46  35 

14 

649 

S 

8 

5  39  31 

160  30  28 

18 

587 

s 

10 

5  36  16 

157  49  25 

22 

8 

36 

30  19 

25 

588 

s 

10 

5  36  24 

157  43  25 

22 

650 

s 

9 

5  39  34 

160  46  28 

18 

589 

s 

9 
9' 

36  26 

160  35  8 

18 

s 

9 

7' 
7' 

37 

46  19 

25 

590 

s 

36  26 

158  37  29 

21 

651 

s 

5  39  37 

160    2  58 

18 

591 

N 

II. 

5  36  33 

157  4°  5 

/ 

37 

3  19 

25 

592 

s 

8 

5  36  34 

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s 

8 

5  55  l9 

J59  J5  23 

30 

— 

8' 

59 

50  23 

28 

572 

a 

9 

5  55  28 

r57  13  4 

28 

a  14 

s 

10 

5  5°  58 

156  26  0 

27 

873 

a 

9 

5  55  29 

J57  44  4 

28 

815 

s 

10 

5  51  2 

156  39  30 

27 

874 

0 

a 

10 

5  55  31 

161  Oil 

23 

0  .  a 
810 

s 

10 

5  51  5 

156  46  0 

27 

875 

a 

10 

5  55  49 

158    4  33 

29 

817 

s 

 / 

10 

5  51  23 

156  15  0 

27 

876 

S 

_/ 

7 

5  55  54 

157  33  34 

28 

818 

s 

8 

5  51  3i 

J59  53  23 

28 

877 

S 

10 

5  55  55 

160  41  15 

31 

819 

s 

10 

5  51  32 

160    3  49 

25 

878 

S 

10 

5  56  0 

160  41  45 

3i 

820 

s 

7' 

5  51  32 

158  27  36 

26 

879 

S 

10 

5  56  2 

161  21  11 

23 

52  I 

s 

9 

5  51  32 

158    6  36 

26 

Sao 

a 

10 

5  56  9 

160  39  15 

31 

822 

s 

10' 

5  51  38 

160  14  15 

31 

881 

S 

_/ 

7 

5  56  12 

157    5  4 

28 

823 

10 

41 

13  49 

25 

00, 

882 

a 

8 

5  5°  18 

158    4  4 

f 

s 

10 

5  5i  42 

159  16  23 

30 

7 

'9 

5  33 

29 

JS24 

s 

10 

5  51  47 

159  36  23 

30 

8S3 

a 

0 

8 

5  56  26 

J57  33  34 

28 

825 

s 

10 

5  51  48 

160  45  45 

31 

884 

"NT 
JN 

T  T  T 
111. 

5  56  31 

158  13  22 

f 

10 

53 

45  l9 

25 

00. 
805 

"NT 
JN 

T  T 
IX. 

5  56  37 

160  56  47 

f 

826 

s 

10 

5  51  49 

158    9  6 

26 

886 

s 

8 

5  56  41 

160  33  15 

31 

827 

s 

10 

5  51  53 

156  16  0 

27 

887 

s 

10 

5  56  44 

158  17  3 

29 

828 

s 

10' 

5  51  56 

156  47  0 

27 

888 

s 

of 

8 

5  56  44 

161  59  11 

23 

829 

s 

10 

5  51  59 

*57    5  34 

28 

889 

s 

IO 

5  56  47 

156  40  0 

27 

83O 

s 

10 

5  52  5 

158  43  36 

26 

890 

s 

7' 

5  56  51 

156  20  0 

27 

831 

N 

III. 

5  52  15 

159  31  38 

/ 

891 

s 

8' 

5  56  57 

159  26  23 

3° 

832 

s 

10 

5  52  18 

156  40  0 

27 

— 

8' 

58 

26  23 

30 

833 

s 

10 

5  52  18 

161  33  11 

23 

892 

s 

8' 

5  57  10 

160  58  41 

23 

834 

s 

10' 

5  52  26 

J57    5  44 

28 

— 

10 

1 1 

60  15 

31 

835 

s 

10 

5  52  26 

160  40  15 

31 

893 

N 

II. 

5  57  16 

J59  35  3 

f 

836 

s 

7 

5  52  32 

159  57  15 

31 

894 

s 

9 

5  57  25 

161  41  11 

23 

— 

7' 

36 

55  43 

3° 

895 

N 

II. 

5  57  26 

159    2  8 

f 

— 

7 

10' 

40 

56  19 

/ 

896 

S 

8' 

5  57  39 

157  24  4 

28 

837 

s 

5  52  37 

159  57  20 

3i 

897 

N 

III. 

5  57  46 

156  25  1 

/ 

— 

10' 

42 

55  33 

30 

898 

S 

10 

5  57  49 

157  40  34 

28 

838 

N 

II. 

5  52  43 

*59  23  54 

/ 

899 

S 

9' 

5  57  52 

161  27  11 

23 

839 

N 

II. 

5  52  45 

*57  21  55 

/ 

900 

s 

10 

5  57  53 

161  22  11 

23 

840 

S 

10 

5  52  48 

160  51  15 

31 

901 

N 

II. 

5  57  56 

157  16  18 

f 

841 

s 

8' 

5  52  51 

161  24  11 

23 

902 

s 

10 

5  58  11 

156  20  30 

27 

842 

s 

9 

5  52  58 

J57  36  4 

28 

903 

s 

8' 

5  58  18 

160  20  15 

31 

843 

s 

9 

5  53  6 

158  13  36 

26 

904 

s 

9 

5  58  35 

157  42  4 

28 

844 

s 

10 

5  53  7 

158  22  6 

26 

905 

s 

i 

5  58  4° 

159  29  23 

30 

845 

s 

10 

5  53  11 

J57  59  34 

28 

906 

s 

8' 

5  58  42 

161  31  11 

23 

846 

s 

9 

5  53  r3 

156  25  0 

27 

907 

N 

II. 

5  58  42 

158  28  8 

/ 

S47 

G 

0 

5  53  *5 

160  43  15 

31 

c 

0 

9 

5  58  44 

161  55  41 

23 

848 

s 

i 

5  53  16 

160  32  15 

31 

909 

s 

IO 

5  58  44 

159  18  53 

3° 

849 

s 

10 

5  53  18 

157  17  4 

28 

910 

N 

© 

5  58  49 

159  12  3 

/ 

9' 

21 

J7  34 

28 

N 

5° 

12  23 

30 

85O 

s 

8 

5  53  24 

161  54  41 

23 

N 

II. 

52 

12  33 

3° 

851 

s 

9 

5  53  24 

J59  49  53 

30 

911 

N 

5  58  59 

158  17  52 

/ 

852 

s 

10 

5  53  25 

160  56  15 

31 

912 

N 

II. 

5  59  0 

158  38  9 

/ 

853 

s 

8 

5  53  33 

158  60  26 

26 

913 

S 

IO 

5  59  1 

161  52  11 

23 

8' 

36 

59  53 

3° 

914 

s 

IO 

5  59  *3 

J57    4  4 

28 

8' 

37 

61  3 

29 

9*5 

s 

8 

5  59  3° 

161  26  41 

23 

854 

s 

9 

5  53  44 

158  29  6 

26 

916 

s 

9 

5  59  35 

160  14  15 

3i 

58 

28  3 

29 

917 

s 

IO 

5  59  45 

157    2  4 

28 

855 

s 

5  53  48 

161    1  41 

23 

918 

s 

IO 

5  59  46 

159  35  23 

30 

856 

N 

II. 

5  53  52 

161  12  35 

/ 

919 

N 

5  59  48 

158  31  3 

29 

857 

s 

10' 

5  53  55 

159  44  23 

30 

N 

© 

49 

31  2 

/ 

858 

N 

II. 

5  53  59 

157  27  17 

/ 

164 


NOTES  ON  THE  FOREGOING  CATALOGUE. 


No. 

3  B.  787. 

4  B.  786. 
7    B.  788. 

15    B.  790. 

20  B.  800. 

21  B.  801. 
24  B.  805. 
39    B.  813. 

41  B.  814. 

42  Is  a  duplicate  of  No.  37  numbered  by  mistake. 
51    B.  822.    5'  error  in  N  P  D  in  B. 

53    B.  821.    B  has  5'  error  in  N  P  D.    This  is  no 

doubt  also  identical  with  B  820. 
66    B.  827. 

74    B.  832.     Probably  identical  with  B.  829,  in 

which  i°  error  in  P  D  exists. 
76    Possibly  =  No.  80. 
83    B.  837. 

85  B.  839. 

86  B.  838? 

110    By  measurement  of  drawing. 

in    A  double  star  in  a  cluster. 

135    B.  864. 

142    B.  867. 

153    B.  871. 

159    fi.  875. 

172    B.  880. 

189    B.  886. 

193    B.  889. 

217    B.  895. 

227    B.  897. 

231    B.  898. 

245    The/ obs  has  10"'  R  A. 
250    B.  912. 

262  Double. 

263  B.  920. 
274  B.  922. 
277    B.  926. 

281  The  1st  neb  in  fig.  6,  PI.  III. 

282  The  1st  of  the  southern  cluster  of  nebulie  in  fig. 

6,  PI.  III. 

283  The  principal  neb  in  the  ditto,  ditto. 

288  The  star  s  p  the  central  star  of  fig.  6,  PI.  III. 

289  The  last  nebula  in  the  southern  cluster  of  nebula? 

of  fig.  6,  PI.  III. 

290  The  chief  star  in  the  centre  of  the  figure  6,  PI. 

III. 

295    B.  927  no  doubt ;  but  the  R  A  of  B.  is  20*  too 

little  if  my  obs  be  correct. 
297    The  very  faint  neb  following  a  double  star  in  fig. 

6,  PI.  III. 
305    Double  10  and  10. 11  m. 
308    B.  936. 
313    B.  940. 
318    B.  941. 

323    B.  939.    R  A  in  B.  is  probably  1 "'  too  small. 
328    B.  947. 

331  B.  950.    The  P  D  of  the  Brisb.  Cat.  is  1600, 

which  is  a  misreading.  My  obs  being  in  the 
midst  of  a  zone  is  liable  to  no  such  mistake. 

332  B.  951. 
336  B.  952. 
339    B.  953. 

3159    Double  40",  9'  and  11  m. 

381    Is  possibly  the  neb.    387  seen  as  a  faint  star  in 

the  equatorial. 
384    The  1  st  faint  nucleus  of  the  cluster  of  nebula;, 

figure  2,  PI.  III. 

388  B.  967. 

389  The  2nd  nebula  of  the  cluster  of  neb,  fig.  2,  PI. 

III. 

393    The  3rd  ditto,  ditto. 

398  The  4th  the  following  and  brightest  of  ditto. 

399  The  small  detached  nebula  of  fig.  2,  PL  III. 
408    Possibly  the  nebula  No.  405,  seen  in  the  equato- 
rial as  a  faint  star. 


No. 

414  Possibly  the  neb  No.  421,  seen  as  a  faint  star. 

418  B.  971.    Double  5th  class,  7  and  n  m. 

423  B.  974. 

428  Double. 

432  1st  of  a  group. 

442  2nd  of  ditto. 

444  The  obs  of  zone  20  is  of  the  middle  of  the  stars 

443  +  444,  seen  as  one. 

445  3rd  of  a  group. 

446  1st  of  another  group. 

448  2nd  of  ditto. 

449  3rd  of  ditto. 

450  Nebulous  in  equatorial. 

452  4th  of  a  group. 

453  B.  983. 

458  4th  of  a  group. 

460  5th  ditto. 

463  6th  ditto. 

464  B.  985. 

468  A  double  st  in  cluster. 

473  B.  989. 

478  B.  991. 

491  B.  993,  ?  i'  error  P  D. 

508  B.  1001. 

522  B.  1004. 

529  B.  1008.    Double,  companion  =  1 1  m. 

567  B.  1016. 

592  /'makes  the  degree  159  ;  160  is  right. 

601  B.  1023. 

615  B.  1025. 

618  Possibly  No.  613  taken  a  second  time. 

651  B.  1037. 

655  B.  1038.  The  great  looped  nebulae,  fig.  4,  PI.  II. 

^  ^Two  stars  of  10  m  involved  in  a  nebula  or  very 

rri.    faint  cluster. 
665  } 

670  The  place  of  this  *  is  better  determined  as  No. 
87  in  the  Catal.  accompanying  the  monograph 
of  30  Doradus,  viz.,  5  40  18,  159  18  26. 
It  is  too  small  for  good  obs  in  the  equatorial. 

678    The  preceding  of  the  double  neb,  PI.  Ill,  fig.  4. 

680  The  n  p  of  the  four  principal  nebulae  of  the  group. 

PI.  III.,  fig.  4. 

68 1  The  s  p  of  ditto,  ditto. 

682  The  following  of  the  double  neb  in  ditto. 

685  The  n  f  of  the  four  principal  in  the  group,  fig.  4, 

PI.  III. 

686  The  s  f  of  ditto,  ditto. 

688  The  v  F  neb  preceding  a  star  in  ditto. 

689  The  said  star  in  ditto. 

697    The  neb  following  this  star  in  ditto. 

706  B.  1047. 

709  B.  1050  ?  if  errors  be  presumed  in  B.  of  20*  in 

R  A,  and  10'  in  P  D.  If  not,  B.  1050  does 
not  exist. 

732  Double  9  and  12  m. 

733  B.  1059. 

766  B.  1065.  The  R  A  of  B  is  probably  30-  too 
little.  B.  1070  is  probably  identical  with  this 
star,  and  with  B  1065. 

776  Double. 

801    B.  1091. 

836    Double  in  f. 

841    Double  8',  12  m. 

844    Double,  10  and  11  m. 

621    These  nebula;  and  clusters  have  been  inserted, 

628  and  their  places  deduced  (in  all  probability 

629  with  quite  as  much  correctness  as  if  actually 
664  taken  in  sweeping),  from  a  very  careful  and 
684       deliberate  drawing  of  the  neighbourhood  of 

707  30  Doradus  made  with  the  20  feet,  and  duly 

710  checked  and  corrected  by  the  known  stars  in 
714       it.    No.  664  is  the  nebula  (a  very  remarkable 

one)  alluded  to  in  the  note  above  on  Nos.  663 
and  665. 


CHAPTEK  II. 
OF  THE  DOUBLE  STARS  OF  THE  SOUTHERN  HEMISPHERE. 


I. — INTRODUCTION  TO  THE  CATALOGUE  OF  SOUTHERN  DOUBLE  STARS. 

(141)  The  principal  object  kept  in  view  during  the  progress  of  my  southern  sweeps  was 
the  discovery  of  new  nebulae,  and  the  determination,  with  some  degree  of  precision,  of  the 
places  of  those  already  known.  The  detection  and  measurement  of  double  stars  was  regarded 
as  of  subordinate  interest,  and  allowed  to  interfere  as  little  as  possible  with  the  former  inquiry. 
During  sweeps,  therefore,  wben  nebulas  were  expected,  little  leisure  was  allowed  for  any  minute 
examination  of  stars,  especially  on  new  ground.  But  in  regions  which  had  been  once  or  twice 
well  swept,  or  where  nebulae  were  thinly  scattered,  or  seemed  to  be  altogether  absent,  stars 
down  to  the  6th  or  7th  magnitudes  were  (at  least  during  the  last  two  years  over  which 
the  observations  were  continued)  seldom  finally  dismissed  from  the  field  of  view  till  they  had 
undergone  the  application  of  one  or  more  of  the  diaphragms,  whether  circular  or  triangular 
(almost  universally  the  latter),  with  or  without  increased  magnifying  powers,  according  to  the 
state  of  the  air.  Of  the  defining  and  dividing  power  of  the  telescope  under  such  circumstances, 
abundant  proof  has  been  afforded  in  the  Catalogues  of  double  stars  observed  with  it  in 
England,  especially  in  the  4th,  5th,  and  6th,  after  the  mirrors  had  attained  a  degree  of  perfec- 
tion which,  though  considerable,  yet  fell  short,  in  my  opinion,  of  that  to  which  they  were 
wrought  subsequently. 

(142)  To  have  executed  a  regular  review  of  the  southern  heavens  with  the  twenty-feet 
Reflector,  for  the  purpose  of  detecting  close  double  stars,  would  have  required  at  least  two 
additional  years,  and  probably  more,  since  such  reviews  can  only  be  carried  on  with  effect  in 
those  states  of  the  atmosphere  when  definition  is  perfect.  Now  in  the  hot  season  tbese  oppor- 
tunities are  comparatively  rare.  The  only  mode  of  observation  in  which  such  a  review  is 
practicable  with  an  instrument  of  this  construction,  is  by  carrying  out  tbe  system  of  zone 
observations  on  the  meridian  with  extensive  prepared  working  lists  of  known  stars.  But 
whereas,  with  the  aid  of  an  equatorial  mounting,  it  is  easy  to  follow  the  diurnal  movement  (as 
explained  above,  Art.  136),  so  that  no  object  shall  pass  unexamined ;  without  such  aid  no  one 
star  can  be  minutely  scrutinized  without  the  certainty  of  missing  others,  so  that  every  zone 
must  necessarily  come  to  be  observed  over  and  over  again,  with  this  especial  object  in  view, 

u  u 


166 


OF  THE  DOUBLE  STARS 


before  it  can  be  considered  as  fully  reviewed.  And,  moreover,  the  stars  must  be  taken  as  they 
come  on  the  meridian  within  observing  hours,  at  favourable  or  unfavourable  seasons,  and 
with  all  the  chances  of  partial  cloud  occurring  on  the  meridian  while  other  regions  may  be 
clear. 

(143)  These  considerations  determined  me  not  to  depart  from  the  line  of  observation 
originally  intended,  and  carried  out  in  the  northern  hemisphere.  Double  stars  occurring  were 
of  course  always  taken,  and  a  measured  angle  of  position  as  accurate  as  a  single  rapid,  and  not 
unfrequently  hurried  setting  of  the  wire,  secured.  But  (except  in  the  circumstances  above 
specified)  no  close  examination  was  made,  unless  some  suspicion,  excited  under  the  ordinary 
sweeping  power  (180),  induced  an  application  of  high  magnifying  powers,  and  in  such  cases 
it  would  occasionally  happen  that  a  long  and  pertinacious  scrutiny  took  place.  But  this  was 
always  felt  to  be  a  departure  from  system  and  a  sacrifice,  as  it  necessitated  an  additional  sweep 
over  the  same  zone  to  be  made  on  a  subsequent  occasion,  so  as  to  fill  up  the  vacancy  in  right 
ascension. 

(144)  Bearing  these  circumstances  in  mind,  it  will  not  be  a  matter  of  surprise  that  the 
Catalogue  of  double  stars,  furnished  by  the  twenty-feet  sweeps,  is  comparatively  deficient  in 
those  of  the  first  or  closest  class — meaning  by  this,  stars  of  which  it  can  be  confidently  asserted 
that  the  angular  distance  of  the  individuals  is  under  two  seconds.  But  independent  of  such 
drawbacks,  though  I  have  no  direct  statistical  enumeration  to  bear  out  an  assertion,  I  cannot 
help  putting  on  record  a  strong  impression  that  the  extra-tropical  part  of  the  southern  hemi- 
sphere is  really  poorer  in  very  close  double  stars  than  the  northern,  at  least  in  those  regions  of 
it  which  come  to  be  observed  on  the  meridian  in  the  best  seasons  for  definition.  The  almost 
total  absence  of  objects  of  this  description  from  the  Catalogue,  in  the  last  six  hours  of  right 
ascension,  is  the  more  striking,  as  these  are  precisely  the  best  hours  for  definition,  coming  to  be 
observed  from  June  to  October,  when  the  atmosphere  is  in  the  most  favourable  condition.  The 
examination  of  at  all  events  a  very  large  number  of  stars  down  to  the  8th  magnitude  inclusive, 
under  circumstances  of  the  best  possible  definition,  when  the  discs  have  been  reduced  to  mere 
points,  enables  me  to  speak  with  some  degree  of  confidence  to  this  feature  of  southern  astro- 
nomy. It  is  hardly  possible  that,  when  so  defined,  an  angular  interval  from  centre  to  centre  of 
moderately  unequal  stars,  exceeding  three-fourths  of  a  second,  or  at  all  events  amounting  to  a 
whole  second,  could  have  escaped  notice.  Yet  it  is  on  such  occasions  that  I  find  entered  in  the 
sweeping  book  such  remarks  as  the  following: — "  July  23,  1835.  The  extreme  paucity  or 
rather  utter  absence  of  close  double  stars  in"  [this  and]  "  the  late  sweeps  in  such  wonderful 
nights  and  with  such  perfect  action  of  the  instrument  is  really  surprising."  "  July  24.  I 
begin  to  think  I  shall  never  see  another  close  double  star.  It  is  wonderful  how  entirely  devoid 
of  these  objects  are  all  the  late  sweeps,  and  that  in  the  finest  picked  opportunities  for  detecting 
them.    It  is  a  remarkable  feature.    Eo  ipso  notantur  quod  non  videntur." 

(145)  On  the  other  hand,  the  subjoined  Catalogue,  which  contains  the  places  reduced  to 
1830,  and  descriptions  sufficient  for  identification,  of  all  the  double  stars  occurring  in  the 
sweeps,  will  be  found  to  comprise  a  good  number  of  such  objects  taken  with  little  selection, 
and  many,  doubtless,  which  may  be  thought  hardly  worth  entering  in  a  formal  catalogue. 
Yet  almost  all  those  objects  offered  something  of  interest  at  the  time  to  recommend  them  to 
notice,  although  I  will  not  deny  that  here  and  there,  in  barren  and  monotonous  regions,  an 


OF  THE  SOUTHERN  HEMISPHERE. 


167 


occasional  entry  may  have  been  made  for  the  homely  but  useful  purpose  of  avoiding  sleep 
(a  thing  not  unattended  with  the  probability  of  broken  bones).  I  have  stated  elsewhere  (Mem. 
Art.  Soc.  ii.  472)  my  general  reasons  for  not  neglecting  double  stars  of  very  small  magnitudes, 
or  minute  companions  of  large  stars  constituting  them  double  stars  of  the  5th  and  6th  classes, 
in  Catalogues  of  this  nature :  reasons  materially  strengthened  by  the  success  which  has  recently 
attended  the  research  of  parallax  by  the  aid  of  small  and  distant  companions  of  conspicuous 
stars  ;  and  which  render  it  desirable  at  least  to  place  on  record  the  companions,  within  pretty 
extensive  limits  of  distance,  of  all  the  larger  stars.  Admitting  the  validity  of  these  reasons, 
the  Catalogue  would  not  have  been  very  materially  curtailed  by  omitting  the  less  important 
stars  to  which  they  do  not  apply ;  so  that  on  the  whole  it  has  been  considered  advisable  not  to 
depart  from  the  principle  all  along  followed  on  previous  occasions,  of  drawing  no  line — making 
no  selection,  unless  the  rejection  of  a  very  few  stars  of  which  companions,  it  is  true,  have  been 
noticed,  but  which  it  would  have  been  palpably  absurd  to  designate  as  double  and  include  as 
such  in  a  formal  Catalogue,  be  considered  in  that  light. 

(146)  The  arrangement  of  the  following  Catalogue  is  in  almost  every  particular  similar  to 
that  of  the  Catalogues  of  double  stars  which  I  have  from  time  to  time  previously  communicated 
to  the  Astronomical  Society,  especially  to  the  5th  and  6th  of  those  Catalogues  printed  in  vols. 
6  and  9  of  their  Memoirs.  It  consists  of  nine  columns,  of  which  the  first  contains  a  general 
number  for  present  and  future  reference,  attached  to  each  of  such  stars  as  I  have  not  found  marked 
as  double  in  any  previous  Catalogue  or  list  which  I  have  been  able  to  consult.  These  numbers 
(pursuant  to  previous  usage)  are  continued  on  from  No.  3346,  the  last  number  of  my  sixth 
northern  Catalogue,  in  regular  progression  to  No.  5542.  Among  the  stars  so  numbered  there 
are  a  few  respecting  whose  double  nature  (owing  to  their  extreme  closeness)  some  doubt  has 
been  expressed.  If  verified,  as  I  dare  say  several  of  them  at  least  will  be,  by  future  observers, 
the  record  here  set  down  will  be  of  interest,  and  will  need  a  reference.  The  unnumbered  stars 
occur  for  the  most  part  in  Struve's  Catalogue,  some  are  noticed  as  double  in  the  Brisbane  Cata- 
logue, and  a  considerable  number  are  identifiable  with  objects  described  in  Mr.  Dunlop's  Cata- 
logue of  253  double  stars,  published  in  the  3rd  volume  of  the  Memoirs  of  the  Astronomical 
Society,  p.  257,  et  seq.  When,  however,  in  comparing  my  observations  with  this  last-mentioned 
Catalogue,  I  have  found  a  star  to  be  double  in  a  different  sense  from  that  which  caused  it  to  be 
registered  as  double  therein, — or  when,  with  agreeing  places,  I  have  met  with  such  discordances 
in  the  descriptions  or  measures,  that  it  is  impossible  to  suppose  the  same  star  to  be  intended  by 
both  observers, — a  number  has  been  affixed.*  Mr.  Rurnker  has  also  given  a  small  list  of 
double  stars  at  the  beginning  of  his  Preliminary  Catalogue  of  Southern  Stars.    This  list  has 

*  A  great  many  mistakes  appear  to  have  been  committed  in  the  Catalogue  alluded  to  either  in  the  places, 
descriptions,  or  measures  of  the  objects  set  down  in  it.  In  the  Catalogue  here  presented,  and  in  my 
micrometrical  measures  with  the  equatorial  subjoined,  are  recorded  my  own  observations  of  such  objects  in  it 
as  I  have  been  able  to  find,  and  which,  when  found,  it  was  deemed  desirable  to  measure,  though  in  several  cases 
with  considerable  doubt  as  to  their  identity.  Where,  owing  to  great  discordances  in  places,  descriptions,  or 
measures,  the  identity  of  the  object  is  brought  into  question,  a  note  of  interrogation  is  affixed  to  the  letter  s. 

After  finally  numbering  the  Catalogue,  and  too  late  for  making  a  general  change,  the  star  No.  4S83  was 
identified  with  A  207. 


168 


OF  THE  DOUBLE  STARS 


also  been  collated,  and  all  the  objects  contained  in  it,  with  the  exception  of  Nos.  8,  22,  23,  24, 
25,  28,  are  found  to  have  been  observed  either  in  sweeping  or  with  the  equatorial,  and  are 
therefore  not  numbered. 

(147)  As  reference  to  a  single  copious  list  of  objects  is  always  preferable  in  point  of  con- 
venience to  consulting  several  smaller  lists,  it  has  been  considered  advisable  to  include  in  this 
Catalogue  all  such  double  stars  (not  previously  noted  by  other  observers)  which  have  been 
encountered  in  the  course  of  an  examination,  with  the  equatorial,  of  the  Brisbane  stars,  as  well 
as  those  which  have  occurred  in  the  partial  and  imperfect  execution  of  a  series  of  zone  reviews 
with  that  instrument,  which  when  commenced  I  found  it  impracticable  to  carry  out,  and  which, 
having  been  begun  in  a  barren  part  of  the  heavens,  proved  very  unproductive.  Thus  this 
Catalogue  serves  at  once  as  an  index  to  the  20-feet  double  stars,  and  to  those  of  the  equatorial 
measurements,  at  least  such  as  may  be  considered  new.  Two  stars,  Nos.  5443  and  5444,  so 
detected,  which  had  been  overlooked  previous  to  numbering  the  Catalogue,  are  annexed  at 
the  end. 

(148)  The  reduced  Right  Ascensions  and  N  P  Ds  of  the  several  stars  are  given  in 
columns  2  and  3,  for  1 830.  The  arrangement  of  these  columns  is  precisely  similar  to  that  of 
the  corresponding  column  in  the  Catalogue  of  Nebulae,  and  requires  no  further  explanation. 

(149)  The  4th  column  contains  the  angle  of  position,  reduced  for  zero,  or  the  mean  of  the 
angles  so  reduced,  given  by  each  observation.  They  are  by  no  means  to  be  regarded  as  of 
equal  authority  with  the  results  of  an  equal  number  of  measures  taken  with  the  equatorial,  for 
a  variety  of  reasons.  1st.  They  are,  for  the  most  part,  much  less  deliberately  taken.  2nd. 
When  taken  with  care,  and  when  time  has  been  allowed  for  a  repetition  of  measures,  a  peculiar 
bias  of  judgment  seems  in  some  cases  to  have  influenced  them,  which  makes  it  necessary  to  be 
cautious  in  combining  them  with  the  equatorial  measures  of  the  same  stars.  This  is,  no  doubt, 
partly  owing  to  the  different  position  of  the  person  and  head  of  the  observer  at  the  two  instru- 
ments— in  the  one  case  looking  down,  in  the  other  up.  To  this  we  must  add  the  difference  of 
inversions  due  to  the  optical  construction  of  the  two  instruments,  the  achromatic  operating  a 
complete,  and  the  reflector  only  a  semi-inversion.  Owing  to  this  cause  the  situation  of  the  line 
of  junction  of  two  stars  observed  on  the  meridian  will  stand  in  a  different  relation  to  the 
optical  bias  of  the  eye  habitually  used  for  observing,  and  thus  angles  obtained  with  the  two 
instruments  will  cease  to  be  comparable.  As  a  general  principle,  indeed,  it  may  be  borne  in 
mind,  that  no  measured  angle  of  position  of  a  double  star,  no  matter  with  what  instrument 
taken,  can  be  considered  free  from  bias,  unless  their  line  of  junction  lie  in  the  principal  section 
of  the  eye,  and  unless  the  diurnal  motion  be  eliminated  either  by  a  clock-work,  or  by  a  per- 
fectly equable  movement  given  by  hand,  a  condition  tolerably  well  satisfied  in  my  observations 
with  the  equatorial,  by  long  practice  in  the  use  of  the  right  ascension  handle,  but  which  the 
construction  of  the  reflector  rendered  almost  impossible  to  fulfil  with  any  degree  of  exactness. 

(150)  In  all  the  sweeps  subsequent  to  Sw.  773,  two  thick  wires  were  substituted  for  the 
single  position  wire,  distant  enough  from  each  other  to  include  the  globe  of  Saturn.  This, 
which  may  certainly  be  considered  as  a  capital  improvement  in  the  art  of  measuring  positions, 
was  imitated  from  the  equatorial,  where  it  had  been  found  very  effective,  and  would  have  been 
introduced  earlier  in  the  20  feet,  but  for  the  obstruction  caused  in  the  field  of  view,  which  it  was 


OF  THE  SOUTHERN  HEMISPHERE. 


169 


apprehended  might  interfere  with  the  observation  of  small  and  faint  nebulse.  In  making  the 
substitution  of  these  for  the  single  wire,  the  zero  of  position  ( —  0°.7)  was  preserved  unaltered, 
a?id  has  been  applied  to  all  the  measures  so  taken  as  they  here  stand  printed. 

(151)  The  5th  column  contains  the  estimated  distances.  I  consider  them  generally  some- 
what too  small  in  the  closer  stars ;  they  are  also  affected  by  the  apparent  size,  neatness  of  defi- 
nition, &c,  of  the  stars,  and  are,  of  course,  in  a  very  high  degree  vague  and  precarious,  serving 
for  little  more  than  general  classification. 

(152)  The  magnitudes  follow  in  the  6th  column.  Accents  are  used  to  denote  half  magni- 
tudes— as  8f  for  8.9  m.  On  the  subject  of  these  magnitudes,  as  compared  with  those  of  M. 
Struve,  the  same  remark  applies  as  in  my  Third  Catalogue,  Mem.  Art.  Soc.  III.  p.  180.  My 
scale  of  magnitudes  is,  generally  speaking,  a  full  unit  below  that  of  M.  Struve ;  for  instance, 
the  star  which,  using  the  20-feet  reflector,  I  call  10  m,  that  excellent  astronomer,  using  the 
Dorpat  refractor,  would  call  9  m.  In  the  higher  parts  of  the  scale  of  magnitudes  the  difference 
is  greater — in  the  lower  somewhat  less. 

(153)  In  the  column  of  remarks,  col.  7,  notes  made  at  the  moment  of  observation  are 
recorded ;  the  colours  of  coloured  stars  mentioned ;  individual  angles  of  position  recorded 
where  a  mean  has  been  taken  of  several  in  col.  4  ;  and  some  subsequent  statements  (indicated 
by  brackets  thus  [  ] )  introduced.  This  column  also  contains  differences  of  R  A,  and  the 
distances  resulting  from  observations  by  the  method  of  oblique  transits. 

(154)  The  8th  column  contains  references  to  other  Catalogues,  with  which  the  stars  in  this 
may  have  been  identified  either  as  single  or  double  stars.  The  following  nomenclature  is 
adopted : — 

Roman  numerals,  followed  by  Arabic,  thus  (II.  47),  denote  Sir  Wm.  Herschel's  classes 
and  numbers. 

H.  followed  by  an  Arabic  numeral  thus  (H.  45),  denotes  the  star  so  numbered  in  his 
Supplementary  Catalogue  of  145  new  double  stars. 

A.  denotes  the  Astronomical  Society's  Catalogue  for  1830. 

B.  The  Brisbane  Catalogue,  to  which,  as  having  been  my  own  working  Catalogue, 
references  are  most  frequent. 

L.  Lacaille's  Ccelum  Australe  Stelliferum,  as  reduced  and  published  by  the  British 
Association. 

A.  Lalande's  Histoire  Celeste,  similarly  reduced  and  published. 

M.  The  Madras  Catalogue,  containing  the  results  of  Mr.  Taylor's  observations  at  the 
H.  E.  India  Company's  observatory  at  that  station.  In  referring  to  this  Catalogue, 
the  numbers  of  all  stars,  occurring  between  R  A.  llh  5m  0s  and  16h  28m  19s,  are 
corrected  by  subtracting  900  from  the  reference  number  in  its  margin,  as  rendered 
necessary  by  the  erratum  unfortunately  subsisting  in  the  numbers  throughout  that 
interval. 

A.  denotes  Mr.  Dunlop's  Catalogue  of  253  southern  double  stars,  Mem.  Art.  Soc.  III. 
p.  267. 

R.  Mr.  Riimker's  list  of  28  double  stars  in  his  "  Preliminary  Catalogue." 

x  x 


170 


OF  THE  DOUBLE  STARS  OF  THE  SOUTHERN  HEMISPHERE. 


<t.  The  first  Catalogue  of  double  stars  by  M.  Struve,  published  in  the  third  volume  of  the 
Dorpat  observations,  containing  795  double  stars,  a  very  useful  and  valuable  Cata- 
logue of  reference  for  southern  double  stars  visible  in  European  latitudes. 

2.  The  second,  or  great  Dorpat  Catalogue  of  Double  Stars. 

h.  My  own  former  Catalogues  of  double  stars ;  which,  being  numbered  consecutively, 
need  no  especial  distinction.  In  the  very  few  instances  where  other  references  are 
needed,  the  nomenclature  of  my  former  Catalogues  is  adhered  to. 

Occasionally,  when  there  has  been  room  in  the  column  of  remarks,  and  not  in  column  8, 
for  the  identification  of  a  star  in  two  or  more  catalogues,  some  of  the  references  are  transferred 
to  the  former  column,  which  also  contains  the  star's  name  and  letter,  if  any. 

(155)  Column  9  contains  the  number  of  the  sweep  in  which  the  observation  recorded  was 
made.  The  corresponding  dates  will  be  found  in  the  synoptic  table  appended  to  the  Catalogue 
of  Nebula  (p.  129.) 


171 


Reduced  Observations  of  Double  Stars  made  with  the  20-feet  Reflector  at  Feldhausen,  at  the  Cape 
of  Good  Hope,  in  the  years  1834,  1835,  1836,  1837,  and  1838. 


No. 


3347 

3348 
3349 
335° 


335i 
33S2 

3353 
3354 
3355 
3356 
3357 
3358 
3359 
3360 
3361 
3362 

3363 
3364 

3365 
3366 

3367 
3368 
3369 
3370 
3371 
3372 
3373 


3374 
3375 


3376 

3377 
3378 

3379 


R  A.  1880.0. 
h.    m.  s.  d. 


0  32.8 
33.I 

1  34.0 

1  47-7 

2  10.5 


N  P  D.  1830.0. 


2  I7.7 
2  57.4 

5  •- 
5  51-3 
o  6  13+ 
o  6  13.9 
o  6  34.2 
0  7  53-3 
0  7  53-5 
o  12  12.2 
o  13  13. 1 
o  13  25.9 
o  14  13.6 
o  16  10.0 
o  16  27.1 

28.2 

o  17  23.8 

o  19  4.9 

o  19  7.9 

o  19  46.9 

O  20  I7.5 

o  20  24.2 

O  21  48.4 
o  23  19.0  : 
O  23  21.2 

o  23  42.3 
44-5 

O  25  22.2 

o  25  22.3 


23.3 
25.2 

o  25  29.2 

30.7 

o  25  34.1 
o  25  37.3 

39.8 

o  28  13. 1 


141    6  42 
6  44 

150  18  20 
158  16  3 
148  24  48 

22  + 

113  36  16 

140  35  o 

108  6  .. 

165  37  35 
126  59  . . 
128  33  o 
130  9  5 
158  50  52 
152  23  7 
113  32  16 

143  27  47 

158  39  55 

109  58  2 
163    2  o 

144  55  7 
55  57 

141  46  42 
158  40  17 
122  55  22 

108  8  6 

155  44  5 

156  51  35 
147  38  21 

151  58  50  : 

109  53  45 
J53  54  ° 

53  48 

166  11  27 
125  54  30 


54  47 

55  5 
146  16  7 

16  16 

117  1  49 
152    5  15 

5  23 

118  21  14 


Position. 


85.0 
75.2 
284.3 

II5-4 
173.0 

J74-3 

*35± 
308.2 

345-8 
286.1 

31. 1 
320.6 

3°4-3 
12.6 

110+ 
10.7 

1 14.6 
73-3 

193.3 
194.9 
174.9 

35-4 
i69± 
251.4 

344-7 
54.1 

334-8 
96.5 
119.4 
170.0 
171.0 
113.3 
167.4 


170.0 
170.8 
249.1 
245.3 

53-5 
352.3 

353-6 
229.1 


3 

67.6 


Magnitude 


15=15 
9  !3 
9'  9' 

10  10 
9  10 

11=11 
7  11 


1 1 


1 1 


8  IO 

7'  14 

10'  1 1 

8  11 

9  11 
9  9' 

10  10' 

9  10 

7'  8 
5'=  5' 
5'=  5' 

9'  11 

6'  8 


6'  10 

8  12 

8  10 

8  15 
7  15 

9  12 


The  middle  of  three  in  a  line  

Much  heyond  merid.  The  middle  of  3  in  an  oblique 
broken  line 

The  north  preceding  of  two   

Mean  Epoch,  1836 .  677   

3rd  Class.    Zone  review  

Ill  denned   

The  nucleus  of  a  great  nebula   

15"  dist  ?    MS.  indistinct  

Fine  double  sjc ,  but  ill  denned  

In  the  great  cluster  47  Toucani   

Neat  double  star  

A  R  A  =  5'.25   

Place  not  well  observed  

A  R  A  =  4'-5  

Pos  mean  of  170.4,  169.7  ;  (i  Toucani  

Pos  mean  of  170.1,  171. 9,  171.0;  a  superb  object  . . 

A  R  A  =  8s.o  

Pos  mean  of  166.4,  168.5.  The  minute  given  by  this 
obs  is  26,  but  this  must  be  a  mistake,  as  also  the 
estimated  dist  15",  which  no  doubt  should  be  5"  as 
here  set  down. 

Pos  170.7,  169.3;  very  fine   

Pos  168.7,  171-8,  171-9  ;  fine   

Pos  by  two  coincident  measures   

Neat  star ;  pos  by  two  measures  agreeing   

Pos  mean  of  353.3,  351-3  ;  very  delicate  


Synon. 


h. 1944 


A.  1 

B.  58,9 


B.  63 


B.  64 


Sweep. 


730 
498 
734 
731 
502 
735 

641 
496 
E 

622 
E 

486 
737 
73i 
501 
641 
730 
73i 
74i 
482 
732 
500 
730 

73i 
620 

74i 
630 
508 
504 
501 

74i 
630 
63, 
622 
636 


484 
486 
732 
500 
643 
734 
736 
643 


172 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1830.0. 
h.  in.  s.  d. 


NPD.  1830.0. 

Position. 

Dist. 

Magnitude. 

o  / 

ji 

I07  39 

30 

962 

30 

7' 

13 

13+  55  43 

38.6 

6 

10 

11 

*53  45 

24 

223.0 

20 

9 

12 

144  18 

22 

4 

10 

11 

123  42 

4 

204.7 

3 

9' 

10 

132  8 

57 

242^ 

4 

9 

10 

7 

57 

240_ 

143  1 

42 

*  103.4 

10 

IO 

10' 

i  231.5 

20 

IO 

13 

147  25 

43  : 

252.1 

'5 

5' 

12 

145  2 

37 

237.6 

*5 

9 

9 

2 

46 

234.9 

r5 

9= 

9 

109  28 

9 

74-7 

28 

9 

9' 

136  6 

49 

3r3-5 

15 

7' 

11 

148  24 

1 

209.5 

20 

5 

H 

23 

43 

2 12. 1 

25 

4' 

J3 

23 

48 

209.7 

20 

5- 

J3 

169  25  50 

83.6 

8 

1 1= 

:II 

165  34  50 

301.9 

2 

1 1' 

12 

no  54 

13 

86.3 

18 

10 

10' 

132  49  58 

0 1 .0 

5° 

9 

61.7 

10 

9 

9 

124  12 

34 

216.8 

2 

, 

9 

12 

!3 

21 

217.3 

2 

9 

145  I 

52 

2 

6 

160.0 

10 

7' 

15 

I42  56 

7 

121.3 

30 

8' 

9 

56 

7 

124.3 

28 

9 

10 

I30  3 

31 

282.4 

12 

9 

10 

156  I 

42 

140.9 

4 

10 

1 1 

I 

39 

14.1.4. 

3 

10 

10' 

125  25 

18 

IO3.4 

5 

9 

10' 

144  2 

53.8 

15 

9' 

12 

IO5  46 

0 
0 

IO 

I38  13 

28 

335-9 

5 

9 

1 1 

>3 

44 

333-7 

8 

10 

1 1 

150  15 

25 

240.1 

8 

9 

1 1 

15 

40 

242.3 

12 

9' 

1 1 

156  16 

33 

338.1 

15 

10 

10' 

16 

l9 

332.9 

12 

IO 

1 1 

156  16 

13 

220.0 

25 

9 

14 

15 

54 

223.6 

18 

8' 

13 

115  58  14 

126.2 

i5 

10= 

=  10 

160  25 

32 

76.8 

*5 

8' 

9 

26 

18 

76.0 

20 

8' 

9 

156  23  24 

212.3 

20 

9 

IO 

106  34 

32.3 

6.7 

7' 

7' 

Remarks. 


Synon. 


3380 
3381 
3382 
3383 
3384 
3385 

3386 

3387 
3388 

3389 
3390 
3391 


3392 

3393 
3394 
3395 


3396 
3397 

3398 

3399 
3400 

3401 
3402 

3403 

3404 

34°  5 
3406 

3407 
3408 


o  31  5.4 

o  31  14.0 

o  31  34.6 

o  32  17.2 

o  32  29.6 

o  32  39.3 
41.0 

o  32  50.5 

o  33  57.1 
o  34  49.1 
49.6 
o  35  7.0 

°  35  l3* 
o  35  41.6 
41.9 

o  36  4.1 

o  36  43.0 

o  36  58.5 

o  37  38.0 


40.0 

o  37  53.0 

55-5 
o  38  55.9 

56.6 

o  39  O.I 
3-4 

o  41  0.2 

O  41  22.6 
25.I 

o  42  8.6 
0  42  30+ 
o  43  30- 
o  44  24.9 

25.0 
o  44  32.3 

33.2 
o  44  40.2 

41. 1 
o  45  0.6 
1.9 

o  45  44.0 
o  45  44.8 

5i-i 
o  47  51.2 

o  50 


The  2nd  of  four  stars  

Blotty  

Pos  estimated  from  diagram  

ic}TriPle  

Pos  mean  of  254.6,  249.5,  252.3   

Pos  mean  of  234.6,  235.3  !  nea*  star  

Large  star  orange,  small  blue   

Pos  mean  of  207.8,  211.3  i  fine  

Pos  mean  of  211. 8,  212.3,  212. 1 
Very  fine  double  star  (ij  Phoenicis) 

Measured  with  power  320  

Pos  65.1,  61.6.  The  latter  preferred,  being  taken 
with  power  1200  and  triangular  aperture.  De- 
finition very  perfect.  This  is  a  very  remarkable 
star.  The  colours  of  both  individuals  are  alike, 
viz.,  a  very  high  orange,  almost  red. 

Pos  61.5,  61.9.  Both  stars  of  a  high  rose-red  colour, 
very  curious. 

Pos  216.8,  216.9  ;  very  neat  

Pos  214.2,  220.3,  214.7,  220.1  ;  difficult  

Small  star  barely  seen  by  glimpses.  Definition  im- 
perfect. 

Pos  155.7,  165.8  ;  excessively  difficult,  though  quite 
sure  as  to  the  existence  of  the  small  star.  Verified 
with  power  320  and  full  aperture. 

Very  neat   

A  neat  double  star  

Pos  140.3,  142.5  

A  very  neat  object  

Class  2.    Zone  review   

The  second  star  of  5   

The  second  of  a  group  of  5   

The  preceding  of  two  double  st  

The  following  of  two  double  st  

X  Toucani  A  R  A  =  4s-5  ;  Pos  78.8,  76.3,  77.2  

A  R  A  =  4^.50   

Mean  Epoch  1836.449   


B.  87 


L.  187 
B.  92 


L.  201 ? 


L.  213 


h. 2000 


B.  116 
A.  2 

o\  17 


DOUBLE  STARS. 


173 


No. 

R  A.  1830.0. 
h.   m.  s.  d. 

N  P  D.  1830.0. 
0       /  // 

Position. 

Dist- 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

34.09 

0 

50  4.6 

i/in  18  c8 

1 1.6 

16 

10 

j  1 

735 

'T7 

3410 

O 

52  29.4 

122 

7 

32 

74-4 

20 

9'= 

=9' 

495 

3411 

0 

S3  51-6 

120 

54 

34 

2.1 

15 

9' 

12 

620 

3412 

0 

53  56-4 

H7 

4  4i  \ 

148.6 

25 

8' 

11 

732 

3x5-4 

18 

5 

3413 

0 

54  I2-7 

I  11 
1  if 

33 

231.5 

3 

IO 

IO 

490 

34J4 

0 

54  J4-8 

141 

10 

25 

1  I.  I 
31.1 

18 

9 

IO 

0 

56  7-5 

1 1 1 
1  3  L 

33 

54 

I  C7.  C 

1 

7 

8 

Pos  mean  of  157-3,  157-8.  Quite  as  close  as  4 
Aquarii.  Perfectly  divided  with  a  power  of  480, 
and  the  2nd  of  the  above  measures  taken  with  that 

T"i C\ tat p  •    fnp  t  it  an  Tr\  nn         A  ttioI  Ant-  ction    1  f\ri  rtnlTT- 

uuwci  ,  1 111   isi  w ilii  i&KJr     j? x  viuiciiu  susinciuii  uiiiy 

of  being  double  with  180. 

L.  294 

488 

•• 

159-7 

Viewed  part  mend  ;  180  and  12  inches  aperture  barely 
elongated  it;  1200  and  12  inches  divides  it  cleanly 
by  a  full  diameter  of  the  small  star.  Pos  taken 
with  this  power.  Distance  cannot  exceed  3  or  f" 
at  farthest. 

489 



3 

0 

56  19.5 

ICO 

60 

33 

108.7 

6 

O 
5 

0 
a 

L. 

297 

736 

21.5 

59 

306.1 

3 

a  = 

=  a 

Pos  305.4,  306.7,  306.3.  Measured  with  power  320 
and  triangular  aperture,  which  shows  it  beautifully. 
A  third  Hs  10  m,  90"  almost  exactly  at  right  angles 

t n  t hp  el  1  rppti rtv\  of  flip  0 fVipr  f  wo 
IAJ  lilt    (XI 1  CL-tlUIl  UL  LUC  U  L  lit  1  IWUi 

501 

23.0 

60 

15 

308.6 

5 

7'= 

=  7' 

734 

34x7 

0 

58  30.2 

137 

37 

37 

17.6 

3° 

3' 

1 1 

B. 

'45 

497 

3418 

0 

58  43.1 

148 

48 

46 

253.6 

9' 

1 1 

735 

A.C  C 

TJ  J 

59  5-6 

48 

28 
V- 

252.0 
325± 

% 

11= 

IO 

502 
643 

34x9 

0 

116 

55 

8 

:il 

1 

1  2.8 

146 

9 

16 

21Q.1 

1 
j 

5 

Eye-piece  deranged  [which  may  be  the  cause  of  the 

flispfirflant'  R  \~\ 

L. 

318 

712 

14.3 

8 

44 

240.7 

4 

i 

9 

B. 

156 

500 

15.0 

9 

6 

237.4 

4 

5 

9 

R.  2 

504 

i3± 

11 

+ 

239.0 

5 

4' 

9 

Prw     "?  n  Ci   f  a  a  X*"  ( rpippf  pii  i  ■   T?  on  crn  11  la  pp 

3420 

1 

5  4»-9 

172 

33 

8 

54-5 

18 

9 

1 1 

633 

1 

5  5°-4 

98 

49 

42 

330.7 

00 

7 

9 

(37  Cett)  

IT 

34 

740 

"Zd.2.  I 

6  28.8 

141 

33 

47 

214.  < 

30 

8' 

8' 

498 

3422 

I 

8  2.0 

146 

3* 

25 

58.4 

12 

8' 

12 

732 

34*3 

1 

9  59-4 

159  46  51 

12.0 

2 

6' 

9 

k  Toueani.  Very  beautiful ;  excellent  and  careful 
measures  with  power  32°  and  triangular  aperture. 

B. 

178 

5O9 

II. 3 

z\ 

O 

9 

Very  fine  double  sfc  but  ill  defined  ;  no  place  taken  . 

L. 

356 

3424 

1 

11  1.8 

99 

40 

5 

86.3 

12 

IO 

10 

740 

3425 

I 

1 1  2.2 

118 

23 

0 

256+ 

2 

11  = 

-ii 

643 

3426 

1 

11  8.9 

157 

17 

31 

34!-7 

2 

7' 

1 1 

Very  neat  s|c  and  well  measured  with  power  320  and 
triangular  aperture. 

B. 
L. 

180 
361 

50s 

3427 

1 

12  48.6 

141 

0 

41 

128.0 

15 

9 

9' 

498 

3428 

1 

13  1.8 

139 

33 

57 

155.2 

20 

8 

IO 

497 

3429 

1 

13  18.9 

114  56  35 

i5± 

5 

7 

9' 

733 

3430 

1 

13  41.6 

148 

14 

24 

246.3:: 

ii 

6' 

1 1 

The  following  of  2  nearly  =  ;  measure  rough,  as  the 
night  will  not  admit  magnifying  ;  stars  well  sepa- 
rated. 

L. 

369 

735 

43.8 

15 

18 

251.7 

13 

7' 

IO 

The  f  of  2  ;  seen  double  with  180,  but  verified  and 
measured  with  320. 

502 

343i 

1 

14  31.7 

95 

30 

20 

91.8 

12 

9' 

12 

739 

3432 

1 

14  51.8 

121 

30 

43 

217.9 

4 

9' 

IO 

494 

3433 

I 

15  17.6 

100 

48 

38 

307.0 

12 

IO 

I  I 

740 

3434 

1 

16  56.8 

149 

*5 

5i 

106.8 

2 

12 

12' 

5°4 

Y  Y 


174 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1830.0. 
h.  m.   s.  d. 


3435 


3436 

3437 
3438 
3439 
344° 
3441 

344* 
3443 
3444 
3445 

3446 

3447 
3448 
3449 
345° 

345 1 

34-52- 

3453 


3454 
3455 
3456 
3457 

3458 
3459 
3460 

3461 

3462 
3463 


1  18  52.5 

53-o 
53-3 
1  19  10.6 
12.5 

1  20 

1  20  21.2 
1  20  37.8 
1  21  4.2 
1  21  21.8 

1  24  16.0 
1  24  35.2 
1  24  51.6 
1  25  21.2 

24.3 
1  27  47.2 

52.6: 
1  28  10.6 
1  28  34.1 
1  29  2.2 
1  30  14.9 
1  31  0.5 
1  31  35.2 

35-5 
1  32  8.6 
1  32  1 1.9 

1  32  43-3 
1  33  19.6 

20.3 
21.6 
24.6 

33  3»-7 

34  43-8 

35  •• 

35  10.0 

36  5-5 
7-1 

36  51.6 

37  3-7 
37  3i-3 
37  37-9 

37  4°-5 

38  25.6 
38  44.7 

45-9 
46.6 


N  P  D.  1830.0. 


150  20  55 

23  IO 
22  8 
121     6  54 

6  13 
108  9  .. 
140  20  58 
i35  29  54 

114  7  5° 
126  28  40 

116  18  35 
170  46  28 
144  15  3 
I**  7  3 
8  12 
150  11  55 
10  33 
120  46  50 
128  10  20 
144    4  8 

133  2  18 
93  22  51 

«36    5  55 

5  52 
128  19  46 
144  18  17 
169  22  5 
H7    3  3 

3  16 

3  32 

4  » 

115  18  54 

,67  53  45 
108  30  . . 
112  28  34 
l64  33  57 
34  53 
127  33  36 
no  54  44 
140  57  36 
93  H  39 
i'5  54  17 

137  40  12 

134  48  31 
48  42 

48  53 


Position. 


355-6 

355-9 
358.5 
126.3 
121. 1 
245.2 

33-9 
212.3 

*97± 
224.7 

208.3 
278.9 
2.6 
263.4 
266.3 
310.7 
308.3 

74± 
56.2 

153-3 

212-f- 

J3I-3 
161. 1 
159.9 
277.0 
103.7 
285.4 
300.8 

300.1 
299.5 
299.5 

IOI.I 

281.7 

344-4 
250+ 
240.8 

3I5-7 
270.0 
161. 7 
268.3 
72.5 

3i-3 
18.8 
20.6 
19.3 


Dist. 


Magnitude 


25 

l'  IO 

25 

8  11 

35 

8  10 

12 

7  IO 

10 

7'  9 

13.4 

•    7  9' 

5 

10=10 

5 

IO     1 1 

4 

10=10 

4 

15  16 

30 

6'  10 

40 

9  IO 

40 

8  12 

25 

9  9' 

20 

8  12 

25 

9  12 

3 

6'  8 

20 

8'=  8' 

18 

7'  14 

12 

9  12' 

3 

9'  11 

12 

10=10 

15 

io'=io' 

7  9 

8 

8  9 

35 

5'  14 

2 

7=  7 

*i 

7    7  + 

4 

6'  6' 

4* 

6    6  + 

4 

11  n' 

8 

IO  12 

8'  8' 

I  c 

J 

8  10 

15 

9  11 

18 

9  13 

5 

10'   1 1 

18 

9'  IO 

15 

8  13 

5 

11  =  11 

3 

6  10 

12 

1 1 = 1 1 

30 

9  9 

20 

9=  9 

20 

9'  9' 

Remarks. 


Synon. 


Pos  355  7,  355.6  ;  the  degree  by  this  obs  is  151,  but 
this  is  presumed  to  be  an  error 

[This place  agrees  best  with  Lac]   

Pos  358.7,  358.3  

Fine  star  ;  large  pale  yell ;  small  pale  blue  

Pos  123.2,  1 19.0;  L  yell ;  S  blue   

Mean  Epoch  1836.348   

Blotty  

Involved  in  very  faint  nebula,  an  extremely  delicate 
and  difficult  object. 

Blotty  

A  R  A  =  i'.87  by  obs  

R  A,  probably  erroneous   

A  fine  double  star   

A  nebula  follows  nearly  on  parallel  

Points  north  <  if  a  *  13  m  

Nisi  Pos  =  272.0   

Neat  double  star  (A.  4)  

A  R  A  =  17*.  5  ;  large  star  single  

p  Eridani.    Pos  302.5,  300.7,  299.1.     Fine  double 
H< .    Minute  by  obs  =  32,  but  mistaken. 

Pos  301.9,  298.8,  299.7  

Superb  double  star.    Pos  298.8,  300.3   

Pos  299.6,  299.3  

Class  3.    Zone  Review  

Nisi  pos  «=  310.7   

Difficult  

Pos  75.4,  71.8,  70.3.    Large  *  white  small  dull  red 
(t  Sculptoris). 

A  third  star  8  m  at  some  distance  

Points  north  of  a  star  9  m. 


L.  405 

L.  404 
X.  2690 


B.  227 
L.  469 
h.  641 


L.  485 
B.  240 
B.  242 
B.  243 

A-  5 


h.  2076 


2.  161 
A.  191 


DOUBLE  STARS. 


175 


No. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

h.    m.  s.d. 

0      1  it 

•54.64. 

1  39  1.6 

167    6  is 

I  S7.0 

2*- 

Q 

12 

Pos  157.8,  156.3,  156.9.   Night  not  favourable.  Set 

746 

miirnnn    tr\  id  n  r     trip  in  pa  sin  t*p  nf   /*fi-7'>        Tf  wi  11 

IIIM    MMM.     Mi     l£l.\Ji'\}     llH      IIH  d     1.11'      Ul     /      '  <  „  -1  .          IV     W  1H 

not  do  for  a  measure,  and  could  I  rely  on  the 
measure  of  that  J"  this  star  must  have  changed. 

3-3 

0  27 

149.5 

8 

11 

T*n*;  T/iS  R    t  Co  ^       T")iffipiilr    nnf  Hpinc  wpII  HpfinpH 

X  \JO     1  J.O.O.     1  SUi  *•          1/1IM1  1I1L 1    UUl    \J\.  lilt'     VYCU  Willi1'!, 

but  a  fine  double  \_:  if  micrometer  not  mis- 
read io0]. 

622 

3465 

I  39  21. 1 

130  47  41 

270.8 

6 

8' 

10 

488 

23.O 

48  1 

273.7 

12 

8 

11 

03s 

3466 

I  40  57.7 

120    7  29 

_  -  _|_ 

52± 

25 

8 

10 

643 

3467 

1  41  27.8 

170    0  15 

346.0 

15 

6 

13 

±5.  259 

02o 

34°  * 

I  41  41.5 

154  34  48 

21.3 

J5 

9 

16 

Mr\c7   1       a      ^>  r\  ft               v  t~r*n  m    1  tt    /1i  flh /til  1  f"          Tf"    10    f"rio  loct 
I  OS  ZZ>4-,  ZU<  7-       IL_Yl  1  t  II  It.  1  y     (U1IH  Ull,        1  L    lb    LUC  MM 

631 

but  one  in  R  A,  and  most  south  but  2  in  declin. 
of  five  stars  forming  a  hook. 

1  42  .. 

129  12  . . 

70.9 

** 

6 

10 

B.  260 

E 

_ . 

347° 

I  42  50.6 

113  28  39 

O  _ 

g 

10 

10' 

641 

3471 

i  45  9.6 

134  33  53 

38.! 

20 

8 

12 

Pos  380  383  

753 

12.6 

34  34 

41.8 

25 

9 

14 

752 

347z 

1  45  12.2 

118  54  53 

50.4 

3 

9'- 

=  9' 

643 

3473 

1  49  20.5 

142  27  23 

192.3 

12 

4' 

14 

Eridctni)  •    Pos  191  -4-j  1 9  3  •  3>     Extremely  deli- 

B.  278 

49 

cate  and  difiicult,  but  quite  certam  01  the  small 
star. 

1AH  A 

34/4 

T    A n  AAA 

1  +9  44-4- 

171    1  20 

2O.9 

25 

g 

13 

T)plipnrp 

r>.  279 

3475 

1  49  45.1 

151    8  28 

30.3 

3 

7'= 

=  7' 

L.  584 

736 

1  51  1.7 

113  44  59 

3°9± 

6 

s  - 

0  - 

—  5 

<T.  51 

641 

3476 

1  52  1.6 

100  21  9 

183.7 

60 

£L 
O 

IO 

650 

3477 

i  53  6.6 

135  21  1 

157-5 

8 

IO 

IO 

624 

7-3 

22  5 

156. 1 

5 

f 

9  = 

f 

=  9 

634 

1  54  50.7 

no  27  7 

6 

9' 

10 

h.  2107 

640 

0.5 

347» 

1  55  10.0 

121    8  23 

138.5 

30 

8 

8' 

494 

3479 

1  55  28.2 

153  35  8 

272.4 

30 

8 

1 1 

631 

1  56  48.1 

109  57  46 

167. 1 

15 

10 

1 1 

h.  2112 

74i 

348o 

1  56  58.2 

127    5  20 

127.3 

15 

.  O  £. 

9 

3481 

I   <o  S6.4. 

57.2 

149  58  33 
59  0 

7.7 

j  j 

5-7 

18 
25 

1 1 

co-i 

J  J 

734 

9 

io' 

60.4: 

58  21  : 

6.2 

10 : 

0/ 
a 

1 1 

The  places  ot  this  J  not  good.  I  he  dist  manifestly 
underrated. 

501 

3482 

2     O  4.7 

155  58  I 

202.8 

30 

15 

L.  642 

631 

7 

/ 

3483 

2      I  9.7 

9-7 

162    4  20 

3°34 
305.6 

6 

9' 

10 

n' 

513 

6 

4  13 

9 

9 

5H 

3  59 

3°9-3 

IO 

482 

5 

9' 

14.7 

5  58 

306.7 

8 

745 

9' 

9' 

3484 

2  2 

120  27 

63.5 

89.2 

8 

E 

9' 

2     4  7.6 

93  11  15 

227.7 

18 

6' 

8 

2.  231 

739 

3485 

2      5  O.7 

140    7  20 

143.0 

3 

9' 

10 

744 

3486 

2      5  32.4 

155    9  39 

220.4 

30 

14 

L.  676 

631 

7' 

3487 

2    6  36.5 

153  49  33 

344-3 

12 

12 

631 

9 

40.2 

49  36 

345-8 

12 

8' 

10' 

506 

3488 

2     7  29.6 

152  27  5 

137.8 

3 

8' 

8' 

Pos  137. 1,  138.5,  137.8.  Fine  star.  The  places  not 
good  in  this  f. 

501 

3489 

2      7  33.9 

161  44  56 

242.6 

20 

8 

12 

5H 

3490 

2     7  5I.3 

156  34  21 

197-5 

18 

8 

508 

3491 

2    8  15.8 

111  47  0 

286.1 

5 

9 

9' 

642 

3492 

2    8  31.2 

123  39  20 

43.0 

15 

10 

10 

635 

176 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1830.0. 
h.  m.    s.  d. 


N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

o  / 

II 

140  20 

55  : 

240.5 

9 

10 

1 1 

142  17 

59 

210.4 

80 

5 

9 

126  13 

6 

120.6 

9  = 

=  9 

14 

56 

124.8 

is 

9  = 

=  9 

15 

28 

122.4 

9  = 

=  9 

10 1  42 

49 

289-t- 

10= 

10 

42 

5i 

ijlc  1 

2< 

10'= 

10' 

158  58 

30 

3^1.4 

IO 

9' 

12 

59 

3 

321.8 

T  C 

9' 

1 1 

146  43 

5i 

8l  7 

J  J 

6' 

10 

118  37 

55 

IO 

7 

16 

150  47 

5° 

4 

9' 

10 

92  52 

46 

OO 

10= 

10 

101  23 

29 

265.8 

IO 

6 

1 1 

112  4 

20 

1/1  T  8 
341.8 

8' 

9 

153  57 

28 

335-3 

20 

8' 

12 

113  27 

0 

03.5 

2  c 

6' 

13 

148  53 

43 

297.3 

T  r 

g 

11 

54 

9 

20 

7' 

11 

121  6 

39 

270.8 

6 

8 

8' 

6 

42 

271.8 

8 

0 
a 

9 

109  6 

2 

23+ 

20 

8 

12 

118  58 

39 

241. 1 

5 

O 

8 

154  36 

17 

115. 5 

12 

9 

13 

168  30 

58 

80.6 

15 

9 

10 

122  16 

32 

53.0 

25 

7 

1 1' 

103  31 

16 

329.3 

15 

10 

1 1 

133  43 

6 

10.7 

6 

8' 

9' 

43 

58 

1 1.9 

5 

10 

11 

9-3 

IO 

9' 

12 

112  8 

51 

94-3 

18 

7' 

10 

8 

35 

97-3 

20 

8 

9' 

115  29 

5° 

37± 

15 

IO' 

1 1 

133  14 

10 

19.7 

12 

9' 

9' 

146  52 

32 

21.7 

18 

9' 

1 1 

52 

17 

21.0 

20 

9 

10 

115  33 

18 

1  io- 1~ 

20 

10' 

11 

139  8 

40 

323.3 

30 

8 

1 1 

102  7 

1 1 

214.3 

12 

8' 

1 1 

159  56 

35 

236.4 

15 

8' 

12 

118  53 

A 

19.6 
299± 

IO  I 
12  i 

8',  12 

,  12 

173  H 

27 

176.7 

"25 

9 

145  34 

56 

199.4 

25 

8' 

9 

33 

48 

198.3 

20 

8 

8' 

139  43 

5° 

263.5 

20 

10 

10' 

44 

20 

259-3 

12 

9' 

10 

166  38 

1 1 

299.6 

35 

7' 

1 1 

Remarks. 


Synon. 


3493 


3494 


3495 
3496 

3497 
3498 

3499 


3500 
3501 
3502 
3503 

35°4 

35°5 
3506 
3507 
3508 
35°9 

3510 


3511 


3512 
35i3 
35H 

35i5 
3516 

35!7 
3518 

35»9 
3520 

3521 

3522 


2  10  18.4 

2  IO  29.3  : 
2  12  36.5 
42.I 

48.9 

2   12  59.4 
62.6 
2   13  42.7 
46.3 
2   14  25.I 
2    14  27.6 
2    15  48.4 
2   l6  l6.2 
2    17  3I.2 
2    I7  55.9 
2  21  32.5 
2  22  IO.4 
2  22  52.3 
53.O 
2  23  O.7 
I.I 

2  25  IO.5 
2  26  23.3 
2  26  24.9 
2  26  56.3 
2  26  58.5 
2  27  14.6 
2   27  49.7 

53-4 

2  28  12.6 
14. 1 


2  28  31.5 
2  28  34.0 
2  28  37.0 
38.9 
2  28  38.0 

2  29  54.3 

2  29  57.7 

1  31  5-3 

2  31  27.6 

2  32  9-5 
2  33  39  5 
40.8 

2  33  45-8 
50.3 

2  34  9-3 


(0  Eridanii)  =  A.  7    B.  327 

A  very  neat  double  star  

Very  ill  denned.  Hardly  more  than  much  elongated, 
and  at  moments  separated.  S  E  very  strong  ; 
some  haze. 

[These  R  As  disagree  sadly.  MSS.  re-examined. 
No  error  detected.] 

A  large  star  follows   

Triple  ?  Excessively  difficult  

The  places  of  this  sweep  are  bad   

Fine  double  star  

Pos  mean  of  302.3,  303.3  

An  elegant  double  star   

Fine  •  

Too  late  for  measure  

Pos  238.9,  243.3  ;  very  fine  star,  but  ill  defined. . . . 

Pos  11. 5,  12.3  

Viewed  and  measured  past  meridian  

Large  star,  yellow  ;  small,  pale  blue  

Yellow  and  blue.  [This  observation  makes  the  minute 
of  R  A  29.  One  or  other  must  be  wrong,  but 
the  earliest  is  chosen  to  avoid  missing  the  object 
in  future.] 

The  preceding  of  two  D  stars  

The  following  of  2.  Pos  roughly  estimated  from  the 
diagram. 

Pos  mean  of  213.7,  214.9  

An  elegant  triple  star  

A  R  A  =  7'-5    L.  864 


L.  717 
L.  711 

2.  266 
h.  2140 


M.  841 

L.  770 


A.  267 


h.  214 


2.  288 


DOUBLE  STARS. 


177 


No. 


R  A.  1830.0. 
h.  m.   s.  d. 


3523 
3524 


3525 

35*6 

3527 
3528 


3529 

353° 

353i 
353* 

3533 

3534 
3535 

3536 

3537 

3538 


3539 
354° 
3541 
3542 
3543 
3544 


3545 


3546 
3547 
3548 
3549 


2  35  .. 
2  35  6.5 
7.0 
9.0 
10.6 
2  35  7.0 
236 

2  36  4i-3 
2  37  .. 
2  37  31.6 
2  38  43.4 

2  39  46.2 

2  40  48.0 

2  41  3.8 
2  41  17.5 
2  41  48.2 
51.2 
2  42  0.0 
0.0 

2  42  20.1 
2  42  33.3 
2  42  35.7 

2  43  22.5 

2  43  46.8 
48.9 
2  46  4.3 
6.3 
8.5 

2  47  17-3 
2  48  3.4 
2  48  13.8 
2  50  18.0 
2  50  24.9 
2  50  30.8 
33-3 


2  51  22.4 

2   51  48.3 
49.6 
2   53  21.6 
2   53  44.4 
2   56  7.4 
2   56  27.O 
29.4 
2   58  6.2 
2   58  37.2 
37.6 


NPD.  1880.0. 


120  17  .. 
Ill     I  17 

1  15 

0  5 
o  35 

151  18  8 

121  48  .. 
116  14  42 
131  15  .. 
164  11  17 

100  34  39 

123  o  54 
171  29  8j 

101  15  39 
130  58  48 
128    7  5 

7  41 
110  57  42 

57  54 
115  16  o 

150  52  28 

118  38  53 

126  32  45 

130  58  48 
59  33 

152  55  3 
54  15 
54  35 

168  50  5 

151  35  10 
150  37  28 

155    1  45 

119  39  12 
133  26  24 

26  28 


100  6  9 
130  59  19 

59  25 
108  34  12 
159  49  50 
112  2  21 
128  44  53 

45  10 
141  59  30 

103  59  11 

59  4° 


Position. 


94-7 


131 

135 
130 

135 
274 

56 
183 

43 
212 
328 


1 1 1.3 

175-7 
207.3 

157.6 

32-3 
150.6 
150.6 
274.4 
275-4 

213.1 


3-5 

32.3 

29.7 
301.0 
290.6 
298.0 

59.8 
4.6 
151. 2 
142.7 

90+ 
192.4 
185+ 
187+ 

65.3 
82.3 
81.4 
82.3 
115. 6 
122.2 
276.1 
273.3 
68.7  . 

12.3 

12.3 


Dist.  Magnitude. 


66.3 
25 


18 


Remarks. 


Sjnon. 


Sweep. 


8  IO 


20 

9 

10 

20 

7 

9 

20 

7 

8' 

45 

7' 

15 

7 

11 

'5 

8 

10' 

1.6 

7'  = 

=  7' 

10 

1 1 

ii' 

18 

9' 

10 

18 

9' 

15 

15 

8' 

12 

10 

8' 

is 

8 

9 

15 

10' 

10' 

6 

6' 

8 

7 

45 

8 

8' 

45 

8 

9 

6 

2  c 
j 

Q 

7 

12 

6 

4 

6 

I  "\ 

j 

15 

10' 

10' 

18 

10 

io' 

15 

9 

12 

12 

10 

*3 

12 

9' 

10 

10 

10' 

7 

10' 

12 

8 

IO 

12 

IO 

10' 

2 

9' 

I  I 

9' 

IO 

2 

IO 

12 

40 

7 

9 

12 

4 

5 

r5 

5 

6 

8 

9 

12 

10 

9' 

12 

12 

7 

12 

4 

10' 

r3 

5 

10 

12 

30 

7' 

i 

15 

9 

IO 

Epoch  37.011 


Hurried  observation   

Good  measure  

A  R  A  =  4'.7  

1834.780  

Fine  object.  Marked  as  double  in  B 
Mean  epoch  =  1836.593   


[The  R  A  in  my  5th  catalogue  is  39"'  15s. 2,  but  the 
wire  is  mistaken. — This  corrected,  the  R  A  comes 
out  38">  43!-6]. 


AB.  Pos  176.3,  175.2  \ 
AC— Pos  205.2,  209.5  J 


111  denned  ;  bad  measure 


Pos  150.9,  150.4.  v  Fornacis 
Pos  150.9,  150.4  


Large  star  yellowish,  small  bluish  A  R  A  =  3s.o. .  . . 
Triple  classes  5  and  6  ;  h.  2161  

A  strong  suspicion  that  this  star  is  a  close  double 
star,  but  no  time  to  verify  it 

Pos.  2.8,  4.3.    Most  delicate  and  beautiful  


The  preceding  of  2  stars 
A  star  9  m  follows  


Fine  *  ;  Pos  148.8,  152.3,  154.3,  1494 
Triple.    Classes  I.  and  II  


Too  ill-defined  for  measure   

Viewed  and  roughly  measured  past  meridian,  having 
lost  time  by  examining  another  star  by  mistake 
for  this 


(OErid.)  Pos  Mean  of  82.7,  81.9  

Superb  D  star.  Pos  791,  83.3,  81.8,  81.3 
A  star  7' m  3'  n  p  


(A-  10)  

Pos  12.4,  12.2 . 


B.  389 
B.  394 
B.  395 

S.  308 


315 
B.  413 

L.  890 

L.  892 

M.  967 
L.  897 


A.  325 
A.  9 


B.  473 
2.  356 


E 
640 

74' 
641 
642 
736 

E 
646 

E 

745 
650 

635 
633 
650 

743 
801 
802 
640 

74i 
646 
736 
643 

636 

743 
638 
736 

755 
808 

747 
755 
736 
808 
643 
489 
639 
752 

650 

743 
638 
64.0 

5r3 
641 
801 
636 
655 
649 
648 


z  z 


178 


REDUCED  OBSERVATIONS  OP 


No. 


355° 


355i 
3552 
3553 
3554 
3555 
3556 


3557 
3558 

3559 
3560 
3561 
3562 
3563 
3564 


3565 
3566 
3567 


3568 
3569 
357° 
357i 

3572 
3573 
3574 

3575 

3576 

3577 
3578 


3579 
358o 

358i 

3582 

3583 
3584 


R  A.  1830.0. 

N  PD.  1830.0. 

h. 

m. 

s.  d. 

0 

J 

a 

2 

59 

10.7 

141 

59 

6 

3 

0 

I2.0 

103 

56 

3 

0 

17. 1 

94 

20 

25 

3 

1 

54.I 

104 

38 

10 

3 

2 

27.7 

161 

8 

13 

3 

2 

57.2 

128 

31 

20 

3 

4 

11. 8 

93 

3* 

48 

3 

4 

54-4 

119 

39 

5° 

3 

6 

27.0 

J35 

3 

29 

29.9 

3 

>5 

3 

5 

104 

3 

55 

3 

5 

C-T  8 

57. s 

104 

39 

34 

3 

7 

4.0 

i54 

33 

35 

3 

7 

26.6 

i74 

53 

5 

3 

9 

9.4 

1 10 

35 

0 

3 

9 

r54 

57 

3 

9 

40.9 

113 

39 

30 

3 

10 

52.5 

150 

8 

5 

54.0 

8 

41 

59.0 

8 

43 

3 

11 

109 

6 

•  • 

3 

11 

22.5 

156 

27 

20 

3 

12 

21.4 

104 

36 

5° 

3 

12 

27.9 

i55 

4 

33 

29.0 

4 

15 

3 

*3 

30.5 

169 

37 

43 

3 

J4 

5.2 

103 

53 

26 

3 

14 

6.6 

no 

56 

41 

3 

J4 

23.1 

'43 

45 

8 

3 

15 

8.3 

IOI 

57 

29 

3 

10 

34-5 

116 

49 

47 

3 

17 

56.6 

14.0 

36 

I  c 

J 

3 

18 

44-7 

I  12 

6 

20 

3 

*9 

7  1  8 

3 1.0 

I41 

40 

32.1 

40 

I 

3 

*9 

I36 

3 

20 

42-3  . 
* 

I72 

27 

6 

3 

20 

5r-3 

122 

48 

± 

53-5 

48 

± 

3 

21 

52.0 

IOI 

43 

59 

3 

22 

24.9 

!34 

15 

0 

3 

26 

27-7 

J53 

32 

5 

3 

27 

41.2 

171 

6 

21 

3 

27 

43.0 

174 

9 

57 

3 

30 

8.7 

in 

1 

47 

3 

3i 

15.8 

141 

45 

53 

46 

11 

Position. 

Dist. 

Magnitude 

68.3 

35 

7 

8 

293± 

5 

IO 

10' 

351.6 

15 

9 

1 1 

134.6 

15 

9 

10 

354-7 

12 

9 

12 

224.1 

15 

9 

10 

348-3 

18 

8' 

1 1 

306.I 

3 

4 

7 

7.11.1 

*  .5  3  •  4 

*  2 

6 

1 1 

y-y 

20 

7' 

12 

1  co-4- 

12 

10 

10 

n  8 

AO 

6' 

1 1 

2"3A  6 

a  j4-u 

12 

11 

12 

J35-3 

12 

8' 

12 

4.5.4. 

8' 

9 

2J.6.  c 

7 

8'  = 

=  8' 

2,7  A. A 

^O 

6 

13 

Z75.0 

3° 

5' 

13 

27 1.9 

8 

13 

1 10.4 

5.8 

5 

9 

40.8 

12 

9 

12 

100-r- 

3 

io' 

12 

97-5 

20 

7 

9 

101. 6 

20 

7 

10 

222.4 

7 

9 

210.5 

18 

9' 

11 

6 

87.4 

15 

10' 

1 1 

3*5-3 

40 

8 

12 

274.3 

20 

8  = 

-  0 

24074^ 

'5 

8' 

11 

4.I.9 

3° 

8 

12 

41.2 

25 

7' 

12 

1  7Q  2 

A. 2 

/ 

0 

y 

243.9 

10 

8' 

12 

15 

8 

10 

49± 

I 

263.3 

15 

7' 

II 

122.4 

60 

4 

12 

320.9 

5 

10' 

1 1 

286.2 

!5 

7 

1 1 

89.0 

12 

10'= 

10' 

354-5 

10 

8' 

13 

357-3 

12 

9 

13 

Remarks. 


The  following  and  larger  of  2,  extremely  ill-defined 
Good  measure  

12  Eridani.    Very  fine  D  star  

With  the  utmost  difficulty  I  get  a  glimpse  of  the 
star  as  wedge-shaped,  but  the  definition  is  growing 
very  bad. 

Pos  234.3,  232.4.    A  most  beautiful  object   

Position  merely  estimated  from  the  diagram   

>..>•••.>.>•■>••••..••..•••.■•  • 

Epoch  1836.901  

A  very  pretty  double  star  

Large  star,  yellow  

Very  ill  defined   

Epoch  1835.814  

A  R  A  =  3'. 6  ;  Pos  222.5,  222-3   

Triple  or  quadruple   

Taken  for  2.  387,  which  was  not  found   

Position  roughly  estimated  from  the  diagram  

Near  a  cometic  nebula.  Pos  estimated  from 
diagram. 

Epoch  1836  

Difficult,  a  3d  j|=  in  same  direction  

No  description   

If  double,  but  too  ill  defined  to  be  sure.  [The 
angle  of  position  though  rude  is  sufficiently  near 
to  M.  Struve's  to  prove  that  the  division  of  the 
star  was  no  illusion]. 

Called  6minB  

Pos  286.6,  285.8  

Points  to  a  star  13m  

Too  late  for  R  A   


Synon. 

B.  473 
2.  357 
2.  358 


A.  353 

B.  501 


L.1033 


B.  521 


B.  529 
A.  12 


h. 2187 


B.  551 


2.407 


B.  566 


DOUBLE  STARS. 


179 


No. 


E  A.  1830.0. 
h.  m.  s.d. 


N  PD.  1830.0. 


Dist. 


Magnitude. 


Remarks. 


Synon. 


Sweep. 


3585 


3586 


3587 


3588 


3589 

359° 
3591 
3592 

3593 
3594 
3595 
3596 
3597 


3598 

3599 

3600 
3601 


360a 
3603 
3604 
3605 

3606 
3607 
3608 

3609 
3610 

3611 


3  32  28.3 
3  32  49-9 

3  33  2-9 
3  33  4!-3 
41.  5 

3  34  46-8 

3  35  3-3 
4-3 
10.6 :: 

3  36  35-6 
3  37  44-9 

3  38  4-6 
6.6 

3  39  20 — 
3  39  54-8 
3  4°  H-9 

3  40  30.6 

3  4°  5!-8 
3  41  28.8 
3  4i  52-6 
3  42  3-3 
3  42  18.7 
21.5 

3  43  19-9 
22.3 
23.5 

3  43  34-9 

37.6 

3  44  i-5 
3  44  18.3 
21.5 
22.3 
3  44  18.7 
3  44  25-o 
3  46  49-3 
3  47  9-7 
29.5 
3  48  30.2 
3  48  43-6 
3  5°  5-3 

3  50  6.8 
10.4 

3  50  38.6 
40.5 

3  5°  40+ 


i75  0  57 
103  11  4 

136  11  6 

130  54  29 

54  37 
150  20  3 

150  22  36 

22  5s 

22  25: 

101  19  9 

103  52  41 

131  11  37 
11  59 

132  26  — 

141  50  53 
144  48  19 

131  11  36 

no  56  24 

173  10  53 

122  18  22 

142  45  20 
128    9  13 

8  45 

140  58  32 
57  3°  : 
57  57 

109  25  45 

25  58 

154  35  55 

113  26  58 

26  50 
26  45 

117  59  32 
161  32  5 
139  17  20 

170  52  4 
51  40 

161  18  55 

171  23  59 

104  o  28 

153  10  15 
10  20 

153    8  28 

8  40 

130  25  32 


276.5 
232.1 
228.7 
158. 1 
327.1 
327.2 
25°± 

229.1 

228.0 
222.9 
320.9 
322.6 
346.8 
344-7 

321.6 
4-3 

137.2 
87.3 

3^-5 
136.7 
260.2 
199.3 
200.5 

227.6 
224.7 
225.7 
66.7 

76.8 
1 1.7 
303.5 
298.3 
301. 1 

347± 
76.0 
301. 1 
165. 1 
168.6 

333-3 
120.3 
233.6 

132.6 
125. 1 

186.8 

183.9 

140.3 


12 

30 

35 
20 
12 
12 
30+ 


11=11 

8'  10 
8  9 
10=10 


8  13 


9  10 

9  12 

9'  12 

10  10' 

8  9 

9'  10 

8'  10 

8  11 

8  10 
10=10 

9  9' 

11  12 


9  10 

9'  11 

9'  10 

8  9 

3'  13 

11  11 
1 1=1 1 

10  12 

10  11 


A  RA  =  8<.o  

Pos  233.9,  23i-3  

Pos  228.5,  228.9  

Pos  by  two  measures  coinciding   

Pos  327.8,  326.7.     (End.  184)  

Plac«  taken  from  the  Brisbane  Catalogue.  Pos  and 
dist.  roughly  est.  from  diagram. 

Following  the  coarse  double  star  B.  586  

The  small  star  not  seen  for  clouds   

Two  very  bright  stars  np  

Pos  mean  of  347.0,  346.7  

Neat  double  star  

4th  class.    Zone  review  

Very  elegant.  Large  star,  yellow.  Small  pale  blue  ; 
Pos  2.8,  5.3,  4.7.  [Extraordinary  discordance  of 
pos  with  the  equatorial  measures] . 

The  southern  of  a  triangle  

f  Eridani.  Superb   

Superb  double  star,  but  very  ill  denned.  Pos  200.7, 
200.3.    Marked  as  double  in  the  Brisb.  Catal. 

This  or  the  nest  obs.  seems  to  have  a  mistaken 
reading  of  io°  in  Pos. 

Neat  star  

Neat  double  star  

A  R  A  =4%5   

Neat  star  

A  R  A  =  i4s-5   

y  Eridani,  marked  as  2.3  m  in  A  S  C,  but  it  is  cer- 
tainly not  above  3.4. 

One  of  a  group  

The  second  in  a  group   

The  5  th  star  in  a  group  

Very  neat  star,  but  the  R  A  liable  to  considerable 
error,  being  beyond  the  meridian  when  taken. 


2.436 


B.  583 

A  15 

B.  586 
A.  14 


2.  451 
B.  594 

B.  602 

L,  1240 

A.  426 
A.  16 


440 


633 
757 
649 
654 
754 
743 
756 

756 

755 
501 
650 
649 
757 
754 
743 
E 

806 
520 

754 
652 
633 
644 

655 
801 
660 

526 

744 
806 

74i 

652 
808 
647 
642 
641 
643 
513 
744 
633 

747 
513 
633 

757 

501 
756 
501 
756 
754 


180 


REDUCED  OBSERVATIONS  OF 


R  A.  1880.0. 
h.  m.    6.  d. 


N  P  D.  1830.0. 


.Magnitude, 


Remarks. 


Synon. 


Sweep. 


361a 


3  52  5.6 
22.8: 


3613 

3 

52  35.8 

3 

52  48.9 

3614 

3 

55  4-9 

3615 

3 

55  16.0 

3616 

3 

55  46-2 

3617 

3 

56  0.2 

2.5 

3618 

3 

56  3i-5 

34.0 

3619 

3 

58  1.9 

3620 

3 

58  - 

3621 

3 

58  22.3 

3622 

3 

58  34-7 

34-9 

3623 

4 

0  5.3 

3624 

4 

1  58.1 

66.5 

68.3 

3625 

4 

4  38.8 

3626 

4 

5  10.8 

3627 

4 

6  - 

3628 

4 

6  - 

4. 

6  17. q 

19.6 

3629 

4 

6  31. 2 

3630 

4 

7  17-9 

3631 

A. 
T 

7  e  1.6 

55.8 

3632 

4 

8  23.0 

3633 

4 

9  43-9 

3634 

4 

10  4.9 

7-3 

3635 

4 

10  47.0 

3636 

4 

11  27.4 

27.7 

3637 

4 

»  55-5 

3638 

4 

12  14.4 

15.9 

3639 

4 

12  18.8 

3640 

4 

12  22.5 

26.6 

3641 

4 

12  34.3 

4 

12  53.8 

3642 

4 

J3  - 

170  32  29 

33  5 

104  59  55 
100  56  49 
127  35  31 

105  36  50 
135  19  26 
102  13  26 

J3  57 
139  60  12 

59  5 
102  14  18 

'34  57  - 
124  18  2 


126  18  26 

17  40 
122  54  52 

165  13  31 
13  18 
13  6 

142  19  46 

99  54  59 
124  12  — 
126  36  — 
100  41  2 

41  19 

106  59  o 
139  24  25 
159  29  46 

29  43 

I20   30  22 

107  13  45 
135      2  56 

2  14 
I46  29  59 

124  13  6 
13  o 
117    8  29 
152  54  10 

53  1 
139  24  50 

166  19  50 

18  10 
!52  37  14 

37  ± 
104  38  15 
124  17  - 


159.2 
159-5 
H7-7 

9.3:: 
42.3 
160.6 
136.0 
61.3 
63.6 
318.4 
3 '7-4 
324± 

110.3 


in. 1 
1 16.0 

302.7 
21.3 
22.7 
19.5 

184.4 

38-3 
303.3 

50.1 
146.6 

140+ 

84.1 

97-5 
226.3 
221.6 

i57± 
9.1 
330.7 

335-7 
326.6 
13.4 
15.9 

353-6 
353-8 
91.8 
71.9 
71.4 
287.8 
283.3 

192.8 

157.6 


12 

5 
20 
20 
20 

15 
18 

29.7 
50.5 
5 

5 

15 
25 

4 

4 
12 

25 
15 
10 
10 

5° 
60 

35 
40 
60 
15 
15 


10+ 
12 


9  = 

8' 

9' 
10 

9' 
9 
10 


Pos  158.6,  160.3  nne  *  ;  RA  very  uncertain  .... 

Neat  double  star  

A  third  star,  10  m  near  

Neat  star  ;  Pos  317-2,  317.6  

Class  5  ;  zone  review  

Fine  star.  It  is  barely  possible  that  this  may  be 
identical  with  the  subsequent  star  by  a  double 
mistake  of  io1  in  the  chronometer  reading,  and  20 
in  the  Polar  distance  index — the  latter  a  thing  most 
improbable.  If  they  be  really  distinct,  the  coin- 
cidence in  other  respects  is  remarkable. 

Pos  110.7,  in. 5.   Neat  star  

Pos  1 16.3,  1 15.8.    Fine  D  star  

Neat  star  

Mean  epoch  1837.962   

Epoch  1838.082  

Pos  146.7,  146.6  ;  a  fine  object.  [Query  if  not 
changed  in  position.] 

(39  Eridani.)  A  beautiful  star.  Too  late  for  a 
measure. 

A  fine  double  star   

A  nebula  follows  

Pos  354.3,  352.9  (a  Reticuli)   

Pos  353.3,  354.3  

Some  doubt  about  the  minute  in  RA   

Delicate;  15"  dist  is  too  far  

Pos  288.8,  286.8  ;  fine  star   

Fine.    A  large  star  near  a  Retic  

Epoch  1837.894  


2.  487 


2.  516 


L.1395 


A.  482 


A.  4S5 


L.1245 


532 


774 
633 
651 

758 
661 
651 
654 

757 
758 
626 

744 
757 
E 

663 


635 
661 
663 

745 
622 
746 
807 
650 
E 
E 

758 
650 

651 
744 
5i3 
509 
644 
65, 
639 
804 

521 
662 
663 
646 
808 

524 
526 
622 

746 
756 

524 

757 

E 


DOUBLE  STARS. 


181 


No. 

R  A.  1830.0. 

h. 

m. 

s.  d. 

3643 

4 

'3 

55-4 

58.2 

4 

H 

8.9 

3  "44 

4 

14 

28.1 

4 

16 

3645 

4 

16 

5-9 

6.6 

4 

16 

14.0 

3647 

4 

16 

24.3 

4 

_  r 
I  0 

35-3 

3648 

4 

17 

4.1 

3649 

4 

20 

28.1 

3650 

4 

20 

53-i 

4 

20 

54-3 

3651 

4 

22 

45.  S 

52.0 

3652 

4 

22 

55.2 

3653 

4 

23 

2.8 

36S4 

4 

23 

18.6 

3655 

4 

23 

4I.6 

3656 

4 

23 

42.6 

36S7 

4 

23 

46.4 

3658 

4 

24 

17. 1 

I7.6 

3659 

A 

4 

-  + 

27.3 

4 

8.2 

3660 

4 

*s 

47.1 

3661 

4 

26 

34.0 

4 

27 

6.1 

3662 

4 

27 

26.5 

27.2 

27.9 

29.7 

3663 

4 

27 

49-3 

3664 

4 

27 

53-1 

3665 

4 

29 

14.0 

20.2 

3666 

4 

29 

19.4 

21.0 

3667 

4 

29 

24.7 

N  P  D.  1830.0. 


134  41  1 
40  40 
IOO  22  19 

116    8  16 

153  40  - 


134  46  o 

45  1 

131  37  11 

108  29  15 


99    9  9 

134  o  39 
104  22  12 
13°  54  39 

147  27  37 
!54  34  55 

153  34  22 
123  57  9 
106  49  30 

157    7  H 

154  29  15 

154  37  3° 
156  39  29 
139  58  42 

58  22 
126  1  43 
102  30  12 

155  52  48 
'57  39  13 
100    5  18 

156  4  51 
5  4 
5  8 
5  1° 


6  20 

125  11  57 
115  22  48 
150  13  31 

12  36 
156  28  42 

28  16 
128  22  51 


115.5 
116. 3 
333-2 
S  37-5 

(  20± 

6.1 

142.3 
139.1 
135.8 
30+ 

35°± 


22.2 
168.5 
178.0 

226.1 

60.5 

59-9 
117.9 
148.5  : 

94-7 
J57-8 
255.1 
336.7 
1 16.7 
1 17. 1 

35.6 

345-7 
251.7 
8.3 
262.8 
47.8 
40.8 

45.8 

46.3 

C  46.7 

5 191.8 

C  7-7 

342.7 

'93± 
53-9 
53.8 
206.7 
204.4 
290.1 


Di>t. 


60 
80 

15 
40 
*5 
6.2 


25 

3 
5 
15 

15 
8 
40 
15 
15 
20 
10 
3 
5 
30 

18 

8 
18 

30 
20 

22 
35 


Magnitude. 


10   -  10 
10'  -  10' 
8  IO 
10,10,1 1 


10  10 

10  =  10 

6  9 

V  9 
9  10 


8  13 

10  10' 

10  10' 

9'  10 

9 
6 


9  + 
'4 
9  9 
10  10' 
10'  13 
8'  9 
8'  10 
9  10 

9'  10 

7'  8 


«  9 

8'  14 
9'  15 

8  12 

8'  10' 
10  =  10 
10  =  10 

9  11 
9  11 
9  11 


Eemarks. 


(1//  Horologii)  

A  R  A  =  6\o. 

Pos  334.5,  331.9  

Triple.  Pos  and  dist  of  the  small  $  estimated  from 
the  diagram. 

(?Reticuli.  Epoch  1835.805.  [Noticed  as  double 
by  Rumker], 

An  ecmilateral  triangle.  Pos  estimated  from  the 
diagram. 

I  am  almost  certain  that  this  star,  the  preceding  of 
two,  is  close  double,  but  could  not  follow  to  verify 
it,  the  telescope  being  north  of  zenith. 

Pos  169.2,  167.8  

Seen  double,  and  measured  with  the  triangular 
aperture  and  180,  which  shows  it  well. 

Fine  star.  Pos  227.6,  224.6.  [Noticed  as  double 
by  Rumker]. 

There  can  be  no  doubt  of  the  identity  of  this  ob- 
ject and  the  next,  the  degree  of  P  D  being  misread 
in  one  or  other  :  153  appears  to  be  the  right. 

Not  a  good  measure  of  pos   

Very  neat  star.    Pos  116.7,  116.8   

Very  neat  D  star.    Pos  118.7,  11 5.6   

Pos  346.6,  344.7,  345.7  

A  R  A  =  4'.o  

Quadruple  or  double-double.  The  small  stars  are 
14  and  15  m,  and  stand  in  the  respective  positions 
188.9  and  1.3,  each  with  its  principal  star. 

A  B^ 

A  C  .  Quadruple  

bd) 

Elegant  double  star   

Very  neat  star  


Synon. 


B.  687 

2-  537 
A- 493 

B.  695 


2.  544 

B.  712 
B.  713 


L.1511 
L.1510 


M1592 
2.564 


570 


Sweep. 

639 

650 
646 

E 

639 
6  54 
754 
65, 

650 

804 
757 
754 

5i9 


5i8 
662 
651 

508 


653 
526 

744 
663 

757 
5i7 
653 

758 
761 
518 

761 

658 


8c8 

662 
646 
756 
5*4 
653 
761 
661 


182 


REDUCED  OBSERVATIONS  OF 


No. 


K  A.  1830.0. 
h.  m.   s.  d. 


3668 


3669 
3670 


3671 
3672 

3673 


3674 
3675 
3676 
3677 


3678 
3679 


3680 
3681 
3682 
3683 


3684 


3685 
3686 

3687 
3688 
3689 

3690 

3691 
3992 
3693 

3694 

3695 

3696 

3697 


4  30  - 
4  30.2  - 

4  31  27.6 
4  31  49.6 

50.0 

50.1 
4  32  14.8 

16.5 
4  32  26.3 

29.2 

4  32  31. 1 
364 


4  32  53-4 
4  33  i-6 
4  33  29.9 

4  33  44-4 

44-  5 

45-  9 
49-7 

4  34  - 
4  34  47-6 

4  35  25-5 
4  36  23.5 
4  36  55-3 
4  37  0.5 
4  37  3°-4 
32.9 

4  37  54-o 
4  38  48-9 
52.7 

4  39  3°-8 
4  39  34-9 
36.9 

4  39  4°-9 
4  39  45-4 
4  4°  3-2 

4  4°  35-9 

4  4i  31-6 
4  42  59-3 
4  43  3-6 

4  44 

4  44  37-5 
4  44  39-° 
39.1 

4  44  43-8 


N  P  D.  1830.0. 


145  24  - 
103  23  — 

I43  12  41 
153    II  ± 

10  34 

9  4i 
140  29  47 

29  55 
125  39  1 
38  28 

168    2  53 

2  35 

3  44 

127  39  49 
!34  58  34 
r57  54  7 
119  54  12 

54  21 
54  36 
54  33 
135  22  — 
152  25  3 

99  7  4 

142  12  59 

137  30  7 

156  27  6 

149  16  59 

17  9 
102  16  15 
158  2  19 

3  2 

133  43  14 
151  32  6 

32  7 

99  0  7 
144  14  31 

155  38  15 

102    3  49 

167  11  27 

i73  15  10 
102  32  9 

135  27  - 

128  52  8 

146  18  34 

18  51 
131  36  45 


Position. 


108.5 
171.9 

308.0 
95.0 
95.6 
93.6 
273.3 
278.8 
289.0 
297.6 

61.7 
62.1 
59-3 

205.3 
51.4 
184.9 
1 74. 1 
1 74. 1 

173-7 
173.8 
327.2 
35°± 

138.5 
21.4 
262.9 

i5± 
260.8 
261.5 
28 1. 1 
294.8 
294.5 

125.6 
213.8 
217.6 
282.8 
143. 1 
60.3 

S  45± 
*  i95± 
42.0 
181.7 
1 16.3 

62.3 

41.3 

265.7 

265.7 

284.6 


82.3 
18 


41.7 
20 

12 

6 
35 
25 

3 

3 

10 
15 


15 


Magnitude 


Remarks. 


6 
6' 

7 
10 


6'  12 
8'  12 
9  =  9 
9'  9' 
9'=  9' 
9  =  9 
8  10 


10  = 
6' 


9 
9 

9 

9  = 

9'  9 
9 
10 

9 


6 


a  Doradus.    Epoch  1836.006   

Pos  1 7 1. 5,  172.2.  Place  that  of  Struve's  Catalogue 
for  1826. 

Large  star,  yellow  ;  small,  pale  blue   

A  RA  =  5  .0  

Haze  coming  on  

Pos  285.9,  290>3<  290.9.    Neat  s)j  

io°  error  no  doubt  committed  in  the  micrometric 
reading. 

Fine  star.   Pos  62.9,  60.9,  61.3  

Fine.    Pos  -  63.5,  60.8  

Pos  59.9,  58.8  ;  ARA  =  3!.2.  This  obs  by  some 
unaccountable  error  gives  the  R  A  32'"  5  .1. 

Pos  173.9,  J73-9.  173-3  

Mean  epoch  1836.479  

Large  star  very  high  red,  a  rich  s|c  fine  colour,  almost 
sanguine.    Pos  estimated  from  the  diagram. 

Pos  138.8,  138.3.    Fine  star. 

Veryfine.    Pos 260.6,  261. 1  

Pos  26 1. 1,  261.9  ;  very  fine,  but  ill  defined  

Too  late  for  a  good  measure  

Presuming  a  mistaken  wire,  without  which  the  R. 
ascensions  of  the  two  observations  are  irre- 
concilable. 

Elegant;  Pos  35.1,  32.5,  33.8   

Pos  217.2,  218.0,  a  very  little  unequal  

Triple.  Pos  of  the  small  star  estimated  from  the 
diagram. 

Very  ill  defined   

Mean  epoch  1836.483  

Very  delicate;  Pos  265.7,  265.8   

Fine  star;  Pos  284.9,  284.3  


Synon. 


Sweep. 


B.  744 
2.576 

L.1551 


L.1584 


L.i 547 


L.1567 
2.590 

L.1572 

L.1583 

S.  596 


L.1707 


M 1726 


M  1727 


E 

757 

525 
808 

756 
524 
526 

744 
663 
801 

670 

747 
746 

661 
639 
760 
644 

5ii 
645 
643 
E 

756 

758 
525 
527 
761 
5,8 
665 

759 
760 

759 

639 
524 
756 
758 
521 
808 
757 

746 
668 
757 
E 

661 
520 
521 
638 


DOUBLE  STARS. 


183 


No. 

K  A.  1830.0. 
h.   m.  s.  d. 

N  P  D.  1830.0. 
0      /  // 

Position. 

Dist 

Magnitude 

Remarks. 

Synon. 

Sweep. 

7608 

4  45  6.7 

128  29  52 

290.8 

IO 

9 

!3 

801 

^6qq 

4.  4.C  18.O 

135  57  51 

141. 5 

5 

i 

13 

527 

3700 

A  A?    {  1.7 

T    TJ    J  J 

in    3  6 

345.3 

20 

/ 

H 

647 

52.7 

4  46  56. 8 

1  18 
H7  45  31 

I3O.3 

18 

!3 

13 

700 

3701 

12 

9' 

3702 

4  47  - 

115  26  — 

22I.O 

21.0 

9 

10' 

/  \" ; ,. ;  Tj  1  ^                  r  \       "17  i    _  0  _  /"  /- 

El 

— 

4  47  8.0 

143  45  27 

53-° 

15 

8 

8  + 

B.  810 
+  811 

525 

8.7 

44  52 

54-7 

12 

6' 

7 

A  18 

521 

9.6 

45  18 

56-7 

15 

7 

8 

807 

3703 

4  47  29.2 

152  10  21 

300.0 

5 

9' 

12 

524 

3704 

4  48  44.0 

131  42  16 

209.8 

12 

IO 

12 

iS04 

37°5 

4  49  10.0 

106  24  55 

I39-3 

16 

l' 

10 

-vr  1 

651 

3706 

4  49  58-4 

147  28  25 

2d  1. 1 

25 

8' 

13 

DO  s 

3707 

4  50  28.0 

150    1  46 

264.3 

3 

9 

13 

524 

3708 

4  52  ± 

177  52  ± 

J5 

IO 

10' 

A  R  A  =  47*'  5  j  the  R  A  may  be  many  minutes 

761 

wrong,  as  I  could  get  no  zero  stars. 

(bis) 

j  /uy 

A   ^2  20. 7 

109   4  40 

318.4 

20 

9 

1 1 

652 

4  53-°  ~~ 

IO-!   16  — 
J  j 

104.3 

4 

s' 

IO 

Pos  104.9,  i°3-8 ;  elegant.     Place  from  Struve's 

2.  601 

757 

V   ■.  1  1  <  1 1 .  1U1  IO_U. 

3710 

4  S3  21.4 

157    11  I 

85.9 

8 

q 

1 1 

pi    •     f       £               1  , 

522 

21.5 

II  45 

83.9 

IO 

12 

x3 

1  nipT  nt  n  /^ln^fpi- 

653 

21.7 

II  40 

83-3 

5 

IO 

12 

riii'of         n     .I        t                    *-U  1 

658 

3711 

4  53  27-1 

131  11  8 

350-1 

9 

8 

J3 

638 

3712 

4  53  5°-3 

158  55  9 

148.8 

1* 

J4 

15 

r fii-imc  flip  mir>lpiic  r»T  a  ct-tifill  npmilg 

512 

3713 

4  53  56-9 

133  26  52 

338-7 

30 

8' 

IO 

804 

37H 

4  54  H  i 

106  32  45 

276.7 

7 

11  = 

=  11 

651 

37IS 

t  55  5-1 

139  43  IO 

1 1 1.7 

12 

7 

IO 

B  8ai 

744 

4-3 

42  40 

III.O 

IO 

8 

9' 

526 

3716 

4  56  i5-° 

156  43  56 

761 

19.1 

43  45 

657 

3717 

4  56  22.6 

129  49  16 

196.9 

IO 

IO 

1 1 

035 

7718 

A   ^6  2A.1 

126  23  28 

166.1 

10 
J 

8 

663 

9 

3719 

4  58  12.2 

157  29  36 

250-t- 

512 

2 

3720 

4  58  3°-5 

105  40  30 

149.6 

20 

8 

IO 

651 

3721 

4  58  5i-5 

170  55  12 

216.9 

2* 

O 
O 

9 

Very  neat  star  ;  Pos  216.7,  216.5,  217.6   



670 

3722 

4  59  J5-2 

164  32  25 

146.8 

20 

9'  = 

=  9' 

5H 

3723 

4  59  26.7 

109  59  12 

54-3 

9 

IO 

652 

4 

3724 

4  59  3i-2 

146    2  15 

272.3 

1^ 

10  = 

:IO 

520 

5    0  10-5 

98  53  38 

84.6 

25 

7' 

IO 

2.  649 

758 

3725 

5    1  23.7 

129  52  38 

140.8 

30 

9'-- 

=  9' 

754 

3726 

5    1  40.8 

135  53  29 

66.8 

15 

9 

9 

805 

3727 

5    3  2.3 

109    6  40 

32.3 

2 

9 

IO 

652 

3728 

5    3  3-2 

131  27  4 

255.0 

12 

6 

1 1 

B.  881 

628 

262.2 

14 

6' 

1 1 

Pos  262.7,  261.7.    Micrometer  set  to  2550.  The 

M1861 

754 

error  is  so  very  great  that  I  can  hardly  suppose  it 
to  have  been  committed.    No  doubt  the  microm. 
must  have  been  read  io°  wrong  in  f  628. 

3729 

5    3  12-9 

135    3  4 

231.8 

IO 

9 

IO 

527 

15.2 

3  54 

227.7 

IO 

10  io4- 

639 

373° 

5    3  561 

125  30  15 

336.9 

IO 

12 

663 

9 

184 


REDUCED  OBSERVATIONS  OF 


Xo. 


3731 


3732 
3733 
3734 
3735 

3736 

3737 
3738 

3739 
3740 

374i 
3742 

3743 


3744 
3745 

3746 
3747 
3748 
3749 
3750 

3751 
3752 

3753 

3754 
3755 
3756 

3757 


3758 
3759 
3760 

3761 

3762 
3763 

3764 


E  A.  1830.0. 
h.    m.  s.  d. 


4  5^-8 
54-3 

5  23.3 

6  3-7 
6  15.0 

6  38.6 

7  I0>7 
13.9 

7  18.6 

7  2fi-5 

8  6.3 

8  54.2 

9  8.5 


5  9  281 
5  10  10.2 

5  10  45'i 
49.9 
5  11  21.4 
5  11  50.6 
5  12  - 
5  11  52-6 
5  12  1.4 
5  12  36.4 

5  13  ~ 
5  13  i-° 
5  13  10.2 

5  H  8.9 
5  H  48-3 

5  J5  J3-7 
17a 

5  16  3-° 
5  16  19.0 
5  16  21.3 
23.0 
5  1 6  54-2 
5  i7  i5-5 

5  17  54-8 
5  18  40.4 

5  19  49- 1 

5i-3 
5  20  58.6 
5  21  7.0 
5  21  33.0 

5  21  23.9 
27.4 

5  23  "-3 
27.1 


N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

0  / 

 — 

146  6 

4 

297.9 

8 

9 

6 

7 

0 
y 

I  x 

103  8 

59 

359-9 

2 

t' 
i 

9 

117  22 

5i 

216.5 

80 

g 

_  g 

169  37  30 

in. 5 

9 

9 

i33  5 

4 

200.5 

10 

122  6 

34 

153-3 

6 

9 

—  9 

7 

32 

151.9 

6 

0 
0 

8 

147  47 

36 

320.7 

15 

9 

12 

126  15 

1 

303.5 

r5 

9 

12 

145  3° 

54 

7-7 

15 

138  s 

4 

277.4 

2 

9 

9 

126  50 

59 

284.7 

3° 

7 

8' 

168  31 

29 

115. 8 

c 
0 

10 

145  46 

2 

254.0 

7 

1.4 

150  10 

37 

122.8 

4 

9 

10' 

10 

46 

I20.8 

3 

9 

10 

100  55 

54 

92.4 

15 

8 

=  8 

128  9 

14 

281.7 

10 

1 1 

124  12 

7' 

10 

108  42 

10 

I7.2 

30 

6 

=  6 

162  16 

22 

3 

8 

8' 

157  46 

1 

IO3.7 

9 

1 1 

152  37 

283.3 

5' 

1 1 

120  14  43 

T  C 

*  3 

10  = 

=  10 

in  25 

5 

295.3 

3 

5 

10 

i*3  34 

24 

319.4 

25 

9 

10 

"4  57 

8 

JQQ— J— 

A 

6 

10 

i*5  53 

21 

T  7/1  6 

12 

8' 

9 

53 

26 

1744 

15 

9 

10 

160  8 

12 

134.6 

18 

10  = 

=  10 

152  7 

29 

286.1 

20 

8 

13 

148  55 

57 

I7O.3 

20 

9 

1 1 

56 

57 

172.2 

18 

g 

121  55 

12 

272.  Q 

18 

7' 

1 1 

101  28 

22 

$  J93-5 
I  88.3 

12 
40 

9 
9 

9  + 
13 

137  25 

48 

10 

10' 

109  50 

7 

3J5-3 

15 

7 

9 

125  29 

43 

£  271.6 

20 

6 
6 

7 
1 1 

30 

28 

S  217-3 
I  268.6 

IO 

20 

7 
7 

7' 
1 1 

no  54 

21 

145.9 

70 

4 

13 

142  28 

2 

285.8 

35 

8' 

8' 

122  34 

2 

212.7 

25 

6' 

13 

133  31 

25 

256.2 

15 

8 

9 

31 

15 

254.6 

12 

9 

10 

150  15 

26 

271.8 

6 

1 1 

13 

15 

16 

270.8 

3 

10' 

J3 

Remarks. 


Synon. 


Sweep. 


k  Leporis ;  Pos  359.3,  0.7,  359.8 

Both  fine  yellow  

A  RA  =6.5  

Neat  star   

Pos  1 54.1,  154.1,  151-8  

Fine  double  star  


A  very  neat  D  %  

Fine  star.    Large  ^  yellow  ;  small  blue  ;  R  A  by  an 
auxiliary  star,  and  liable  to  error. 

A  R  A  =  14' .0  ;  large  star  single,  and  very  yellow 

Very  delicate   

Pos  121. 9,  123.7  

Elegant;  Pos  121.7,  119.9  

Pos  92.3,  92.6  ;  fine  

Very  neat  


Superb  star;  Pos  17.3,  17. 1  . 
[Lacaille's  RA  is  im  greater]. 


Fine  double  Hj  near  a  Reticuli 


Most  beautiful  double  star,  but  too  late  for  a  good 
measure. 


A  very  fine  D  star.    Triple;  the  3d  is  in  the  same 
exact  line,  10  m,  dist  30" 


Chief  star  of  a  large  cluster 


Pos  193.1,  193.9  JTriple 


Pos  316.3,  314  3  • 


Fine  triple  star 


I  Pos  217.3  by  ^wo  coincident  measures  , 


/3  Leporis  ;  A  R  A  =  2'.  5 
(0  Pictoris)  fine  star.    A.  20 
Delicate   


Difficult  (dist  probably  underrated) 


2.  661 
L.I753 


L.  1759 


L.1780 

B.  905 
B.  908 


a.  170 
L.1831 


A.  641 


L.1827 
2.  710 


A.  659 

B.  961 

M2008 


521 
520 
757 
5" 
670 
639 
645 
644 
665 
661 
521 
805 
661 

670 
521 
756 
524 

758 
659 
E 

652 

5i4 
522 
524 
645 
647 

663 
530 

659 
651 
75i 
756 
664 
665 
644 

758 

527 
652 

662 

663 
652 

525 
644 

804 

528 

756 

524 


DOUBLE  STARS. 


185 


No. 

E  A.  1830.0. 

N  P  D.  1830.0. 

b. 

m.  s.  d. 

0      1  11 

376S 

5  23  25.0 

109  33  40 

3766 

5 

25  14.9 

107  56  34 

3767 

5  25  28.5 

137   12  31 

30.2 

12  49 

5 

25  50.4 

T 17    1  6  11 

1 3X  z"  31 

64.4 

25  13 

3768 

5 

26  2.5 

156  44  10 

5-4 

43  5i 

3769 

5 

26  22.6 

130  29  49 

3770 

5  26  30.8 

114  27  43 

3771 

5 

28  52.4 

J59  !5  35 

3772 

5 

29  16.9 

121   33  52 

3773 

5 

29  30.3 

172  27  13 

3774 

5 

29  34.0 

146    6  58 

3775 

5 

29  34.9 

i59  16  5 

3/7" 

5 

30  4.2 

T  T  7    7  7    1  8 

lll  3^  i° 

1777 

il  1 1 

5 

30  - 

7.778 
SI  1° 

5 

30  21.7 

145    0  0 

3779 

5 

30  25.6 

157    0  50 

3780 

5 

32  - 

i°7  57  — 

378i 

5 

32  9.6 

131  23  17 

3782 

5 

32  52.2 

131  18  2 

3783 

5 

33  2.8 

37*4- 

5 

33  2i-9 

T  n  ft   in   1 8 

37-3 

3785 

5 

33  3°-9 

104  21  39 

3786 

5 

34  i-3 

J43  35  55 

3787 

5 

34  24-3 

144  40  3 1 

24.4 

39  56 

3788 

5 

34  27-8 

116  26  28 

1780 
il°y 

5 

34  5°-3 

140  13  0 

379° 

5 

35  4-6 

157   0  10 

3791 

5  36  i-9 

no  45  32 

3792 

5  36  8.2 

149  10  27 

10.0 

9  42 

3793 

5 

37  24 

138  19  50 

3794 

5 

37  44-i 

124    1  59 

3795 

5  38  38-9 

166  27  9 

3796 

5 

39  53  4 

159  11  22 

3797 

5 

40  - 

136  22  — 

3798 

5  4°  13-4 

114  33  19 

13.6 

34  3 

5  4°  39-9 

103  25  28 

3799 

5  4i  i-5 

108  45  58 

Position. 

349-4 
154.8 
219.9 
225.7 

173.8 

172.7 

28.3 
30.9 
271.8 
271.3 
10.0 

72.9 

226.9 
275-5 

2I± 
228.8 
162.3 

349-3 
103.6 

343-5 


136.3 

63-5 
262.1 

5i-3 
48.6 

120.9 
92.6 
243.3 
241.5 
151. 3 
1.1 
i8o± 

54.8 
148.8 

145-7 
102.8 
266.3 
67.3 

i8o± 
304.3 

44-4 
359-3 

44.4 

132.8 

175-4 
65.9 
64.6 
120.9 
149.5 


Dist. 

Magnitude. 

15 

10  10 

25 

_  /  

3  12 

25 

6  14 

25 

5"  12 

12 

8  8 

10 

9  9+ 

10  11 

2 

10  11 

4 

10  11' 

4 

io'  12 

12 

7  13 

3 

11  13 

5 

io'=io' 

15 

9  IO 

II  14 

4 

II'  12 

30 

CT  S 
51.5 

6'  0' 
0  9 

12 

IO  12 

2 

io'  12 

.  . 

7,7,8,8,8 

18 

9  11 

25 

10  12 

7'  IO 

-  1 

35 

7'  IO 

O  II 

20 

IO  IO 

12 

IO  II 

10 
J 

8  10 

3° 

8  10 

25 

7'  9 

9  9 

9 

8 

8  9' 

18 

9  12 

15 

8  12 

12 

7  " 

25 

7  13 

60 

5  12 

9 

8'  14 

12 

13 

12 

14 

18 

13 

20 

13 

25 

12 

50.5 

8  9 

20 

9  9 

18 

8  9 

20 

IO  IO 

25 

9  9' 

Remarks. 


a  Leporis  

The  following  and  larger  of  two   

A  star  6  m  precedes,  making  with  the  large  the 
double  f  A  21. 

Pos  173.7,  173-9  [Mr.  Maclear's  observations  give 
this  R  A  the  preference]. 

Fine.  [There  seems  to  be  a  mistake  of  10".  in  this 
R  A.    It  is  marked  as  double  in  the  Brisb.  Catal.] 

Involved  in  a  thick  nebulous  mist  like  dust  

Forms  nucleus  of  a  bright  nebula  

Measured  past  merid  

Extremely  delicate ;  a  fine  object  

In  a  cluster  

Pos  277.0,  273.8,  275.7  

Difficult   

Triple  or  quadruple.    In  a  cluster,  Class  VII  

Epoch  1834.947  

The  large     B  994,  not  far  distant  to  the  south  .... 

Probably  close  multiple,  being  described  in  J  760  as 
a  nebula. 

Quintuple  6th  and  7th  classes  Zone  Review  

Pos  52.1,  50.6  

Elegant.   Pos  48.6,  48.7.    Obs  makes  the  minute  of 
R  A  32. 

Has  a  #  7  m,  3'  south   

Fine  star  

The  second  of  2  stars  9  m,  the  chief  of  the  great 
clustering  region  of  the  Nubecula  Major. 

A  neat  double  star  

A  star  7  m  3'  sp  and  one  6'm,  6'  nf  

Very  fine  object  

Chief  star  of  a  cluster  

A  R  A  z=  13*0  (y.  Montis)  

J  Septuple,  or  multiple.  The  chief  star  in  the 
}■  centre  of  the  great  looped  nebula  in  the  Nubecula 
j  Major   

J 

Mean  epoch  1836.009   

Pos  63.0,  66.3  

[Struve's  magnitudes  are  7,  10]  

A  very  elegant  double  star  

~3~i 


Synon. 

A.  673 

B.  973 

B.  976 
A  22 


L.1944 


L.i  946 


L.1972 
L.1967 
L.2037 


B.1038 


S.  801 


Sweep. 

652 
652 
527 
805 

804 

528 

654 
522 
754 
772 

53° 
657 

535 
668 
520 
657 
769 
E 
521 
658 

E 

772 
772 

75i 
805 

527 

757 
765 
521 
520 
530 
762 


652 
664 
665 
762 
663 
746 


653 
E 

640 
530 

757 
652 


186 


REDUCED  OBSERVATIONS  OF 


No. 

R  A.  1830.0. 
h.    ra.  s.  d. 

N  P  D.  1830.0. 

0     /  // 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

1800 
j 

5  41  28.5 

146  56  24 

227.8 

6 

1 1 

12 

665 

3801 

5  41  44.8 

136  39  42 

*y  j  j 

30 

5' 

14 

B.  1043 

8o<; 

3  802 

5  42  5.6 

145  47  23 

■504..  I 

4 

8' 
0 

I  I 

M.  2172 

520 

3803 

5  42  — 

114  C  <  — 

I  Id.  : 

20: 

7 

IO 

E 

3804 

5  4-3  38-5 

I02  49  36 

50.6 

IO 

9 

12 

757 

•?8oc 

5  44  40.2 

133  33  25 

I25.8 

4 

9 

528 

4.0.4 

33  3^ 

120.  ? 

7  J 

5 

IO 

804 

3806 

5  45  7-3 

129  30  1 

II4..C 

12 

10' 

=  io' 

772 

7807 

5  46  15+ 

131  43  50 

267.7 

4 

7 

J3 

A  very  fine  object.    The  R  A  is  only  a  rough 
app  roximati  on. 

772 

3808 

5  46  47-2 

147  41  8 

3O9.O 

3 

11 

=  11 

665 

3809 

5  47  - 

176  24  — 

224.3 

12 

9' 

12 

A  R  A  —  1,4  s  r        T?    A    TtiflT    Hp    Qpvpral  minntp^ 

i—X  j.v  n  —  1    1  _j.  •             iv    xi.    11 1  ct y      L/t     oc v vi ui  uiuiut^s 

wrong,  as  I  could  get  no  zero  stars  in  this 

761 

(bis) 

3810 

5  47  9-7 

151  10  59 

I70.3 

30 

y 

j  1 

756 

3811 

5  47  ^7-o 

115  13  46 

245± 

20 

8' 

9 

646 

3812 

5  47  28.5 

149  53  42 

aj 

9 

IO 

Pos  189.3,  189.8;  the  first  measure  with  power  320 

664 

189.5 

.... 

764 

759 

3813 

5  47  54-3 

157  48  32 

313.6 

30 

8 

3814 

5  47  55-7 

164  55  32 

1 74. 1 

3 

10  : 

=  10 

746 

3815 

5  48  28.5 

155  54  56 

140+ 

40 

IO  . 

=  10 

761 

3816 

5  48  39-9 

137  59  47 

177.9 

25 

7 

J3 

B.  1080 

527 

40.9 

59  28 

178. 7 

20 

7 

*3 

526 

3817 

5  49  2I-4 

170  26  54 

229.0 

20 

9 

10 

668 

3818 

5  5°  34-7 

117  20  43 

169.3 

15 

12 

769 

9 

3819 

5  5i  29-5 

125  18  19 

104.4 

30 

4 

14 

(y  Columba)  delicate,  bears  a  little  illumination  

A.  746 

662 

3820 

5  52  39-3 

159  56  37 

96.3 

j  J 

7' 

IO 

L.21 16 

75i 

40.0 

55  55 

748 

40.1 

56  25 

in. 3 

30 

657 

7 

IO 

5  53  22-7 

104  32  10 

86.0 

25 

1 1 

2.  832 

757 

9 

3821 

5  53  36.1 

in    0  27 

212.0 

25 

9' 

647 

9 

3822 

5  53  36-1 

143  26  45 

$  3°4-3 
(  !33-4 

70 
20 

rt 
0 

7 

7 
1 1 

A  and  B  J 
±5  ana  U  J 

Jj.2104 

765 

37-5 

26  52 

*  3°4-5 

60 

7' 

7 

g 

525 

(  136.6 

1  c 

0 
i! 

J3 

s 

3823 

5  53  58.9 

121    3  39 

i3i-5 

Pos  132.8,  130.3.    Both  stars  orange,  or  even  red  ; 
very  decided  colours.     (Compare  this  with  the 
next  observation.) 

535 

3 

9 

=  9 

60.7 

3  3° 

131. 8 

"Xh 
j  2 

9 

=  9 

Pos  133.3,  i3°-4-    Both  stars  pale  yellow   

...... 

645 

3824 

5  54  33-5 

140  24  25 

273.1 

10 

14 

762 

5 

3825 

5  55 

117  25  43 

342.8 

25 

7' 

1 1 

.      ,      •  *i 

7 

53i 

3826 

5  55  35-8 

131  28  54 

149. 1 

12 

10 

13 

772 

39-5 
5  56  21.2 

27  40 
131  10  3 

i5i-3 
242.3 

20 
30 

10 

9' 

12 
9' 

754 
772 

3827 

3  Oio 

5  56  36-4 

H3  55  '4 

132.5 

'5 

10 

^20 

9 

36.6 

54  58 

133.7 

12 

10 

1 1 

521 

3829 

5  56  53-° 

152  46  21 

353-8 

12 

524 

15 

9 

5  57  9-3 
5  58  44-5 

I26± 

»-7 

8 

2.843 

757 
769 

3830 

104  21  25 
118  39  43 

8 

10 

11 

9 

=  9 

46.0 

40  48 

Elegant.  Pos  2.6 ,  0. 5  ;  dist  probably  under  estimated 

53i 

*-5 

4 

8' 

=  8' 

3831 

5  58  49-3 

131    9  8 

138.2 

Pos  138.2,  138.3;  micrometer  set  to  134.5  the 
measure  cannot  be  borne. 

772 

3 

9 

=  9 

52.5 

J34-5 

754 

9  9 

2 

9 

=  9 

3832 

5  59  9-5 

123  16  23 

146.9 

9' 

=  9' 

662 

15 

3833 

5  59  26~ 

113    5  - 

6 

I  I 

E 

DOUBLE  STARS. 


187 


No. 

R  A.  1830.0. 

N  P  D.  1830.( 

b. 

m. 

s.  d. 

0  / 

0 

3834 

5 

59 

46.7 

135  4 

3«3S 

6 

0 

6- 

113  7 

6 

0 

20.0 

138  26 

30 

3836 

6 

2 

32.2 

*39  54 

5 

J    J  / 

6 

ZZ.1 

j  j  j 

TAC  C6 

'43  3" 

3  5 

6 

4 

19.3 

103  6 

2 

3838 

6 

+ 

47.2 

154  58 

53 

3839 

6 

6 

14-7 

108  16 

16 

3840 

6 

8 

25.6 

120  27 

28 

3841 

6 

8 

31.1 

148  27 

13 

3842 

6 

8 

32.5 

112  8 

49 

3843 

6 

9 

18.6 

150  J7 

5 

21.2 

17 

31 

3844 

6 

22.6 

J59  39 

1  c 

384s 

6 

9 

54-" 

112  39 

CA  7 

54-/ 

3846 

6 

10 

T 

I  "30  2 
*  jy 

J.  < 

3847 

6 

1 1 

25.O 

104  27 

C  T 

g 

44-9 

155  29 

J7 

46.6 

29 

25 

40  .U 

29 

0 
0 

3848 

1 2 

1 1.5 

136  59 

34 

I3.3 

59 

3 

c. 

D 

*3 

5b-3 

'49  8 

5 

5 

'4 

14.7 

12^ 

43 

25 

3850 

6 

14 

26.7 

104  31 

29 

3851 

6 

15 

35-5 

151  33 

51 

3852 

6 

15 

43.0 

134  43 

29 

6 

16 

20  c 

102    5  2 

2Q.8 

^2 

28 

3853 

6 

16 

IT?  T7 

3 

3854 

6 

16 

59-4 

144  26 

*3 

62.5 

26 

3 

3855 

6 

17 

4.Q.Q 

164  26 

35 

3856 

6 

18 

A.  T 

TIC 

9 

3857 

6 

iS 

18.3 

126  37 

II 

*9 

38 

— t- 

3858 

6 

J9 

34.1 

123  56 

6 

3859 

6 

J9 

40.8 

n6  43 

28 

3860 

6 

20 

19.2 

130  52 

41 

22.2 

5* 

28 

3861 

6 

20 

51.2 

148  s 

5i 

3862 

6 

21 

39-5 

157  30 

1 1 

3863 

6 

22 

18.6 

112  29 

35 

3864 

6 

22 

48.7 

104  51 

5 

Position. 

Dist. 

Magnitude. 

245.9 

I* 

6 

10 

8 

1 1 

343-5 

2? 

7 

7' 

294.1 

6 

10 

10 

14. 1 

12 

8 

!3 

286.1 

12 

8 

12 

33t-4 

5 

9' 

I0' 

306.4 

4 

1 1= 

II 

229.7 

8 

10= 

:io 

165.8 

4 

10 

12 

215. 1 

18 

10 

10' 

324.7 

'5 

9 

9' 

321.6 

15 

8' 

90.7 

8 

9 

J3 

51-3 

25 

Q 

12 

5*-7 

25 

0 

12 

67.3 

3 

9 

10 

48.3 

6 

g 

1 14.2 

25 

7' 

c 
0 

ixz.i 

20 

8' 

9 

1 12.8 

25 

8 

9 

318.6 

3 

/ 

9 

9' 

A 
T 

10  = 

■  IO 

223.6 

QO 

y 

6 

7 

^o.6 

to 

7' 

10 

52-3 

39-4 

7 

7' 

43-3 

10 

9 

*3 

80.7 

ie 

3 

9' 

1 1 

6.3 

3 

9 

296.3 

25 

7 

Z0J.0 

J5 

7 

12 

77.0 

12 

9 

1 1 

128.8 

10 

_/ 
9 

1 1 

128.1 

12 

9 

12 

82.3 

6 

i  — 

10 

4.8 

30 

7 

10 

257.6 

12 

7' 

12 

261.3 

12 

6 

!3 

313.8 

3 

7' 

8 

252.9 

15 

9 

9' 

223.0 

12 

7' 

12 

223.9 

7 

9 

10 

58.3 

2 

9'= 

=  9' 

6 1. 1 

2 

9' 

9' 

276.9 

12 

8 

1 1 

121+ 

2 

6' 

9 

43-3 

20 

i 

12 

Remarks. 

247.5,  244.3  Power  320  ;  very  fine  if.  

Class  4,  zone  review   

Superb  double  star.    Pos  342.6,  344.5   

j  Triple   

Pos  330.5,  332.3  ;  L  red  S  very  green  

Strongly  suspected  to  be  double   

A  third  more  distant  

Large  star,  ruddy   

Neat  star  

Marked  as  "double"  in  Brisb.  Cat  

(??  if  A.  26)  

ARA=  4!.o  

Pos  320.3,  3   

—  Possibly  =  A.  27   

Large  star,  yellow.  [If  this  be,  as  I  suppose,  iden- 
tical with  the  star  measured  with  the  equatorial 
the  P  D  in  this  obs  must  have  been  misread  5'.] 

Large  star,  ruddy  

An  elegant  double  j)j  .     A  third  *  near  

A  third     9  m,  exactly  in  the  line  

Viewed  past  merid.  The  three  stars  are  positively 
not  in  a  straight  line.  The  3d  star  7' m.  This  obs 
makes  the  degree  of  P  D  127,  but  as  it  was  looked 
for  and  found  by  126,  that  must  be  the  true 
degree. 

Pos  314.7,  312.9.  Fine  object.  A  star  6  m  pre- 
cedes to  the  south. 

Pos  223.3,  222.6  

Neat  star  ;  R  A  precarious   

A  beautiful  D  star ;  past  merid  


Synon. 
B.1132 
A.  23 

2.875 


B.1201 


B.1211 


2.  903 


L.2267 
B.1229 


L.2274? 


L.22S 


Sweep. 

805 
E 

762 
526 

521 

757 
539 
677 
535 
5i8 
768 
756 
664 
657 
532 
768 
762 
676 
518 
639 
515 
527 
544 
764 

772 
E 

676 
756 
528 

757 
676 
804 
521 
767 
672 

544 
540 
801 


663 

53° 
772 
529 
664 
764 
522 
768 
676 


188 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1880.0. 
b.  ra.    s.  d. 


386S 
3866 
3867 

3868 

3869 

3870 

3871 
3872 
3873 


3874 
3875 

3876 
3877 

3878 
3879 


3880 
3881 
3882 
3883 


3884 


3885 
3886 

3887 
3888 
3889 
3890 

3891 

3892 


6  22  51.4 
6  23  21.8 
6  24  20.5 

6  24  37.7 

6  26  11. 5 
19.6 
6  26  40.1 
43.6 
6  27  32.1 
6  28  10.1 
6  28  30.5 

34-4 
6  28  54.9 
6  29  25.0 

25.5 
6  29  28.2 

31.7 

6  29  31.8 

33-4 
6  31  19.3 

21. 1 
6  31  31.9 
6  31  54.1 

56.0 

56.2 
6  32  29.9 
6  33  28.2 
6.33  46.2 
6  33  58.7 
6  34  5-9 
7-3 


6  34  17.0 
6  36  28.5 


35-5 


6  37  17-5 
6  37  45-5 
6  37  56.6: 

6  38  59-3 
6  39  - 
6  39  26.2 

6  39  - 

6  41  21. 1 

23.5 


N  P  D.  1830.0. 
011 

Position. 

Dist. 

Magnitude 

107  42  43 

64.3 

18 

9' 

1 1 

114     2  10 

112+ 

3 

8 

12 

I38  24  20 

278.6 

30 

9 

1 1 

16c    7  til! 

141. 7 

18 

7 

13 

51.8 

25 

7 

14 

121  54  47 

249.3 

25 

7' 

9 

54  33 

30 

6' 

9 

165    1  40 

13.8 

25 

8 

'3 

1  30 

1 1.4 

18 

7' 

13 

119  29  43 

353-1 

10 

7' 

8 

l69  53  43 

25.1 

19.4 

10 

10 

147  29  7 

9 

10 

29  15 

289.6 

18 

8 

12 

108  31  20 

260.9 

20 

7 

8' 

148  37  51 

224.5 

3 

6 

12 

37  39 

232.0 

2j 

6 

12 

126  38  57 

297.3 

20 

6 

13 

38  24 

292.8 

18 

6 

*3 

112  28  30 

326.6 

15 

0 
a 

12 

28  56 

338-5 

15 

8 

11 

112  53  32 

351. 1 

12 

9 

9 

CI  *2< 

j  j  j  j 

T  C 

J 

8' 

9 

125  48  13 

12.4 

8 

11 

12 

160  29  40 

97-5 

12 

10= 

10 

29  40 

95-4 

18 

9  = 

=  9 

29  49 

102.4 

15 

10= 

10 

156    8  11 

262.0 

2 

1 1= 

1 1 

130  27  4 

157-3 

30 

8 

12 

134  54  35 

332-5 

20 

7' 

11 

J34  53  5° 

56.8 

5 

10 

1 1 

138    4  37 

316.8 

20 

6 

9 

4  5 

321.8 

20 

5' 

8 

145  12  3 

275.7 

25 

7 

12 

128  1 2  2 5 

279.3 

6' 

7 

14 19 

274.5 

8 

7' 

8 

159  56  55 

174.0 

4 

9' 

12 

152  38  41 

341.0 

12 

9 

1 1 

132  22  54 

257.1 

3 

10 

1 1 

168  46  6 

1 1 3.4 

7 

1 1 

140  17  - 

266.1 

42.8 

6' 

8' 

162  37  15 

36-9 

12 

9' 

12 

120  47  — 

222.0 

5.0 

6 

10 

170  56  22 

32.9 

20 

9  = 

=  9 

57  33 

31. 1 

18 

9  = 

=  9 

Remarks. 


Synon. 


£  ^  I  Triple.    Sky  dull   

A  fine  double  star  

Distance  by  oblique  transits  

Class  III  

Blotty  

v  Canis  Majoris.    IV.  81  

Pos  226.3,  222.6.    Power  320  

Pos  232.5,  231.5  ;  (ji  Pictoris)   

Very  neat  star  

Pos  by  MS  222.8,  but  this  contradicts  a  diagram 
made  at  the  time. 

Triple.   A  3d  star,  14  m  dist  25*  

One  of  a  small  group  

ARA  =  3'.o   

Well  defined   

Elegant  D  star.    Pos  261. 1,  262.8  

The  preceding  of  two  

The  following  of  two  

V  Puppis,  L  yellow,  S  fine  blue.    Pos  316.2,  317.3 

L  pale  yellow,  S  pale  blue.    Pos  321.7,  321.9  .... 

[N.B.  The  equatorial  measures  make  the  pos  321.8 
as  much  as  4°  wrong,  therefore,  probably,  there 
has  been  a  mistake  of  50  committed  in  reading  the 
micrometer  in  this  obser.] 

Large  star,  red   

Obs  makes  the  minute  of  P  D  =  8,  but  there  can 
hardly  be  a  doubt  of  identity  between  this  * 
and  that  of  /  659,  one  or  other  being  5'  mis- 
read. 

Fine  star.  Pos  274.8,  274.3.  [There  is  no  doubt 
by  the  agreement  of  the  P  D  with  Lacailles  that 
this  obs  is  correct  in  P  D.  It  was  twice  found  in 
the  equatorial  by  this  P  D.] 

Pos  175.2,  172.8   

A  third  star,  10' m,  s  f  

1  RA  =  1C.5   

Mean  epoch  1836.495   

Mean  epoch  1838.018   

Pos  33.7,  32.1,  A  R  A  =  8\o   


L.2330 
B.1274 
L.2337 


a.  237 
B.1292 

B.1291 


B.1320 
+  1321 

A.  31 


L.2408 
L.2418 

A.  32 


L.2502 
B.i 340 

M.2677 


DOUBLE  STARS. 


189 


No. 


E  A.  1880.0. 
h.  m.  s.d. 


N  PD.  1830.0. 


Position. 


Dist. 


Magnitude 


Remarks. 


Synon. 


Sweep. 


3893 

3894 
3895 


3896 
3897 


3899 
3900 


3901 

3902 
3903 
3904 

39°5 
3906 


3907 
3908 
3909 
3910 
3911 
3912 
39J3 
39  H 
39IS 
3916 

39i7 
3918 

39i9 
3920 


3921 
3922 

3923 
3924 


6  41  31.4 
31.7 
6  41  56.3 
6  42  7.8 
8.6 

10.0 
6  44  24.1 

24.6 
6  45  30.1 

6  46  33.4 

6  47  49.3 

6  47  55-5 
6  47  59.8 
6  48  19. 1 


20.5 
6  49  1 1. 1 
6  49  24.5 
6  49  56.1 
6  50  2.8 
6  50  17.0 
6  52  11. 1 
6  52  35.0 

38.5 


6  S3  2.7 
6  53  8.3 
6  53  17.9 

6  53  19-5 
6  54  24.8 
6  54  29.2 

54  4°-3 

55  1.8 
55  5-8 
55  17-9 
55  *»-9 

6  56  57.2 
6  57  17.9 
18.6 
6  57  39.1 


40.5 
6  57  45.8 
6  57  59.1 

65.7 
6  58  0.6 
6  58  13.8 

18.8 


127  44  21 
45  3 
155  34  8 
137  37  36 

37  10 

37  *5 
118  31  38 

32  8 
133  28  43 

I04    1  35 

146  2  24 
170  28  33 

124  o  44 
io3  49  53 

50  14 

127  17  50 

112  25  24 

108    7  59 

174  58  12 

164    2  25 

125  12  3 
145  22  12 

22  3 


127  30  28 

105  5  11 

137  11  49 
155  42  26 
166  38  30 
140  27  45 

118  47  57 
113  15  30 

155  44  1 
120  53  23 

120  31  52 
158  15  12 
125    4  30 
4  19 

138  45  15 

44  43 
148  9  19 
150  37  27 

37  28 

119  26  22 
150  37  12 

37  22 


28o± 
200-t- 
212.7 
60.8 
62.3 

64.3 
i63± 
161. o 

79-3  : 

275-5 

306.8 
310.8 
284.7 
339± 

337.2 
218.8 
43.0 

49± 
235.8 
103.6 
268.3 

38.7 
220.5 


227.1 
297.1 
273.3 
60.9 
43.2 

47-7 
128.7 
315.6 
267.2 
102.3 

96.7 
318.8 
268.3 
255.4 
106.9 


102.7 
270.4 
236.9 
232.1 
197.8 
353-8 
357-7 


60 

5' 

20 

8 

12 

25 

_i 

1 

1 1 

25 

8 

10 

4U 

7' 

10 

T  P 

10 

10 

g 

Q 

7 

9 

T  r 

Q 

Ij 

10: 

=  10 

18 

9 

9 

6 

10' 

12 

2 

6 

11 

2 

4' 

10 

2 

6 

9 

20 

7 

11 

20 

8 

9 

10 

10 

10 

15 

9 

12 

4 

10' 

12 

15 

9 

12 

18 

9 

=  9 

20 

8' 

9 

20 

9' 

12 

3 

10: 

=  10 

8 

9' 

1 1 

30 

9 

12 

19.6 

7 

12 

6 

11 

12 

6 

9' 

10 

12 

7' 

J3 

20 

<?' 
0 

'3 

5 

10': 

=  10' 

4 

9' 

10 

6 

1 1 

12 

15 

9 

12 

15 

8' 

10 

5 

9 

9 

2i 
'■I 

9' 

9' 

8 

8 

12 

15 

8' 

12 

15 

7' 

13 

12 

9 

10 

20 

9' 

10 

18 

1 1 

1 1' 

Coarse,  very  unequal  

Pos  by  estimation  from  diagram   

L  orange,  S  contrasted  B  

Glimpses  of  a  3rd  star  strongly  suspected — dist  12* 
Pos  o°. 

L  orange,  S  blue  

A  star  8' m,  3'  n  p  

Very  delicate,  Power  320,  R  A  missed  and  deter- 
mined by  an  auxiliary  ^  >  therefore  precarious. 

A  delicate  and  beautiful  D  star.  Pos  mean  of 
275-3>  275-7- 

Fine  and  delicate   

fi  Cants.  Just  time  to  apply  the  triangular  aperture, 
but  not  to  measure  the  position.  Most  beau- 
tiful. 

Pos  mean  of  337.3,  337.1.    Beautiful  object  

Pos  239.3,  232.3   

The  obs  gives  53m  33^.3  for  the  R  A.  Either  the 
wire  has  been  mistaken  in  this,  or  the  minute  in 
one  of  the  two  observations.  The  former  is 
presumed  to  have  been  the  case. 

Neat  star  

A  R  A  =4<-75   

A  R  A  =  5s.o ;  dist  by  oblique  transits   

Two  more  bright  stars  in  field  

[Pos  probably  misread  io°]  

Pos  106.5,  I07-3>  106.6;  micrometer  set  to  103,  the 
measure  of 7*526  ;  it  cannot  pass;  I  suspect  this 
star  to  have  changed. 

Fine  star.    Pos  104. 1,  101.3  : :  

The  preceding  of  two  D  star,  in  a  rich  field  

A  third,  9  m,  nf  

The  following  of  two  D  stars,  in  a  rich  field  

~!Tc 


A.  845 

B.  1361 

2.  990 


L.2520 
2.  997 


S.  541 


B.1436 


L.2613 


659 
661 
515 

5*7 
544 

762 
769 

53i 

528 

757 

521 

670 
809 
676 


757 
801 
768 
675 
666 
672 

54i 
521 
520 


661 
676 

544 
766 
671 
762 
53i 
534 
766 
678 
535 
538 
54i 
809 
762 

526 
664 

756 
682 

53" 

756 

682 


190 


REDUCED  OBSERVATIONS  OF 


R  A.  1880.0. 
h.  m.    s.  d. 


N  P  D.  1830.0. 


Dist. 


Magnitude 


Remarks. 


Synon. 


39^5 


3926 

3927 
3928 


3929 


393° 


3931 
3932 


3933 
3934 

3935 
3936 

3937 
3938 

3939 
394.0 


3941 


39+2 
3943 

3944 
3945 


6  58  24.3 


6  58  45.6 
6  59  4.4 
6  59  24.4 

6  59  33-9 

36.1 

39-5 

7  o  28.7 
7    o  38.2 

38.2 

7    0  47.9 

7    1  - 
7    2  4-9 
33-4 


7  2  43.6 

7  4  5-6 
8.1 

7  4  42-2 

7  5  24-3 

7  6  19. 1 

7  6  38-3 

7  6  39-3 

7  6  39.8 

7  6  56.2 

7  7  i-3 


1.4 


7  7  25-3 
7    8  19.5 

7    8  30.2 

7    9  28-7 
28.8 


136  39  31 


166  55  2 
164  3  15 
124  31  28 

33  ± 

161  48  3 
48  2 
48  5 

102  54  22 
148  55  4i 

55  29 

103  43  18 

132   4  - 

167  32  50 
31  58 


109  29  17 
in  32  15 

31  25 
139  42  22 
163  29  3 
150  24  48 
112  36  59 
107  40  48 
120  41  1 
145  18  16 

150    6  59 


6  24 


123  22  52 
134  21  59 

152  44  26 
113    1  40 
o  47 


105+ 


288.6 
21.3 
158.8 
154.4 

238.7 
227.3 
236.9 
73.8 
76.2 

78.5 

f  2  54 7 
*  351-8 
40.9 
276.5 
276.5 


153.1 

229.5 
238.3 

96.6 
266.3 

29.1 
252.6 

246± 

95-4 
41.7 

313.8 


310.0 


31.3 

2IO± 

284.I 
70+ 
63.O 


20 

5 
3 

12 
12 
10 
12 

2 

2 
3 

12 
72.9 
6 


9  =  9 

5'  7 

8  9' 

9  " 
8'  10 
9  12 

10  10' 

7  7 


7  » 
8'  12 

8  10 


9  12 

8  9 

8  9 

9  10 
11'  13 
10'  10' 

7'  8' 

10  10 

9  12 


ii— 1  j 

5' 

9'  12 
7  8 
7  8 


In  the  best  moments  with  power  320,  satisfied  of  its 
being  double  ;  but  the  definition  to-night  is  bad, 
and  my  eyes  are  inflamed  with  a  cold.  Should  be 
re-examined. 

A  R  A  =  7  .0  

2  other  companions  np  and  sf   L.2612 

2  others  near  on  opposite  sides,  seen  too  late  for 
taking  place  directly. 

Chief  of  a  cluster  of  7th  class   

Fine  -X- ;  Pos  74.8,  774,  with  320  and  triangular  B.1475 
aperture. 

Pos  77.9,  79.3   A.  39 

Pos  253.3,  2-56.1  iTricle 

Pos  352.6,  351.1  $lnPle   

Mean  epoch  1836.001   B.  1473 

Small  star,  reddish,  or  purple    L.26 

[The  obs  gives  R  A  4"'  32s.i,  but  if  a  mistake  of  wire 
be  allowed  it  comes  out  as  here  set  down.  No 
doubt  of  identity  of  the  stars  with  each  other,  or 
with  L.  2689.] 

Pos  27.9,  28.7,  30.8   

Pos  41.7,  41.8  ;  both  yellow.     [Noticed  also  as  B.1507 
double  by  Rumker] — No.  5  of  his  list.    Is  also 
A  41. 

Pos  312.6,  315. 1  ;  exclusively  close.    I  think  this  is    B.  1508 
the  closest  double  j(c  I  ever  have  had  fairly  sepa- 
rated with  320  and  the  triangular  aperture.  With 
this  aperture,  however,  180  shows  symptoms  of  its 
being  double. 

Pos  309.3,  310.7,  307.1.  The  first  measure  taken 
with  320  and  9  inches  aperture  ;  the  second  with 
480  and  do.,  the  last  with  800  and  do.  With 
1200  and  the  whole  aperture,  the  angle  obtained 
was  305.3,  but  the  measure  was  uncertain,  as  I 
could  not  illuminate  the  field  sufficiently  to  see  the 
wires  well.  With  this  last  power  and  aperture, 
dist  =  ij  diam.  of  large  star.  Had  not  attention 
been  excited  by  the  beautiful  double  stars  occur- 
ring earlier  in  the  f,  I  do  not  think  this  would 
have  been  detected  (as  it  was)  with  180.  It  was 
a  mere  suspicion. 

Pos  estimated  from  diagram.    S  H«  distant,  and  very  B.1520 
small. 

A  third,  1 1  m  more  distant ;  Pos  276  +   

Large  star,  orange ;  small,  pale  blue   

L  very  high  yellow,  S  contrasted  blue  


DOUBLE  STARS. 


191 


No. 


E  A.  1830.0. 
h.  m.   s.  d. 


3946 

39+7 
3948 

3949 

395° 
395i 

395* 
3953 
3954 
3955 
3956 


3957 

3958 
3959 

3960 


3961 
3962 
3963 
3964 

3965 
3966 

3967 
3968 

3969 
397° 
397i 


7  10  9.2 

9-7 
10.2 
13.8 
7  10  40.0 

7  11  7-3 
7  11  35.1 

7  11  40.0 

7  11  58.0 

59-5 
7  12  6.9 
7  12  12.6: 

18.2 
7  12  23-3 
7  14  4°-3 
7  15  9-6 
7  15  12.0 

7  16  5-3 

1 1.1 

7  16  7-5 

9.0 

7  16  — 
7  16  13.6 
7  16  15.2 

7  16  — 
7  16  34.2: 

38.3 
42.7 
7  17  m-i: 
7  17  38-7 
7  17  38-8 
7  17  46-3 

7  17  47-6 
7  18  46.2 

46.7 
7  19  22.8 
7  20  19.8 

26.8 

7  20  57-7 
7-  21  0.5 
7  21  26.9 
7  22  22.7 


N  P  D.  1880.0. 


160  13  20 
13  12 

13  5 
13  13 

122  57  40 
126  48  50 
135   56  18 

114  33  48 

120  29  22 
29  49 

in  43  55 

140  42  24 
41  19 

H3  44  52 

163  38  45 

122  41  37 

155  54  19 
138  12  31 

12  13 
125  36  7 

35  27 

141  53  - 

164  19  10 

142  o  25 

138  14  - 
138  12  33 

J3  7 

12  30 

147  21  32 

146  27  39 

133  26  9 

110  41  21 

125  31  o 

126  57  27 
56  49 

145  14  56 
131  45  55 
47  18 

123  58  43 
135  17  23 
H7  35  35 

121  30  29 


Position. 

Dist. 

Magnitude. 

20 

5 

7 

206.0 

7  7 

25 

5 

200.7 
77  / 

18 

5' 

7 

3OO.3 

25 

5 

6 

286.I 

2 

11 

12 

211. 8 

70 

3 

8 

270.3 

IO 

8' 

10 

f  85.8 

8 

5' 

11 

I  73-3 

*5 

5' 

12 

79-9 

2 

8 

9 

80.0 

2 

8' 
0 

9 

168.3 

3 

9' 

=  9' 

67.6 

4 

10 

1 1 

65.3 

8 

9' 

11 

271.3 

15 

8' 

12 

323.1 

*5 

_/ 
9 

12 

92.3 

8 

9' 

11 

27.7 

25 

9 

10 

164.2 

8 

9 

1 1 

163.7 

4 

9 

195-5 

15 

8 

9 

194.4 

J5 

8 

9 

200.8 

15 

8' 

12 

13-5 

15 

7 

7' 

8 

1 1 

156.8 

2? 

8 

9 

158.6 

25 

7' 

9 

I56-5 

20 

8 

9 

248.8 

10 

9 

12 

104.7 

7 

8 

10 

257.5 

3 

10 

11' 

1  ?o-t- 
j  — 

A 
T 

10 

10 

307.2 

25 

6 

13 

137.8 

10 

i- 

=  7' 

140.6 

10 

7 

7' 

137.6 

25 

7 

15 

127.7 

25 

7' 

12 

130.6 

30 

7 

II 

224.8 

20 

8' 

9 

272.3 

2 

9 

11 

189.3 

l8 

9 

12 

50.4 

15 

7' 

8 

Remarks. 


y.  Piscis  Vol.    Pos  297.0,  297.1.  Fine  

ARA  =  3%o.  Pos  297.1,  296. g,  296.9   

Superb  double  star  

Pos  300.9,  299.7  ;  superb   

L  yellow,  S  blue  (tt  Argus  =  A.  43)   

^  q  j  Triple  ;  chief  of  a  fine  cluster   

Fine  double  star  

Fine  double  star  

Both  red ;  R  A  very  precarious  

This  R  A  to  be  preferred  

The  preceding  of  2  ;  R  A  ill  taken  

[The  place  agrees  with  that  of  A.  45,  but  it  cannot 
be  the  star  observed  by  him.] 

Fine  star  

Fine.    Pos  193.8,  195.0   

Double  nearly  in  parallel   

Points  to  a  coarse  D  star,  7'  or  8'  dist.    [Noticed  as 
double  by  Rumker,  No.  6.] 

Class  3 ,  zone  review.    The  preceding  of  two  

All  the  R  As  of  this  f  are  bad.    [The  following  of 
two  double  stars :  marked  as  double  in  B.] 

One  of  a  group  of  about  a  dozen  

The  first  and  chief  of  a  cluster  of  8th  class.  Pos 
estimated  from  diagram. 

Fine  star  

Pos  139.3,  142.0   

A  third  star,  8  m  prec  

Large  %  orange   

Large  star,  very  red.   [N.  B.  Both  Right  Ascensions 
re-examined  and  found  correctly  reduced.] 

A  3d      iini  near  

Fine  (is  A.  49.)   


Synon. 


Sweep. 


B.1530 
A.  42 


B.1536 

A.  905 

B.  i 542 


B.i  547 


B.1576 


B.1578 

B.  1582 
+  1583 


L.2790 
L.2801 

B.1602 


L.2815 


B.1622 


546 
523 
545 
673 
54i 
659 

544 

530 
678 

535 
768 
680 

525 
520 

547 
534 
766 

553 

526 
809 

54i 
E 

547 
525 

E 

680 

553 
526 

697 
520 
804 
768 


659 
661 
552 
804 

554 

841 

544 
764 

535 


192 


REDUCED  OBSERVATIONS  OF 


R  A.  1830.0. 
h.  m.   s.  d. 


NPD.  1830.0. 


Position. 

Dist. 

Magnitude. 

A  A  -Q 

18 

10  11 

44-3 

20 

9'  " 

39-5 

25 

8'=  8' 

76.2 

20 

5  10 

73-6 

30 

5'  9 

36.3 

8 

9  10 

..I 
322^ 

1S 

/  _/ 
9=9 

240.3 

3 

8'  11 

243.5 

3 

8  11 

330.3 

8 

9  10 

S  129-5 
i  327-i 

6 
5 

9  11 

9  '3 

132.5 

8 

9  11 

69.7 

12 

8  9 

92± 

9  11 

7J-5 

g 

69.3 

6 

10  =  10 

59-9 

10 

11  =11 

126+ 

10 

8  n 

326.7 

18 

8'  9 

699 

IT2.I 
j 

12 

8=8 

■joc  8 

c 
3 

10  II 

4  *3  I  7  "2 

X  255-9 

T  c 

60 

7  14. 

7  8 

86.3 

II 

9    9  + 

83.5 

1^ 

9  9 

85.5 

12 

10  10+ 

219.8 

50 

8  9 

40 

7  12 

295.9 

12 

9'  11 

300.3 

'5 

9  11 

a  3  c  8 

18 

10    1 1 

225.3 

18 

9  10 

345-3 

30 

8  9 

206.7 

15 

9'  10 

122.4 

15 

9'  9' 

16.1 

20 

9  9 

f    12. 1 

I  206.8 

12 
25 

8  11 
8  13 

249.7 

5 

10  11 

35°± 

25 

7  8 

244.8 

12 

6'  12 

248.6 

15 

6  13 

Remarks. 


Synon. 


3972 


3973 

3974 

3975 
3976 

3977 
3978 
3979 

3980 
3981 
3982 


3983 
3984 
3985 


3986 
3987 
3988 

3989 

3990 
3991 
3992 

3993 

3994 
3995 

3996 


7  22  28.6 
29.5 
30.5 


7  23  48.3 
50.0 
7  24  25.9 
7  24  41.3 
7  25  49.6 
52.1 
7  26  + 

7  26  31.0 

33-5 
7  26  31.7 
7  26  34.7 
7  27  31. 1 
31.7 
32.0 
7  27  52.8: 
7  28  6.5 
7  28  32.9 

7  28  49.6 


7  29  14.8 
7  29  16. 1 
7  29  29.3 

35-9 

7  29  34.6 
7  30  57.3 
7  31  20.4 

27.5 
7  31  25.7 
27.1 

7  33  3°-3 
7  33  32-9 
7  33  58-1 

7  34  9-3 

7  34  33-° 
7  36  10.8 
7  37  38-1 
7  38  23.0 
26.4 


152  11  53 

11  16 

12  6 


132  57  16 

57  47 
no  34  40 
102  30  41 
144  56  41 

56  55 
171  18  - 

158  33  21 

33  22 
151  15  4i 

117  49  1 
126   4  1 

3  52 

4  8 
147  12  32 

138  51  9 

118  o  9 

104    6  50 


103  29  1 
144  48  8 
157  47  4° 

47  4° 

140  28  50 
168  49  17 
138  28  30 

28  22 
150  55  27 

54  46 

137  20  1 
164  40  23 
133  35  3i 
150    2  46 

138  39  45 

in  42  41 

104  17  38 

i74   9  - 
7  16 


A  third  star  13m  make  an  obtuse  angled  and  nearly- 
isosceles  triangle  with  these  two.  It  does  not 
appear  to  have  been  noticed  in  either  of  the  other 
observations,  in  which  the  star  must  have  been 
ill  seen,  as  is  evident  by  the  magnitudes  affixed. 

Pos  77.0,  75.5  ;  L  yellow,  S  very  fine  blue  

L  yellow,  S  blue ;  A  R  A  =  2s      (<r  Argus)  .... 

L  pure  white,  S  a  very  remarkable  brick  red  

A  neat  double  star  

Very  neat.    Pos  242.7,  244.3   

R  A  estimated,  being  too  late  for  transit  

I  Triple  

A  star  6mnf  

The  pos  probably  read  io°  wrong   

Ill  defined.    The  first  of  3  st  in  a  line  

Triple.  A  3d  star  n  f  

Coarsely  triple  R  A  7  33  32.9,  Nisi  28".  Lacailles 
R  A  agrees  with  the  latter  alternative. 

A  fine  D  H<  1  chief,  or  almost  so,  of  a  splendid 
cluster.  PD  by  obs  1030,  but  the  cluster  is  VIII. 
38,  and  104  is  the  true  degree. 

Chief  of  a  large  fine  cluster  of  small  stars  

j  Triple  

Transit  missed.  Viewed  and  measured  after  passing 
merid. 

Pos  85.3,  85.6;  with  320  and  whole  aperture,  with 
which  it  is  finely  separated. 

Large  %  red.  N.B.  The  right  Ascensions  in  this  f 
are  liable  to  uncertainty  of  several  seconds. 

This  R  A  to  be  preferred   

Nisi  R  A  =  35"'  1 1\6,  there  being  left  a  doubt  as  to 
the  wire  observed. 

j  Triple  

Position  estimated  from  diagram   

R  A  from  Mr.  Maclear's  determination.  PD.  Rough 
Pos  249.3,  248.0  ;  Place  as  observed  


B.  1631 
A.  51 

2.1115 
B.1641 


L.2867 

£.1121 


L.2948 
B.1673 


B.I702 

<r.  278 
B.1734 


DOUBLE  STARS. 


193 


No. 


3997 


3998 

3999 
4000 


4001 


4002 
4003 
4004 
4005 
4006 


4007 
4008 
4009 


4010 
401 1 
401a 

4013 
4014 
4015 
4016 
4017 
4018 
4019 
4020 
4021 
4022 

4023 


R  A.  1830.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

h. 

m.  s.d. 

0 

7 

38  43-7 

163 

S3 

23 

98.0 

I5 

44.2 

53 

J4 

3 
4 

46.5 

53 

30 

101.3:: 

1 

7 

39  7-3 

142 

6 

6 

181. 3 

10 

7 

39  !3± 

144 

0 

36 

3 

7 

39  13-8 

148 

15 

57 

14. 1 

16 

0 

230.3 

18.0 

16 

4 

230.3 

1 

7 

39  29-J 

157 

3 

59 

303.7 

4 

7 

39  33-8 

140 

3 

30 

*  JT'  J 

60 

7 

40  29.3 

139 

5a 

33 

87.3 

18 

7 

40  41.9 

113 

46 

18 

127.8 

T  r 
1  J 

7 

41  39.2 

152 

59 

46 

111.1 

12 

7 

42  1.6 

146 

18 

24 

215.3 

30 

7 

42  2.4 

134 

50 

J4 

299.3 

2.9 

5° 

26 

3OO.3 

« 
0 

7 

42  50.3 

117 

49 

33 

272.8 

15 

7 

43  11.0 

142 

54 

46 

228.8 

20 

7 

43  47-o 

121 

44 

22 

I29.7 

10 

7 

43  53-7 

162 

11 

52 

II7.7 

l8 

54.2 

1 1 

43 

I 14.3 

15 

54.5 

1 1 

54 

1 1  5.7 

2C 

j 

I  I5.O 

18 

7 

45  5-o 

177 

1 

33 

235.3 

IO 

7 

46  15.9 

156 

38 

5° 

3OO.2 

20 

7 

46  23.9 

149 

5i 

46 

IO5.5 

12 

5* 

40 

IOO.7 

15 

7 

46  28.7 

IO7 

53 

18 

I99.7 

12 

7 

46  42.8 

!53 

15 

24 

153.6 

15 

7 

46  46.7 

107 

21 

5° 

22  1.8 

20 

7 

47  15-4 

140 

57 

46 

168.3 

15 

7 

49  1.2 

140 

28 

15 

206.5 

IO 

7 

49  »3-9 

149 

10 

41 

325.2 

6 

7 

49  33-5 

131 

24 

2 

155.6 

4 

7 

5°  37-9 

165 

18 

17 

320.2 

15 

7 

5°  57-i 

148 

6 

57 

236.I 

12 

7 

5i  5-6 

in 

1 

26 

7-5 

15 

7 

51  35.6 

160 

20 

23 

227.7 

1 

37.6 

20 

30 

226.8 

1 

Magnitude. 


7  =  7 


9 
10 


6'  11 

6  11 

9'  12 

7'  8 

8'  13 

9'  10 

8'  12 

6  12 


9  =  9 
8'  14 

9  =  9 
5  9' 


13 
9' 
*3 
J4 

8'  9 
9  =  9 
9'  9 


Remarks. 


Synon. 


Fine  star.    Pos  99.4,  96.7  

Pos  102.7,  99-3>  99-3  >  very  beautiful  double  s)5- 
Quite  as  close  as  t]  Corona?. 

In  the  best  moments  when  the  star  collects  itself, 
certainly  seen  double,  but  no  measure  can  be  got. 
The  south-easter  rising  rapidly,  and  stars  dilated 
with  momentary  intervals  of  concentration.  After 
sweeping  on  20"'  I  returned  to  this  star  and  got  a 
measure  as  here  set  down  in  an  interval  of  steady 
good  definition,  but  being  so  far  out  of  merid.  the 
angle  is  of  course  open  to  much  error. 

Both  yellow   

R  A  very  rough,  taken  past  merid  

The  night  too  bad,  with  any  management,  to  get  even 
a  glimpse  of  the  small  star. 

Beautiful  double  star.  Pos  232.7,  227.9,  with 
power  320,  and  12  inches  aperture. 

Beautiful  double  star,  but  extremely  difficult,  being 
of  the  order  Pervicinae.  Pos  234.3,  226.3, 
measured  with  power  320  and  12  inches  aperture. 

The  last  of  3  stars  in  an  obtuse  angled  nearly 
isosceles  triangle. 

R  Ascension  not  good  in  this  f;  A.  55  =  B.  1740  4- 
1741. 

This  obs  makes  the  minute  43"' ;  one  or  other  is  of 
course  mistaken.  In  such  cases  the  earlier  is 
preferred  to  ensure  being  in  time  in  future 
observations. 

Both  stars  pale  yellow   

Z  Piscis  Volantis,  L  yell,  S  pale  blue.  Pos  117.6, 
117. 8. 

ARA  =  3s-5.     Pos  115.4,  113.3   

Pos  115. 2,  118. 1,  113. 7.    Superb  star  

Pos  114.8,  115.3,  IJ4-9-    Fine  D  star  

Ill  defined   

Very  debcate.    Requires  illumin  

Very  delicate.    Measured  when  past  meridian  

Points  to  a  third  

Has  a  third  star  n  f   

Ill  defined   

Very  ill  defined   

Beautifully  divided  

Very  delicate   

3~^~ 


B.1731 


B.1737 


L.2976 


B.1762 


L.3019 
B.1779 
a-  57 


B.  1800 


Sweep. 


683 
547 

672 


763 
763 
679 

664 

764 

538 

680 

526 
768 
524 

552 
542 
528 


531 
525 
535 
523 

683 
673 
672 
674 

538 
524 
764 
677 
773 
675 
763 
680 
764 
772 
548 
664 
677 

546 
745 


194 


REDUCED  OBSERVATIONS  OF 


R  A.  1880.0. 
h.   in.    s.  d. 


4024 

4025 

4026 

4027 

4028 

4029 
4030 


4031 


4032 

4°33 
4034 


4°35 

4036 

4°37 
4038 
4039 
4040 
4041 


4042 
4043 


4044 
4045 
4046 

4047 

4048 


7  S3  i3-i 
14.5 

7  53  17-5 

7  53  38-6 
7  53  57-i 
57-5 
7  54  25-1 
7  54  46-2 
7  54  54-5 

7  55  25  ° 
27.6 

7  55  *9-6 
31.4 
32.6 
33.0 
35-5 
7  55  — 
7  55  41-0 
7  56  19-3 
20.4 
22.2 
7  56  26.7 
7  56  32.2 
7  56  35-3 
7  57  - 
7  57  i-9 
7  57  4-° 
7  57  42-° 


7  58  - 
7  58  22.8 
24.6 

7  58  26.6 
7  58  44-3 

7  59  I2-5 

8  o  25.0 
8    2  50.6 

53' 
53-9 


N  P  D.  1880.0. 


119    3  3 

2  57 

138  47  9 

134  27  16 
150  21  26 
21  23 

139  30  56 
153  37  38 
130  50  34 

102  43  41 
43  49 

150  24  46 
24  30 
23  39 

23  16 

24  2 

136  50  — 

137  20  48 
132  17  41 

18  25 

17  48 

121  59  7 

147  29  5 

117    4  1 

130  50  — 

127  43  6 

125  56  40 

in  57  17 


144  11  - 

136    5  1 

5  28 

144  33  46 

J39  57  53 

123    5  8 

178  42  53 

131  41  56 

4i  35 

41  50 


Dist.  Magnitude 


82.5 

12 

9 

10 

82.7 

12 

9 

10 

S  47-6 

18 

6 

14 

>     1A  S? 

t  34-o 

AO 

6 

1 2 

279.8 

3 

12: 

=  12 

I  IO.9 

12 

10; 

=  10 

43.2 

20 

  0' 

—  a 

91.3 

10 

IO 

1 1 

344-9 

40 

7 

9 

148.2 

3 

'47-7 

4 

9' 

=  9' 

352.6 

23 

9 

10 

355-5 

6 

8 

9 

357.1 

5 

7' 

9 

35*-5 

8 

9 

10 

354-5 

35J-5 

30.8 

7 

9' 

64.3 

12 

8' 

9 

A 

*r 

8' 

1  j 

293.0 

4 

9 

10 

293.4 

4 

9 

1 1 

131.7 

30 

7' 

9 

78.6 

3 

10'= 

=  10' 

337-7 

12 

8' 

J4V4 

20. 1 
J 

/ 

8' 

51-7 

8 

10= 

=  10 

138.3 

18 

8' 

9 

179.3 

3 

7 

15 

207.I 

20 

8 

9 

207.3 

25 

8' 

9 

219.8 

*3 

9 

1 1 

84.6 

20 

7' 

10 

S  147-7 

8 

13 

<  3!7-3 

8 

'3 

208.5 

IO 

10 

10 

207.8 

8 

9' 

10 

207.1 

9 

9: 

=  9 

Remarks. 


Synon. 


Sweep. 


j  Difficult  and  very  delicate   

Double.    No  description   

Fine  D  star.    Pos  42.7,  43.8   

Large  star  white,  S  rich  ruby  coloured  approaching 
to  sanguine.    Very  remarkable. 

Very  neat  star.    Pos  148.8,  147.7  

Pos  146.3,  149.3,  147-5.  This  obs  makes  the  R  A 
59'. 6,  but  this  is  owing  to  an  obvious  mistake  of 
the  wire,  which  is  rectified  in  the  reduction. 

In  a  cluster  

Chief  double  star  of  a  fine  cluster  

One  of  the  large  stars  in  a  fine  cl  

Pos  355-3.  353-7  

Mean  epoch,  1836.555   

Neat  star  

L  yellow,  S  decided  purplish  red  

80  or  100  stars  in  the  field  

Mean  epoch,  1837.045   

A  most  delicate  and  difficult  object.  The  night  is 
not  such  as  to  give  perfect  definition,  although 
pretty  good  ;  so  that,  although  /  have  no  doubt, 
I  should  like  to  see  the  star  again  under  more 
favourable  circumstances. 

Class  4  or  5.    Review  of  B   

Red  and  blue   

L  pale  rose  ;  S  greenish  blue ;  very  peculiar,  and 
richly  contrasted  colours. 

By  diagram  triple,  the  small  H=  being  double  

A  B  ) 

^  £  <  Triple.  R  A  open  to  very  great  errors  .... 
The  chief  of  about  60  stars  in  field   


B. 1839 


B.  1848 


2.  1178 


B.  1866 


B.  1872 


B.  18S7 


77i 
53i 
680 

542 
681 
682 
526 

55° 
772 

676 


524 
664 
764 
681 
682 
E 

553 
542 
528 
686 
535 
543 
531 
E 

540 
66i 

768 


E 

553 
5*7 

55i 
526 
786 

674 

712 
528 
529 


DOUBLE  STARS. 


195 


A.  1830.0. 
m.  s.d. 


NPD.  1830.0. 

o        I  II 


3  4!-4 

4  i-4 


8    4  16.2 
17.2 

8    4  17.0 

8  4  45.0 
8    4  46.0 

8    5  19. 1 

8  5  21.3 
8    5  29.3 

34.6 
8    5  39.9 

45-3 
8    6  46.7 

8  7  4.9 
8    7  20.8 

8    7  26.4 

8  7  - 
8  7  28.9 
8    8  1.3 


8    8  20+ 

8  8  29.9 
8  8  39.2 
8    8  41.2 

8    8  46.8 
53.8 


8  47.5 

9  - 
9  °-3 
9  6.6 
9  8.7 

10  32.1 

10  57.4 
11 


4074      8  12  23.5 


Position. 


127  51  19 
I32    7  3 

8  19 

136  50  29 
49  28 


105    9  4 

126  47  27 
125  19  8 

150  35  26 

151  5i  45 
159  22  15 

22  40 

157  o  59 
1  46 

132  29  5 
125  23  19 

158  7  40 

121  37  48 
125  56  - 
156  40  17 
129  49  57 


126  50  30+ 

158  53  29 
143  32  6 
133    o  54 

173  14  17 
14  12 


166  58  4 
135  19  - 
104  38  15 

153  59 

60  2 
72  27  49 
109  25  49 
126  47  . . 


!39  43  39 


316.3 
87.3 

86.6 
85.0 
220.0 
217.2 

303.3 

263.4 
120+ 

S  92-3 
i  310-3 

\  285.7 

I  3J9-7 
6.6 

6.0 
359.8 

355-° 
292.1 
1Q0-+- 
17-5 

339± 
177.0 
14.9 
343-4 


346-3 

278.7 

224.4 

136.5 

<  65.1 
I  88.0 

S  67-° 
I  89± 


300.3 
256.7 
103.5 
204.7 
201.9 

4-3 
178. 1 
170+ 


267.3 


Dist. 


Magnitude. 


30 

4 
4 

30 
21.6 
4 
5° 


10  11 

8  9 


9  9 

6  14 

9  10 

8  10 

8  13 


Remarks. 


33.2 
30 

5 


Neat  star.  Marked  as  double  in  the  Brisbane  Cata- 
logue. 

Pos  83.8,  86.3  

Also  three  more,    y  Argus   

Pos  218.7,  216. 1,  216.7.  Besides  the  two  principal 
stars,  are  three  others,  11,  11,  and  13  m,  arranged 
in  an  exact  right  line. 

Dist  set  down  as  2",  but  it  is  probably  a  mistake  of 
writing  for  20",  as  the  diagram  makes  the  stars 
distant. 

[Place  from  the  Brisbane  Catalogue.]   

Too  ill  denned  for  measure.  Pos  estimated  from 
diagram. 

^Triple  • 

I  Triple  

Both  stars  ruddy  yellow,  a  marked  shade  of  colour, 
and  both  exactly  of  the  same  tint. 

Both  yellow.    Measure  interrupted  by  clouds  

Pos  estim  from  diag  made  with  320,  very  ill  denned. 

£  Volantis.  Superb  D  star,  but  ill  denned.  Pos 
18.7,  16.3.    Is  No.  7  of  M.  Rumker's  list. 

Epoch  1836.988  

L  yellow  S  blue.    [This  obs  makes  the  P  D  1280, 

but  Lacaille  and  Taylor  agree  in  making  it  129. 

The  star  being  a  large  one,  a  mistake  on  my  part 

is  presumed.'] 
L  white,  S  so  very  red  as  to  give  the  large  star  by 

contrast  a  bluish  tint. 

A  bright  *  (B.  1896)  6'  dist,  s  p  

Pos  135. 1,  137.9  

1  Triple.    A  fourth  near  

Triple,  very  ill  denned.  N.B.  This  obs  makes  the 
R  A  18"  instead  of  8m.  The  two  observations, 
however,  evidently  relate  to  the  same  star,  and 
the  earlier  time  is  of  course  preferred. 

Mean  epoch,  1836.490   

2  or  3  companions  besides  

Though  I  have  not  a  doubt  that  this  is  really  a 
double  star,  yet  the  stars  generally  are  so  strangely 
denned  to-night,  and  put  on  such  unaccountable 
appearances,  that  it  must  be  re-examined. 


Synon. 


B. 1914 
A.  63 


B.  1916 

1917 
A.  65 


B,  1922 


L.  3211 


Sweep. 


A.  1006 

B.  1938 
B.  1940 

A.  66 

B.  1939 


M. 3501 


L.  3234 


L.  3371? 


B.  1948 

2.  1214 
L.  3258 


661 
691 

685 
686 

553 
527 

675 

661 

786 


682 
546 

545 
556 

538 
542 
809 
538 

678 
E 

557 
772 


659 

673 
763 
542 

666 

667 


548 
E 

687 
55° 
773 
688 
677 
659 


6S0 


196  REDUCED  OBSERVATIONS  OF 


No. 

K  A.  1830.0. 

X  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

h.  m. 

s.  d. 

0 

a 

4°75 

8  13 

2.4 

155 

45 

204.9 

2 

10 

10 

55° 

3-i 

45 

16 

267.O 

2 

10 

10 

773 

4076 

°  *3 

10.8 

J57 

'7 

55 

1  I2.3 

2 

'3 

557 

a  i3 

1 5.0  : 

i8.a 

J34 

31 

30 

g 

225. 1 
227.6 

A 

8' 

8' 

B. 

1973 

685 
542 

»4 

T 

3 

9' 

=  9' 

4c-- 

8  13 

16.1 

152 

20 

30 

298.3 

15 

9 

10 

682 

4078 

8  13 

20.4 

113 

33 

31 

I32.9 

12 

8' 

1 1 

559 

4079 

8  13 

39.0 

!45 

21 

48 

*73-5 

20 

7 

14 

[Lacaille's  P  D  would  be  145  15.]  

L.3278? 

552 

4080 

8  13 

55.8 

136 

36 

10 

2I5.3 

4 

9 

9  + 

553 

4081 

8  14 

— 

137 

40 



B. 

1977 

E 

4082 

8  14 

5-9 

139 

-14 

48 

86.3 

3 

IO: 

=  10 

680 

7-4 

44 

35 

86.8 

2 

IO: 

=  10 

526 

4083 

8  14 

25.2 

125 

41 

8 

1 10.7 

25 

IO 

12 

Surrounded  with  evident  nebula,  which  seems  to 

786 

belong  to  both  stars.    Extremely  ill  denned. 

27.1 

40 

5i 

113. 8 

25 

9' 

12 

Not  quite  positive  that  the  nebula  involves  both 
stars.    N.B.  In  a  field  with  70  stars. 

54i 

27.3 

41 

5 

A  neb  attached  to  and  involving  a  star.  (Definition 

809 

bad.) 

27.9 

40 

5° 

1 10.7 

30 

9 

1 1 

T         1J-                    ,    .  ,  //-j- 

Involved  in  pretty  bright  nebula  50  in  diameter. .  . . 

540 

4084 

8  14 

26.0 

148 

37 

58 

J  158.7 
*  266.1 

60 
4 

0 
10 

9 
10 

A  and  (B  +  C)  regarded  as  one  star  B  and  C.    The  ) 
small  star  double.  j 

B. 

1978 

664 

4085 

8  14 

57-i 

125 

56 

17 

270.0 

5 

5' 

14 

B. 

1983 

661 

57 

*5 

265+ 

3 

5' 

15 

K, vrri'lnpl v  ilifTiciilf    lippnn^p  fVip  ^*  will  Tint  Vipnr  flip 

809 

full  aperture,  being  ill  defined. 

4086 

8  15 

42.2 

175 

27 

4 

76.7 

80 

8' 

10 

B. 

2007 

674 

f  321.0 

1 

. 

8 

=  a 

A  and  B.          ~\  Quadruple.  The  large  star  strongly 

772 

4087 

8  16 

6.9 

130 

27 

2 

I  34°-9 
C  3 

1  c 

j 

8 

14 

(A  4-  B)  and  C.  >    suspected  to  be  close  double  with 

3° 

8 

'5 

(A  4-  B)  and  D.  y    power  180,  but  could  not  bring 
it  up  to  a  disc,  the  definition  being  bad  to-night  j 
320  and  9  inches  aperture,   however,  divided  it 
cleanly.    The  measure  inaccurate,  the  star  being 
considerably  past  meridian  when  taken. 

4088 

8  16 

49-4 

118 

34 

290+ 

25 

6 

1 1 

L. 

3298 

771 

8  16 

59-7 
3 1.6 

134 
132 

18 
13 

18 
58 

269.8 
14. 1 

10 

IO 

8 

1 1 

9' 

686 

4089 
4090 

8  17 

15 

691 

4091 

8  19 

8.8 

J33 

4-3 

43 

294.9 

y 

12 

691 

15 

4092 

8  19  46.9 

129 

1 

46 

204.7 

10 

10 

1 1 

661 

4093 

8  20 

5-J 

128 

29 

53 

122. 1 

8' 

=  8' 

L. 

3324 

54° 

*5 

4094 

8  20 

9.6 

124 

58 

48 

21 1.3 

20 

9' 

10 

8  20 

15.6 

160 

58 

41 

52.7 

60 

6 

6 

L. 

3355 

546 

4095 

8  20 

36.0 

162 

57 

53 

*  236.3 

8 

10 

J3 
io' 

683 

336-5 

15 

10 

4096 

8  21 

13.9 

150 

27 

10 

91.3 

10 

9' 

10 

682 

4097 

8  21 

15.4 

150 

26 

20 

356-1 

10 

9' 

1 1 

682 

4098 

8  21 

52.5 

129 

32 

30 

274.9 

15 

8' 

1 1 

555 

4099 

8  21 

55.0 

129 

29 

30 

21 1.9 

20 

8' 

12 

555 

4100 

8  22 

23.2 

107 

46 

56 

J79-3 

20 

11 

677 

9' 

4101 

8  22 

28.7 

139 

46 

1 1 

228.8 

=  9' 

526 

4 

9' 

4102 

8  23 

132 

1 

B. 

2046 

E 

4103 

8  23 

32.5 

162 

5i 

6 

(  287.4 
*  158.4 

30 
45 

5 
5 

«3 

»4 

Pos  288.7,  286.3,  288.3  ;  A  R  A  =  7'.o  1 

B. 

2055 

683 

DOUBLE  STARS. 


197 


No. 

R  A.  1880.0. 
h.    m.  s.  d. 

NPD.  1830.0. 

0      1  11 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

8  23  41.2 

137   21  SI 

1-235-5 

I  39.7 

2 
15 

6 
6 

10 
9 

~\  Beautifully  triple.    Measures  incomplete  by  reason 
[     of  a  sudden  gust  of  the  S.E.  wind,  which  con- 

i       Toundpd   all  int"n  nr>  inflierino*iii«liql~tlp  lilnt"  T^lip 

1             1      "  1  M  H  VI     rill     1  1  1  l.l_l     till    llllllOllllU  UlSllaiJlC    Ill'M  .          x  UC 

)     star  is  called  A  Argus  in  some  catalogues. 

B.  2056 

527 

A2.7 

21  40 

/  239.7 

25 

5' 

9 

_ 

\  T)pl lpntpl^  t"i*iv\lp  •  T.  winf"p  (  W  email   *A*        t»q1p  KIiip 
/  J--*  Clio  a.  1.  CIV  L11LHC  f  AJ  WlllvC  y  xX  J  olHaH           \_y  UalC  U1UC 

553 

I  34.8 

20 

c' 

J  I 

8  23  41.9 

134     9  18 

346.6 

\ 

J 

6 

9 

B.  2054 

691 

43.0 

IO  II 

349.0 

4 

6' 

8' 

A.  70 

685 

4.IO5 

8  23  52.5 

168  40  48 

69.5 

8 

10' = 

10' 

670 

8  24  56.3 

I  2  D       0    I O 

138.8 

ifi 

8 

10 

rT ifipjiillp's.  T!  A  rliflTprc 

t     e.  > 
ij.3304 . 

540 

4IO7 

8  25  9.5 

128  30  10 

S  325-4 
I  98-7 

3 

30 

7 
7 

10 
9 

A  B  ) 

L-  3375 

661 

4IO8 

8  26  12.2 

150  32  6 

232.6 

20 

9 

10 

778 

15.0 

32  52 

229.6 

18 

9' 

10 

682 

4.IOO 

8  26  31.5 

165  52  18 

124.0 

3° 

8 

8' 

L.  3437 

671 

41 10 

8  28  1.8 

156  33  34 

221.4 

25 

7 

1 1 

B.  2088 

556 

41  1  1 

8  28  35.3 

139  21  41 

1 10.2 

680 

4 1 1 2 

8  29  25.4 

138  14  42 

30.2 

8 

Q  = 

=  Q 
7 

526 

4113 

8  30  5.5 

128  10  34 

201.9 

10 

IO 

661 

4114 

8  30  14.5 

130  24  12 

230.0 

2 

1 1 

1 1 

772 

4115 

8  ^0  4-6*2 

T^i      fi.    r  7 

\  155-6:: 
i  21.3 

20 
40 

6' 
6' 

12 
*3 

>->■  3434 

786 

47.6 

8  31  10.2 
8  31  10.7 
8  31  40.5 
8  31  53.8 

9  l6 

159-3 
0.2 

20 

6' 

12 

787 

41 16 
4117 
4118 
4119 

136   54  51 
150   54  29 
162  53  58 

138  50  IO 

50  40 

6 

8 

Q 

7 

»3 
11 

553 
682 

194.3 
20.I 

8 

8 

20 

9 
9 

683 
526 
680 

221.8 

10 

12 

B.  21 15 

231.7 

10 

g 

11 

One  or  other  position  seems  to  be  io°  wrong  in  the 
reading. 

4120 

a  32  37. o 
42.3 

lI°  57  37 
18 

40 
4  — — 

fir  t 
85.I 

O.O 

5° 
35 

2 

5' 
6' 

1 1 

T ,          f„_m  .].".,  

a.  hi?. 

771 

1 1 

564 

r  en 
55" 

527 
440 

4-12  I 

4.122 

4123 

8  1 1  60 

fi   *5  ■?  'ydc 

8  33  49-7 

*53    1  44 
•35  37  39 
142  59  59 

12 

0'  = 

q 

=  9' 
7 

12 

/  <  1    ■     (■      £   "1  „ „J                                                   T  . 

25 

4124 
4125 

8  33  5i-6 
8  34  19.3 

105  20  27 
152  15  48 

122.8 

35 
8 

5 

14 
1 1 

A.  1063 

B.  2135 

675 
432 

23O.3 

7 

20.4 

15  47 

225.9 

8 

5' 

Very  delicate,  ill  defined.    Pos  228.0,  223.8.  (This 
last  measure  probably  wrong.    The  bad  definition 
hardly  explains  the  extraordinary  disagreement  in 
the  magnitudes.) 

682 

4126 
4127 

8  34  54.2 

142  28  59 
136    2  30 

28± 

15 

30 

7 

1 1 

B.  2143 
B.  2141 

440 

553 

57-7 

5 

1 1 



4128 

8  35  36-1 

149  42  59 

220.2 

if 

7' 

8 

B.  2153 

764 

4120 

1  7 

8  36  16.7 

125  54  12 

346. 1 

6 

9 

'3 

661 

4130 

8  36  30.8 

146  56  30 

216.4 

3 

7' 

10 

B.  2159 

55i 

4131 

8  36  45.9 

73  34  5° 

144.2 

20 

10  = 

=  10 

688 

4132 

8  36  48.3 

172  42  38 

321.3 

5 

11  = 

=  11 

The  northern  of  an  elongated  group  of  10  consider- 
able stars,  with  smaller  intermixed. 

667 

8  37  34.6 

142  30  21 

309.3 

So 

6 

6' 

B.  2168 
+2169 

763 

4133 

8  38  18.7 

132    2  43 

60.3 

45 

5 

13 

B.  2179 

691 

20.1 

1  24 

2  26 

62.1 

35 
40 

6 

12 

685 
529 

20.6 

61.9 

5' 

1 1 

4134 

8  38  24.7 

159  46  57 

105.8 

35 

5' 

9 

B.  2184 

546 

4135 

8  38  30.8 

7>  58  57 

49.8 

30 

7 

«5 

688 

3  E 


198 


REDUCED  OBSERVATIONS  OF 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Dist. 


Magnitude, 


Remarks. 


Synon. 


Sweep. 


4.136 

4137 
4138 

4»39 
4140 


4141 
4142 

4H3 
4144 


4H5 
4146 

4H7 
4148 
4149 


4150 

4151 
4152 
4153 

4iS4 
4iS5 

4156 


4157 

4158 
4JS9 
4160 


4161 
4162 


8  39  59.1 
60.9 
8  40  2.3 
8  40  28.1 
8  40  34.4 
8  41  2.5 

8  41  3.9 

9.6 


8  41  45.6 
8  42  38± 
8  43  15.8 
8  43  41. 1 

42.5 


44  5*-1 

45  26.2 

45  57-4 

46  - 

46  19.5 

47  25.6 
26.8 

47  42.0 

444 

48  44.2 

48  44.9 

49  3i  i 

49  46-7 

50  17.8 

51  12.0 
51  28.2 


51  39-5 

51  5i-3 
68.4 

52  1.6 
52  13.0 

52  19.6 

52  45-7 
47.2 

53  5-3 
53  26-9 


144    6  10 

5  39 
164  18  28 
128  53  52 
149  19  57 
102  47  17 

148    6  13 

6  27 


118  10  32 

146  59  35 

112  35  15 

125  16  51 

18  7 


143  23  16 

102  35  51 

151  38  o 

143  29  26  : 
127  33  30 
107  36  16 

34  54 

131  n  21 

10  44 

142  52  9 

153    2  17 

134  23  48 

121  26  6 
150  47  35 

149  59  58 

144  52  36 

74    3  49 

124  56  58 
56  41 

'74  3  58 
142  56  19 

101  59  17 

148  34  30 

34  33 
136  34  29 
in  20  25 


64.0 
60.0 
192.4 
321.3 

45-3 
280.1 

r  289.7 

\  357-3 
(.  217.6 

286.6 


329+ 
219.4 
131. 8 
3°9± 

319.8 


257.1 
99.2 

353-2 
106. 1 
202.1 

H3-7 
144.4 

267.3 
262.7 

255± 
338.6 
121. 6 


243.8 
197.8 

322.3 
351-4 

31. 1 

279.7 
280.6 

60.0 
100-t- 

280.9 

7i-7 
71.7 

3*9-3 
219.0 


(?  Argus.    A  R  A  =  7'.o 


A.  1077 


4 
35 
3 
4 
12 
100 
5° 

J5 

20 

3 
6 

30 

12 
4 

25 

70 


9  10 

8  10 

8'  10 

7  13 

7  12 


10  13 

9  11 
6  14 


9  9 
11=11 

5  H 
7'  » 

9  =  9 
8'  12 


*3 


12  13 

6  7 


"? Noted  as  double  in  Brisb.  Pos  290.8,  288.6  .... 
) 

Pos  286.9,  286.3.  A  fine  double  star.  It  has  two 
companions  12  m,  near.  This  R  A  to  be  pre- 
ferred to  that  of  f  764  ;  those  of  that  f  being 
precarious. 

Very  fine  D  star.    R  A  roughly  taken  

Very  elegant  star   

Excessively  difficult,  but  remained  satisfied  of  its 
being  double. 

Very  difficult,  definition  being  too  bad  for  using 
power.  Measure  a  mere  rude  approximation. 
Perfectly  certain  of  its  being  double  ;  the  small 
s)t  in  good  moments  being  separated. 

Bears  some  illumination  

Unless  R  A  =  8  46  58.7   

Excessively  ill  defined.  (In  which  case  magnitudes 
and  distances  are  always  difficult  to  estimate.) 

Pos  337.7,  339-6  

Obs  gives  R  A  50™  4.7,  but  it  is  evident  from  the 

zeros  that  the  wire  was  mistaken,  which  rectified 

gives  as  here  set  down. 

A  and  B.  Triple.  An  exact  equilateral  triangle, 
the  other  if.  1 3  m  precedes. 

Difficult,    (c  Carina.)  

Large  star  very  red.  A  third  very  small,  and  closer 
suspected.  [If  this  be  A  73,  his  P  D  is  14' 
wrong.    B.  2286  is  marked  as  double  in  B.] 

Pos  30.5,  31.7;  39.2  rejected,  probably  misread 
10  degrees. 

[In  one  or  other  of  these  observations,  a  mistake  of 
20  seconds  in  R  A  must  have  been  committed.] 

Pos  59.3,  61.4,  59.3   

Large  star  red  

b'  Carina.    [Called  4  m  by  Lacaille.]   

L.  3639  =  B.  2293  4-  2294   


B.  2206 
R.9 


S.  585 


B.  2272 


B.  2281 
B.  2286 


A.  74 


B.  2296 


552 
440 
683 
661 
432 
687 

764 
543 


53i 
684 

555 
787 

809 


763 
687 
682 
763 
540 

675 
56, 

554 
529 
440 

55° 
691 

678 
432 

543 
55i 


S.  1300  688 


787 
809 

667 
440 

687 

684 

764 

527 

558 


DOUBLE  STARS. 


199 


No. 

R  A.  1830.0. 
h.   m.  s.  d. 

N  P  D.  1830.0. 

0      /  // 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

4.103 

8  53  49.0 

166  38  52 

320.7 

J5 

9 

12 

67 1 

4.164 

8  54  42.6 

155  32  23 

144. 1 

12 

8 

IO 

Ti  vp  1 1  n w    Si  vijiIp  nlnp 

L.  3666 

55° 

44.9 

30  39 

142.6 

IS 

8 

12 

773 

47.0 

33  3 

144. 1 

15 

8 

IO 

\  p r v  npjif"  ^tsir 

«8 

8  54  50.8 

75    1  52 

126.4 

30 

9' 

IO 

h.  115 

688 

4165 

8  56  - 

141  31  - 

87.9 

1.4 

6 

8 

TVTphti  pnnpVi    tS?7  *>  f\  C 

B.  2320 

E 

8  56  8.0 

115  38  25 

273.7 

O 
O 

10= 

IO 

T'Iip  mipr  vpnrlincr  frivps;  Tt  n    hut  it  w  nhvimic  from 

1  1H     lllll   1    1  C7<l*_Ll  llji,    t|H  C3     /  J  *  /  J     U  U.L     11*  i3    \J  I J  V  1U  ua    11  Ulll 

lit    «iiJ-0  z, 

563 

the  diagram  that  the  fig.  2  has  been  omitted  in 
writing  down  the  measure.    See  also  h.  2482. 

66 

8  c6  2  c  2 

y  -J  1      fh  n9 

j  s 

150.3 

1 0 

8  = 

:  8 

r  in  p  ■    w  rw  i  rn  il  ■  T/inn 

L  ^660 

678 

4107 

8    c6   *2Q  "2 

I55  41  J7 

3 

8 

15 

Exceedingly  delicate.    Pos  22. 8,  21. 7 .    £N.  B.  The 

minute  01  R  A  given  by  this  obs  is  57,  but  as  this 
disagrees  with  the  result  of  f  773-  which  is  56  ,  the 

PtivliPr  10  nrptpvrpn 
Cat  llCi   lb  UIC1C1  ICUi 

40.7 

41  33 

23.3 

2 

9 

773 

4.168 

8  56  59.4 

120  39  30 

67.8 

3 

12= 

12 

c  ^  1 

4169 

8  57  8.4 

127  31  34 

282.6 

65 

9 

12 

540 

8  57  32.9 

11  4.6  4.6 

300.3 
j  y  j 

7 

IO 

1 1 

h.  118 

688 

ill  70 

8  58  30.3 

149    15  l8 

254.6 

A 
T 

11  = 

1 1 

432 

4171 

8  58  35.4 

159    3  11 

235.6 

20 

IO 

IO 

673 

4172 

8  58  53.6 

114  43  15 

2  I3.6 

6 

9 

563 

s 

4I73 

121  32  7 

5 

II, I] 

,11 

678 

4174 

8  59  23.8 

105    2  20 

258.7 

c 

J 

11  = 

.1 1 

687 

4175 

8  59  33.0 

in  ii  1 

128. 1 

1  c 

J 

8 

1 1 

B.  2332 

682 

33.0 

4.0  4.1 

110.6 
J 

20 

7 

1 1 

778 

4176 

8   ;q  70.2 

131     26  IO 

2.Q1.1 
y  j  j 

1  e 

j 

810 

9' 

9' 

4-177 

8  59  46.3 

145    40  II 

S  278.8 

I  295± 

T  C 

J 

IO 

8 
9 

9 

IO 

A.  B  )  t    i  .1  1 

L.  3689 

55i 

8  59  47.0 

74   4  35 

59.0 

6 

10' 

2.  1317 

688 

9 

4178 

9    0  16.3 

147  10  28 

164.8 

3 

6 

14 

Power  320,  pos  166.3,  163.3  ;  extremely  difficult, 

B.  2337 

764 

and  not  well  defined. 

16.7 

10  17 

164.2 

4 

J3 

Tori's  ific        t^>i  t     ifi-i  t       lVTpHQiirPf^  with  tS?o  nnd 

664 

12  inches  aperture.    Very  difficult,  by  reason  of 
the  extreme  smallness  of  the  companion,  which 
with  9  in.  is  barely  discernible. 

1  c  6 — 1 — 

j  — 

Measure  difficult,  and  spoiled  by  the  presence  ol 
another  person  in  the  gallery. 

684 

25 

4J79 

9    0  36-3 

124    3  25 

290.3 

12 

IO 

IO 

787 

4180 

9    *  10— 

133  16  23 

125-4- 

25 

8' 

IO 

69 1 

4181 

9    1  13.6 

144    3  9 

150-+- 

ii 

:l  I 

440 

1 1= 

4182 

9    2  18. 1 

106    9  55 

83+ 

25 

12 

675 

8 

4.18-3 

Q      2  4.<C.'3 
y        tj  j 

I  T  A      A  (~\      ry  (-, 
1  1U      i^S-J  J.\J 

144.9 

18 

6' 

9' 

v               /                t  r     7      1        7      ~  / 

A.  1 1 15 

678 

46.2 

41  3 

140.5 

15 

12 

564 

7 

9     3  12. 1 

72  46  48 

52.8 

1 

9  = 

=  9 

Too  late,  and  the  measure  therefore  open  to  much 
error. 

2.  1322 

688 

4184 

9    3  4i-9 

l65  37  34 

218.7 

15 

8 

'3 

782 

4185 

9    4  36-9 

153  21  50 

242.7 

15 

9' 

9' 

773 

4l86 

9    4  47-i 

134  37  10 

274.3 

8 

10' 

io' 

542 

4187 

9    5  ~ 

134    0  - 

IO 

E 

3 

4188 

9    6  - 

132  55  - 

286.9 

2.9 

6' 

i 

B.  2387 

E 

4189 

9    6  50.9 

143  15  24 

105+ 

15 

9 

12 

440 

4I9O 

9    6  55-° 

147  16  13 

19.5 

7 

7 

12 

B.  2391 

764 

4191 

9    8  2.7 

132  31  29 

6.8 

4 

6' 

*3 

A  most  beautiful  and  delicate  object.     The  small 

B.  2400 

542 

star  best  seen  with  an  illuminated  field. 

5.0 

31  25 

9.9 

4 

6 

685 

200 


REDUCED  OBSERVATIONS  OF 


No. 


4192 

4'93 
4194 

+195 

4196 

4J97 
4198 

4199 

4200 
4201 
4202 
4203 

4204 

4205 

4206 

4207 
4208 

4209 


4210 
42 1 1 

4212 


4213 


4214 
4215 
4216 


4217 
4218 


4219 


R  A.  1880.0. 
h.    m.  s.  d. 


9     8  3°-5 
9     8  40.8 
9  10  0.9 
4.1 

9  10 


9  11  5-3 

9  12  4.0 

9  12  29.0 

9  12  33-i 
35-5 

9  J3  321 

9  >4  5-3 

9  15  6-5 

9  15  '8-7 

9  '5  47-3 

9  16  19.6 

9  '7  7-6 

9  !7  38-4 

9  18  18.2 

9  18  43-4 

9  19  16.8 

17-3 

9  20  — 

9  20  — 

9  21  9.6 


26.9 
9  21  13.4 
13.7 
14. 1 

9  21  31.2 

9  22  31.5 

9  23  24.6 

9  23  28.4 

9  25  38.2 
9  26  5.4 
8.3 

9  26  34-7 
9  26  35-7 
9  27  - 


N  P  D.  1830.0. 


139  38  14 

112  27  5 
172  59  57 
60  25 
154  11  .. 

10  . . 

141  12  56 

142  6  9 
129  49  50 

117  4  3 

3  36 

121  2  37 

118  16  25 
135  16  56 

122  1  46 

159  5  55 
170  28  1 

28  20 
170  25  48 

26  44 

164  10  44 

144  10  26 
126  32  29 

137  33  10 

32  33 

156  45  37 
174  58  - 

131  51  o 


49  26 
151  13  10 
13  21 
13  16 
13  40 

166  53  54 
138  44  52 
159  13  35 
121  10  13 

167  10  4 
i25  37  54 

39  25 
74  52  11 

132    1  51 

72  59  - 


6.0 
126.4 

44-3 
48.8 
58.7 


126.5 

!95± 
182.3 

io8± 
1 10.5 

7i-5 
100+ 

152.7 

54-3 
9.4 
352.4 
356.6 
248.2 
244.3 

f  338-5 
I  347-7 
308.5 
127.5 

f  336-3 
\  1.9 

/  336-5 
1  3-5 
236.2 
113. 2 

67.3 


65.8 
318.3 
324.6 
326.6 
319.0 
193.3 
260.1 

335-5 
209.9 

278.9 
28.9 
25.9 

82.8 

320.8 


Magnitude. 


9  9 

8  12 
11  =  11 

10  10 

9  9' 


3 

IO 

1 1 

15 

9 

11 

IO 

IO 

IO 

12 

9 

IO 

15 

8 

8' 

2 

8 

9 

2 

11'= 

ii' 

15 

8 

1 3 

j 

12 

10= 

IO 

IO 

9' 

IO 

3 

1 1 

13 

5 

12 

13 

3 

IO 

13 

4 

IO 

'3 

5 

6 

40 

6 

1 1 

16 

9 

10' 

25 

8' 

9 

8' 
0 

12 

25 

9 

IO 

12 

9 

r3 

4 

9 

IO 

i-7 

6 

IO 

15 

7 

14 

20 

7' 

J3 

7 

7' 

IO 

IO 

6 

12 

6 

6' 

12 

8 

8 

IO 

IO 

IO 

IO' 

6 

1 1 

Ii' 

10 

IO 

IO' 

8 

7' 

8 

20 

7 

J3 

3 

8' 

12 

4 

8 

12 

45 

7 

9 

20 

8 

IO 

Remarks. 


Difficult  and  ill  denned  

About  10'  preceding  and  nearly  in  the  same  parallel 
with  a  superb  globular  cluster. 

A  neat  double  star  following  a  0  

Both  yellow  

A  3rd  star  1 1  m,  exactly  in  the  same  line,  continued 
backwards,  pos  2°.3. 

Neat  star,  pos  110.0,  110.9   

Fine  double  star  

Pos  estim  from  diagram  ;  a  3rd  s|c  near  south  of  both 

R.  10,  marked  as  double  in  B  

The  preceding  of  two  D  S  in  field  

R  A  missed,  being  past  merid   

The  following  of  two  in  field  

R  A  missed  being  past  merid   

A  B.  pos  337.8,  339.3  X  Delicate  and  beautifu,  _ 

By  diagram  III.  class  

tci*¥*  

A  B  > 

AC  J 

Pos  233.8,  238.6.    Both  orange   

Epoch  1835.082.  £  Octantis.  Considerable  doubt 
of  its  being  really  a  double  star. 

[N.B.  One  of  these  2  right  ascensions  is  affected  by 
a  mistake  of  the  moveable  for  the  fixed  wire.  On 
examination  of  all  the  circumstance,  it  appears 
certain  that  this  is  the  erroneous  one.] 

Pos  317-3,  317-4,  320.3  ;  beautiful  

Pos  325.0,  324.3.    Fine  star  

Small  sfc  red.    Observed  with  Mr.  Maclear   

Pos  320.0,  318.0  

Pos  193.9,  192.8  

R  A::  

R  A::  

£  Antlise  ;  pos  209.7,  210.1,  marked  as  double  in 
B.    ?  if  A  78,  as  his  position  is  88°  53'. 

Neat  double  star  

7  Leonis  

Points  almost  exactly  to  a  third   

Evidently  not  a  single  star,  but  the  definition 
to-night  is  not  good  enough  to  divide  and 
measure  it. 


synon. 


L.  3801 
B.  2452 


B.  2470 


sweep. 


B.  2941 


B.  2498 
L.  3866 


B.  2515 
A.  78  ? 

L.  3941 


<T.  35O 


1372 


566 

532 
667 

779 
55° 

433 
762 
440 
810 

564 
771 
678 
771 

774 
678 
429 

549 
780 

549 

780 

547 
762 
809 

775 

776 

537 
E 

772 


744 
432 
777 
778 
433 
782 
680 
429 
678 

782 
787 
54  » 


774 
688 


DOUBLE  STARS. 


201 


No. 


R  A.  1830.0. 
h.   m.  s.d. 


4220 


4221 
4222 
4223 
4224 
4225 
4226 
4227 

4228 

4229 

4230 

4231 
4232 

4233 
4234 

4235 
4236 
4237 

4238 

4239 
4240 

4241 
4242 


4243 
4244 
4245 

4246 

4247 
4248 

4249 

4250 
4251 
4252 

4253 
4254 

4255 
4256 

42  57 


9  27  39-4 
39-9 

42.6 

9  27  57-6 
9  28  6.2 
9  28  30.9 

9  28  43-5 
9  29  20.6 

9  30  25-3 
9  30  30.8 

9  31  29.8 

9  32  40.2 

9  32  56.2 

9  32  56-9 

9  33  10.1 
10.5 

9  34  35-6 

9  34  43-1 

9  35  >3-8 

9  36  12.0 

9  36  13-5 
9  37  «-7 

9  37  39  3 

9  38  6-5 
9  38  14-9 
16.4 
9  38  29.8 
9  38  53-2 
55-4 
56.5 

9  39  29-6 
9  39  33-5 
9  39  34-3 

9  4°  34- 1 

9  41  i-9 
9  41  9-7 

9  41  32.2 
33.1 
9  42  35-6 
9  42  39-5 
9  43  - 
9  43  2.8 

9  43  - 
9  44  0.2 

9  44  4-8 
9  44  IJ-3 


N  P  D.  1830.0. 


138  15  26 

15  25 

IS  4 

142  41  26 
160  22  35 
128  45  39 

120  28  21 

160  23  15 
167  30  44 

118  29  18 

121  33  34 
128  9  52 
167  17  29 

r3°  53  39 

146  46  48 

46  20 

110  21  34 

141  30  59 

140  23  4 

119  58  54 

119  56  54 
73  39  37 

141  9  19 

127  49  3 

149  15  20 
15  o 

156  8  36 
130  53  20 

52  45 

53  8 

161  9  10 

120  41  10 
135    8  6 

127  24  24 

141  14  24 
159    o  35 
o  27 
124  14  3 

13  39 
126  11  7 

150  15  21 
154  18  ± 

122  32  8 

i34  56  - 
H7  54  33 
97  18  23 

139  23  50 


Position. 


200.1 
196. 1 

197.O 

133-5 
329.I 

119.8 
230.1 
121. 6 
344± 
I35± 
329.3 
(  328.1 
I  !33-° 
204.6 
301. 1 
302.3 
268.8 
220+ 
87.3 

5°± 
3  io~t~ 
125.5 

S  5°± 
(  23°± 
193.0 

55-7 
54-4 
302.7 

357-  8 

358-  3 

359-  3 
66.1 
30+ 

216.5 

<  144.4 

<  23-5 
87± 

312.5 
320.3  : 
122.9 
129. 1 
72.6 
314.8 

33-8 

79.8 
3H-3 

120-1- 


Dist. 


Magnitude. 


7  =  7 
6'  7 


9  13 
11  12 
10 

8  8' 
10'  12 

9  9 
10  13 
10=10 

9  !3 
11=11 
1 1 
H 
10 


9  10 

9'=  9' 
ii'=ii' 


II 

12 

9 

1 1 

9 

11 

9 

12 

8' 

11 

9 

10 

9 

1 1 

7 

12 

8' 

10 

8 

1 1 

8 

10 

1 1 

J3 

9'= 

=  9' 

8 

12 

7 

15 

7 

15 

9' 

10 

9' 

10 

9 

10 

9  =  9 
10=10 


1 1=1 1 

5'  i2 
9'  10 


Remarks. 


Synon. 


Sweep. 


142 


Pos  20.7,  19.6  ;  crawling  and  tremulous   B.  2546 

Pos  195.7,  196.6.    Elongated  with  180,  divided  and 
measured  with  320  in  intervals  of  S.E.  gusts. 

Pos  with  320,    198.3,  197.3,  195.5.     A  superb 
double  star. 

The  chief  of  a  p  L  rich  cluster  

Reduction  of  place  somewhat  doubtful  

Sextuple  

Fine  

Reduction  of  place  somewhat  doubtful  

A  R  A  =  3s.o  

Position  rough   

A  B.    Pos  estim  from  diag   

(A  +  B)  C. 

H\  Triple  large  *  orange  red  

Very  neat  double  star  

Pos  by  diagram   

Pos  by  diagram   

AB^Trinle 

Pos  66.5,  65.8  

Very  neat  star  ;  pos  by  diagram   

|TripIe   

Large  star  very  red  

Pos  314-8,  3 1 1.3,  311.5-    A  large  star  n  f  

In  an  extra  merid  f.    Pos  ?  ?  

Pos  123.3,  121. 8,  123.6   L.  4031 

Very  neat  star  

A  third  %  11  m  near  

sf  »  Argus.    A  neat  D  H«   

Class  6.    Review  of  B  

Glimpses  between  clouds   


B.  2644 


776 
553 

680 

763 
429 
810 
678 
429 
782 
564 
678 

540 
782 
772 

784 
684 
561 
440 
566 
771 
771 
688 

440 

540 
684 

435 
568 

555 
772 

554 
429 
678 
553 
540 

440 
429 
537 
54i 
809 
572 

777 
430 

678 

E 

43  S 
647 
442 


202 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1830.0. 
h.   ni.   s.  d. 


N  P  D.  1830.0 


Dist. 


Magnitude. 


Remarks. 


Synon. 


4258 

4.259 

4260 
4261 
4262 
4263 
4264 

4265 

4266 
4267 
4268 

4269 


4270 
427i 

4272 
4273 

4274 

4^75 
4276 

4277 

4278 

4279 
4280 

4281 

4282 
4283 


4284 

4285 
4286 
4287 
4288 


9  44  i7-o 
21.9 

9  44  45-5 
45.8 

9  44  47-9 
9  45 

9  45  4°-8 
9  46  4i-7 
9  47  n-5 
9  47  37-2 

37-5 
9  48  8.9 
9.8 

9  48  39-3 
9  50  26.4 
9  50  28.7 

35-7 
9  51  11. 6 
9  51  22.3 
9  51  24.6 

9  51  27.9 
9  51  35-4 
35-7 
9  52  33-4 

9  r-  39-6 
40.9 

9  53  2-7 
9  53  15-9 
9  53  23.3 
9  54  1 1-4 
12.2 

9  54  19-7 


55  13-9 

55  55-5 

55  59-° 

56  52.4 

58.4 

57  - 

58  6.3 
6.5 
6.6 


9  58  14.0 
9  58  36-3 
9  58  47-o 
10    o  — 
10    1  44.0 
10    2  36.7 

39.1 


165  6  44 
6  31 
I31  43  !7 
43  !9 
147  25  38 
108  41  5 
102    8  1 

149  37  5° 

140  42  30 
134  28  53 

28  46 
169  43  1 
43  22 

141  16  24 
131  37  30 
123  29  27 

28  40 
137  36  23 
104  8  34 
158  22  30 

22  57 
165  46  30 
125    4  48 

4  42 
175  13  10 

134  8  37 
8  41 

139  12  25 
123  52  52 

l67  55  59 
117  50  45 
52  13 

148  27  15 

73  5°  28 
122  52  41 

107  16  52 
169  36  9 

36  37 
141  15  - 

140  58  24 

59  *9 
58  10 

58  50 

135  4  21 

108  28  14 
112  18  50 
158  32  - 
i25  57  45 
165  14  49 

14  27 


162.7 
159.2 
162.0 
161. 7 
118. 5 
86.8 
101.7 
72.3 
215+ 
239.0 

238.7 
227.7 
222.2 
88± 
156.2 
70.4 
65.8 
316.9 
313-8 
208.7 
206.5 
302.5 
312. 1 

3H-7 
263.7 
138.1 
'36-3 
35°± 
63.6 
298.8 
29.6 
31.7 

i  3°9-6 

'  18 

1 19.7 

314.6 

270+ 

276.3 

287.6 

204.8 

178.3 

182+ 

182+ 

182.0 


72.8 
326.0 
2.0 

!95± 
1 10.8 
290.5 

287.3 


12 
10 

15 
12 
12 
12 
12 
30 

25 
8 

15 

16 

15 

2 
6 

25 
20 

12 
16 

6 

4 

30 
8 

10 
70.9 
10 


9 

9' 

9 

10 

9' 

12 

10 

12 

8' 

12 

8 

10 

9 

12 

9 

12 

10= 

=  10 

7 

9 

6 

10 

8' 

9 

1 1 

9 

1 1 

10= 

=  10 

11= 

ill 

7 

12 

9 

II 

8 

II 

8' 

9' 

10 

12 

4 

13 

6 
8' 

13 

8' 

8 

J3 

i 

11 

9' 

10 

11 

12 

10 
8 

12 

8' 

8 

9 

8' 
10 

9 

13 

1 1'= 

11' 

9' 

13 

7' 

8 

9' 

10 

10  10 

7  8 

8  9 
8  9 

8  9 
8  9 

7'  11 
8  =  8 
8'  10 

8  10 

1 1  —  1 1 
8'  8' 

9  =  9 


A  star  7' m  s  f  

Pos  71.8,  72.8  

Neat  star  

Pos  238.7,  239.3  ;  &ne 


Very  ill  defined  

Dist  by  3  oblique  transits  =  8".o4 


Pos  1 58. 1,  154.3  . 


Pos  315.7,  318.1, 


jj  Antlise  

Large  star  single  with  1 80 . 
A  R  A  =  11.5   


The  middle  star  of  3 


AB    )m    .  , 

AC|Tn,,le 


H.  145,  No.  25   

Neat  star  ;  A  R  A  =  3>.o 


Mean  epoch,  1836.537 


Pos  estimated  by  meridian  wire . 

A  very  fine  double  star  

Viewed  in  place  

L  very  yellow  


Pos  est  by  diagram.  Place  very  rude 
289.7,291.3   


B.  2723 
A.  81 


Pos  209.7,  207.8  

Pos  207.3,  205.7.    In  an  extra  merid  f 


B.  2758 
h.  825 

B.  2760 
R.  12 

B.  2759 


B. 2766 


L.  4106 


Sh.  no 


B.  2824 
L.  4147 


L.  4146 
a.  356 


DOUBLE  STARS. 


203 


No. 

R  A.  1839.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

xtGrnarKS. 

Synon. 

Sweep. 

h. 

m.  s.d. 

0      1  n 

4.289 

10 

2  45.8 

i53  45  5i 

241. 1 

0 
0 

10=10 

i^xcessiveiy  ill  denned,  so  as  nardly  to  be  measurable 

430 

49.9 

45  56 

233.6 

IO 

10  10 

568 

IO 

3  4-9 

72  48  39 

95-4 

2 

9'  10 

rC\  G  r\  A    t     r\r\  t 

2.  14.13 

688 

4290 

IO 

3  *3-6 

134  57  21 

305.3 

*5 

7  «' 

774 

16.0 

56  15 

310.5 

15 

8  11 

776 

300+ 

12 

8  12 

Pas  pcf~iiYinf"Pfl  frr»m  ^iaornin 

695 

4291 

IO 

3  39-° 

147  49  10 

216. 1 

^ 

11=11 

A  m nncr  m an v  Gfnr^ 

435 

4292 

3  57-2 

154  59  21 

122.0 

35 

6  10' 

D.  25/1 

568 

IO 

4293 

IO 

4  57 

105  15  4 

278.8 

12 

9  10 

687 

4294 

IO 

4  387 

162  24  31 

r 

2D3.4 

10    1 1 

547 

4295 

IO 

5  0.0 

36.4. 
J  *T 

20 

6  11 

L.  4203 

C  C7 

jji 

lL2  (J  6 

IO 

5  27-6 

72  23  8 

137.9 

12 

9  12 

688 

A2Q7 

IO 

5  52-i 

144  16  29 

302.6 

6 

IO=IO 

436 

5  53-3 

16  41 

307.7 
Oil 

10 

0  IO 

J 

552 

102.1 

12 

10  II 

784. 

2  8 
429 

IO 

6  25.7 

ICQ   1A  IO 

278.5 

1 1  =  1 1 

429 

2J 

4299 

IO 

6  48.4 

140    3  40 

320-t- 

50 

9  9+ 

442 

4300 

IO 

8  5-9 

122  25  29 

IO3.5 

9  9 

535 

7.2 

26  40 

IO9+ 

5 

io'=io' 

678 

4301 

IO 

8  49.9 

154  52  1 

2O.3 

5 

9  9 

568 

IO 

9  8.3 

103  33  31 

128.0 

15 

9  10 

h.  831 

687 

4302 

IO 

10  417 

147    8  9 

A  double  star  in  the  vertex  of  a  great  crescent- 

552 

shaped  nebula. 

42.9 

II9.8 

25 

10    1 1' 

784 

8  9 

4303 

IO 

12  I^-S 

in  45  31 

89.3 

10 

8  9 

559 

A.7QA. 

IO 

12  32.5 

122  16  17 

289.7 

12 

8  11 

B.  2945 

678 

1 1 2  4.7  1  c 

*r/  j 

2I3-5 

18 

8  10 

R  A  liable  to  error  for  want  01  zero  stars  in  this  J  . . 

558 

A3o6 

IO 

13  - 

I  <s  7   4Q  — 

J  J  T7 

139.8 

1.4 

7  =  7 

B.  2955 

E 

4307 

13  17.0 

140    42  4O 

245± 

12 

8  11 

B.  2951 

442 

4308 

IO 

14  7-3 

l6l    12  59 

S  60.4 

15 

9  =  9 

lc\  TriPle  

546 

i  332-2 

8 

9  J4 

25.8:: 

12  s 

57-3 

15 

10=10 

R  A  very  precarious  throughout  this  J1,  for  want  of 

429 

zero  stars. 

4309 

IO 

14  21.5 

119  28  58 

5°± 

15 

10=10 

564 

43 10 

IO 

14  33-5 

'73  14  45 

278.0 

9  10 

T»                O  H 

779 

3 

IO 

14  34-3 

145  11  9 

S  103.4 

5 

5'  IO 
5  10 

A  rS.     irOS  103.0,  101.5,  I037j  105.4  v 

Jj.  2972 

436 

£  188.2 

30 

357 

11  13 

S  1054 

7 

5  10 

A  B.    Pos  106.2,  104.8,  105. 1  ) 

K.  13 

552 

\  188.0 

30 

5  9 

A  C.    Dist  estim  from  diagram  $ 

43" 

IO 

H  59-5 

102  31  10 

122.3 

4 

7  H 

TTl  JI  1  J)    1  "  4    1    1  <_'/»__  1 1  

687 

4312 

IO 

15  28.5 

117    7  17 

268.1 

30 

7  11 

L.  4276 

776 

4313 

IO 

15  45.0 

118  42  52 

138.3 

7 

10=10 

45i 

A-7 14 

TJ  X 

IO 

15  56.8 
59.1 

156  39  59 
40  31 

11. 3 
9.1 

18 

20 

9  9 
8  8' 

556 
538 

4315 

IO 

16  18.0 

133  15  48 

210.3 

25 

9  9' 

686 

18.9 
16  57.1 

16  1 

131  53  30 

209.6 
238.7 

30 
12 

9  10 
8'  13 

774 
810 

43l6 

IO 

43J7 

IO 

17  36.0 

135  18  38 

191.7 

20 

9'  12 

694 

4318 

IO 

18  7.8 

123  20  22 

23.8 

8 

10=10 

446 

43 19 

IO 

19  40.1 

143    1  25 

130+ 

10 

9  12 

438 

4320 

IO 

20  14.4 

138  55  0 

335.0 

15 

9  12 

442 

4321 

IO 

21  45.3 

119  44  12 

225+ 

10 

6  10 

A.  125 1 

45i 

432a 

IO 

22  22.2 

114    0  30 

IOI.I 

8 

7'  13 

558 

204 


REDUCED  OBSERVATIONS  OF 


Xo. 


R  A.  1830.0. 
h.  m.    s.  d. 


4323 
4324 

4325 

4326 
4327 
4328 


4329 


4330 

4331 
4332 

4333 
4334 
4335 


4336 


4337 
4338 

4339 
4340 

434i 

4342 


4343 
4344 
4345 
4346 

4347 
4348 
4349 


435° 


10  22  58.7 
10  22  58.9 
61. 1 
10  23  54.1 

55-3 
10  24  8.5 
10  24  — 
10  24  25.3 
10  24  26.7 
10  24  38.7 


41.2 
41.5 
10  24  46.4 


10  25  46.2 
46.2 
10  26  15.7 
10  26  22.5 
10  27  3.0 
10  27  3.3 
10  27  14.3 

17.4 
22.3 

10  28  21.8 
10  28  27.6 
10  29  7.3 
8.7 

10  29  25.8 
10  30  54.6 

10  32  9.6 

10  32  21. 1 

10  32  32.5 


10  33  42.9 
48.4 

10  33  43.1 
10  34  12.2 
10  34  33.4 
10  35  - 
10  35  39.0 
10  35  41.9 
10  36  28.1 
28.6 

10  36  40.6 


N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude 

0 

/ 

a 

151 

43 

40 

215.2 

15 

10 

10' 

136 

28 

42 

64.7 

5 

10= 

=  10 

29 

1 1 

64.6 

8 

10= 

=  10 

120 

28 

16 

167.7 

12 

8' 

9 

28 

41 

169.6 

10 

9' 

10 

129 

3 

16 

65 

H3 

38 



352.2 

113.7 

8 

8 

141 

0 

20 

105.0 

15 

9' 

10 

73 

55 

3 

255-7 

10 

9' 

1 1 

1 34 

11 

21 

24.2 

25 

6'. 

=  6' 

11 

38 

37-7 

'5 

i- 

=  7' 

1 2 

2 

34.7 

20 

=  7' 

142 

5i 

20 

IO.± 

15 

5 

9 

136 

7 

47 

160.6 

30 

5' 

10 

7 

52 

160.8 

30 

6 

9 

120 

3 

263.3 

'J 

11' 

11' 

136 

6 

1 2 

160.3 

25 

7 

1 1 

96.1 

30 

6 

12 

124 

31 

25 

268.0 

5 

10= 

=  10 

159 

12 

39 

217.5 

10 

9' 

IO 

9 

215.7 

10 

9': 

=  9' 

12 

0 

2 10.8 

8 

10 

10 

119 

36 

22 

ii 

10 

1 1 

102 

40 

9 

229.3 

8 

10 

153 

15 

36 

34.8 

20 

9 

9 

15 

23 

37.8 

25 

8' 

9 

108 

28 

28 

246.0 

5 

9 

IO 

i47 

44 

30 

91.5 

3 

IO 

10  4- 

102 

36 

37 

$  61.3 
)  80.1 

30 

j 

7 

13  = 

12 
=  I3 

123 

3* 

28 

124.8 

i 

11= 

=  11 

144 

42 

34 

{  IOC. 1 

i  178.0 

60 

*5 

6 
8 

8 

16 

119 

51 

44 

52.5 

18 

9 

13 

51 

42 

50.1 

'5 

8' 

11 

154 

11 

57 

98.7 

3 

10' 

1 1 

163 

41 

44 

96.7 

20 

H3 

*3 

0 

34°± 

3 

9' 

12 

150 

8 

81.3 

26.5 

8 

IO 

149 

1 

10 

149 

4 

35 

129 

11 

33 

248.8 

3 

1 1 

h' 

11 

48 

243.9 

2 

9' 

IO 

248.1 

2 

9' 

IO 

148 

50 

55 

Remarks. 


Pos  estimated  from  diagram  

Epoch  1837.099  

Dist  by  oblique  transits  =  i6'.65.  Fine  [No 
doubt  an  error  of  10°  in  reading  the  position, 
which  is  assumed,  and  a  mean  position  used  in 
calculating  the  oblique  transits.] 

Fine  double  s)c   

L  white ;  S  red.  Pos  estimated,  the  wire  being 
broken.  [Obs  gives  56'  for  the  P  D,  but  both 
Lacaille  and  the  equatorial  observation  agree  in 
making  it  51.] 

L  orange  ;  S  blue   

Pos  161. 7,  159.9;  L  pale  yell   

Large  star  orange  coloured   

Extremely  ill  denned.  The  stars  appear  like  balls 
with  photospheres. 

Pos  215.9,  215.6.    Careful  measures   

Places  not  good  in  R  A  in  this  f,  for  want  of  zero 
stars. 

Requires  verifying  

Pos  23 1.2,  227.4  

B.  3013  4-  3014  

A  very  neat  double  star  involved  in  a  nebula   

A  and  (B  +  C)  as  one  star  ) 
B  and  C  (close  double)  > 

A  B.    A  R  A  =  5<-75  j  L  yell,  S  blue  

B  C.    [X.  velorum.     The  large  stars  constitute 

the  double  He  A.  95-     The  nearer  not  noticed 

by  A.] 

The  minute  in  R  A  by  this  obs  is  34,  but  there  is 
some  reason  to  prefer  the  R  A  0^449. 

Dist  estimated  from  the  diagram   

Mean  epoch,  1837.276   

The  double  star  (g)  in  the  catalogue  of  n  Argus 
p  in  the  catalogue  of  tj  Argus. 

Stars  most  beautifully  defined  and  tranquil  

Viewed  and  measured ;  no  place  taken  

The  star  S  in  the  catal  of  n  Argus. 


Synon. 


B.3041? 


Sweep. 


2.  1446 
B.  3058 
+  3°59 


A.  88 


L.  4336 


B.  3069 


B.  3083 


2.  1453 
A.  93 


B-  3J35 
+  3136 
A.  95 


433 
695 
776 

535 
678 

554 
E 

442 
688 
774 


686 
542 
438 


553 
695 
678 
553 
547 
446 

556 

546 
429 

452 
687 
430 

55° 
560 

435 

700 

446 
436 


449 
452 

55° 
547 
438 
E 


574 
554 
810 


DOUBLE  STARS. 


205 


No. 


4351 


4352 


4353 
4354 
4355 
4356 


4357 
4358 

4359 


R  A.  1830.0. 
h.  m.    s.  d. 


4360 

4361 
4362 


4363 
4364 
4365 
4366 


4367 
4368 


4369 


4370 
4371 
4372 
4373 
4374 
4375 
4376 


10  36  41.2 
10  36  45.2 
10  36  52.2 

55.4 

10  37  8.4 

.I0. 37  - 
10  37  18.1 
10  37  23.8 

24.6 

10  37  28.2 
10  37  29.3 

10  37  29.4 

10  37  33.8 


10  37  35.2 

10  37  39.2 
10  37  54.1 
10  38  0.5 


10  38  5.3 
10  38  8.5 

IO  38  20.0 
IO   38  24.8 

28.7 
29.4 
IO   38  28.6 

10  38  49.1 
10  39  8.7 

10  39  14.0 

10  39  14.2 

10  39  28.9 
10  39  59.9 
10  40  17.4 
10  41  14.0 
io  42  13.5 
10  42  22.3 
10  42  28.7 


N  P  D.  1830.0. 


157  51  15 
150  17  15 

139  59  4° 

59  59 

148  42  17 

149  11  — 
149  3  49 
148  39  22 

39  3° 

148  58  ss 

149  11  34 

149  12  26 
148  40  56 


148  41  7 

149  2  o 
132  48  57 
148  50  40 


H9  7  34 
148  27  55 
117  15  26 

148  46  57 


47  4° 


47  28 


145  39  32 
132  34  56 

159  58  o 

148  35  42 

104  22  4 

J48  40  16 
148  38  42 
117  51  22 
130  32  22 
148-  32  55 
128  44  47 
159  37  26 


Position. 


232.3 
176.2 
220-t- 

;  212.3 
1 226.7 

228.4 

150.5 


147-3 

204.7 
199.4 

245-3 
238.6 


102.7 
106.8 
in. 3 

302+ 

206.1 


99± 
$  46.8 
I  30.3 

35-3 


157.1 

109.3 

<  38.8 
(  282.1 


$  J9-3 
(  16.8 


331.8 
226.1 

298.3 
126.2 


30 


<5 


'5 


Magnitude 


9  9 

8'  12 

6'  12 

6'  14 


7  9 


8  11 


9  11 


9  11 


9  9 
10  10 

9'  9' 


9  15 

2  16 

2  15 

1  17 


1 1  =  1 1 
8'  9 


12  =  12 

9'  10 


Remarks. 


Synon. 


Sweep. 


Marked  double  in  B.    Can  hardly  be  A.  97   

A  B  1  „   .  . 

AcjTnPle  • 

(y)  in  Catal  of  n  Argus  

Z'"  in  Catal  of  jj  Argus,  June  21,1836   

t  in  Catal  of  77  Argus  

O  in  Catal  of  r)  Argus.  Place  from  monograph, 
June  18,  1836. 

Place  taken  in  the  usual  course  of  sweeping  

Measured  April  24,  1837   

P  in  Catal  of  n  Argus  

Z"  in  Catal  of  n  Argus.    Measured  June  21,  1836 

Measured  April  24,  1837   

Z'  in  7]  Argus  Catal.    Measured  June  21,  1836  .... 

April  24,  1837.    2  measures  

[Marked  as  double  in  B.  But  one  of  its  consti- 
tuents is  a  first  class  double  star.  See  next 
star.] 

Measured,  April  24,  1837.    ^A  +  B^  C  

The  triple  star  K  in  Catal  of  ij  Argus.  Measure  of 
A  B  taken,  April  24,  1837. 

(p)  in  Catal  of  n  Argus  

Star  D  in  monograph  of  n  Argus,  marked  as  double 
in  B. 

Viewed  and  measured  hastily  

Double  star  No.  597+601  in  Catalogue  of  n  Argus 

The  star  y  in  the  Cat  of  n  Argus  

The  first  of  3  st  in  an  equilateral  triangle  

n  Argus.  The  two  closest  stars.  [N.B.  These  stars 
were  subsequently  effaced  by  the  increased  bright- 
ness of  »;.] 

[The  large  %  much  over,  and  the  small  much 
underrated,  and  the  measure  entitled  to  no  con- 
fidence.] 

[True  place  per  mean  of  Catalogues  of  Johnson, 
Taylor,  and  Rumker,  used  as  the  zero  point  of 
the  micrometrical  measures.    See  monograph.] 

AC) 

g  £  >  Triple.    Marked  as  double  in  B.    Is  A.  99 . . 

The  double  sjc  /3  in  Catal  of  n  Argus   , 

}Aandi(B  +  C)  >M- 

Double  star  m  in  Catal  of  ?/  Argus   

Double  star  a  in  the  same  Catal   

6  in  Catal  of  n  Argus  

~3^G 


B.  3181 


B.  3190 


B.  3194 


A.  1281 


B.  3203 


2.  1474 


557 

433 
442 

553 


435 


432 
434 


774 
432 

449 
432 

435 


542 

567 


700 


452 
554 

540 
546 


206 


REDUCED  OBSERVATIONS  OF 


No. 


4377 
4378 
4-379 
438o 

438i 


4382 


4383 


4384 
438S 
4386 
4387 
4388 
4389 
439° 
4391 

4392 
4393 

4394 
4395 
4396 

4397 
4398 


4399 
4400 
4401 

4402 

4403 
4404 
4405 
4406 
4407 

4408 


R  A.  1830.0. 
h.    111.  s.  d. 


10  44  21. 1 

10  45  - 
10  46  34.7 
10  46  37.6 

37.6 
10  46  45.4 

46.2 

47.2 
10  48  2.2 


3-7 

10  48  8.0 


10  48  50.5 
10  48  56.9 
10  49  22.5 
10  49  24.0 
10  50  2.5 
10  50  12. 1 
10  50  34.2 
10  51  4.2 
5-8 

10  51  23.7 
10  51  23.7 
24.6 
10  51  40.0 
10  52  58.7 

i°  S3  3°-3 
31.4 
10  54  19. 1 

10  54  30.8 
31.4 
32.7 
34.6 
10  55  28.4 
10  57  5.9 
10  57  44.8 

10  58  7.6 

10  58  54.4 

10  59  0.1 

10  59  0.9 

10  59  3.4 

10  59  6.4 

10  59  18.7 


N  P  D.  1830.0. 


162  42  20 
149  3  - 
138  24  50 
158  59  20 
60  IO 

127  51  o 


5°  S3 
153    4  24 

3  46 
159  48  50 


116    o  27 

131  8  28 
142  35  10 
146  38  38 

J34  57  35 

120  38  47 

172  18  45 

123  59  7 

58  9 

160  26  38 

158    7  59 

7  23 

132  12  48 
149  25  9 

126  7  20 

5  56 

148  56  10 

146  20  54 
21  31 

21  14 

21  33 

149  35  58 

150  26  58 
144  20  33 

127  36  30 

'33    9  3 

147  46  40 
142  21  jo 

>72  59  55 

133  7  43 

130  32  15 


Position. 


276.6 
344-4 
45± 
127.6 
125.8 
38.1 
38.9 

42.3 
8.1 

8.4 
275.8 


45± 
252.7 
io± 
i6o± 
214.6 
336.7 
328.3 

6S± 
6o± 
159.6 
131.5 
129.5 
254.1 
3-5 
257-7 
267.2 


255-5 
253.9 

249.7 

250+ 

312.5 

193.6 

230+ 

i  1 17.7 
\  85± 

237.0 

300.0 

45± 

10.2 

294.1 

\  35°-6 
(  150.6 


Dist. 


3 

30.9 
20 
15 
15 
25 
30 

28 
15 


Magnitude. 


10' 

i 
9 
9 
9 


IO 

9 
7 
9 


!3  = 

IO 

IO 


9 
9' 

9' 

9' 

10  = 


Remarks. 


Epoch,  1836.164  

Pos  36.7,  39.6  

{This  obs  gives  127  54  50  for  the  P  D,  but  there 
must  have  taken  place  some  slip  of  the  apparatus.'] 
Fine  star   

[The  obs  actually  gives  49™  1  i8.o  for  the  R  A.  But 
the  wire  was  undoubtedly  mistaken.  See  the 
next  obs.] 

Pos  277.6,  273.9,  275-9-  Something  caught  my  eye 
with  180  indicating  an  elongation.  Star  in  conse- 
quence examined  with  480 ;  superbly  separated. 
It  is  one  of  the  closest  D  ^  si  have  encountered 
in  my  observations. 

Pos  estimated  from  diagrams  

Estimated  position.    Wire  broken   

Position  estimated.  Wire  broken  

159.9,  159-3-    Fine  double  *  

In  the  following  part  of  a  cluster  

A  very  close  double  and  a  close  triple  star  involved 
in  nebula. 

Neat  star  

Position  estimated  

Pos  313.6,  311. 3  

L  red ;  chief  of  a  cluster   

A;g|Xriple   

In  a  cluster  

[B.  3394  does  not  exist.]   

Dist  =  8".  8  3  by  3  oblique  transits   


Synon. 


B.  3252 


B.  3288 


B.  3300 


B.  3314 


B.  3397 


DOUBLE  STARS. 


207 


No. 


R  A.  1830.0. 
h.  m.  s.  d. 


N  P  D.  1830.0. 


Position. 


Dist. 


Magnitude 


Remarks. 


Synon. 


Sweep. 


44°9 


4410 
4411 
4412 

44i3 
4414 

44i  5 


4426 

4427 
4428 
4429 

4430 
443 1 

4432 


4433 

4434 
4435 
4436 
4437 

443  8 


10  59  26.1 


131  42  53 


10  59  48.7 

11  1  58 

1  49.6 

2  18.8 
5  247 
5  45-9 

48.1 


4416 

II 

5 

53-3 

4417 

II 

5 

55-5 

4418 

II 

6 

9.0 

4419 

II 

7 

11.0 

4420 

II 

7 

24.4 

24.6 

4421 

II 

8 

1.4 

4422 

II 

8 

26.5 

4423 

II 

8 

29.7 

343 

4424 

II 

1 1 

37.0 

4425 

II 

12 

II  13  32.8 

343 
11  14  8.0 
11  14  15.6 
11  14  19.4 

21.0 
11  14  43.0 
11  14  47.2 

47-5 
11  16  1.9 


11  16  46.1 
11  17  19.8 

11  18  42.2 

11  18  54.6 

11  19  6.7 
11  19  11. 6 

15-3 
11  19  15.5 

,6.5 


105  2  42 
142  4  10 
118  40  52 
123  39  21 
149  23  58 
153  14  59 
H  39 


160  30  59 
144  30  3 

118  58  47 
124  9  29 
146  35  19 

35  9 
136  59  48 

119  11  12 
134  58  36 

57  23 


132  37  41 
37  27 
172  50  15 
119  58  2 
149    3  40 

3  4» 
119  57  52 

144    5  34 
5  59 
154    1  40 


72  36  5 
150  42  55 

144  32  34 
139  45  40 

143  55  20 
112  46  41 

45  55 
128  56  25 

56  48 


270+ 


265± 


205.3 

265± 

269.0 

33°± 
278.4 
128.5 
127.4 


161. 7 
i5°i 
259.4 
111.8 
282.7 

277-3 
68.7 

35»-5 
273.8 
282.1 

35i4 


175-3 
176.0 

*35-3 
280.7 
148.5 
148.0 

222.7 
220.3 
280.5 


316.7 
292.2 

248.5 

*  i»5± 
i  3°5± 
o± 
324.6 
320-t- 

196. 1 

196. 1 


7  15 

11  11' 

9'  9'+ 

10  11 

5  12 

6  14 
6  13 


10  11 

9  10 
10  =  10 
10  10+ 
9'  12 
10  12 
6'  10 
9'  » 
9  9 
9=9 

o'  10 


7  13 

8  13 
1 1  =  1 1 

11 


9 
9' 
9' 
9 
10 
10 
6 


1 1 


7  10 
9  10 


12 
12 

9  + 

13 
10 
11 


7  11 

7  13 


Too  ill  defined  for  measure  ;  attempted  with  320,  but 
growing  worse  and  worse,  desisted,  as  I  ceased  at 
length  to  be  sure  of  seeing  the  small  star.  I  have, 
however,  no  doubt  of  its  being  double.] 

Certainly  double,  but  too  ill  denned  for  measure  ; 
only  by  extreme  patience  and  waiting  for  glimpses 
could  be  satisfied.    Very  difficult. 

Difficult   

S  E  wind ;  dreadfully  ill  denned  (y  Carina)   

(This  R  A  agrees  with  B)  

[The  star  is  no  doubt  identical  with  that  of  f  773, 
No.  9,  but  to  conciliate  its  R  A  with  that  of  the 
other  observation,  a  double  mistake  of  the  2nd 
wire  for  the  first,  and  of  5"'  error  in  reading  the 
chronometer,  must  be  admitted,  which  done  the 
R  A  comes  out  as  here  set  down.] 

A  third  $  14  m  in  same  line  

Pos  256.5,  262.0  

L  red  ;  pos  281.5,  284.0   

Points  exactly  to  a  3rd  star   

Pos  352.5,  350.4  

Fine.    Observed  with  320  

Pervicinse  ;  measured  with  320,  which  barely  divides 
it ;  in  a  very  fine  interval  between  thick  clouds. 

Violently  suspected  to  be  close  double,  class  I. 
Twice  marked  as  elongated  with  highest  power. 

L  yellow  

The  second  of  a  group   

The  preceding  of  two  

Ill  defined   

The  following  of  two  

222.0,  223.5   

Suspected  double  with  180,  and  though  ill  defined 
almost  sure  ;  320  with  a  triangular  aperture 
cleanly  divides  it ;  measure  good,  though  tremu- 
lous. 

Fine  star;  pos  292.7,  291.8.  [Marked  as  close 
double  in  .B.] 

ic!TriPle  

L  very  red  

Pos  estimated  from  diagram  


B.  3400 


B.  3462 
B.  3467 


L.  4675 
B.  3501 


L.  4718 


B.  3562 


B.  3574 


L.  4750 


554 


555 

700 
438 
452 
448 
434 
773 
55° 


546 

437 
452 
446 
476 
692 

553 
452 
774 
685 

782 
E 

774 
542 

779 
452 
435 
434 
452 
436 
692 
773 


432 
436 
442 
483 

559 
690 

810 
574 


208 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1S30.0. 
h.  in.    s.  d. 


N  P  1).  1830.0. 


Position. 


Dirt 


Magnitude 


Eemarks. 


Synon. 


Sweep. 


4439 


444° 
4441 

4442 
4443 
4444 
4445 


4446 


4447 
4448 

4449 
4450 

445 1 
4452 


4453 
4454 
4455 
4456 

4457 
4458 

4459 
4460 


4461 

4462 
4463 
4464 
4465 

4466 
4467 

4468 
4469 
447° 
4471 

4472 

4473 


11  19  50.9 
11  20  23.6 
26.5 


11  21  20.4 

II  21  54.4 

II   22  I2.7 

II   22  53.6 

II   23  20.I 

II   23  53.3 
56.8 

II  23  544 
I  I  24 


I  24  304 

I  24  39.8 

I  24  40.9 

I  24  47.9 

I  25  21. 1 

I  25  24.2 

1  25  54-3 

1  26  12.8 
1  26  49.5 
1  28  — 
1  28  14.4 
16.1 
1  28  39.7 
1  28  53.9 
1  29  41.2 
1  31  4.2 
6.9 
7-3 

11  31  20.3 

11  31  45.7 
11  32  6.3 
11  32  11. 1 
11  33  16.0 
17.4 

11  34  4-5 
11  35  15.2 
16.2 

11  35  17-3 
11  35  42.9 
11  36  59.7 

11  37  37-8 
11  37  49.7 
if  39  39.2 


120  18  22 
131  44  19 
44  18 


167  35  29 
144  56  28 
143  43  40 
158  41  2 

137  44  4 
148  30  19 
30  33 

141  31  18 
118  19  52 


153  °  25 

132  45  28 

120  55  2 
162  57  33 

135  22  35 
152  57  21 

72  15  15 

138  27  30 

124  13  57 
122  38  — 
113  30  15 
30  1 
149  8  o 
162  57  28 

137  58  25 
i46  47  53 

47  59 

48  14 

155  3  57 
172  7  40 
122  38  8 
132  12  53 

121  32  48 

33  34 
148    1  35 

136  9  43 

9  59 
172  9  30 
74  26  31 
119  32  46 
155  47  36 
118  15  12 

138  4  54 


101.5 
168.0 
168.8 


166.1 

i75± 

230+ 

105.7 

139.9 

126.3 

129.7 

117.5 
29.9 


348.8 
91. 1 
170+ 
36.9 
212.0 
32 1. 1 
217.0 

130+ 
30.5 
244.9 
122.9 
120.5 
115. 8 

37-3 
i6o± 
178.0 
177.3 
177-7 

S  124.3 

t  37-i 
258.7 
248.3 
158.7 
44-5 
3!5± 
317.7 
144.3 
144.8 
158.6 
166.1 
318.2 
272.9 

39  5 
98.7 


7  11 
13  =  13 

7  10 
10  =  10 

8  9 
8  9 

7'  9 
12 
H 

10 


9  9 

9  10 

5'  14 

9'  10 

9  13 


Fine  star  

N.B.  I  find  a  memorandum  to  the  effect  that  this 
star  is  triple,  for  that  B  3595  is  a  fine  1st  class 
double  star,  but  I  suspect  some  error.  At  all 
events  it  has  not  been  verified  by  subsequent 
examination. 


A  third,  more  remote  

Position  estimated.    Wire  broken 

Neat  star  

Very  delicate   


L  very  yellow.  The  preceding  and  northern  of  two 
yellow  stars,  6  m. 

Pos  29.4,  30.4  (17  Hydra?  =  H.  III.  96).  The  obs 
gives  7.9  for  the  seconds  of  R  A,  which  arises 
from  the  moveable  wire  having  been  mistaken  for 
the  fixed. 


Points  to  two  large  stars 


\  Hydrse 


217.4,  217.7,  215.8  ;  90  Leonis.  [There  can  be  no 
doubt  that  these  measures  are  all  misread  io°. 
See  all  earlier  measures  of  this  star.] 

Very  neat  star  


Mean  epoch,  1837.031 


Has  a  bright  star  n  p . 


A  3d  sK  9' m  n  p   

Pos  a  good  estimation  by  meridian  wire 

Clouds  

Pos  177.6,  177.8  

icH16  

Very  neat  star  

Fine  star,  large  sf:  yellow  


A  third,  larger  than  13m 


Large  sfc  yell.    Small  blue 


A  R  A  =  8-.o. 


B.  3594 
+  3595 


B.  3604 


B.  3631 


A.  1354 


A.  1356 

B.  3645 


2-  1552 


B.  3670 


B.  3696 


B.  3721 


B.  7716 


404 

554 
542 


587 
437 
438 

557 
776 
432 
543 

576 
452 


55° 
686 

444 
585 
553 
55o 


442 
446 
E 

690 
559 
435 
547 
442 

437 
692 
436 

55° 

779 
54i 
686 

445 
443 
435 
553 
776 
779 
688 

445 
568 

452 
566 


DOUBLE  STARS. 


209 


No. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

{Magnitude 

Remarks. 

Sjnon. 

Sweep 

h.  m.   s.  d. 

0      /  // 

4474 

II  40  6.0 

I43    12  20 

95± 

15 

g 

438 

4475 

II  40  47.I 

I  co  •so  18 

125.4 

2 

434 

4476 

II  41  5.3 

137  19  23 

171. 1 

20 

9' 

10 

776 

4477 

II  41  49.3 

109  53  4 

108.3 

15 

g 

9 

561 

4478 

II  44  18.2 

122  57  35 

341.1 

2 

c 
i 

c' 

A. 1378 

54 » 

J 

18.4 

57  27 

33r± 

2 

5 

=  5 

Almost  a  perfect  separation,  but  the  position  of  the 
telescope  does  not  allow  following  itT  though  a 
1  longer  examination  would  be  desirable. 

444 

18.9 

57  V 

337-7 

H 

4 

5 

572 

19.3 

58  0 

342.7 

15 

5 

5' 

Pos    341.5  ;   344.0 ;  well  divided  with  triangular 
aperture  and  a  passable  measurement. 

445 

22.2 

57  45 

337-5 

12 

5 

5' 

446 

4479 
4480 

I  I  44  44.4 

II  46  8.9 

113  38  55 
143  43  13 

90.8 
184.5 

5 
3 

9 
9 

IO 

690 
576 

J3 

II  46  37.O 

151  38  0 

263.7 

20 

9 

10 

B.  3828 

432 

II  48  7.0 

121  19  11 

81.4 

20 

8 

8 

B.  3836 

445 

7.O 

19  17 

79-5 

20 

8 

=  8 

A.  116 

444 

7-7 

11  48  39.8 

'9  59 
in  35  30 

85± 
198.3 

20 

9 
8 

-  9 
=  8 

443 
690 

4481 

3 

4482 

11  49  17.5 

132  46  10 

292.7 

15 

8' 

H 

788 

4483 

11  49  22.3 
25.3 

160  25  22 
25  5 

105.3 
108.3 

12 

10: 

=  10 

583 
567 

12 

9' 

=  9' 

4484 

11  49  43.5 

129  59  42 

299.2 

i£ 

6 

12 

Very  delicate  and  beautiful.    Small  star  perfectly 
seen  and  well  defined. 

B.  3850 

810 

4485 

11  50  46.8 

131  22  39 

181.7 

18 

9' 

IO 

554 

4486 

11  5 1  - 

167  16  — 

178.3 

1.6 

6 

6' 

B.  3865 

E 

4487 

11  51  36.5 

125  48  20 

126.5 

3 

9 

9 

573 

128.3 
140.6 

3 
6 

9 
9' 

10 

Y'lPwfM  '>iwl    iyi       cli                liiif    tirv  i\l'ir>o 

574 
432 

4488 

11  51  43.0 

150  25  10 

1 1 

4489 

11  51  47.5 

113  31  0 

147.8 

0 
0 

9  ■ 

=  9 

vr       1  1 

690 

4490 

11  53  55-i 

174  41  15 

144.6 

30 

6' 

IO 

B.  3884 

779 

66.1 

42  -4r 
133  10  18 

H3-7 
41.8 

20 
30 

i 
9 

IO 

,     tj        a   T>    k                 s  -       £  1 

781 
686 

449 1 

11  55  1.1 

9 

5.0 

10  35 

42.4 

28 

9 

9 

788 

4492 

11  55  7-4 

143  46  23 

272.7 

15 

8 

12 

B.  3897 

576 

4493 

11  55  52.7 

145  40  0 

5  9°-9 

8 

9' 
9' 

IO 

A  R  1 



784 

(  3 1 1-6 

I  c 

j 

14 

4494 

11  56  59.4 

138  54  24 

(  714. 

*5 

9' 
9 

9' 

AB)m.  , 

xc!TnPle  

566 

(  7-7 

0 

1 1 

4495 

11  57  22.1 

122    0  44 

319.0 

4 

7' 

9 

B.  3918 

445 

318.8 

3 

7 

9 

A  very  fine  double  star 

444 

449 6 

11  57  27.6 

107  57  19 

30.0 

10 

8 

9 



56, 

4497 

11  57  28.1 

136  48  52 

323.9 

6 

11 

12 

776 

449 8 

11  57  36.2 

154  45  56 

58.8 

15 

7 

9 

B.  3921 

581 

4499 

11  57  42.3 

125  57  25 

45-9 

12 

10= 

=  10 

571 

4500 

11  57  54.6 

"6  55  3 

32.7 

5° 

6' 

B.  3922 

574 

9 

4501 

11  58  8.0 

m  39  57 

297.7 

30 

5' 

1 1 

B.  3923 

55° 

4502 

11  59  48.7 

165  31  49 

359-3 

18 

9' 

IO 

5S6 

12    0  37.3 

100  53  27 

$  89  9 

12 

7 

9 

A  B  ) 

2.  1604 

59i 

I  93-° 

60 

7 

8 

4503 

12    1  52.9 

147  52  10 

249.8 

6 

9' 

11 

435 

4504 

12    2  45.6 

172  24  35 

214.4 

30 

6 

IO 

779 

12    2  53.4 

96  39  2 

272.3 

5 

10 

11 

h.  845 

697 

3  H 


210 


REDUCED  OBSERVATIONS  OF 


N'o. 


R  A.  1830.0. 
h.  ra.    s.  d. 


4505 


4506 

45°7 


4508 


4509 
4510 
4511 
4512 
4SJ3 
45 14 
4Si5 

4516 

45  !7 
4518 


45 19 
4520 
4521 


4522 

4523 
4524 

45*5 
4526 


4527 


12   2  55-5 
558 

12    2  57.5 
12    2  58.3 
12   4  2.2 
2.5 

13-5 
12    4  59.7 


54.6 
56.6 
24.9 
30.9 
56.2 

2.7 
15.0 

6.5 
19.3 
52.1 
20.8 
29.5 

37-5 
9.2 


1 1 


12 
12 
12 
12  10 
12  10 
12  10 
12  12 
12  14 
12  14 
12  15 


12  15  10.7 

12  15  £1.1 

12  15  29.3 

12  15  36.4 

12  17  II. 2 


II-5 


12  17  22.0 

12  17  59.6 

12  l8  46.6 

12  20  24.2 

12  20  56.3 

12  21  46.2 

12  22  47.I 

12  24  l8.2 


XPD.  1830.0. 


119  39  53 
42  17 

105  50  26 
113    1  45 

133  57  3 
57  10 
56  36 

134  46  37 

144  50  19 
50  20 
96  17  53 
116  9  37 
126  32  18 
144  34  24 

'S3  3  35 

122  20  44 

116  29  17 

158  49  47 

100  31  27 

153  2  51 

109  18  54 

130  25  56 


121  27  4 

141  53  10 

121  57  59 

147  10  35 

152  9  30 


9  15 


9  15 


158  32  7 

146  40  26 
149  5  48 
146  52  48 
142  15  30 
146  9  39 
100  8  43 
112  53  47 


Position. 

Dist. 

Magnitude. 

267.3 

12 

8' 

13 

270.0 

12 

8 

12 

280.8 

8 

6 

8 

15.8 

4 

8 

*3 

227.4 

20 

8 

9 

226.9 

20 

9 

10 

222.9 

20 

9 

10 

247.2 

4 

5' 

7 

32.4 

30 

9 

10 

32.6 

30 

9' 

10 

289.3 

10 

8  = 

=  8 

124-1- 

*5 

9 

12 

35-8 

12 

9' 

10 

302.1 

12 

10 

10' 

3*3-5 

30 

5 

16 

93± 

25 

8' 

11 

n6± 

12 

10= 

:io 

51.1 

*5 

9 

II 

170.3 

15 

9- 

=  9' 

98.5 

15 

0' 
a 

I  I 

186.3 

15 

8 

9 

208.1 

10 

8 

10' 

209.0 

10 

8' 

11 

go-t- 

5 

10= 

.10 

215+ 

35 

9 

9' 

279.5 

6 

10 

12 

335-6 

4* 

9  = 

=  9 

1 19.0 

42 

3  = 

=  3 

197.7 

120 

<1 
J 

c 

J 

148.7 

60 

3 

*3 

100 

3 

H 

93-7 

120 

3 

11 

115.6 

5 

2 

2 

197.8 

1 20 

2 

5 

146.2 

r  „ 
OO 

2 

12 

1 18.7 

IOO 

2 

15 

107. 1 

I30 

2 

13 

118.7 

155.6 

61.8 

5 

8' 

9 

276.0 

7 

10' 

11 

338.9 

30 

9 

11 

263+ 

12 

9 

9' 

38.0 

120 

2 

5 

191+ 

15 

9 

9' 

94-3 

2 

11= 

1 1 

Remarks. 


Synon. 


A  fine  double  star   

[P  D  uncertain,  owing  to  a  sudden  jump  in  the 
zero  stars.    The  former  to  be  preferred.] 

Fine  double  star  

An  elegant  object   

[Probably  10s  error  in  time]  

Pos  245.9,  248  6.  Both,  stars  yellow;  a  very  fine 
object. 

Fine  star  

Too  ill  defined  for  measure   

A  third  *  ic  m  nearly  n  of  B,  dist  10'  

£  Cruris.    [Small  star  probably  underrated.]  

Very  ill  defined   

[Lacaille's  R  A  exceeds  this  by  35'.  A  mistake  in 
the  wire  supposed  would  give  12  15  49.1.] 

L  fine  yellow,  S  blue;  past  merid  

Pos  335  6,  336.8,  334-3.  [Marked  as  double  in  B.] 
A  B.    Pos  121. 6,  120.5,  117. 2,  116. 3;  a  Cruets  .. 

A  C.    Pos  198.6,  196.8  

AD  

A  E  

A  F.  [The  angle  probably  misread  io°.  The  dia- 
gram agrees  with  this,  and  the  true  reading  was 
doubtless  103.7.] 

AB  

A  C. 

A  D. 

AE. 

A  F. 

AB  

[Query  if  R  A  should  not  be  i2h  16™,  which  has 
tivice  been  registered  in  the  eqtiatorial  measures.] 

Double.    No  description   

A  third  n  f  

Pos  37.5,  38.4  (y  Cruris)   


a.  402 


B.  3967 
R.  14 


2.  1619 

B.  3994 

2.  1635 
L.  5138 


B.  4042 
AC.  1426 
-f  1427 
A.  122 
R.  ,5 


A.  124 
2.  1649 


DOUBLE  STARS. 


211 


No. 


E  A.  1830.0. 
h.  m.   s.  d. 


N  P  D.  1830.0. 


Position. 


Magnitude 


Remarks. 


Synon. 


Sweep. 


4.528 
4529 
453° 

4531 
4532 

4533 

4534 

4535 

4536 
4537 
4538 
4539 


454.0 


454i 
4542 

4543 
4544 


4545 
4546 

4547 

4548 
4549 


12  25  13.9 
12  25  19.6 
12  25  42.6 

12  26  40.7 
12  26  52.6 

12  26  56.2 
12  26  59.6 
12  27  26.9 
12  28  38.8 

39-3 
12  28  51.5 
12  29  29.0 
12  29  58.2 
12  30  18.3 
12  31  44.1 
12  32  11.0 


1 1.9 


13.3 


12  32  24.5 
25.0 
12  32  25.5 

33-6 
38.4 
12  32  29.7 
12  33  35.8 
12  33  45.3 
12  33  54.0 


12  34  49.4 
12  35  14.7 
12  35  41.0 

41.6 

12  36  40.1 

12  36  55.7 


121  9  30 
168  2  59 
136  20  28 

141  16  5 
101    5  10 

122  10  4 
128  55  35 

97  21  4 

147  10  8 
10  20 

156  15  39 

100  34  51 

133  50  10 

119  51  24 

172  43  45 

138  1  46 


1  14 


1  33 


102    4  53 
4  33 

l6l   51  12 
15 

5°  53 
152  2  14 
113  40  35 

H7  57  53 
168  31  54 


164  15  9 
141  49  23 
150    2  53 

2  42 

145  32  24 

113  30  30 


163.8 
322.6 
243.8 
236.9 
i5± 


265+ 

77-5 
312.7 
279.5 
278.4 
336.4 
267.7 
101.7 

355± 
274.2 

34°± 


340.8 


34°± 


120+ 
125.3 
170.0 
165.4 
166.3 
130+ 
60.6 
98.4 
299.3 


189.3 
222.1 
52.8 

47-3 
173-5 
i35± 


>5 


15 


7  12 

9  '3 

9'  H 

9'  J3 

9'  10 


10  11 
6  12 

9'=  9' 
10=10 
10=10 
7'  12 
8'  10 
9  Ji 
9  « 
10  10' 


4  =  4 


7  =  7 

7  7' 
9  =  9 
9  =  9 
9  9' 

7'  12 
9  11 

8  14 


9  9 

8'  10 

8  11 

7  10 

5  9 

10'  11 


Viewed  and  measured  past  merid  

An  elegant  triple  star  forming  nearly  an  equilateral 
triangle.    Between  2  bright  stars,  7  m. 

A  R  A  =  2!.o  

L  red,  S  blue-green   

Neat  star  

(y  Centauri.)  [Pos  estim  from  diag.]  Seen  de- 
cidedly elongated  in  a  position  as  per  diagram, 
with  320  and  triangular  aperture,  but  all  attempt 
at  a  measure  confounded  by  constant  boiling  and 
working  of  the  star. 

180  with  triangular  aperture  shows  it  elongated; 
320  fairly  double  and  almost  divided.  Pos  with 
320  =  338.3,  with  480  (which  shows  a  black 
division)  =  343.3. 

Seen  decidedly  elongated  with  320  and  diminished 
aperture,  but  so  violently  agitated  and  ill  defined 
that  no  measure  could  be  got.  That  set  down 
may  err  200. 

(y  Centauri.)  A  star  4  m,  which  I  am  very  much 
inclined  to  believe  close  double,  but  could  not 
verify  it  owing  to  bad  definition.  Tried  320,  but 
it  will  not  bear  that  power. 

A  very  fine  double  star  

Fine  star,  but  ill  defined  

Pos  171.9,  168.6,  169.6  

Pos  166.6,  166.0  

In  cluster.    Pos  est  from  diag  ?   

Large  star  red  

At  times  sure  of  the  existence  of  the  small  star,  at 
others  I  cannot  see  it.  It  will  not  bear  power 
to-night.  I  should  like  to  see  it  again,  though  on 
the  whole  there  is  hardly  a  doubt,  e  e  difficult, 
however. 

Viewed  again,  past  merid,  the  stars  being  now  much 
clearer  and  better  defined.  No  doubt  remains. 
I  see  the  small  star  steadily,  but  it  is  e  e  F,  and 
not  above  2^"  dist.  Power  240  insulates  it  com- 
pletely. 

Pos  189.4,  1893  

Pos  221.6,  222.7  

L  red,  S  blue  

L  yell,  S  bluish  


5205 


2.  1639 


L.  5214 
h.  848 


B.  4126 
2.  1664 


A.  1463 


2.  1669 


B.  4178 


B.  4182 


445 

586 

553 
776 
438 
59i 

443 
456 
697 
434 
435 
580 

59i 
455 
443 
779 
766 


566 


695 


553 


59' 
698 

583 
567 
569 
778 
690 

434 
783 


783 


569 
576 
434 
432 

43  6 
690 


212 


REDUCED  OBSERVATIONS  OF 


No. 


+55° 

+551 

4552 
4553 

4554 
4555 

4556 

4557 
4558 


4559 
4560 


4561 

4562 

4563 
4564 

4565 
4566 

4567 


4568 


4569 

457o 
457i 
4572 
4573 
4574 
4575 

4576 


R  A.  1830.0. 
h.  m.  s.d. 

NPD.  1830.0. 
0      /  // 

Position. 

Dist. 

Magnitude 

12 

37  56-2 

156 

12 

46 

93-4 

'5 

8 

9' 

58.4 

11 

18 

X9.3 

12 

8' 

9 

12 

39  I0-5 

113 

53 

4 

321.2 

20 

IO: 

=  10 

13.2 

53 

30 

3I7-5 

12 

IO 

10' 

12 

41  44.2 

'35 

55 

59 

3J3-7 

25 

9' 

IO 

12 

42  10. 1 

1 18 

49 

!3 

348.6 

8 

IO 

1 1 

12 

42  31.6 

99 

*5 

3 

308.3 

30 

8 

9 

12 

42  35-5 

120 

8 

46 

28± 

18 

6 

IO 

12 

44  10.2 

132 

s 
0 

40 

302.1 

25 

g 

'3 

I  2 

44  39-6 

146 

'4 

29 

15-5 

45 

5 

g 

39-7 

9 

15.9 

40 

5 

5 

45  7-1 

1 17 

18 

83.0 

7 

g 

10. 0 

84.3 

4 

6' 

0 
0 

45  43-7 

137 

28 

4U 

349-5 

15 

9 

I  2 

46  4  *  •  1 

119 

*3 

182.8 

20 

9 

9 

4.1.7 

12 

39 

181. 1 

20 

9 

=  9 

12 

47  2-3 

126 

28 

1 

158.0 

12 

9 

12 

12 

48  36.7 

128 

0 

0 

251.4 

25 

7 

H 

40.0 

I 

0 

251.4 

25 

6 

J3 

12 

49  3°-5 

166 

55 

54 

41.3 

12 

IO 

10' 

12 

49  5" 

144 

58 

4i 

128.8 

2C 

J 

9 

9' 

12 

49  51-6 

i37 

36 

31 

77,  7 

12 

9 

9' 

12 

5i  45-2 

122 

42 

r7 

229~f~ 

e 

7' 

8 

12 

52  43-i 

144 

45 

24 

22  1.6 

18 

9 

1 1 

12 

52  44-3 

171 

48 

25 

7  C  1 

28 

8 

11 

12 

55  1-2 

167 

32 

10 

2I9.4 

6 

15 

12 

56  27.2 

137 

32 

33 

87  7 

°7-3 

5 

!3 

27  8 

32 

e. 

D 

83.3 

12 

5 

16 

81.9 

IO 

5' 

14 

12 

56    51. 1 

151 

12 

!3 

278.6 

12 

9' 

II 

53-4 

1 1 

15 

270.3 

'5 

9 

12 

12 

57  i3-6 

154 

*3 

46 

185.0 

4 

7 

IO 

I5-3 

23 

42 

187.0 

5 

7 

9 

12 

57  47-2 

'45 

46 

29 

242.0 

4 

8' 

11 

47-5 

46 

14 

238.0 

6 

7 

10' 

12 

58  16.6 

126 

16 

40 

226.0 

*5 

9' 

1 0 

!3 

2  1.7 

124 

*3 

11 

266.4 

15 

7' 

IO 

13 

2  21.3 

121 

21 

57 

307.4 

25 

9 

9' 

*3 

3  23.2 

H5 

21 

34 

56.5 

4 

IO 

1 1 

!3 

4  40.8 

121 

20 

37 

163.3 

18 

8 

13 

5  25.7 

116 

57 

42 

76.1 

20 

9 

9 

26.2 

57 

30 

74-4 

15 

9' 

IO 

13 

5  39-8 

146 

9 

47 

129.7 

6 

7 

10' 

*3 

6  1.2 

100 

27 

12 

53-i 

5° 

7 

8 

2.2 

27 

38 

58.5 

45 

6' 

7 

Remarks. 


Synon. 


Neat  double  star  

Between  two  B  stars  

Has  a  L  *  s  p,  and  another  n  f   

Pos  16. 1,  15.0  

Pos  16.5,  16.4,  15.2   

Fine  D  star,  but  ill  denned   

Obs  gives  R  A  12  47  12.7,  but  if  a  mistake  of  the 
wire  be  presumed,  the  result  is  as  here  set  down. 

Well  measured  

[Pos  215.4  *M  MS.,  but  this  is  irreconcilable  with 
the  diagram,  which  represents  the  small  star  as 
about  20°  s  p  {or  in  pos  250),  so  that  no  doubt 
the  reading  must  have  been  251.4,  and  the 
figures  transposed  in  the  writing  down.] 

[In  this  obs  the  pos  as  measured  agrees  with  the 
diagram.] 

B.  4268  4-  4271  

The  2nd  of  3.    The  3rd  is  north  of  both  

Pos  221.8,  221.3.    Both  red  

A  R  A  =  i2%5   

Points  exactly  toa3rd  *  =  14m  

f  Centauri.  A  most  beautiful  object,  but  ill  defined 
to-night.    Bears  lamp  illumination. 

Pos  82.0,  84.7.  The  most  delicate  object  imagin- 
able, but  too  ill  defined  for  measures. 

Viewed.  A  most  beautiful  object.  Another  measure 
gave  78.8,  but  this  was  condemned  on  re-exami- 
nation. 

Large  star  very  red  

L  very  red,  S  white   

Fine  ^c.    Pos  185.2,  184.7   

(0  Muscce.)    Fine*-    Pos  187.8,  186.3   

Fine.    Pos  241.8,  242.2   

Pos  236.8,  239.3.    Fine  *   

Pos  129.8,  129.6   


B.  4191 


2.  1682 
L.  5301 
B.  4233 
A.  1485 
A.  126 


B.  4263 


A.  127 

L.  5360 

B.  4290 
B.  4306 
B.  4316 


B.  4323 

A.  129 

B.  4330 


L.  5426 


B.  4378 

(7.  434 


DOUBLE  STARS. 


213 


R  A.  1830.0. 
h.    m.  s.  d. 


4577 
4-578 
4579 


4580 
4581 
4582 
4583 
4584 
4585 
4586 

4587 
4588 
4589 
459° 
4591 


4592 

4593 
4594 
4595 

4596 

4597 


4598 
4599 

4600 
4601 
4602 


4603 
4604 


4605 
4606 


13  6 

13  8 

13  10 

13  11 

13  13 

13  13 

!3  13 

13  14 

13  14 

13  15 

13  16 

13  16 

13  16 

13  17 

13  18 

13  18 

13  20 


2.2 

2.2 
18.2 
18.5 
43.1 
46.1 

7-4 
41.8 

0.9 
36.2 
32.2 

28.0 
33.0 
27.8 
42.1 
44.6 
6.0 


6.8 

13  20  14.7 

13  23  0.9 
13  24  20.6 
13  25  29.6 
30.2 
*3  25  37-5 

13  26  22.5 
13  27  26.1 
26.5 
13  27  29.8 
13  27  42.9 
13  28  41.4 
13  28  49.4 
13  29  14.8 
13  29  58.3 
60.1 
61. 1 

13  31  8.7 
13  3i  15-5 
17.1 
17. 1 
13  31  41.4 
13  32  11. 6 
18.2: 


NPD.  1830.0. 


148  55  5 


126 
153 


150 


6  32 

9  46 

9  8 

5  4^ 

4  47 

137  40  - 

168  53  14 

163  17  52 

153  35  46 
173  30  45 

173  34  55 
156  59  - 
96  41  14 
132  9  40 
129  16  36 
144  1  27 
166  40  44 
150    3  21 


1  59 

149  49  10 

112    6  55 

169  42  29 

124  45  45 

46  7 

'54  53  59 

119  45  28 

115  37  23 

37  22 

164  15  13 

119   4  28 

96  59  S3 

138  7  42 
128  49  24 
134  50  30 

50  o 

50  40 

139  46  24 
117  22  25 

23  18 

23  44 

119    3  8 

112  35  25 

36  30 


S  231-6 
I  53-8 
159.1 

98.0 
98.5 
342.6 

342-3 
10.2 
281.9 
23.0 
232.0 
270.3 
300.3 
149.4 

77-3 
90.0 
141.4 

99-3 
136.6 
46.7 


45.2 
222.8 

90.3 

99-5 
100.6 
94.8 
94-5 

195.1 
194.9 
191.4 
40.5 

220.8 
120.0 
277.6 
189.3 
190.1 
190.4 

1 46. 1 
282.8 

287± 

281.5 

28l± 

350.8 
355± 


Dist. 


3 
70 
60 

1 
10 

15 
40 

8 
15 
3-7 

4 

3 
30 

*5 
25 
6 


Magnitude 


8  10 

9  10 
10  '10' 

6  12 

8  11 


I  I  : 

7' 

9  = 


Remarks. 


Synon. 




Pos  96.9,  99.1.    Fine  star  

Pos  99.4,  97.6.    Elegant  object   

Coarse.    B.  4420  -+-  4421  

(z  1  4-  z  2  Centauri)  

Epoch,  1836.192   

A  R  A  =  5  .5  

Mean  epoch,  1837.450   

A  beautiful  D  star  

Pos  by  parallel  wire   

In  centre  of  a  F  but  much  comp  cluster.  [N.B.  This 
obs  gives  for  the  minute  of  R  A  21,  and  for  the 
degree  of  P  D  149.  Both  are  wrong,  by  com- 
parison of  this  and  the  next  obs.  In  f  596,  an 
object  whose  N  P  D  =  1490  3'  could  not  have 
been  observed.] 

In  a  cluster  

Points  a  v  1  south  of  a  3rd  star,  at  about  3  times  the 
distance. 

R  A  uncertain  for  want  of  zero  stars   

A  neat  double  star  

Neat  

Mean  of  93-7,  95.8  

Pos  94.3,  94.8.  Power  320  and  large  equilateral 
triangle  aperture,  beautifully  denned. 

Fine         Pos  195.3,  1945   

Too  ill  defined  for  measure  (f  Hydrse)  

A  double  ij5  s  f  a  nebula   

Fine  double  star  (,  8 1  Virginis)  

Wind  gusty  

[This  obs  gives  P  D  =  135°  o'  40",  but  the  other 
observations  show  by  their  agreement  that  this  is 
10'  wrong  read  off.] 

Has  a  nebula  following  

R  A  uncertain  for  want  of  zero  stars   

~3~i 


B.  441 1 

A.  133 

B.  4431 

B.  4437 


B.  4460 
J743 

L.  5548 
L.  5551 
B.  4474 


B.  4540 

A.  1552 
A.  138 
L.  5592 

2.  1763 


214 


REDUCED  OBSERVATIONS  OF 


R  A.  1880.0. 
h.  m.  s.  d. 

N  P  D.  1830.0. 
0      1  11 

Position. 

Dist. 

Vlagnitude. 

Remarks. 

Synon. 

Sweep. 

4607 

13  32  17.8 
21.9 

161    8  20 

73-7 
78.6 
172.8 

1 2 

9' 
9' 
8  = 

1 1 

598 
567 
572 

7  5 

12 

11 

4608 

17   72  7J..I 

A 
T 

=  8 

rfl«S    177  O      T77  7 

L.  5649 

7  CO 

6  42 

167.7 

A 

9  = 

=  9 

Vprv  tiTlp  Qfar 

446 

T 

'3  32  3^-9 

T<5      <7  T  1h 

I  tLO     —  1      —  V 

89.8 

7  O 

8 

9 

a  r>  A        f*rt         'lit                       4'  J 
za  IV  j\  —  5  .0.          142,  oiti  no  .stars  14  «1  noticed 

between  the  two  large  ones.] 

T> 

B.  4597 

+  4598 

5  oZ 

4009 

13  33  37.1 

13  33  53-1 
13  35  31.7 

126  48  40 
114    6  56 
169  25  9 

150.4 
71.4 
3 1 1.4 

8 

9 
8' 

573 
453 
783 

25 
25 

_ 

h.  2671 

4010 

7 

!3 

461 1 

13  35  48.9 
13  36  53.2 

128  36  8 
ioi  34  23 

ioo-t- 
160.3 

3 
25 

10= 

:io 

460 
698 

6 

12 

2.  1780 

4612 

13  37  0.4 

125  23  57 

346.6 

25 

5 

H 

B.  4627 

572 

24  1 1 

QllPTTJ  IT  it"  nnvp  nnf"  Pdmrnnirtnc 

446 

17    7  7    7  8  *7 

TCI    IA  I 

7  c  8 
35.0 

8 

8 

T*fti  1 1  n    i/i  7       T.  rpfl    S  crrppn  —  A  Tyi*? 

T>      A  £_  _ 
LJ  .  avZU 

+  4630 

co6 

4613 

13  37  37-9 

119     30  58 

22Q-4- 

15 

9' 

9' 

451 

4614 

17    78    l8  7 

J32  '7  55 

277.8 

l5 

9' 

10 

788 

4615 

*47  *3  7 

'45-5 

JS 

9' 

10 

RaI*1i  irpllnnr 

694 

17    70  CO 

136  31  17 

250.0 

9 

10 

T*rw  7  cX  7  7C77 

zi.  144 

695 

C  7 
J '  J 

31  41 

260.9 

7 

9 

9' 

463 

Co 

30  51 

259.9 

g 

9 

9' 

464 

40 1  0 

17    70  Q.8 

160  19  20 

347-5 

9' 

12 

567 

4617 

I  7   A.I      C  1 

119    1  5^ 

255± 

4 

8 

12 

504 

13  41  10.6 

TAT     C  7  A.8 

285.8 

18 

7 

8' 

Pos  285.6,  287. 8,  285.1.    ?  if  A.  147.    Is  certainly 
R.  18. 

B  a6<c 
+  4656 

C76 

46l8 

13  41  II. 6 

128  37  22 

339.6 

12 

9 

1 1 

460 

4619 

13  41  32.2 

137       I  3 

196.8 

20 

8' 

10 

464 

13  4-  2.1 

122      8  27 

1 12.2 

15 

6 

7 

(k  Centauri  =  A.  148.    Pos  112.4,  112. 3,  111.9; 
good  measures  with  triangular  aperture. 

B.  4662 

701 

4620 

13  42  8.6 

I46    58  4 

83.5 

2 

1 1= 

=  11 

436 

4621 

13  42  8.6 

l62   59  3 

3195 

15 

10= 

=  10 

585 

4622 

13  42  49.7 

155    18  56 

262.3 

3 

10 

10 

568 

4623 

13  43  20.0 

128   32  O 

332.0 

5 

8 

14 

460 

4624 

13  43  26.9 

I36    17  27 

355.4 

15 

6 

12 

B.  4668 

463 

13  43  28.0 

121      5  37 

183.6 

18 

6' 

9 

A.  1580 

7OI 

13  43  54.0 

139  51  4 

77-5 

20 

8' 

8' 

B.  4672 

566 

4625 

Til     A  A  9.0 

0  c 
9-5 

1 2 

9 

9' 

4.C7 

9-7 

44  43 

7.4. 

I  c 

9 

10 

686 

4020 

13  44  16.7 

1  rn     IX     A  t~\ 
1  k  U    Z,  0    il  u 

53. 8 

3 

11= 

=  11 

C67 

29  45 

60.O 

3 

9' 

9' 

A  rough  estimation  of  A  R  A  from  a  foregoing  star 
makes  the  R  A  6^.7  in  this  observation. 

584 

4627 

13  44  22.5 

161    8  5 

27I.3 

8 

9' 

12 

A.  tliirrl  ^far  T*»  m  Tipar 

584 

4628 

»3  45  - 

136  27  — 

3' 

1 1 

E 

4629 

13  45  37.0 

167  34  19 

356-5 

4 

10 

10' 

782 

4630 

13  45  44.8 

154  48  33 

3II.7 

5 

8' 

9 

580 

45.8 

48  22 

313. 1 

4 

8' 

8' 

Pos  314.8,  314.1,  310.3  ;  another  s  f  

581 

4631 

13  45  50.0 

*59  33  5 

86.2 

12 

10 

10 

584 

4632 

!3  45  56-3 

154  57  57 

9-3 

6 

6 

1 1 

Pos  9.5,  9.1.     The  following  and  southern  of  2 
double  stars. 

L.  5740 

581 

4633 

13  46  0.0 

146  52  44 

$  267.9 

70 

7' 

10 

43  6 

*  3OI-4 

12 

10 

14 

BCiTriPle 

4634 

13  46  4.3 

145  11  38 

310.6 

8 

9 

1 1 

[This  cannot  be  A.  151,  as  he  makes  the  position 
exactly  north.] 

694 

463S 

13  46  37.2 

167  50  4 

250.7 

12 

10 

10' 

783 

DOUBLE  STARS. 


215 


No. 

R  A.  1830.0. 
h.    m.   s.  d. 

N  P  D.  1830.0. 

0        t  it 

Position. 

Dist. 

Magnitude.! 

Remarks. 

Synon. 

Sweep. 

4636 

13  47  29.9 

129    8  53 

29.6 

I| 

10  10' 

Pos  30.5,  28.7.    Place  by  a  hurried  and  imperfect 

461 

observation.    Viewed  also  by  Mr.  Maclear  and  a 
friend. 

32.6 

8  20 

22.2 

li 

10  II 

A  double  star  involved  in  a  very  evident  nebula  2'  or 



573 

2  J'  in  diameter.     Three  stars  are  near  it  ;  one 

E  9  m,  and  two  others  (C  D),  13  m.    Pos  of  the 

middle  star  D  of  the  three  from  the  double  star 

=  28.°3.    See  Plate  VI.  fig.  10. 

33-7 

8  49 

2 

9  =  9 

A  close  double  star  in  a  very  evident  large  bright 
luminous  atmosphere,  2'  diameter.    A  neighbour- 
ing star  quite  as  bright  has  no  such  photosphere. 
The  star  was  not  noticed  as  double,  till  too  late 
for  procuring  a  satisfactory  measure  (41.3  4^  was 
taken),  verified  with  240  and  320.     Wind  hot 
from  north,  and  furious,  but  definition  excellent. 

460 

34.1 

9  n 

27.3 

,  1 
J4 

10  11 

ros  27.3  by  direct  measure  01  A  r>.    Ihe  line  01 
junction  passes  about  one  diameter  of  the  small 
star  (D)  on  the  side  towards  (C),  between  the 
stars  C  D.    When  better  seen,  I  judge  the  line 
of  junction  to  pass  as  much  outside,  or  to  the 
following  side  of  D,  and  in  this  opinion  I  remain. 
28.3  is  the  measure  of  A  and  D  carefully  taken  ; 

574 

and  if  we  say  28.3  for  the  position  of  A  B,  it  will 
probably  be  not  i°  wrong.    220,  as  in  f  573,  is 

certainly  too  small. 

25.8 

2 

10=10 

Pos  24.9,  26.7.    In  v  F  neb.    A  H<  9  m  follows 
about  4'  dist. 

718 

4637 

13  48  4.7 

101  42  58 

124.6 

15 

9  =  9 

698 

4638 

13  48  59.4 

136  23  12 

S  3i5± 

5 

10  12 

A  B  I  r    .     ,      .  , 

464 

i  125+ 

A. 

10  13 

4639 

13  50  41.0 

118  26  18 

342.4 

6 

9'  10 

45i 

4640 

13  52  10.6 

99  33  23 

*34-3± 

4 

I  think  it  is  double,  but  the  night  is  so  very  unsatis- 

698 

9  =  9 

factory  that  I  cannot  get  a  sharp  glimpse. 

4641 

13  54  16. 1 

'57  35  35 

66.6 

12 

9'  n 

579 

4042 

13  54  34-9 

152  37  18 

S  5-3 
C  330-5 

8 
25 

8  16 

6  II 

A  B  ) 

A  C  ) 

±5.  4751 

581 

4.64.7 

TUT) 

11    CA  1%.0 

126    27  IO 

I  70.  C 

I  c 

J 

7  11 

A  3rd  9.10  m  s  p.    The  R  A  is  38s  too  great  for 
identity  with  L.  5798,  but  a  mistake  of  2nd  wire 
for  x  (or  leaving  field)  reconciles  the  discordance, 
and  gives  13  54  4.8. 

L.57Q8  ? 

13  55  24.0 

125  43  25 

129.5 

A.  154 

446 

4644 

13  55  32.6 

172  42  35 

69± 

8 

1 1  =  1 1 

779 

4.64.  c 

'46  53  4 

23 1.8 

10 

9    1 1 

436 

4646 

13  56  6± 
13  56  28.7 

137  31  ± 
142  52  7 

125-1- 
27.1 

A  fine  double  star,  class  III.  in  a  cluster.     Pos  by 
estimation  of  diagram. 

463 

18 

8'  9 

B.  4763 

468 

4b47 

13  5b  39. 0 

137  30  9 

295.9 

4 

10=  10 

....     .          .   ...        .        ,  , 

1  he  middle  ot  a  semi-ellipse,  tormed  oy  seven  stars 

695 

10  m,  which  itself  forms  part  of  a  cluster. 

41.7 

29  1 1 

294.5 

5 

9'=  9' 

The  middle  of  a  semi-elliptic  group  in  a  cluster  .... 

464 

4648 

13  56  58.0 

166  31  54 

208.0 

15 

10  10' 

782 

4649 

13  57  8.0 

148  54  45 

64.4 

12 

8'=  8' 

Pos  65.0,  65.0,  63.3.    Both  stars  of  a  fine  rose  red 

790 

colour,  or  rather  a  brick  red.    A  star  8' m,  which 
precedes  at  3'  dist,  is  purely  white. 

10.4 

54  H 

69.4 

10 

9  =  9 

Pos  70.3,  67.8,  70.0.    Both  stars  are  of  a  full  scarlet 

582 

colour.     Two  small  stars  s  p  and  a  large  one 

preceding  are  white.     A  very  interesting  and 
remarkable  object.    When  a  little  lamp  light  is 

in  the  field,  the  stars  of  the  double  star  appear 

of  a  fine  rose  red,   the  others  snow  white. — ■ 

[N.B.  As  the  measures  64.4  and  69.4,  differing 

5  degrees,  are  each  the  means  of  three  measures, 

there  can  be  very  little  doubt  of  a  rotatory  move- 

ment.   The  interval  of  the  observations  is  2  years 

and  35  days  :   1835,  May  3  ;  1837,  June  7.] 

216 


REDUCED  OBSERVATIONS  OF 


No. 

A     1 QQA  ft 

K  A.  IPoU.U. 

h.    m.  s.  d. 

V  T>  T»    1  QQft  ft 
O       1  II 

Position^ 

Dist. 

Magnitude. 

4.650 

13  57  »3-4 

Il8  22  53 

62.4 

IO 

S' 
0 

I  I 

4.651 

13  58  - 

I4O   42  — 

134.0 

63.0 

5 

9 

4.652 

13  58  19.2 

164    57  17 

79-4 

15 

9 

4653 

13  58  21.9 

132    39  O 

.34.8 

25 

6' 

J4 

4654 

13  58  27.6 

J55  57  21 

9.2 

10 

9 

1 1 

4655 

!3  59  53-2 

126  10  5 

268.5 

5 

9' 

1 1 

55-5 

"  5 

269.3 

5 

8' 

12 

4656 

14   0  14.2 

141  16  47 

285.3 

15 

9 

=  9 

4657 

14   0  18.0 

164  57  4 

80.7 

18 

7 

10 

4658 

14    1  3.4 

158  56  15 

259.2 

2 

!3 

13 

46  CQ 

14    1  4.0 

144  40  9 

115. 8 

12 

7' 

11 

4.660 

14   2  13.8 

162  37  33 

108.3 

2 

I  I  : 

=  11 

466  I 

14   2  17.0 

118    5  38 

49.0 

2 

IO  : 

=  10 

4662 

14   2  25.7 

122    7  27 

90.8 

5 

IO 

10+ 

4663 

14   4  11. 5 

128  22  0 

120.1 

18 

9 

=  9 

4664 

14   4  41.8 

118  26  48 

18+ 

20 

9' 

9" 

4665 

H    5  57-5 

132  28  45 

105.0 

15 

8 

io' 

4666 

14    6  8.7 

137  23  8 

22.3 

12 

9 

10 

10.7 

22  54 

25.8 

10 

9 

1 1 

4667 

14    7  5.0 

162  46  0 

139.4 

2 

9 

9' 

4668 

14    7  52.6 

123    4  7 

274.2 

4 

10 

12 

4669 

14    8  30.5 

139    6  54 

275.6 

8 

9 

IO 

467O 

14    8  40.6 

"5  25  5 

26.6 

12 

9 

12 

467I 

1 -j-    S  tj.(3. <j 

169  23 

128.5 

4 

8 

9 

4672 

14  9  27.8 

*32  »5  55 

301.6 

3 

6 

10' 

14 10  30.5 

147  39  52 

162.8 

15 

6 

8' 

S  165.6 

8 

5 

g 

33.0 

40  29 

<  1.6 

35 

5' 

1 1 

4673 

14 11  12.9 

141  37  32 

148.8 

7 

10 

1 1 

4674 

14 12  45.2 

102  58  12 

272+ 

18 

9 

9' 

14 13  38.9 

96  58  55 

165.3 

4 

7' 

=  7' 

4675 

14 14  9.8 

144    1  35 

342.1 

5 

10 

10' 

4676 

1 4-  15  -6.1 

T  1  8     f  T     A  A 

14.0  5  44 

261.5 

8 

84- 

*4  '5  33-7 

100  53  53 

320+ 

4677 

14  15  36.3 

138  16  11 

I58.3 

7 

10 

1 1 

4678 

14  16  15.9 

113  39  0 

319.9 

3 

11' 

13 

4679 

14  16  22.2 

in  20  55 

3'3± 

20 

8 

9 

4680 

14  17  25.9 

164  52  1 

359-7 

8 

9' 

12 

468l 

14  18  35.6 

145     1  18 

354-9 

15 

8 

H 

4682 

14  19  12.3 

J3i  45  0 

347.6 

12 

8 

14 

4683 

14  21  22.3 

151  31  25 

63.6 

15 

9 

=  9 

4684 

14  21  49.0 

154    7  28 

266.8 

12 

7' 

4685 

14  23  45.5 

135  24  27 

75± 

2 

3 

IO  : 

=  IO 

4686 

14  24  44.1 

126  15  49 

87.0 

8 

9' 

=  9' 

Remarks. 


Synon. 


Mean  epoch,  1837.006   

Pos  9.0,  9.5  

A  s(f  10  m  n  p  and  one  =  9  m  in  same  meridian, 
more  remote. 

Very  neat  

Pos  134.7,  141-8,  139.3  ;  half  weight  allowed  to 
134.7. 

Pos  129.3,  127.7.    Elegant  %  

Pos  301.7,  301.8,  301.3.  Lyell.  Shlue.  [Lacaille's 
star  differs  3'  in  P  D,  probably  some  slip.] 

Pos  163.2,  163.2,  161. 8.    Fine  jfc   

A  B  J 

AC  J(y  Centauri)  triple,  dreadfully  ill  defined  .... 

Fine  double  star  

In  the  following  part  of  a  cluster  

In  cluster ;  very  ill  denned   

Suspected  close  double,  but  too  ill  defined  for  cer- 
tainty. Pos  estim  from  diagram.  [N.B.  There 
can  be  no  doubt  that  this  sj:  is  S.  1837,  with  5' 
misreading  in  P  D.] 

R  A  somewhat  uncertain  for  want  of  zero  stars  .... 

The  n  f  of  two  

Seen  elongated  with  the  sweeping  power  (180). 
Tried  320,  but  the  night  would  not  bear  it.  After 
a  long  and  troublesome  examination,  I  succeeded 
in  getting  a  sure  elongation  with  a  notched  disc, 
with  240  and  12  inches  aperture.  Very  delicate. 
Distance  cannot  exceed  \  or  at  most  I  of  a  second. 


B.  4778 
B.  4777 


B.  4793 


L.  5864 
L.  5887: 

B.  4864 
R.  19 


S.  1833 


S.  1837 


DOUBLE  STARS. 


217 


No. 

R  A.  1830.0. 
h.  m.  s.  d. 

NPD.  1830.0. 
0      /  // 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

400  7 

14  25  13.3 

125  48  23 

83-5 

I| 

9' 

9'+ 

446 

14.2 

47  57 

78.2 

9 

=  9 

Pos  78.6,  77.7,  with  320  and  12  inches  aperture. 
Beautifully  divided,  and  well  measured. 

572 

4688 

14  25  41.4 

153  31  59 

68.6 

3 

10' 

1 1 

785 

4689 

14  26  6.6 

168    2  47 

47.6 

16 

10 

10 

593 

a6qo 

14  26  14.0 

135  22  32 

24.0 

25 

1 

10 

B.  4974 

463 

4691 

14  27  4.5 

144  57  ii 

272.3 

5 

694 

6.2 

57  28 

267.7 

12 

n' 

y 

10 

577 

14  28  5.4 

150    7  25 

214.8 

20 

a  Centauri.     Both  yellow,  nearly  of  the  same 
colour.    Pos  212.8,  214.8,  214.8,  212,3,  214.6. 

A.  1053 

+  l654 

578 

5-7 

7  44 

215.0 

Pos  215.6,  215.4,  214.1.    The  worst  definition  of 
the  stars  I  think  I  have  ever  seen. 

713 

6.1 

6  17 

214.8 

20 

1 

1 2 

596 

7.0 

7  37 

215.4 

25 

1 

3* 

Pos  214.1,  217.3,  217.3,  213.8,  214.6.  Definition 
beyond  anything  superb. 

582 

7-4 

7  39 

216.3 

Pos  216.6,  216.5,  215.9.    Stars  working.  Defini- 
tion curiously  hairy. 

7i5 

14  28  52.1 

154  13  37 

247.'? 

18 

3 

0' 
0 

(cc  Circini.')    L  white,  S  yellow,  superb  *fc.  Pos 
242.1,  245.3,  242.4. 

A.  1655 

;8i 

J 

52.4 

13  49 

245.3 

20 

4 

9 

A.  166 

785 

4.602 

T  7 

IA  20  AO. 7 

T       7     '  J 

131  55  21 

208.  c 

y  j 

10 

9 

9  + 

4<;  <; 

TJJ 

A  I.  A 

T  T 

56  10 

3OO.  I 

6 

9' 

9 

A  CI 

45/ 

4.6q'3 
TU7J 

IA  SO  7A.O 

162  AS  12 

20A.A 

18 

10 

10 

c6o 
5uy 

14    3O  38.8 

TAA  26  A7 

20A  C 

*w4'3 

5 

9 

=  9 

Fine   .... 

A.  168 

6qa 

4O.6 

27  3 

200.5 

5 

8' 

8' 

577 

14  33  ~ 

144  53  - 

6 

7' 

Class  5.    Rev  of  B.  "  double"  B  

B.  5026 

E 

4694 

14  33  25.7 

114  16  30 

45± 

Strongly  suspected  to  be  close  double  extremely 
unequal,  but  no  time  to  verify,  and  a  S.  Easter 
rising. 

A.  1663 

690 

4695 

14  33  49.4 

164  13  15 

292.1 

15 

7 

11 

L.  6044 

606 

4696 

14  34  52.3 

134   9  17 

210.0 

6 

H 

B.  5041 

455 

4 

4697 

14  34  57.6 

159  49  10 

139.2 

15 

8 

9 

ii.  5040 

598 

61.5 

49  7 

141. 6 

15 

8 

8' 

597 

4698 

14  35  12.1 

141  39  7 

261.4 

10 

5' 

r3 

Delicate.    Too  much  wind  for  a  measure   

B.  5044 

711 

14  36  10.8 

1 14  42  38 

136.8 

7 

5 

7 

A.  1667 

453 

4699 

14  36  26.2 

148  41  14 

126.7 

35 

7 

B.  5051 

713 

38.0 

41  34 

127.4 

40 

g' 

L  orange,  S  greenish  blue.    [N.B.  Both  observa- 

715 

tions  rightly  reduced.    An  error  of  10s  in  one  or 
other  chronometric  reading  must  have  been  com- 
mitted.] 

4700 

>4  37  7-5 

IOO  21  23 

222.4 

25 

y 

698 

47°  1 

14  37  43-2 

126     4  12 

87.5 

5 

10 

10+ 

44S 

4702 

14  38  2.1 

I25      7  21 

212.7 

10 

9 

1 1 

B.  5062 

446 

4703 

14  38  47.4 

167  48  26 

225+; 

10 

8 

12 

Pos  estimated  from  diagram  

587 

4704 

14  38  59.9 

151    58  48 

276.3 

5 

9' 

11 

596 

4705 

14  39  20.6 

140  53  5 

184.8 

9' 

12 

693 

5 

4706 

14  39  54-4 

136  41  54 

217.4 

7 

8' 

IO 

Pos  218.5,  216.3.    Both  stars  high  yellow,  almost 
orange. 

B.  5073 

695 

4707 

H  39  55-9 

155  42  35 

219.7 

ij 

.7 

8 

B.  5071 

579 

4708 

14  41  29.5 

94  45  55 

330.6 

12 

10'  = 

=  10' 

608 

4709 

14  41  30.4 

145  20  16 

225.6 

12 

12 

694 

9 

4710 

14  41  39.0 

131  22  34 

265.3 

12 

9' 

456 

9 

4711 

14  41  44.7 

124  19  13 

330.0 

8 

12 

448 

9 

14  42  5.8 

135    8  32 

225.6 

18 

8 

1 1 

B.  5089 

695 

6.S 

9  39 

223.5 

!5 

8 

11 

A.  171 

455 

3  K. 


218 


REDUCED  OBSERVATIONS  OF 


No. 

4712 

4713 
47H 


47 1 5 

4716 

4717 
4718 


4719 


R  A.  1830.0. 
h.  m.    s.  d. 


4720 

4721 
4722 

4723 

4724 

47^5 
4726 

4727 

4728 

4729 
4730 

4731 
4732 

4733 
4734 


4735 
4736 


14  43  3.2 
4-3 

14  43  12.5 
14  44  12. 1 
12. 1 
20.6 

14  45  2.1 
2.7 

14  46  28.8 
14  46  37.7 
14  47  1.3 


2.7 

14  47  10.9 

13.8 
14.2 
14  47  32.2 


14  48 
14  48 
14  48 
14  49 

14  49 

14  51 
14  51 
14  52 

14  S3 
r4  S3 


iS-7 
56.3 

59-3 
14. 1 
16.2 
58.3 
59.1 
8.2 
35-8 

33-  4 

34-  9 
25.5 
26.9 
33-7 


14  S3  42.7 
14  54  24.9 
14  56  42.7 
14  56  55.8 
14  57  36.1 
38.7 
!4  58  39-5 


41.0 
14  59  14.7 

18.5 
14  59  20.8 


N  P  D.  1S30.0. 


!44  43  37 
43  48 
100  14  48 
152  51  40 
51  8 
50  44 

137  11  9 

10  39 
113  58  27 
128  37  40 
124  41  42 


41  45 


148  14  42 

14  46 

H  34 
no  37  44 

95  10  57 
in  41  55 

125  39  49 
120    o  59 

1  18 
141  13  42 
14  12 

126  13  44 
134  50  36 
139    4  12 

4  57 
117    9  19 

9  43 
136  23  5 

159  29  40 
126  33  28 
167  13  11 

!37  39  4 
129    6  37 

7  35 
144  40  58 


41  13 
149  44  46 

44  8 
114  23  21 


Position. 


222.1 
223.7 
129.7 
147.6 
146. 1 
143-9 

275± 
273.1 
2.0 
215. 1 
60+ 


72.0 

42.3 

37-7 
43-1 
279.7 


92-3 
257.8 

344-5 
344.2 
171.0 
171. 6 
233.5 
350.9 
99.4 
96.8 
36.2 

37-3 
109.8 

3*4-3 
316.5 
259.8 
72.8 
328.0 
323.3 
242.7 


237.1 
27.8 
27.3 

166.8 


Dist. 


Magnitude 


9=9 

8  8 

9'  10 

8  9 
8'  8' 

9  9' 

7  8 

6'  7 

9'  » 

9  10 

9  « 


Remarks. 


9  9 

9'=  9' 
6  i 


10  =  10 
9  10 

11  =11 
6'  9 
8  10 
7'  12 


10  =10 
9=9 
9=9 
5'=  5' 


10  10 

8  n 

9  11 
9'  10 
8  11 
8  12 
5  iS 


6  14 
7'  12 
8  ,3 
11  =11 


Pos  222.6,  221.7  ;  fine  

Pos  224.3,  2*3-1 ;  fine  if-  

There  is  reason  to  suspect  the  right  ascensions  of  the 
last  two  hours  of  this  f. 

Fine  star   

Very  fine  double  star  

Very  neat  star  

Very  delicate.  Pos  estimated,  distinctly  separated 
with  12  inches  aperture  and  180,  but  too  late  for 
a  measure,  the  whole  aperture  having  left  some 
doubt,  and  time  being  in  consequence  lost. 

Delicate.  Query  if  it  have  not  also  some  kind  of 
nebulous  or  furry  appendage.  I  remember  fancy- 
ing something  of  the  kind  in  last  night's  obser- 
vation of  the  same  object. 

Pos  43.1,  41.9,  41.9-  [N.B.  This  obs  makes  the 
minute  of  R  A  48,  but  both  the  other  observa- 
tions agreeing  in  47,  that  must  be  preferred.] 

L  yellow,  S  more  yellow  ;  a  curious  coloured 
star,  not  a  bad  miniature  of  a  Centauri  (is  H. 
145.28  =  Sh  190). 

Pos  344.3,  344- 7.  Fine  

Pos  343.8,  344.5.    Neat  *   

The  chief  of  a  pretty  bright  group   

[B.  5144  does  not  exist]   

Wind  violent   

Very  fine  double  star  

Fine  star   

(tt  Lupi).  Suspected  with  180,  plainly  seen  double 
with  320  and  the  whole  aperture,  in  spite  of  much 
flare,  which  rather  assists  the  division. 

Pos  325.3,  323.3  

Wind  violent   

The  southern  of  3   

Wind  violent   

Pos  241.7,  243.8.  Large  star  pale  yellow.  A  most 
delicate  and  beautiful  object.  The  small  star  one 
of  the  most  minute  companions  to  so  large  a  one 
in  the  whole  list  of  such  objects. 

Pos  236.3,  237.8  

Elegant  star   


Synon. 


Sweep. 


B.  5112 


B.  5123 


A.  1690 

h.  2757 

B.  5 141 
B.  5145 


B.  5166 


B.  5193 


694 

S77 
698 

785 
581 
596 


DOUBLE  STARS. 


219 


R  A.  1880.0. 
h.  m.   s.  d. 


N  P  D.  1830.0. 


Position. 


Dist. 


Magnitude. 


Remarks. 


Synon. 


Sweep. 


4737 
4.638 


4739 


474° 
474i 
4742 

4743 
4744 

4745 
4746 


4747 
4748 


4749 
475° 
475i 
4752 


4753 

4754 
4755 
4756 
4757 


14  59  31.5 
14  59  34.4 

43.8 


15 
15 

15 


15 
15 


15 

15 

15 
15 


o  — 
o  7.6 
8.2 
o  9.2 

9-7 
10.4 
o  10.2 

0  46.3 

15  0  56-7 
15    1  29.0 

1  35.0 

1  43.8 

2  6.8 
2  9.1 


9-3 


15 


15 
15 
15 
15 

15 

15 
15 
15 
15 


2  42.4 

2  54.4 
56.3 
57.2 

3  45-7 

4  7-i 
4  47-4 
6  31.3 

33-5 
6  45.4 

6  45.4 


4758 
4759 


8  31.0 
8  33.3 
15  9  46.8 
15    9  53-3 


56.7 


15  9  56.4 
15  10  33.9 


165  39  7 
126  10  49 

12  5 


136  25  — 
Hi  *5  57 
26  42 
138    5  4 

4  57 

5  33 
117  48  48 
131  40  20 
164  57  o 
122  11  15 
169  35  5 
125  35  57 

94  56  26 
148  25  14 


25  46 


H5    3  55 
130  48  8 
48  20 
48  30 

146  44  23 
137  25  44 
164  35  20 
123  56  32 

56  52 
»37  J5  l5 

137  15  15 

97  36  ± 

147  21  30 
126  4  30 
113  37  38 

148  41  30 


42  9 


96  34  41 
169  36  40 


270.3 

S  160.0 

I  24.8 

*  *534 


247.6 
247.6 
142.8 
145.8 
144.0 
30+ 

i39-5± 
203.3 
199.6 
59.0 

S  164.4 
$  100.0 


11.4 
6.7 
12.0 
255.0 
23.2 
298.7 
6.5 
9.8 
136.5 

173-5 
4-7 
306.7 
201. 1 
i8o± 
1 10. 1 


102.9 


77-5 
48.4 


10 
6 


10 
9 


13 


9  + 
9 
9' 

1 1 

12 

9' 
11 
11 

7 


A  third  star  s  f   

i  Triple.  Nisi  PD  =  1260  4'  19".  Wind  furious. 
S    R  Ascensions  precarious  in  this  f. 

\  [Nisi  P  D  =  1260  5'  45".  The  R  A  of  this  obser- 
\  ration  is  to  be  preferred.  The  P  D  in  one  or 
the  other  observation  requires  a  negative  sign  in 
the  index  reading,  which  has  been  inadvertently 
omitted,  and  no  ground  exists  to  decide  which  is 
right. 

Class  5  or  6  

(£  Lupi)  

A  R  A  =  6!.5  

( /.-  Lupi)  

Pos  1454,  146.3  

Pos  144-3,  I44-2>  r43-4  

Excessively  close  {if  double)  


Pos  199.3,  200.0. 


A  B )„ .  , 
BCiTrlPle 

A  third  (?  if  *)  

A  very  composite  or  multiple  star,  consisting  of  a 
chief  star  8' m,  and  perhaps  a  dozen  of  12,  13, 
14  m,  all  within  the  distance  of  a  sixth  class 
double  star.    Ill  defined. 

Curiously  multiple.  One  of  its  companions  is  close 
double,  pointing  to  the  large  star  which  is  8  m. 
The  smaller  stars  are  12  or  13  m.  Such  mul- 
tiple stars  are  rare.  It  is  a  close  group,  not 
above  i|'  diam.  In  the  diagram  10  companions 
are  laid  down. 


Double.    No  description 


Pos  14.0,  10.1 . 


[Right  reduced,  but  B's  R  A  differs  23s] . 
Pos  298.3,  299.1  


Pos  136.7,  136.4;  (ji  Lupi.)  /.t1  +  /u2  Lupi  =  A. 
180. 

/i1  Lupi.    Close  double.    Mean  epoch,  1836.221  .. 


Fine  star  

Requires  verification   

(y  Circini.)  Pos  109.8,  110.4.  A  momentary 
glimpse  with  180  induced  me  to  apply  320  with 
12  inches  aperture.  It  was  then  cleanly  divided, 
and  these  are  good  measures. 

A  beautiful  object.  Pos  104.4,  101.3.  The  first 
with  480,  which  separates  the  stars  by  ^  diameter; 
the  other  with  the  same  power  and  an  aperture 
reduced  to  6  inches. 


A. 1717 

A.  176 

B.  5201 

+  5*°5 
A.  177 


1914 


B.  5238 


A.  1728 


2.  1925 


B.  5283 


10  12 
8  11 


A  R  A  =  6  .25 


587 
460 

447 


E 

711 

468 
693 
467 
464 
45i 
457 
605 

794 
593 
446 

608 
713 


582 


694 

45  6 
718 

457 
577 
463 

569 
446 
448 
463 

E 

609 
582 
446 
5S8 
575 


717 


609 
703 


220 


REDUCED  OBSERVATIONS  OF 


No. 


4760 


4761 

4762 

+763 
4764 

476S 
4766 
4767 
4768 
4769 
4770 

4771 
4772 

4773 

4774 
4775 
4776 

4777 


4778 
4779 
4780 

4781 
4782 

4783 
4784 


4785 
4786 


4787 


4788 


R  A.  1830.0. 
h,    ra.  s.d. 


15  10  58.0 
15  II  10.5 

15  11  15.5 
16.2 
15  11  40.6 
15  11  52.4 
15  13  0.0 

15  13  32.7 

15  14  53.0 

15  15  0.7 

15  15  17.7 

15  15  29.4 

15  16  9.1 

15  17  12.7 

15  J7  — 
15  17  27.6 
15  18  16.3 
15  18  391 
IS  18  55.6 
15  19  3.0 

4.8 

15  19  25.2 

25.8 


25.8 
28.2 
19  55-4 


IS 


20  6.8 
20  10.8 
1 1.9 

20  47.0 

21  2.0 

21  58.6 

22  — 

23  4.7 
5.6 
6.7 

23  52.1 


15  23  53.1 


15  24  12.1 
18.9 

15  24  - 


N  P  D.  1930.0. 
0     /  0 

Position  t 

Dist. 

Magnitude. 

166  55  7 

19.3 

20 

9 

10 

!34    5  ± 

I73-3 

40 

4' 

10 

154  44  11 

2-3 

15 

9 

9  + 

44 

3.1 

20 

10  = 

=  10 

169  36  34 

45.0 

20 

9 

10 

144  45  26 

320.7 

10 

163  47  14 

248.8 

25 

0 

12 

122  26  17 

97.1 

8 

9' 

IO 

132  15  27 

128.5 

15 

9 

10 

116    8  58 

140.0 

3° 

8' 

1 1 

109    0  43 

1 14.9 

8 

9' 

=  9' 

in  18  48 

19 1.1 

12 

8 

9 

164  19  9 

206.2 

7 

10: 

=  10 

147  30  10 

187. 1 

4 

9' 

9' 

140  50  — 

250.1 

12.0 

8 

12 

163  26  30 

266.7 

8 

8 

8 

100  21  43 

I3I-9 

5 

8 

9 

118  15  58 

8.5 

10 

7 

10 

109  18  5 

4.0+ 

10 

10  = 

=  10 

131  19  37 

226.5 

0 

6' 

9 

20  50 

224.0 

3 

7 

146  48  51 

299.8 

5 

8 

10 

49  3 

297.2 

4 

8 

9 

49  10 

200.7 

6 

8 

9' 

48  11 

29I.8 

4 

8' 

1 1 

142  16  42 

2O3.7 

15 

8 

8  + 

06  IX  2A 

I7.6 

18 

9 

11' 

I69     58  46 

269.8 

9 

9  + 

58  25 

27I.3 

3 

9' 

9' 

132  21  25 

I96.4 

12 

9' 

10 

131    17  59 

266.5 

25 

IO9   35  26 

277+ 

12 

6 

9 

137     O  - 

238.2 

43: 

7' 

IO 

113    54  IO 

1 19.4 

10 

7 

=  7 

54  23 

123. 1 

12 

7 

=  7 

55  * 

121. 1 

20 

8 

=  8 

123  50  22 

11  = 

=  11 

130  35  30 

95-5 

1 
3 

4' 

4' 

169   4  10 

316.4 

15 

9' 

10 

4  16 

303.5 

10 

8' 

9 

134  23  - 

348.5 

3-i 

5 

8' 

Remarks. 


(t  Lupi)  =  A.  182.  Place  by  Catalogue  in  R  A. 
Pos  173.2,  173.5. 

Large  star  red  

The  obs  gives  1630  NPD.  B  makes  it  1620  by 
18  obs.    I  have  misread  i° — if  it  be  the  same 

Both  ruddy  

L  red,  S  blue  

Pos  191-7,  190.6  

Very  neat  star  

Neat  star  

Mean  epoch,  1837.094   

[S'sPD  for  1826  is  1000  17']   

Pos  9.5,  7.5.    Fine  sj:   

North  of  zenith,  too  late  for  measures  

L  white,  S  yellow.    Pos  225.4,  227.7  

Pos  224.5,  223.4  

Fine  Pos  297.7,  296.8.  N.B.  This  obs  makes 
the  minute  of  R  A  18,  which  being  a  manifest 
mistake  is  corrected. 

Pos  300.7,  298.8  

Pos  292.0,  291.5.    Neat  star  

A  very  pretty  double  star  

Neat  star.    Position  rude  

Mean  epoch,  1836.961   

Pos  122.5,  123.7.    Very  fine  D  *   

The  preceding  of  2  stars  2'  dist,  very  strongly  sus- 
pected double. 

(y  Lupi.)  Pos  97.6,  94.3,  95.7.  Cleanly  divided 
with  480,  and  the  black  division  well  seen.  Mea- 
sures perfectly  good,  and  to  be  depended  on. 
With  800  well  separated  ;  with  1  So  and  triansrular 
aperture  perceived  to  be  double.  [This  shows 
the  dist  to  be  underrated  at  two-thirds  of  a 
second.] 


[One  or  other  of  these  positions  must  have  been 
erroneously  read  off,  or  the  micrometer  displaced 
before  reading.] 


Mean  epoch,  1836.443.    f  Lupi 


Synon. 


A.  1739 


B.  5302 


Sweep. 


2.  1939 
B.  5349 

B.  5351 
B.  5355 


L.  6420 
S.  673 


AC.  1760 


B.  5384 


DOUBLE  STARS. 


221 


No. 


4789 


4790 

479 1 
4792 


4793 

4794 
4795 

4796 

4797 
4798 

4799 


4800 


4501 
4802 

4803 
4804 

4805 
4806 
4807 


4809 
4810 

4811 

4812 

4*13 
4814 


R  A.  1830.0. 

N  P  D.  1830.0. 

h. 

s.  d. 

0 

II 

15 

a+ 

20.8 

143 

54 

26 

23.6 

54 

50 

23.6 

55 

5i 

23.6 

54 

57 

26.8 

56 

2 

15 

26 

56.7 

168 

10 

30 

T  r 

xi 

28 

18  1 

137 

47 

C2 

J 

15 

29 

± 

161 

53 

52 

*5 

29 

24.2 

147 

33 

21 

15 

29 

28.8 

98 

*3 

24 

15 

29 

55-9 

137 

43 

42 

57-7 

43 

32 

15 

30 

52.8 

141 

17 

39 

15 

'31 

10.4 

148  34 

18 

1 1.4 

34 

25 

15 

31 

— 

148 

9 

— ■ 

15 

31 

50.0 

139 

40 

5 

J5 

32 

0.9 

173 

43 

15 

32 

13.7 

158  27 

15 

15 

32 

25.3 

*54  54 

9 

29-3 

54 

g 
0 

29.7 

54 

8 

15 

32 

40.7 

100 

35 

17 

15 

32 

42.1 

ns 

13 

42 

43-3 

2 

44.3 

13 

"32 

15 

32 

24.8 

166 

41 

22 

15 

35 

51.4 

132 

2 

22 

54.1 

3 

31 

15 

35 

52.4 

117 

30 

58 

!5 

36 

43-4 

98 

49 

17 

44.6 

49 

2 

15 

37 

142 

4i 

!5 

37 

3.6 

144 

14 

0 

15 

37 

36-3 

1 10 

42 

12 

I  c 

J 

11 

4/ 

CA  6 

144 

3* 

O 

57.0 

3i 

23 

15 

38 

41.6 

133 

53 

II 

15 

39 

150 

10 

15 

39 

11.8 

135  56 

36 

12.5 

57 

20 

J5 

39 

31.2 

131 

53 

9 

15 

40 

19.6 

92 

42 

44 

15 

40 

37-7 

127 

35 

48 

37.8 

34 

35 

15 

41 

21.6 

149 

39 

39 

15 

4* 

29.2 

126 

1 1 

1 

!5 

41 

37.6 

160 

35 

30 

Position. 


89.5 
89.3 
88.3 
88.5 
90.0 
349.0 
117. 2 

IIO.O 

94-3 

6.9 
16.7 
20.5 

147-7 
222.1 
221.7 
116.6 
256.3 
138.6 
80.1 
156.2 

158.1 
155.8 
49.4 
190.4 
189.5 
190.5 
i6o± 
287.9 
282.7 
214.8 

102.4 
135.2 
321.7 

357-3 
16.0 

21.3 
58.3 

S  5°-9 
I  257-° 
66.0 
67.2 
64.5 
166.3 
76.4 

78.0 

97.0 

328.3 
3*3-7 


Dist. 


12 
15 
15 
"5 
12 
18 
IO 

6 
5 

5 
15 
15 
12 
10 

4 
34-4 
20 
18 
10 


Magnitude 


20 
2 

43 : 
49: 

!5 

12 

3 

ij 
4 

5 
2 


35 


9 

=  9 

9' 

10 

10 
8' 

1 1 

8' 

9 

=  9 

8 

1 1 

10 

10 

7 

8 

7' 

10 

7' 

=  7' 

9 

13 

9 

1 1 

10 

17 

8 

1 1 

8 
8 

12 

8' 

8 

13 

8 

12 

10 

1 1 

7 

=  7 

if 

7 

=  7 

2 

i 

7'+ 

20 

9 

9'  + 

5 

10 

=  10 

4 

9' 

=  9' 

4 

9' 

=  9' 

12 

9' 

10 

i£ 

10 

12 

3 

10 

12 

40 

8 

9 

20 

8 

=  8 

16 

10 

10 

33.0 

6 

1 1 

12 

9 

12 

12 

8 

15 

25 

7 

10 

8  9 
II  =11 


8'  10 


9  " 

6  11 

9'  11 

8'  9 


Remarks. 


[An  error  of  im  in  R  A  corrected]  

Another  7'  mag  to  north   

Exactly  in  the  parallel  by  the  horizontal  wire  

Pos  348.3,  349.8.  

R  A  not  regularly  taken  on  the  wires  

L  very  orange,  S  green  

Mean  epoch,  1836.683   

Pos  155.6,  157.3,  155-7 j  tQe  two  last  wit-a  320- 
Fine  star. 

Pos  159.3,  156.8.    Very  fine  %   

Pos  155.3,  156-3  

Neat  star  

Pos  190.2,  190.8  

Very  ill  denned   

Epoch,  1837.342   

Small  s|j  extremely  faint   

Two  more  companions  forming  a  curve   

I  Epoch,  1836.244  

Pos  64.9,  67.0.    L  white,  S  red   

Pos  165.4,  166.9,  168. 1,  165.0  

Pos  97.8,  96.3,  with  320  and  12  inches  aperture. 
(k  Circini)  a  most  delicate  and  beautiful  object. 

Wind  violent   

Marked  as  double  in  B  


Synon. 


B.  5413 
A.  190 

2.  1962 


L.  6472 

B.  5439 
L.  6404 

B.  5442 
R.  20 

2.  1966 


L.  6516 


B.  5484 


B.  5486 
A.  193 


2.  1974 


B.  5507 


B.  550S 


Sweep. 


694 
599 
711 
468 
703 
463 
606 
717 

609 
695 
463 

599 
7i7 
575 
E 

693 

594 
709 
600 

580 
581 

59i 
464 

454 
455 
704 
456 
718 

45i 

609 

59i 
E 

696 
722 
696 

694 
455 
E 

463 
464 
456 
608 
461 

412 

718 

460 
567 


222 


REDUCED  OBSERVATIONS  OF 


No. 


4815 

4816 

+817 

4818 
4819 


4820 
4821 

4822 
4823 


4824 
4825 
4826 
4827 

4828 
4829 


R  A.  1830.0. 
h.  m.   s.  d. 


4830 
4831 


4832 


4833 

4834 
4835 


4836 
4837 


15  42  18.0 
15  42  21.8 

15  42  54.7 

iS  43  5-8 
15  43  6.8 

rS  43  44-3 
15  46  1.9 
2.3 

15  46  10.3 
15  48  - 


IS  47 
15  48 
15  48 

!5  49 
15  49 
15  5° 
15  Si 
15  S^ 

15  S2 
15  52 

IS  35 
IS  55 
15  55 


20.0 
33.8 
49.4 
51.9 
16.8 
40.5 
± 
30.0 
14.8 
15.1 
52.3 
53.0 
i-7 
5-i 
17.7 


15  55  33-8 
34-9 
15  56:  - 

15  56  9-3 
9-7 

15  56  29.7 

IS  56  39-i 
40.8 

15  57  9-° 
15  58  42.4 
15  59  19.9 
15  59  58.2 
59-8 


16 
16 


16 


o  23.3 
o  33.6 
33-7 
36-7 
o  49.4 

49.9 


N  P  D.  1S30.0. 


124  23  24 

139  49  28 
173  38  5 

135  29  28 

135  30  28 
156  10  17 
123  27  11 
29  13 

120  28  31 

121  32  — 

128  39  30 
133  19  10 
127  54  31 

54  21 
109  26  21 

135  47  O 
147  17  ± 
119  13  33 
133  S6  4 
54  47 
132  50  50 
149  39  13 
100  54  20 
100  58  35 
168  14  5 

109  19  38 
20  3 

132  32:  — 
126  17  43 

17  6 

123  23  1 

95  49  33 

49  5 

135  51  50 

122  11  13 
117  39  38 
i43  46  31 

47  4 
45  3° 

124  24  29 

133  12  10 
11  42 
11  40 

97  47  27 

48  6 


Position. 


140.3 
10.3 
323.6 

S  292-5 
i  3i9-i 
298.5 

354-1 
46.5 
48.0 

146.0 
145.1 

91.0 
227.2 

20.7 

23.4 
320.3 
240.5 
251.2 

78.1 
170.0 
173.0 

90.7 

359-1 
80.5 

ioo± 
12.7 

25.6 
29.5 
232.7 
356.6 
360.0 
359.2 

\  342-6 
t  17-7 

S  23°-5 
I  185.0 

142.0 
86.3 
20+ 

85-3 
85.9 
85.7 

296.6 
80.0 
79.0 
75.6 

256.7 

254.6 


Dist. 


15 
IO 

15 
IO 

5 
5 
15 
15 
12 

20 
21. 1 

5 
15 
12 

15 

20 

4 
15 

2 
15 
15 

3 

12 
5 

10 
90+ 

18 
18 
21.2 
40 
40 
40 

15 
15 

20 
35 
20 

3 

IS 
20 
10 
12 

7 
3i 

8 

6 

6 
20 


Magnitude. 


9  12 

8  9 
8  12 
10  10+ 
10+ 1 1 


9  11 

6'=  6' 
6'=  6' 


9  9+ 


10=10 
8  15 
5'  9 
S  9 

8  8 

9'  11 
6'  9 
10=10 

9  11 
10=10 

9  12 
8'  10 


Remarks. 


10  II 
IO  II 

7  12 
7  12 

7  12 

10=10 

7  7  + 

9  =  9 
9'=  9< 

9  =  9 
10=10 

8  9 

9  =  9' 
9'=  9' 
9  =  9 
8'  11 

5'  17 


A-  195  

Pos  322.1,  325.8,  323.2,  323.3  

ABL.  , 

Bcrr,ple  

The  s  f  of  two  double  st  

Splendid  D  H«  •    Pos  46.7,  46.3   

Pos  48.3,  47.8.    Superb.     (£  Lupi  —  Scorpii  = 

A.  196.)  [N.B.  This  is  not  to  be  confounded 
with  £  Scorpii,  Sh.  No.  216.] 

[Nisi  P  D  =  122  32,  in  which  case  the  star  is 

B.  5550.]    Mean  epoch,  1836.887. 

(n  Lupi).    Pos  20.7,  20.8.    Wind  violent  

Pos  24.2,  22.4,  23.5.  S  blue.  Perhaps  A.  197 .... 
Pos  precarious.    No  time  

Tos  250.3,  252.1  

Neat  star  

P  D  not  good  

[Is  one  of  these  stars  variable  ?]   

L  very  red,  S  white   

(?  Librce.)    Superb  D  star   

Near  ?  Libra;.    Neat  sjs   

A  third  =  14  m,    following   forms    a  triangle 
(S  Apodis). 

Pos  26.5,  24.7.    (/3  Scorpii.)   

Epoch,  1834.348  

The  middle  of  3  

Wind  violent.    (?  position.)  

AB  > 
AC  ) 

A  B  ) 

A  C  \  [^'c  ^arffe  *  n0'  n°i'ced  as  c'ose  double.']  . . 

Pos  141. 3,  140.7.    Neat  %   

Fine  star.    (Noticed  as  D  by  B.)   

Chief  *  in  middle  of  a  superb  cluster  

Chief  of  a  cluster   

No  R  A,  and  P  D  bad   

Neat  star  

Neat  *   

Pos  76.0,  75.4,  75.5   

[Obs  gives  960  P  D,  but  f  609  agreeing  with  2, 
makes  it  97.] 

[A  mistaken  wire,  proved  by  the  re-examination  of 
both  observations,  corrected.] 


Synon. 


B.  5515 


B-  SS35 
+  S536 


B.5550? 

L.  6614 
A.  1821 
R.  21 
cr.  498 

B-  5559 


Sweep. 


2.  1998 
2.  1999 
B.  5584 
+  5586 

A.  1836 
c.  506 

B.  5598 


2.  2005 


B.  5613 


79 1 
693 

594 

463 

463 

579 
592 
791 


794 
E 

462 
472 
460 
461 
722 
463 
582 
45i 
455 
454 
472 

7i7 
59i 
59i 
587 

722 
601 
E 

461 
460 
462 

791 

608 

609 
463 
794 

451 
469 
468 
694 
791 
472 
454 
455 
697 

609 


DOUBLE  STARS. 


223 


B  A.  1830.0. 
h.    m.  s.d. 

N  P  D.  1830.0. 

6     t  it 

Position. 

Dist. 

Magnitude. 

Keniarks. 

Synon. 

Sweep. 

4838 

16 

1 

38.4 

139 

37 

49 

136. 1 

20 

9 

10 

465 

4839 

16 

1 

47.O 

117 

57 

33 

84.5 

3 

i 

10 

/         C  "\ 

A.  1849 

451 

16 

2 

36-7 

109 

0 

29 

336.6 

60 

5 

6 

Ct 

A.  1851 

722 

16 

4 

37-9 

97 

1  j 

37 

o± 

20 

8 

2.  2018 

697 

9 

16 

4 

57-i 

99 

58 

34 

1 0 

8 

11 

2.  2019 

59° 

58.0 

58 

43 

152.6 

20 

8 

11 

591 

4840 

I  D 

z  3 

I24. 

a3 

21 

293.3 

4 

9 

9' 

592 

4841 

ID 

7 

1 1.1 

*39 

44 

5 

348.5 

*5 

0 

12 

/      O     TV  TV.  _____  __\ 

A.  1862 

465 

4842 

ID 

7 

Zo.Q 

I30 

47 

25 

200.8 

20 

9 

1 1 

463 

I  D 

Q 
O 

49.4 

I20 

29 

18 

324.3 

35 

/*/ 
0 

7 

Pos  322.9,  325.7.    [iWarAed  as  double  in  B.~]  .... 

B.  5685 

794 

50.7 

29 

t5 
IO 

321+ 

20 

7' 

0 

A.  1866 

45 1 

0 

4.84  7 

l6 

I  0 

29.1 

122 

54 

„  r 
30 

270.6 

15 

7 

J3 

L.  6796 

79 1 

ID 

IO 

^Z.  I 

133 

29 

32 

Iq6.7 

40 

5 

B.  ?6qq 

455 

9 

if. 
ID 

IO 

34-7 

IO9 

4i 

51 

22.6 

15 

_/ 

8 

a.  515 

722 

7 

35-5 

41 

25 

23.I 

15 

8 

0' 

601 

8 

ID 

1  0 

51.9 

"5 

42 

274.3 

15 

./ 

A.  1872 
IV.  21 

474 

9 

4 

9 

52.8 

10 

21 

273.4 

'5 

3 

11 

A  superb  double  3jc .    f  N.B.  JMuch  over  and  under- 

Sli i->  a 

Ulli  »J_ 

453 

rated.'] 

4844 

16 

II 

0./ 

149 

1 

43 

69.3 

4 

10 

10' 

717 

4845 

16 

3-4 

130 

49 

45 

I4O.5 

1 

7 

7' 

suspected,  with  lull  aperture  ;  0  inches  equilateral 
triangle  has  too  little  light  j  cleanly  divided  with 
320  and  12  inches  aperture. 

B.  5708 

456 

4846 

16 

I  2 

6.2 

137 

49 

45 

155.8 

12 

9 

1 0 

695 

6  Q 

4* 

42 

I56.2 

12 

9  - 

-  9 

T">  _   1  J   T¥  

463 

4847 

ID 

IZ 

13-5 

120 

39 

24 

222.1 

6 

10= 

:I0 

478 

l6 

IZ 

14.2 

i53 

39 

25 

24.2 

15 

7' 

12 

B.  5709 

600 

17.0 

38 

33 

20.6 

35 

7 

9' 

580 

4848 

l6 

I  2 

58.9 

122 

47 

25 

ire  (i 
155.0 

6 

7 

7 

L.  6815 

702 

61.2 

47 

21 

158.6 

c 
0 

7'= 

=  7' 

592 

61.6 

49 

45 

157.2 

0 

7 

7' 

Neat  s|»     '  p  D  tli6  J*  being  over  tbe  zenith 

79 1 

0 

61.9 

J55-3 

5 

7' 

8 

e    t  r       t      tt^    f  {  1  a  a    r  in  lVT  sj  \ 

794 

48 

0 

4849 

16 

44.2 

155 

39 

35 

150.7 

20 

8 

11 

579 

44-4 

39 

150.4 

lS 

10 

11 

709 

2 

485O 

l6 

_ . 

x4 

0.0 

119 

17 

53 

352.1 

4 

7 

7' 

M.  7607 

45i 

48SI 

16 

J4 

8.8 

112 

37 

33 

96.9 

15 

8 

11 

788 

48S2 

l6 

14 

32.6 

127 

29 

44 

115.8 

6 

IO 

1 1 

460 

4853 

l6 

14 

44.8 

1  i  1 

9 

336.8 

25 

e 

7 

B.  5723 

463 

46.0 

54 

336-3 

25 

5 

9 

695 

9 

4854 

ID 

J5 

H7 

21 

n  f 

6 

Class  i.    "  Very  difficult" — "  to  be  verified."  .... 

B.  5726 

E 

16 

15 

23.5 

113 

3 

4 

o± 

6 

7  = 

=  7 

( C     ct   fiith ii/oJu  1       ^Ji">   nfnpr   ^frnr    nut"  it^   ■?    en jyi _ 

I  Sf     fc*      \J  ft  ILUxjXj  III  •  j           11U     l_J  LU  O I      OLCll       UUt     HO  ~ 

A.  I877 

793 

panions,  on  an  intensely  black  ground. 

Sh.  228 

25.9 

2 

45 

2.1 

2 

7' 

7' 

In  a  great  blank  space.    Has  2  stars  8  m  near  .... 

II.  19 

588 

4855 

16 

17 

38.5 

i57 

47 

0 

299.3 

4 

10 

10' 

579 

48S6 

16 

18 

36.6 

142 

13 

27 

240.7 

3 

10 

11 

468 

4857 

16 

18 

43.1 

136 

5 

27 

73.1 

5 

8' 

10 

L  white,  S  red.    Pos  72.4,  73.9   

463 

4858 

16 

J9 

4.0 

167 

8 

1 

104.8 

20 

5 

(|3  ApodisJ)    Difficult.    Large  sjs  single  and  well 

A.  1886 

587 

denned. 

4859 

16 

10 

13.2 

117 

56 

53 

274.5 

10= 

:IO 

45i 

12 

4860 

16 

20 

22.4 

169 

18 

45 

23°i 

8 

8 

12 

705 

25.5 

19 

4 

235.1 

15 

9' 

12 

573 

486l 

16 

21 

18.7 

i37 

44 

39 

5± 

10 

6 

IO 

[Pos  dist,  and  mag  merely  estimated  from  the 

L.  6860 

463 

diagram.] 

4862 

16 

22 

15-3 

151 

10 

28 

180.7 

10 

9' 

9' 

596 

4863 

16 

*3 

Si.8 

143 

24 

56 

1 24. 1 

9' 

IO 

468 

4 

224 


REDUCED  OBSERVATIONS  OF 


No. 


R  A.  1830.0. 
h.  m.    s.  d. 


N  P  D.  1880.0. 


Position. 


Magnitude. 


Remarks. 


Synon. 


4864 
4865 
4866 


4867 


4869 

4870 
4871 

4873 
4874 

4875 


4876 

4877 
4878 
4879 
4880 
4881 
4882 
4883 
4884 
4885 


4886 


4887 


4890 

4891 
4892 

4393 
4894 

4895 

4896 

4897 

4898 


16  24  9.6 
16  24  18.3 
16  25  39.9 
40.8 


16  26 

16  26 
16  26 

16  27 

16  27 

16  27 

16  27 

16  27 

16  27 

16  28 


41.0 
41.2 

23-5 
25.8 

53-  4 
54. 1 

54-  4 
46.2 

49.1 

55-  3 
56.6 

3-3 


16  28  37.8 

16  29  31.3 
16  29  37.8 
16  29  38.4 
16  30  — 
16  31  37.7 
16  31  57.4 
16  32  38.2 
16  34  37.4 
16  34  52.2 

56-3 

16  35  22.0 
16  36  50.2 
16  37  36.6 
16  39  4.1 
16  39  32.3 

34.2 
16  41  25.0 

26.9 
16  42  3.3 
16  42  8.6 
16  43  - 
16  43  13.7 

16  43  17.4 

16  43  43.2 

16  45  1 1.1 

16  45  17. 1 


96  12  50 

173  41  23 

146  38  12 

38  57 


38  26 

38  45 

133    2  5 

2  17 

139  59  19 

120  35  34 

36  18 
126  51  31 

137  26  — 
117  27  58 
139  1  - 
150  35  47 
117  24  58 
114  52  51 

138  25  19 

138  12  35 

117  39  13 
107  24  o 

!36    3  - 

137  8  13 

138  40  8 
132  3  46 
172  2  42 
138  o  o 

1  41 

93  46  57 

126  34  17 

118  25  13 
109  17  21 

127  12  28 

11  47 
136  37  13 

37  52 
114  23  44 
131  30  26 
131  33  - 
152  55  22 

118  38  28 

136  34  18 

148  54  2 

116  22  47 


314.4 
130.5 
125.9 


129.2 
127. 1 
295.5 
294.8 

77-9 
60.3 

59-3 
10.2 
47.1 

265.5 
72.1 

298.8 

275± 
67.9 

("265.9 
'  164.9 
I  14-3 
90.0 

!-3 

339-9 
1 51.0 
258.5 

!73-4 
183.4 

7-7 
196.5 

245.3 

94± 
149.8 

90.0 
310.8 
9.0:: 

5-2 
329.3 

327-3 
129. 1 
297.7 

119.5 

95± 
24.8 
22.1 
125.0 


30 
27.6 

8 
31.8 

2 

8 

10 
12 
15 
10 
10 
20 
31.9 
5 

12 

30 
30 


9  J3  14 
9  " 
7    7  + 
9  =  9 


7  10 

7'  11 

9  9 

9  9 

6'  12 

7  i° 

10  11 


1  '.j 

9' 
7' 

9 
9'- 
10= 


8  10 


9  + 
9'+ 
=  10 

9 

9 
9 

8  + 
=  10 


=  I3 


Triple  classes  I.  and  II  

Pos  311-7,  316.8,  3147.    Ill  defined   

Beautiful        Pos  131. 7,  129.3   

Pos  126. 1,  127.2,  with  320  and  the  whole  aperture  ; 
124.4  with  800  and  15  inches;  tried  1200,  but 
could  not  illuminate  the  field  sufficiently  for  a 
measure. 

Pos  128.7,  i3°-7>  128.3  

Beautiful         Pos  125.5,  128.7   

Pos  297.8,  294.2,  294.5  

Pos  295.6,  294.0  

Haze  increasing  


Wind  violent   

Mean  epoch,  1836.864   

The  preceding  of  2  double  st . 
Mean  epoch,  1836.719  


The  following  of  2  double  st  

Pos  66.7,  69.0  

A  B.    Pos  266.1,  265.8  "1 

A  C.  J  Quadruple 

AD.  3 


A  3rd  *  11  m  near.    Pos  95  ±  by  diagram 

Epoch,  1837.348  

In  a  cluster  


C  A.    Place  of  the  *  C.    A  *  7  m  also  precedes 

8*.o  somewhat  north. 
A  B.    Place  of  the  star  A.    [N.B.  The  small  star 

10  m  was  not  noticed  in  f  465.] 


A.  209 


Fine  sfc .     Place  bad.     Lamps  going  out ;  wind 
violent. 


Pos  5.0,  5.4  

In  a  vacancy  of  the  milky  way,  which  is  here  entirely 
free  of  ground  stars. 


B.  5770 


B.  5777 


B.  5783 
B.  5781 


h.  1292 
B.  5792 


B.  5825 


B.  5841 


L.  6999 


Chief  of  a  fine  cluster  

Class  2.  In  the  cluster  with  No.  4892 
Distance  by  oblique  transits  =  5"-5o  . 


Fine  s|c.    Pos  24.2,  25.5 


B.  5874 


DOUBLE  STARS. 


225 


No. 

E  A.  1830.0. 
h.  m.   s.  d. 

N  PD.  1830.0. 
0       /  // 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

4899 

16 

45 

28.8 

135 

38 

2 

56 

AO 

55 

270.O 
261+ 

1 

9 
10 

10 

463 
464 
712 

30.2 
8.4. 

I 

1 1 

4900 

16 

4-6 

4-  - 

1 40 

22.9 

20 

7' 

12 

L.  7036 

4901 

16 

4.6 

24..  I 

I48 

35 

4 

134-3 

2 

8 

=  8 

Has  a  large  H«  s  f .  [N.B.  The  obs  gives  the  degree 
of  P  D  149,  but  this  is  contradicted  by  the  obs  of 
f  712,  which  gives  148,  making  the  place  pre- 
cisely that  of  B.  5907. 

B. 

59°7 

717 

25.8 
S.O 

34 
15 

37 
53 

133. 1 
229.6 

3 
5 

8 

=  8 

712 
722 

16 

47 

IO9 

6' 

8 

AC.  1937 

4902 

16 

47 

l6.I 

117 

*9 
In 

33 
29 

31.8 
38+ 

12 

8 

1 1 

453 

723 

31-5 

J5 

8 

12 

Hat  _       _  V           *     1  /           *  i         n            • .  i       ii           />                    a*  \ 

Measure  hurried  (north  of  zenith,  therefore  no  time). 
[N.B.  If  the  discordance  of  R  A  between  these 
obs  arises  j  as  is  jprobabie ,  from  the  moveable 
wire  having  been  mistaken  for  the  fixed,  this 

ohftpmntifi'}}  jc  ihftf  in  hi  oh  win^t  ho  vo'i  ont  oil  "1 

4903 

16 

4; 

I9.8 

T  Tn 
119 

54 

58 

88.5 

t  r 

'O 

9 

12 

45 1 

4904 

16 

47 

4O.5 

165 

6 

57 

1 83.2 

3 

8 

10 

L. 

7028 

5S7 

4905 

16 

4S 

38.5 

144 

48 

34 

65.4 

20 

8' 

11 

Pos  64.5,  66.3.  Large  star  intense  ruby  red,  S  fine 
contrasted  blue. 

469 

_ 

-f- 

67.8 

30 

V 

10 

696 

4906 

16 

An 

28.3 

13s 

38 

5s 

232.4 

10 

8 

12 

467 

A9°7 

16 

49 

39.6 

113 

56 

41 

49.I 

15 

8 

8' 

793 

4908 

16 

2I.O 

129 

2  8 

10 

179.9 

if 

10: 

=  10 

A  neat  star  in  tbe  followiug  angle  of  a  condensed 

ffrmm  in  a  plncfpi* 

glUUU  111  d  bXUMCl. 

456 

4909 

16 

5i 

140 

50 

2  04.. 4- 

17. 1 

8 

8' 

TV/Too**         ,  1      -0./;  „  T  /- 

B. 

j  J  j 

4910 

16 

5i 

3-8 

125 

27 

265.7 

5 

11: 

=11 

791 

4911 

16 

5i 

13.2 

I  10 

9 

59 

0 

722 

4912 

16 

5i 

21. 1 

172 

35 

4 

123.7 

25 

7 

13 

B. 

5928 

594 

4913 

16 

5* 

25.4 

136 

59 

33 

243.6 

3 

9 

11 

463 

4914 

16 

5* 

49.0 

162 

28 

16 

259.3 

9 

9 

Pos  258.8,  259.8.  [The  R  A  may  be  wrong  several 
seconds.]    The  s  f  of  two. 

605 

55-7 

28 

9 

262.9 

9' 

9' 

Pos  264.8,  263.3,  260.5.  Dist  by  oblique  transits 
=  3"-43- 

606 

15 

4915 

16 

53 

14.3 

127 

38 

12 

3  1Q.O 

6 

9 

1 1 

461 

4916 

16 

55 

3r-3 

139 

'3 

3d 

276.4 

7 

9 

—  9 

466 

49J7 

16 

c  c 

J  J 

T  A  A 

6 

28 

331-! 

8 

12 

469 

7 

57-7 

5 

48 

324.4 

8 

12 

696 

9 

16 

55 

55-3 

156 

58 

23 

328.4 

35 

7' 

IO 

L  yell,  S  blue.  A.  214.  Dist  by  oblique  transits 
-  28"-58. 

L. 

7107 

612 

4918 

16 

56 

34.6 

132 

27 

18 

283.8 

8 

9 

1 1 

455 

16 

56 

52.2 

103 

41 

32 

16.7 

2 

8 

=  8 

Pos  16.7,  17.9,  15.5,  17.6.  It  is  not  so  very  close  ; 
180  with  the  full  aperture  to-night  shows  it  very 
well.  The  3  first  measures  taken  with  320,  which 
separates  the  stars  by  one  full  diameter.  When 
the  6-inch  equilateral  triangle  is  put  on,  it  seems 
to  shrink  up,  and  in  that  state  it  does  look  so  very 
minute  as  to  account  completely  for  the  illusory 
distance  of  half  a  second  in  the  last  sweep. 

2. 

21 19 

720 

53-5 

41 

30 

IO± 

1 

8 

=  8 

\_Pos  estimated  from  diagram.']  I  think  this  is  the 
closest  double  star  I  have  seen.  No  time  for  a 
measure  (being  north  of  zenith),  and  the  triangle 
not  having  been  applied  till  past  the  middle  of  the 
field.    Discs  perfect  points. 

719 

2 

4919 

16 

57 

7.0 

Il8 

'9 

48 

267+ 

18 

9' 

IO 

45 1 

16 

57 

44-5 

136 

30 

36 

168.4 

5 

8 

9 

Fine.  Pos  168.3,  168.5;  A.  213.  Marked  double 
in  B. 

B.  5968 

464 

4920 

16 

58 

19.1 

148 

22 

2 

329-3 

32- 

8 

11 

B. 

5973 

712 

4921 

16 

58 

30.0 

121 

27 

10 

'39± 

4 

9' 

IO 

478 

4922 

16 

58 

31.6 

IO9 

58 

5i 

3i4± 

25 

7' 

11 

722 

3  M 


226 


REDUCED  OBSERVATIONS  OF 


No. 


4923 
4924 
4925 

4926 


4927 
4928 


4929 

493° 
493i 

4932 
4933 


4934 
4935 
4936 

4937 
4938 

4939 
4940 
4941 
4942 


4943 
4944 
4945 
4946 

4947 
4948 

4949 

495° 
495i 


R  A.  1S80.0. 
h.  m.   s.  d. 


j6  59  9.4 
17  o  7.2 
17    1  3.7 

17    2  39.9 

41.7 

42.7 
17    3  48.0 


4  34-8 
4  45-5 

4  50.8 

5  33-7 
343 

5  36-6 
5  4°-9 

5  45-7 
45-9 
5  56-2 
7  3-7 

7  17-9 
7  25-4 
7  30.2 

7  3°-8 

7  4i-i 

8  — 

9  424 
9  - 

7  9  52-3 
7  10  25.6 
7  11  6.4 


7  11  4°-7 

7  "  5i-7 

7  12  38.4 

7  13  29.2 

7  13  35-3 

7  14  8.7 

7  14  i8-7 

7  15  3°-7 

7  15  47-8 


N  PD.  1830.0. 


108  2  30 
159  O  40 
152  36  49 

129  37  39 

33  15 

33  26 
93  5°  34 

140  55  29 
128  26  45 
116  20  34 

135  53  20 
53 

144  9  42 
149  14  51 

107  57  54 

59  25 
165  40  32 
116  25  46 

148  50  42 
124  47  2 

i35  59  4° 
167  57  55 

"4  5  44 
146  16  — 
96  14  35 
146  17  - 
121  38  30 

141  43  47 
146  12  20 


155  59  9 

136  58  27 

137  44  25 
124   2  54 

171  46  44 
112  38  22 
135  40  42 
40  + 

147  23  51 
150  31  33 


Position. 


Dist.  Magnitude, 

I 


i84± 

3 

8 

9 

00  8 

12 

10' 

1 2 

I184 

J  T 

20 

i%— 

j 

n 

j 

<  330.8 

10 

7 

12 

I  212.0 

12 

7 

13 

S  332-7 

15 

7 

1 1 

I  210.4 

18 

7 

12 

S  337-1 

8 

8 

11 

I  211. 7 

12 

Q 
O 

1 1 

99± 

H 

8' 

10 

142.8 

4 

10 

11 

299.8 

12 

9 

IO 

41.3 

6 

6  = 

z  0 

226. 1 

10 

q 

II 

224.7 

10 

9 

II 

44-7 

10 

9' 

II 

260.5 

a 

8  = 

=  8 

228.8 

12 

9 

12 

226.5 

8 

0 
y 

10 

236.8 

9 

12 

T?4.^ 

J  JT  J 

6 

8 

11 

88.1 

IO 

10 

11 

130+ 

81.8 

8 

9 

9' 

228.7 

30 

8' 

13 

35s-3 

15 

5 

e. 

D 

108.4 

24.6 

8' 

8' 

23.7 

IO 

9 

9i 

224.4 

30.8 

8 

9' 

94.1 

2 

10 

1 1' 

'39-3 

3 

ii  — 

-ii 

327.2 

12 

3 

12 

f  321.2 

25 

4 

12 

*  64.6 

5° 

4 

12 

243.2 

2 

11 

11' 

170.6 

15 

9  = 

=  9 

112. 1 

4 

9 

10 

109. 1 

12 

10' 

11 

75-3 

12 

8' 

8' 

103.8 

18 

8 

1 1 

269.2 

2 

6' 

7 

266.8 

2 

7' 

8' 

310.7 

10 

io' 

1 1 

303.6 

40 

6 

12 

Remarks. 


Synon. 


A  double  star  taken  by  reason  of  its  remarkable 
situation  in  a  nebula. 

}  Triple.  Large  %  high  orange.  [Probably  some 
S  accidental  slip  of  the  telescope  before  reading 

8/PD.] 

^  Large  star  orange   

S  Triple.  L  very  red.  [N.B.  Lacaille  gives  P  D 
(    =  1290  33'.] 

Ill  denned  with  320.  Also  a  hurried  measure,  as 
(being  north  of  zenith)  the  star  cannot  be  followed 
beyond  the  meridian. 

A  late  and  hurried  measure  gave  46.0  for  pos 
(36  Ophiuchi.) 

Pos  224.5,  225.0  

Pos  259.5,  261.5.  Excellently  separated  and  mea- 
sured with  320  and  the  full  aperture.  [The  dis- 
tance therefore  probably  not  less  than  1".] 

A  R  A  =  5!.o  

(38  Ophiuchi.)    A  late  and  hurried  measure  gave 

pos  =  339-5.     No    other    double  star  near 

36  Ophiuchi. 

Pos  estimated  from  diagram  

Superb  double  star.    III.  25  =  Sh.  245   

Mean  epoch,  1835.895   

Pos  23.1,  23.8,  24.3   

Mean  epoch,  1835.895   

(y  Aral.)     Pos  328.3,  326.2.    A  3rd  *  13  m, 

20. .  . .  30"  dist.    Pos  50  +  by  diagram. 
A  B  }Pos  A  B  =  320.7,  321.8.    Tried  328.3.  It 
AC  )    will  never  do  for  a  measure. 

An  elegant  little  double  star  

Close  to  a  large  nebula  

Pos  74.5,  76.5,  74.8.    Both  yellow  

Pos  268.5,  270.0.    Fine  He   

Viewed  

(E  Arte)   


L.  7171 


a.  2132 


A.  1967 
Sh.  243 


B.  6016 


L.  7220 
1-35 


B.  6027 

L.  7224 
2.  2149 

A.  1983 


B.  6072 


B.  6081 


DOUBLE  STARS. 


227 


No. 


K  A.  1830.0. 
h.  m.   s.  d. 


4952 


4953 


4954 


4955 
4956 
4957 
4958 

4959 
4960 
4961 

4962 


4963 
4964 
4965 


4966 
4967 
4668 
4669 
4670 

497i 
4972 

4973 
4974 
4975 

4976 

4977 
4978 

4979 


4980 
4981 

4982 
4983 
4984 


17  15  52.6 


17  16  23.1 
17  16  41.4 
17  18  28.5 
37.6 

17  18  42.3 
17  19  37.6 
17  19  43.5 
17  20  9.1 
17  22  2.6 
17  23  3.2 
17  23  19.0 
19.8 
17  23  36.6 

37-i 
17  24  35.3 
17  25  17.6 

17  25  48-5 
50.6 

53-3 

17  26  — 

17  26  55.1 

17  27  — 

17  27  — 

17  27  52.9 

17  29  11.2 

17  32  25.2 

17  32  34.3 

17  33  2.6 

17  33  29.7 

17  33  38.6 

17  34  - 

17  36  30.3 
17  36  38.0 
17  36  39.3 
17  36  43.8 
44.1 

17  36  46.7 
46.9 

17  37  57-5 
17  37  58.6 

17  38  - 
17  38  38.4 
17  39  3-7 


N  P  D.  1830.0. 


148  45  52 


109  20  43 

133  49  9 

161  59  52 

59  4i 

139  43  56 

152  48  56 

136  29  30 

130  28  16 

144  30  o 

98  22  6 

149  48  19 

48  13 

122  27  50 


27  15 
131  48  21 
101  7  22 
141    4  58 

4  26 

5  25 
95  46  - 

124  S3  31 
143  32  - 
H3  34  - 
i43  55  8 
138  32  59 
112  16  11 
145  56  6 
160  10  2 
135  6  2 
166  7  8 
145  20  — 


160  27  59 

93  25  27 
143  32  3 
150  19  19 
19  23 

103  13  40 
13  41 

155  9  58 
140  13  25 

138  13  - 

156  28  53 
142  25  29 


Position.  Dist 


Magnitude. 


I76-S 
169.9 
284.2 
293.1 

178.5 
167.3 
93.0 
59.0 
118.5 
90.3 

153-9 
156. 1 

95-5 

102.3 
325.6 
233.8 
233.8 
225.8 
227.4 

;  162.7 

!  i°-9 
276.3 
43.8 
1 1.5 

52.5 

73-5 

11.0 
193.2 
270.3 

29.5 
115.1 

98.5 

44-5 
»39± 
267.0 
239.8 
240.8 

203.9 
205.0 
139.3 
203.6 

59.8 
15. 1 
5-9 


43.1 
25 
15 


4  13 
11  =  11 

10=10 
10=10 
9  =  9 

9'=  9' 
10=10 

10  10 
6'  13 

6  13 

8  11 
6'  8 

9  9 

8  8' 

9  9' 
7'  12 

10 

9  =  9 

11  12 
13=13 

9'  10 

9  10 

8  9 

10  11 

10  ii 

8  9 

7  15 
6'  10 


Remarks. 


9  9 
9'  *3 
10=10 


7  9 
9  9' 
8'  10 


Place  the  centre  of  a  field  in  which  are  7  or  8 
double  stars,  all  about  10"  distance,  and  12  and 
13m;  and  all,  especially  those  in  the  central 
group,  having  an  approximate  general  parallelism 
of  direction. 


Pos  169.5,  i7°-4-    Pine         A.  217 


Obs  makes  the  minute  of  R  A  19  instead  of  18. 
The  earlier  preferred. 

(a  Arm)   

Dist  by  oblique  transits  =  2".23  

12  inches  aperture  


n  p  is  a  remarkable  group  of  stars  12  m 


Besides  this  there  are  at  least  15  or  20  more  st, 
13  m,  clustering  close  round  the  L  star.  Very 
curious. 


Chief  of  a  cluster  . 
L  orange,  S  yellow. 


A  third  near   

AB)T.  , 

The  chief  of  a  cluster  

At  the  n  f  border  of  a  cluster  . .  . 
In  the  s  f  part  of  the  same  cluster. 


A  third  precedes  . 


Dist  by  2  oblique  transits  =  z<)".yz  

Mean  epoch,  1836.510.    [Probably  a  binary  star 
in  a  rapid  state  of  angular  change.] 


(V  Arm.)    Pine  object  

Pos  241.3,  238.7,  239.3  

[If  this  be  Lacaille's  star,  his 
wrong.] 


P  D  must  be  3' 


Pos  205.6,  203.6  

Dist  by  oblique  transits  =  6".2 1   

Neat  star.    Pos  204.6,  202.7.    The  latter  a  delicate 
measure  with  320. 

Mean  epoch,  1837.405   


Synon. 


B. 6085 


A. 2001 


B.  6125 


2.  2183 


h.  591 


B.  6185 
B.  6193 


B.  6204 
L. 742 1 ? 

2.  2204 


B.  6210 


Sweep. 


582 


722 
455 
597 
606 

465 
600 
464 
456 
469 
609 
716 
480 
478 


794 
456 

59 1 
468 
789 
465 

608 

791 
468 
696 
696 
465 

793 
469 

597 
464 
607 


598 
608 
789 
480 
716 

617 
719 

600 
466 

E 

612 
468 


228 


REDUCED  OBSERVATIONS  OF 


No. 


4.985 
4986 
4987 
4988 

4989 
4990 
4991 
4992 

4993 
4994 

499S 
4996 

4997 

4998 
4999 

5000 
5001 
5002 
5003 
5004 
5005 
5006 
5°°7 

5008 
5009 


5010 


501 1 

5012 
5013 
5014 


R  A.  1830.0. 
h.  m.    s.  d. 


17  39.  J9-S 
17  39  42.9 
17  40  37.2 
17  41  58.1 

66.5 
17  42  29.9 
17  42  41. 1 
17  42  46.2 
17  42  50.1 

53.2 
17  43  16.7 
17  43  40.0 

40.7 
17  44  38.6 

17  44  4^-6 
48.1 
17  46  74 
17  46  32.8 
17  47  0.8 
17  47  29-8 
33.8 
17  47  39.0 
17  47  5i-° 
J7  47  5!-S 
17  48  12.7 
17  49  12.4 
17  49  - 
17  49  45.8 
17  51  44.9 

17  52  6.6 

17-  S3  42-8 
46.2 

17  53  49-5 
17  S3  5°± 


17  54  14-4 
16.4 

17.1 
17  54  20.7 
17  54  28.9 
17  54  46.7 
!7  55  - 


NPD.  1830.0. 


152  56  34 
116  16  35 
170  26  29 
168  57  41 

57  34 
135  7  12 
112  17  46 
116  36  22 
147  37  19 

37  9 
103  17  5 
142    9  4 

10  2 
101  17  52 

152    9  41 

7  48 
101  53  45 
105  46  5 
146  55  14 
165  11  28 

11  17 

126  54  39 
162  19  49 

"3  57  5 
120  13  15 
132  2  55 
135  48  - 
149  11  43 

127  14  25 

113  i  32 

156  24  8 
24  32 

114  14  15 

98  10  6 


114  19  11 

20  46 

20  34 

i3«  44  45 
124  56  31 
105  3  15 
133  24  - 


Position. 


268.8 

33°± 
133.2 
302.3 
304.1 
26.4 

179.0 
2.1 
3.8 

3°5-9 
209.3 
211. 7 
I4°± 

262.8 
245.8 
265.7 
I57-I 
293-3 
176.0 
172.7 
117.4 
297.7 

39-5 
104+ 
307.1 

28.2 

333-7 
220.4 

%  21. 1 
i  211. 3 

235-4 
239.6 
20.8 


35°-3 

352.2 

355-° 
1 94. 1 

339± 
69.2 


Dist 


IS 
12 

5 
6 
12 
12 

18 

3 
7 
15 
iS 

12 
18 

3 
3 
12 

25 
15 

6 
10 

3 
6 

15 

26.7 
30 
8 

5 
'5 
1 2 

IS 
2 


Magnitude 


3° 
25 

4 

0.7 


9 
6' 

9 
9' 

10= 

7 


10 

12 
13 
=  9' 
IO 
10 

=  9' 
IO 

8+ 
10 

9 

9' 

12 

13 
1 1 

IO 

9 


8  10 


8'  11 


9 

11: 
7 
9 
7' 
6 

9 

7 
7 

9 
10 

IO 


=  I  2 

IO 

9 
13 


Remarks. 


One  or  two  more  companions   

Pos  302.3,  302.3.    Dist  by  obi  trans  =  9".22 . 


Course  double  star.  Chief  of  a  cluster 
Pos  1.2,  3.0  


A  third  closer  suspected ;   [Pos  estimated  from 
diagram.] 

Ill  defined.  [This position  must  be  rejected]  .... 
Well  defined.   A  neat  star  


Pos  156.5,  156.3,  158.6  (h.  2814) 

By  diagram,  very  unequal  

Pos  176.5,  175.6;  j 
Pos  172.5,  172.9  ;  S 


Dist  by  oblique  transit  =  1 3".04  ^ 


Both  stars  high  yellow 


Mean  epoch,  1836.427   

Another  star  6' m  n  p.    Single . 


A  B  "JThe  triple  star  H.  145.40  in  the  trifid  nebula 
A  C  5    H.  IV.  41. 


The  star  y  in  the  monograph  of  M.  8.  Place  by 
micrometric  measures  from  9  Sagitarii.  Pos  mea- 
sured, Sept.  5,  1837. 

Violently  suspected  double,  and  indeed  set  down  as 
a  tolerably  decided  observation,  after  very  long 
examination  with  320  and  a  triangular  aperture. 
But  a  re-examination  the  next  night,  July  20, 
1835,  with  a  newly  polished  mirror  in  excellent 
action,  with  powers  180,  320,  480,  and  Soo,  the 
latter  defining  it  well,  left  me  satisfied  that  the 
supposed  companion  was  a  mere  illusion.  To 
me,  therefore,  the  star  is  single.  However,  the 
star  was  tremulous  and  restless. 

A  double  s|e  following  the  nebula  M.  8,  in  cluster 
VI.  13. 

The  star  G  in  the  monograph  of  M.  8.  Place 
determined  by  micrometrical  measures  from  9 
Sagittarii.    Pos  taken,  Sept.  5,  1837. 

In  cluster  VI.  13   


Both  yellow  

Too  late  for  measure  . . 
Mean  epoch,  1836.734 


Synon. 


A.  2050 
L.  7474 

B.  6267 

M.  8300 

B.  6273 
B.  6280 

Sh.  379 


2.  2262 


B.  6308 


716 

453 
611 
611 

593 
455 
793 
453 
582 
712 
617 
789 
468 
721 

481 
716 
617 
699 
696 
605 
607 
461 
606 
453 
794 
456 
E 

712 
461 

588 

612 

709 


608 


453 


474 
45  S 
592 
617 
E 


DOUBLE  STARS. 


229 


No. 

B  A.  1830.0. 
h.   m.  s.  d. 

N  P  D.  1830.0. 
0       /  0 

Position. 

Dist. 

Magnitude. 

Bemarks. 

Synon. 

Sweep. 

5015 

17  55  54-5 

135  46  II 

262.6 

3 

6 

11 

A  most  beautiful  and  delicate  object.    Pos  263.0, 

B.  6310 

725 

262.3. 

17  56  39.2 

IO7    12  5 

140.3 

12 

9 

11 

h.  2818 

699 

5016 

17  56  42.4 

94  32  57 

89.3 

5 

10 

1 1 

608 

5017 

17  56  50.7 

138  52  43 

320.4 

-5 

9 

IO 

465 

5018 

17  57  2.5 

149  51  56 

258.9 

8 

10 

1 1 

716 

5019 

J7  57  14-5 

156  50  8 

33M 

45 

7' 

12 

The  first  star  so  bright  as  7.8  m,  seen  nearly  this 
whole  hour  [in  the  usual  mveeping  zone  of  30.] 

612 

^020 

17  57  27.2 

149  55  41 

11. 3 

10 

IO 

12 

716 

5021 

17  57  40.3 

146  27  18 

3 

n 

1 

1  c 
1  5 

One  of  the  most  difficult  double  stars,  by  reason  of 

L.  7564 

696 

the  excessive  inequality  of  the  individuals.  It  is 
the  following  or  two  about  2^  distant,  and  the 
small  star  points  exactly  in  the  direction  of  the 

j.            l,                       V    ll       1            T                        "U1    J  4- 

preceding  star,  by  wnicn  alone  1  was  enabled  to 
get  a  measure.  Distinctly  seen  with  long  atten- 
tion, verifying  a  first  imperfect  glimpse  narciiy 
more  than  a  mere  suspicion.  Mirror  newly 
polished,  and  in  fine  order. 

5022 

17  58  18.0 

142    s  42 

1 14.7 

3 

IO 

13 

599 

5023 

17  58  45.6 

130  36  47 

275.9 

5 

9'- 

—  8' 

—  0 

456 

5i-5 

36  46 

275.8 

8 

IO 

IO 

This  obs  makes  P  D  26',  but  the  star  was  twice  found 
by  the  PD  of  f  456  in  the  equatorial  measures 
(which  see)  so  that  io'  misreading  must  have 

479 

5024 

n   c  ri   1  'y  0 

I7  59  3zo 

153    6  16 

1.6 

30 
j 

5 

I  I 

B.  6329 

481 

5025 

-7  59 

130  39 

100.4 

4.7.0 

9 

9 

IVIean  epoch  1836  506 •  •  •  ■ 

E 

5026 

1 7  59  34.4 

114    7  47 

i3°zh 

793 

5027 

17  59  44-4 

144  23  25 

59.2 

*5 

2' 
0 

9 

469 

5028 

18    0  21.5 

129  22  20 

151.7 

20 

9 

9  + 

718 

26.9 

22  0 

-53-4 

15 

9 

9 

462 

T02Q 

18    0  25. S 

147  52  34 

121. 7 

2 

8': 

=  8' 

L.  7584 

712 

5030 

18    1  17.2 

113  41  47 

281.0 

30 

5' 

-3 

A.  2093 

453 

5031 

18    I  co.c 

137  24  14 

101.2 

18 

9 

9  + 

464 

l8     2  — 

133  14  - 

335-» 

-2 

7 

10' 

Tj^  1    _  0  c  r  _ 

B.  6342 

E 

5033 

18     2  20.8 

138  53  11 

120.5 

10 

8 

1 1 

A  third  dist  30    pos  about  300  as  estimated  by 

L.  76 1 1 

465 

diagram. 

S°34 

18    3  30.4 

136    3  55 

93^t 

Tx 
-4 

9 

9' 

B  6 1  ao 

464 

33.0 

3  49 

9 

IO 

463 

-2 

5°35 

18    3  35.4 

in    5  35 

267+ 

18 

4 

-3 

A. 2096 

793 

3036 

18    5  13- 

124   9  30 

\  7 

IO 

E 

I  8 

18      21  — 

121  11  30 

7 

IO 

E 

D    J I 

W8 

18    6  13.5 

161  51  38 

299.6 

q' 

B.  6361 

614 

12 

IO 

17. 

50  52 

304.7 

18 

8 

IO 

605 

18  7  54.7 

145  37  55 

358-7 

30 

8 

8' 

L.  7649 

469 

5039 

156   9  8 

I29.3 

18 

9' 

IO 

612 

18    8  15.5 

138  20  16 

-54-3 

11  = 

=  11 

467 

5040 

18  10  si. 3 

2 

5041 

18  12  0.5 

143  43  3 
136    0  26 

260.5 
177-5 

2 
-5 

7' 
9 

9 
12 

B.  6385 

789 
725 

5042 

18  12  12.0 

5043 

18  16  51.7 

173  34  46 

10.7 

30 

6 

13 

L.  7615 

594 

145  37  56 
138    6  11 

358.2 
22.8 

6 

9 

7 

9' 
12 

469 

725 

5044 

18  17  8.2 
18  18  4.3 

6 

5045 

5046 

18  18  14.9 

138  27  36 

81.4 

4 

10= 

=  10 

465 

18  21  38.9 

128  49  50 

359.8 

3° 

7 

7' 

B.  6428 

718 

18  21  59.1 

100  54  38 

250.8 

12 

7' 

12 

2.  2325 

59- 

138    7  - 

6' 

E 

5°47 

18  22  — 

7 

5048 

18  23  12.2 

161  33  27 

353-7 

35 

5' 

B.  6436 

614 

3  N 


230 


REDUCED  OBSERVATIONS  OF 


No. 


5049 
5050 
5051 

5052 
5053 
5°54 

5°55 

5056 

5°57 
5058 

5°59 
5060 
5061 
5062 
5063 
5064 
5065 
5066 

5067 


5068 


5069 


R  A.  1S30.0. 
1.  m.  s.  d. 


5070 
5071 
5072 
S°73 
S°74 


5°75 
5076 
5077 
5078 
5079 
5080 
5081 


8  24  40.4 
8  24  46.2 
8  25  6.0 
8  25  12.9 
8  26  43.5 
8  29  — 
8  29  37.2 
43.8 
8  29  42.4 

44-3 
8  31  - 
8  31  38.3 
8  34  3.1 

8  34  16.3 

8  35  - 
8  35  53.6 

8  35  57-7 
8  36  13.2 
8  36  49.6 
8  37  19.0 
8  39  2.2 
3-5 

18  39  29.9 
32.8 
34-4 

18  40  8.1 
9.6 

18  40  42.1 


44.6 

45-7 
18  41  7.1 
18  43  31.5 
18  43  53.9 
18  45  58.3 
18  47  24.6 


25.4 
8  48  - 
8  48  44.0 
8  48  59.5 
8  50  35.4 
8  50  47.8 
8  51  18.7 
8  51  49.7 


N  P  D.  1830.0. 


137  12  1 

147  32  16 
118  57  2 
104  49  29 
131   35  2 

145  55  - 
137  48  18 

50  6 

143  I  24 

»  7 
H5  5°  - 

144  5  31 
141    o  32 

139  47  52 

140  36  — 
164  23  + 
152  22  21 
169  11  11 
127  10  6 

148  6  34 
131  14  56 

15  2 

141  7  23 
8  31 
8  30 

144  32  6 
33  55 

152    o  59 


1  40 

1  6 
112  12  11 

170  14  4 
112  56  44 
168  50  51 
129  44  46 


44  51 
154  1  - 
153  14  30 
126  28  35 
135  56  2 
138  26  35 
126  20  9 
144    1  6 


Position. 


272.3 
108.0 
230.6 
299.9 

»33-7 

330.0 
326.1 
80.3 

77-7 
198.8 

75-7 
295.3 

S  257-o 
(  205.1 

289± 
206.1 
121.0 
271.5 
20.3 
88.3 
90.0 
273.0 
276.3 
274.2 

361.2 

358-7 

<  87+ 
t  86.7 


S  81.7 

i  86.1 


90.8 

53-i 
61.3 
60.3 
346.5 


244.8 
108.6 
205.0 
93-7 
3>3-4 
244.4 
247.5 
166.3 


Dist. 

Magnitude. 

25 

7'  12 

10  io' 

5 

9  10 

20 

8'  8'+ 

3 

10=10 

0  9 

10 

9  11 

20 

8'  9 

10 

9  =  9 

12 

8'  8' 

32.1 

7  10 

8 

1 1=1 1 

12 

9  r3 

12 

7  12 

15 

!3 

8  12 

3 

AO 

T 

4  1S 

3 

11'  13 

20 

6'  12 

20 

7'  10 

8 

8'  11 

12 

6'  10' 

15 

10  11 

_  1 

10  11 

ii 

9'  10 

10 

9  " 

15 

9'  11 

2 
3 

9  =  9 

J5 

8  12 

1 

9  =  9 

12 

8  13 

12 

7  •  12 

15 

8  8' 

15 

9  12 

6  10 

30 

9  10 

12 

6'  ,3 

12 

6'  13 

1.8 

8'  8' 

6 

10  11 

4 

9  10 

15 

8  9' 

18 

9  9 

5 

8  9 

18 

10  10 

Remarks. 


Synon. 


134.1,  1334,  neat  He  . . . 
5th  class.    Zone  review 


Pos  80.5,  80.2 . 


Mean  epoch,  1835.916.  [Nisi  P  D  =  145  56.] 
Another  15m  nearly  south   


Triple 


Class  2,3.  Zone  review 
(\  Pavonis)  


Neat  star  

Very  exactly  in  the  parallel   

Delicate.    A  sfc  1 3  m  follows  a  little  to  the  north  . . 

A  3rd  11'  or  12  m  follows  

Pos  274.5,  274.0.     Perfectly  divided  ;  definition 
excellent. 


A  B  ^  Triple.     The  large  star  being  sus- 

(A  +  B)  C  i  pected  to  be  close  double,  was 
verified  with  480.  320  was  not  enough,  but  the 
night  does  not  bear  magnifying  well,  and  it  is 
with  the  utmost  difficulty  I  can  discern  a  sepa- 
ration. The  line  of  junction  points  very  nearly 
to  the  small  stars. 

A  very  close  object.     Barely  seen 


(A  +  B)  C 


s 


double  with  240  ;  well  divided  with 
480. 


A  R  A  =  7.0  

(1/  Sagittarii.)    CI  IV.  or  V  

Dist  by  oblique  transits  ~  z6".%j   

The  position  (208.8)  is  noted  as  "wrong"  in  the 
original  MS.  The  diagram,  estimated,  would 
give  about  230  or  240  for  the  pos. 

Pos  244.0,  245.6  

Mean  epoch,  1835.517   


L. 7770 


2337 

B.  6460 
L.  7810 


B.  6477 

B.  6489 
L.  7858 
L.  7869 


B.  6512 


A.  2179 
L.  7932 

B.  6546 
L.  7954 


DOUBLE  STARS. 


231 


No. 

5082 
5083 

5084 
5085 


5086 
5087 
5088 


5089 
5090 
5091 

5092 
5093 
5094 
S09S 


5096 
5097 
5098 
5099 
5100 
5IOI 
5102 

5103 
SI04 
5105 

5106 
5107 


5108 

5 109 

5110 
Sin 


R  A.  1830.0. 
h.    m.  s.  d. 


18  53  5-5 
18  54  3.2 
4.2 

18  54  54.1 


18  55  30.5 

33-3 
34.6 
18  56  5.6 
18  56  28.6 
18  56  31.4 


18  56  32.4 

18  56  57.0 

18  57  38-5 

19  1  - 
19    1  16.9 

19    1  29.0 


1  35-5 

2  21.5 
22.3 
24.4 

2  35.0 

3  2-5 
3  18.4 

3  44-2 

4  36.6 

5  57-o 
7  4-6 

7  i6-3 
7  4°-5 
7  5°-4 

5i-5 
9  6.1 
9  42.2 

51.1 


19  10  22.7 
23.4 

19  12  24.6 

19  12  28.7 

29.1 
19  13  9.5 
19  13  28.5 


N  P  D.  1830.0. 


109  28  58 

126  25  5 
24  IO 

127  17  50 


150  17  51 

17  56 

18  6 

144  36  18 

144  24  4 
139  S3  - 


139  50  28 
100  57  58 
121  13  15 
107  43  - 
137  38  4 

133  20  55 

124    6  2 

121  12  20 

12  9 

11  58 

100  51  28 

107  52  35 

126  31  30 

140  16  4 
146  26  12 
115  38  3 
151  34  36 

162    5  23 

141  20  58 
139  49  4 

50  2 
169  7  36 
123  20  50 

19  27 

134  46  17 
46  15 

148  32  52 

157  37  38 

37  58 
119  57  58 
123  11  55 


91.0 
107.4 

8.5 

5-7 

38.7 


36.4 
239.1 
236.8 
236.7 
295.3 
24.7 
70.0 


in. 8 
247.0 
198.7 
61.3 

353-4 
i  220.2 
[  213.6 

243.3 
248.6 
255.4 
250.2 
70.2 
88.8 
254.3 

37-9 
163.8 
311.5 
335-3 

238.8 
36.2 
230.7 
225.2 
207.4 
127.4 
132.4 

79-4 
76.0 
76.8 


139-5 
13.3 


121.0 
90.0 


Dist. 


6 

15 
12 
15.2 
18 

20 
10 

15 
IS 
20 
20 
15 

4 

3 

12 
20 
20 
10 

7 
15 


Magnitude. 


6  =  6 


6  =  6 
8  11 
8  11 
8  11 
10  11 


11  12 
10=10 
8  10 
8  9' 


10 
11 

7  + 
9+ 
9 
9 
10 


10 
7 
9 
9 
9 
9 

10  12 
10=10 
9  12 
6'  12 
8'  9 
10  10+ 

8  13 

9  =  9 
9  « 
9  10 

9  n 
8  9 
8  10 


9  10 
9  9 


Remarks. 


Synon. 


I  Elegantly  triple 


[This  obs  gives  55  for  the  minute  of  R  A.  The 
earlier  minute  preferred.] 

(y  Corona  Australis.)  Pos  28.8,  28.6.  [N.B.  No 
doubt  ought  to  be  38.8,  38.6.  The  diagram 
agrees  better  with  this,  and  the  equatorial  mea- 
sures corroborate  it.~\ 

(7  Cor.  Aust.)    Superb  D  star.    Pos  36.3,  36.5... 

Very  neat  ^;  a$  near,  n  f  

Pos  237.8,  235.7  

In  the  same  field  are  the  next,  and  two  other  nearly 
simDar  double  stars,  and  one  much  fainter  and 
closer  which  precedes,  forming  a  curious  family 
group. 

One  of  the  same  group  of  5  double  stars  

Good  measure  

Mean  epoch,  1836.571   

Pos  352.4,  354.5  

BCJTriPle 

Pos  242.7,  244.0  

Definition  terribly  bad ;  position  and  distance  in 
consequence  very  uncertain.    Yet  a  superb  sky. 

Pos  35.7,  36.8   

Dist  by  oblique  transit  =  i6".56  

[Probably  a  mistake  of  10s  in  reading  the  chrono- 
meter in  one  or  other  of  these  observations.'] 

(3  1  Sagittarii.    Pos  79.5,  79.3   

A  R  A  =  2'. 5.    Pos  76.3,  76.7,  75.1  

I  Triple   

Double  star.    No  particulars   


A.  2206 


h.  1367 


L.  8028 


B.  6612 


2240 
A.  226 


Sweep. 


722 
461 
483 

485 


461 

726 
480 
481 
710 
710 
467 


467 
591 
794 
E 

463 
472 

791 
476 
619 
794 
59 1 
722 
483 
729 
710 

474 
716 

614 
468 
729 
467 
611 
476 
791 

463 
472 
490 
71a 

612 

610 

794 
476 


232 


REDUCED  OBSERVATIONS  OF 


No. 

R  A.  1830.0. 

N  P  D.  1830.0. 

h. 

m. 

s.  d. 

0 

11 

5I12 

r9 

'3 

35-i 

108 

32 

5113 

>9 

25.0 

II9 

37 

44 

5114 

l9 

14 

- 

144 

39 

5 1 1 5 

!9 

IS 

29.2 

130 

12 

1 2 

5116 

'9 

1 6 

6.4 

168 

52 

14 

5117 

l9 

16 

12.7 

134 

12 

45 

5118 

19 

16 

19.9 

161 

O 

47 

5119 

>9 

iS 

2-7 

Il6 

20 

4 

5120 

T9 

18 

39-9 

120 

3 

22 

5121 

»9 

18 

49.0 

I46 

47 

35 

5122 

*9 

18 

50.7 

165 

59 

11 

5123 

»9 

J9 

9-7 

156 

45 

52 

5124 

19 

*9 

29.4 

108 

2 

31 

5125 

IQ 

20 

I?.  Q 
J  y 

I40 

16 

18 

5126 

*9 

22 

29.5 

169 

+8 

34 

5127 

J9 

22 

54.  i 

I76 

30 

6 

5128 

'9 

-3 

40.9 

108 

58 

18 

5129 

*9 

24 

59-3 

137 

7 

20 

5130 

^9 

26 

24.0 

I40 

14 

33 

5131 

19 

26 

41.0 

121 

16 

45 

Si32 

»9 

27 

19.2 

I56 

40 

37 

5*33 

*9 

27 

29.0 

117 

20 

17 

5*34 

19 

-7 

36.2 

I3I 

55 

5° 

5»35 

J9 

29 

2.9 

H5 

52 

15 

<;n6 

J9 

3i 

3.2 

i57 

31 

55 

5 1 37 

J9 

31 

20.9 

163 

12 

2 

5138 

*9 

31 

38.1 

'  J4 

A  I 

41 

22 

44.6 

y 

SH9 

'9 

31 

48.4 

133 

5(-< 

45 

5140 

"9 

33 

47.8 

155 

19 

26 

5  H1 

19 

33 

55-7 

152 

12 

49 

5142 

J9 

34 

9.1 

138 

46 

16 

5143 

19 

3  5 

32.3 

136 

53 

43 

33-9 

53 

39 

5 '44 

»9 

35 

36.4 

"5 

55 

51 

5H5 

*9 

36 

47-7 

125 

24 

5i 

5146 

19 

37 

16.2 

144 

4 

34 

5*47 

J9 

37 

374 

120 

25 

24 

5148 

'9 

37 

57-9 

i35 

47 

29 

5 '49 

19 

37 

59-9 

169 

!3 

18 

*9 

39 

2.7 

i45 

23 

31 

4.0 

23 

30 

5!5° 

l9 

39 

!5-3 

141 

39 

31 

Position. 


C  229.6 

I  5°± 
(  i8o± 


121. 9 

i  i3°-9 
I  270.7 

66.8 

297.3 

267.7 

9.2 
290.4 
171.7 
277.3 
284.3 

2.7 

95-5 
294.5 
327.7 
284.1 

[  "2.7 
I  125.9 

120.7 

145.0 

5  318.0 
I  212.7 

132.0 
14.6 
135-9 
177-3 
262.3 

{  J9'-3 
t  3°8-7 

36.1 
32.9 

134-5 
89.3 

34J-7 
321.6 
332.5 

337-8 
13.2 
152.4 
2S0.8 
81.3 

3174 
150.9 

147-7 
148.9 
261.3 


Dist. 


Magnitude. 


12 

6 

11' 

6 

II 

0 

7 

-J. 

9 

  1 

-  9 

9 

12 

8 

9 

12 

13 

9' 

=  9' 

8 

11 

10 

10' 

9 

13 

9 

=  9 

10: 

=  10 

9 

9 

1 1 

"  + 

10 

11 

8 

10 

10 

10+ 

9' 

9' 

8' 

12 

9' 

9' 

9' 

9' 

8 

11 

9 

9' 

9 

12 

9 

11 

'5= 

=  15 

7 

12 

12 

9 

10 

8 

11 

9' 

12 

7 

1 1 

11 

12 

10= 

10 

10 

10 

9 

10 

8 

10 

9 

12 

10 

12 

7 

12 

8 

9 

Remarks. 


Synon. 


7  7  + 
9  12 


^  Quadruple.   The  two  distant  stars  estim  by  diagram 

A  B.    Some  doubt  >  „     ,  „ 

A.  c.  j  Epoch,  1837.663  

A  3rd  if.  in  the  same  line,  opposite  

L  white,  S  purple  

Very  neat  star  

Neat  star  

Dist  by  oblique  transit  =  I7".9i  

Dist  by  oblique  transit  =  9*-54   

A  R  A  =  7'-5.    A  large  star  s  f   

Bc1Trirle   

11]™^   

Dist  by  oblique  transit  ess  21  ".48  

Good  measure  

Very  delicate.    Taken  at  first  for  a  very  faint  nebula 

Pos  A  B  189.3,  193.0,  191. 7  ) 
Pos  A  C  309.9,  30S.3,  307.9  J 

Fine  double  star  

Two  others,  11  and  13  m,  near  

Dist  by  oblique  transits  =  43".  11.    Another,  8  m, 
near. 

L  yellow,  S  pale  green   

Fine  object  


L.  8098 
B.  6656 

L.  8105 


B.  6717 


L.  S190 
L.  8194 


B.  6740 

A.  227 

B.  6745 


Sweep. 

722 

794 
E 

488 
611 
472 
614 

474 
475 
712 
607 
603 
722 
466 
611 
595 
722 

463 
465 

618 
610 
475 
479 
710 
610 

606 

463 
489 
472 
708 
726 
467 
463 
490 

474 
492 
710 
478 
463 
611 

469 
710 
6,5 


DOUBLE  STARS. 


233 


No. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

Remarks. 

Synon. 

Sweep. 

h. 

m. 

s.d. 

0 

/ 

It 

5151 

J9 

39 

53-5 

127 

18 

30 

358-7 

IO 

9 

IO 

485 

19 

40 

22.4 

114 

52 

10 

312.8 

IO 

_/ 
9 

IO 

h.  2899 

474 

22.7 

52 

33 

321  + 

IO 

IO 

Clouded  thick  over  immediately  on  this  obs.  [Pos 

473 

*i**<J/*/T'#*  1  fill  0          M^rio    ?i//.v'     wisi/rov    ~tfi0    fi  0/  i  ivi  /1  tori  /1*ivf 
jjl      (£/  lUfXls  •       X  fit:  ±rx  O  •    fWU/tco    £/fc    trit(//(tiCcW  (lt\(. 

only  3",  ^Mif                5e  some  mistake,  as  the 

tiiuyiur/t  t  >j it 1 1  (lit (lis  tCj  iitiii  wuuiw  cty/cc  i/ette/ 
with  10  or  12".] 

<I52 

J  J 

J9 

4.2 

45-7 

I20 

41 

42 

151. 5 

3 

9 

IO 

477 

46.1 

4i 

14 

157.2 

3 

9' 

IO 

619 

J    J  J 

»9 

+4 

0.8 

169 

34 

27 

126.8 

25 

7 

>3 

L.  8218 

611 

*9 

44 

7-9 

114 

21 

6 

170.6 

20 

i 

1 1 

L.  8262 

474 

5X54 

.1 

TT 

I4.O 

122 

An 
nri 

A/7 

200.1 

5 

q' 

IO 

47° 

5iS5 

19 

44 

51.6 

15I 

2S 

*5 

193.0 

4 

IO 

II 

480 

• .  •  > 

192.7 
129.3 

3 

IO 

/ 

IO 

1 1 

726 
492 

5156 

!9 

46 

22.3 

125 

l6 

7 

IO 

19+ 

25.0 
42.4 

*5 
4S 

55 
33 

126.7 

270. 8 

18 

9' 

9 

IO 

49 1 
463 

5*3/ 

!9 

46 

136 

12 

J3 

C  T  C8 

*9 

46 

52.1 

165 

2 

8 

IA7  C 

9': 

=  9' 

607 

pi  rn 

>  1 39 

J9 

4b 

11. 0 

130 

57 

29 

34,lJ 

20 

9 

9' 

488 

1 1.2 

56 

36 

jj  j 

20 

9 

9' 

470 

5 160 

J9 

48 

45-9 

136 

40 

26 

t6^  c 
j-i 

l8 

9 

12 

46  ■? 

5161 

J9 

49 

28.2 

J34 

49 

57 

316.8 

8 

IO 

10' 

489 

5162 

J9 

49 

36.1 

161 

17 

H 

291.7 

7 

8' 

11 

5  stars  10  and  1 1  m  precede,  forming  an  elliptic  arc. 

614 

Distance  by  oblique  transit  =  8".34- 

5163 

IQ 

40 

52. ■? 

ici 

1j5 

«  T 

J  1 

2A 

255-3 

8 

Q 

Not  well  divided  with  180,  well  elongated  with  320. 

B.  6780 

727 

Fine  $c  1  but  wants  light  for  the  6  inch  equilateral 
triangle. 

52.4 

31 

49 

248.5 

7' 

8 

Jros  247.9,  249.1.    rine  5|j  ;  measured  witn  power 
320. 

708 

5164. 

J9 

5° 

27.6 

"7 

38 

42 

124.6 

JO 

9 

9' 

475 

5165 

J9 

S3 

31.6 

122 

32 

23 

306.4 

30 

6' 

J3 

Ju.  0322 

5 100 

J9 

53 

54-3 

177 

l6 

52 

252.7 

0 

IO 

10' 

463 

5Ib7 

19 

56 

30.6 

154 

6 

14 

32.1 

12 

9 

IO 

±>.  oisoo 

727 

32.3 

6 

47 

34.2 

g 

9 

IO 

33-5 
49-5 
50.9 

6 

26 
6 

35.2 

g 

8 

TVT 

708 
478 
495 

5168 

19 

56 

120 

13 
12 

7' 
8 

9 
12 
1 1 

L.  8346 

47 

79.2 

18 

51.2 

12 

18 

83.2 

15 

7 

12 



477 

5x69 

J9 

57 

18. 1 

137 

10 

28 

129.3 

2 

10' 

1 1 

463 

c  170 

J9 

58 

25.2 

125 

39 

30 

3  IO. 5 

12 

8 

1 1 

27.6 

39 

15 

3I7-4 

15 

8 

1 1 

491 

5171 

'9 

59 

1.0 

154 

55 

29 

)  3°5-4 
i  334-3 

12 

25 

7 

10 
10' 

A  B  ) 

B.  6807 

727 

5172 

l9 

59 

41.2 

137 

32 

21 

i-3 

40 

8' 

11 

725 

5*73 

20 

0 

2.7 

126 

31 

20 

1 18.7 

15 

5' 

14 

M  9260 

485 

5J74 

20 

0 

4-7 

140 

47 

40 

240.2 

18 

7' 

13 

6,S 

7-3 

48 

31 

242.5 

15 

7' 

H 

729 

5I7S 

20 

0 

41.8 

172 

27 

22 

S  112. 7 

6 

IO 

11 

AB)T.  . 

707 

(  198.1 

9 

11' 

AC5TrlPle 

5176 

20 

1 

i.6 

161 

22 

6 

327-3 

13= 

=  13 

614 

5*77 

20 

z 

8.9 

H7 

28 

3i 

23.2 

4 

9: 

=  9 

B.  6812 

470 

5178 

20 

2 

50.4 

124 

37 

27 

7-3 

3 

7 

IO 

L.  8373 

492 

50.8 

37 

35 

12.0 

2 

7 

IO 

Pos  10.7,  13.2.     An  elegant  D  :{;,  best  seen  with 
12  inches  aperture. 

49 1 

SI79 

20 

3 

7.6 

136 

33 

24 

139-5 

3 

10= 

=  10 

463 

3  o 


234 


REDUCED  OBSERVATIONS  OF 


No. 

5180 
5181 
5182 

5183 

5185 
5186 

5187 
5188 


5189 


5190 

5191 
5192 


R  A.  1830.0. 
h.  m.  s.J. 


N  P  D.  1830.0. 


Position. 


Dist. 


Magnitude. 


5194 


5195 

5196 

5197 
SI98 

5199 
5200 
5201 

5202 
5203 
5204 
5205 
5206 
5207 

5208 


20  3  31.5 
20  4  52.6 
20    4  57.9 

20    s  15.9 

20  5  41.8 
20  6  28.1 
20  6  38.8 
20  9  7.1 
12.8 
20    9  31.6 

20    9  57.9 
60.2 

61.8 

20  10  39.7 
40.6 

20  10  52.8 

20  11  5.0 
20  11  59. 3 
103.3 


5193    20  12  36.1 
39-5 


20  13  23.8 
25.0 


20  13  41.5 

20  13  51.5 

20  14  7.0 

20  15  30.0 

20  16  9.3 

20  16  28.2 

20  17  9.4 

20  17  17. 1 

20  19  4.1 

20  20  6.9 

20  20  19.4 

20  20  47.3 

20  22  10.1 

20  24  3.1 

20  25  5.4 


118  38  47 

122  24  28 
171   30  9 

126  57  l8 

I36  26  46 

I30  41  52 

149  15  II 

167  44  39 

44  3° 
144  47  15 

119  43  47 
43  44 

43  39 

127  26  21 
25  20 

132  34  15 

121  35  15 
177  42  1 
41  44 


147  16  14 
14  41 
16  26 

159  37  20 
36  57 


125  17  40 

152  59  26 

153  o  11 

127  2  ss 

167  27  17 

158  55  53 
134  35  2 
165  55  18 

120  34  48 
129  41  23 

»3S  55  a 

126  4  30 

121  56  33 
124  29  48 

29  10 

128  48  38 
48  15 


221.3 
6.8 

352-7 
S  222.8 

*  183-7 
131.5 
118.7 

64.6 
91.4 
92.1 
324.1 

S  324-7 

*  73-5 

\  329± 
i  7^-3 
$  321.0 

*  65.6 
296.8 
292.8 

S  268.7 
I  299-9 
257-3 
328.4 

325-5 
33i± 

331-4 
333-2 

247.6 
251. 1 


136.8 

283+ 
211.3 
234.7 

207.5 

317.8 

121. o 

12.2 

82.0 

125.7 

31.2 

60.7 

189.9 

257.3 

256.2 

270.7 

270+ 


25 
5 

25 
3 

25 
4 

4 

4 

40 
15 
3 

25 
20 
18 

20 
15 

3 
3 


Remarks. 


Synon. 


10  II 
IO'  12 

5'  12 
6  13 
14 
8  ,3 


8 

12 

10 

10+ 

9 

9 

8' 

15 

7' 

8 

10 

8 
8 

8 
11 

7 

8 

7 

1 1 

9 

10 

9 

10 

6 

15 

16 

10': 

=  10' 

8 

8  + 

9  10 

9'  10 

7'  14 

8  15 


S  10  11 

I  IO  10 

9'  15 

7'  13 

9'  10 

8'  ,3 

8'  11 

10  11 

7'  » 

9'  10 

10  13 

8  9' 

8  13 

8  12 

8  11 

7'  " 

10  11 


Pos  64.1,  65.2  

Neat  stars.   A  R  A  =  2'.o  

A  R  A  =  3\o  

Very  delicate.    A  good  measure   

A  B  )  Another  neat  D  *  n  f.  [N.B.  This  obs  gives 
AC)     8m  for  the  minute  of  R  A.] 

I  A  fine  triple  star   

*  

1 

^  Triple.    Very  delicate  

Pos  329.1,  328.7,  327.5  

Fine     .    Too  far  from  merid  for  any  good  place  or 
measure. 

L.    Very  red  

Follows  a  Pavonis  36  .5,  and  is  1'  north  of  it  

Follows  a  Pavonis  on  its  parallel  

Pos  246.0,  249.3  ;  extremely  delicate   

2524,  249.9  >  one  °f       most  beautiful  and  delicate 
double  stars.    A  slight  dew-cloud,  though  it  does 
not  destroy  the  sharpness  of  definition,  yet  renders 
the  measures  difficult.    Great  care  however  taken. 
)  Triple.  The  small  star  lies  exactly  half-way,  and  in 
J     the  line  of  junction  of  the  two  larger. 

The  preceding  of  two  

The  following  of  two  

L  white;  S  purplish;  Dist  by  oblique  transit  =  15*.  3  3 
Pos  12. 1,  12.4.  Dist  by  oblique  transit  =  i6'.72  

Among  many  

Pos  259.3,  255.3  

A  third  near   

Pos  est  by  diagram  


L.8331 
L.  8385 

A.  230 
M.  9319 


B.  6838 
L.  8409 


Sweep. 


M.  9354 


B.  6849 


L.  8413 


A.  232 


L.  8476 


DOUBLE  STARS. 


235 


No. 


5209 


5110 
5211 
5212 

5213 
5214 

5215 
5216 
5217 
5218 


5219 
5220 

5221 

5222 


5"3 
5224 

5225 
5226 
5227 
5228 
5229 
523° 
523* 
5232 

5233 
5134 


R  A.  1830.0. 
h.   m.  s.d. 


20  25  35.9 


20  27  7.1 

20  29  l8.2 

20  29  28.8 

20   31  3.9 

20   31  51.8 

20  32  H 

20  32  42.I 
20  34  42.7 
20  34  48.4 

20  34  55-7 
60.6 
64.6 
20  35  12.5 
20  36  17.0 

20  36  24.3 

20  37  13.8 
20  37  21.7 


22.4 
22.5 
20  38  32.5 
20  39  18.5 

21.5 

20  39  48.2 

20  39  52.9 

20  40  3.3 

20  40  29.5 

20  40  53.2 

20  41  43.3 

20  41  57.4 

20  42  57.5 

20  43  23.6 
23.9 

20  44  32.0 
34.8 


NPD.  1830.0. 


137  52  35 


117  52  27 
117  38  52 

i32  59  34 
114  45  58 

121     6  43 

165  55  33 

126  7  30 
128  12  56 

155  4  57 
121    5  23 

5  7 
5  ° 
125  19  25 
117  28  37 

156  19  28 

134  36  20 
153    3  7 

2  51 

2  46 
2  47 
147    o  59 
124  23  47 

23  35 
131  52  17 
117  59  22 
128  31  5 
131  32  6 
134  14  18 

166  3  40 
161  40 
146  33  29 

173  55  56 
56  6 
124  46  3 

45  55 


Position. 


193.2 


123.9 
270.0 
301.0 
272+ 

137.9 
312.3 

187.3 

'97-5 
231.8 
187.9 
188.9 
190.3 
327.0 
357-7 

124.3 

279.3 
97.8 

97-5 

101.5 
98.9 
1 14. 1 
167.5 

168.4 

109.5 

70.8 


101.7 
66.1 
164.2 
1 1 1.5 
12.4 

276.8 
274.5 
91.2 
93.8 


Dist 


45 


*5 


Magnitude. 


3  16 


10  10 

9'  'I 
6  10 
8'  10 

9'=  9' 
8  9 


12 

=  9' 
11 

13 

*3 

13 
1 2 


10  10+ 

8  13 
6'=  6' 

6  =  6 

7  =  7 
7  =  7 
9'=  9 
5  9 

S'  9 

7  10 

7'  8' 

8  10 

8  12 

9  " 
8    8  + 

9'=  9' 
6'  13 

6'  12 

10=10 
9'  10 


Remarks. 


(a //i^')  Pos  193.5,  193-0.  With  the  utmost  care  I  see 
well  a  companion  16  m  as  here  described,  which 
had  eluded  all  my  prior  examinations  of  this  star. 
But  the  night  is  most  glorious.  As  to  any  com- 
panion at  5"  dist,  as  stated  by  Mr.  Dunlop,  there 
is  now  most  certainly  none,  nor  could  this,  I  ap- 
prehend, have  been  seen  with  his  instrument  and 
power.  With  12  inches  aperture  I  see  it ;  with  9, 
with  the  utmost  difficulty  it  is  discernible,  but  so 
seen  I  should  estimate  its  distance  at  full  60". 

\Tlie  pos  set  down  is  27.3  ( — 0.7  for  zero)  but  the 
diagram  contradicts  this,  and  doubtless  it  should 
have  been  written  273.] 

R  A  by  obs  20  32  15.4 ;  but  there  is  a  remark  "just 
out  of  the  field,"  so  that  this  is  a  few  seconds  too 
great. 

Dist  by  oblique  transit  =  7".62  

[16  probably  a  mistake  in  writing  for  6.]  

Very  beautiful  object  

A  most  beautiful  object  

[The  diagram  contradicts  the  reading  of  the  position 
wire  which  gives  224.3  f°r  position.] 

Dist  by  oblique  transit  =  8*.  194,  presuming  124.3  to 
be  the  true  angle  of  position. 

A  star  5  m  precedes   

Superb  D  He  ;  Pos  97.8,  97.8  with  480.  Excellent 
measures. 

Pos  98.7,  96.3  ;  very  fine  ;  measures  taken  with  320 
and  apertures  12  inch  circle  and  equal  triangle. 

Pos  102.3,  100.7  ;  superb  star  

Pos  99.5,  98.8,  98.3   

Pos  168.2,  166.8  (a  Microscopii)  

Pos  167.4,  169.4  

Small  %  blue  

L  pale  yell ;  S  pale  blue  

No  particulars.  Double  

Lyell;  S  blue  

Dist  by  oblique  transit  =  i6".66   

Pos  113.0,  in. 3,  110.3  

A  third  12  m  precedes,  making  nearly  an  isosceles 
triangle. 

Very  ill  defined ;  small  ^  barely  seen  

A  R  A  =  18s   


Synon. 


A.  2417 


h.  2982 
L.  8512 


L.  8546 


L.  8555 


M. 9584 
B.  6917 

R.  26 


B.  6922 
M.  9606 

M. 9611 
M.  9613 
L.  8586 


L.8573? 


L.  8528 


Sweep. 


729 


475 
475 
728 

473 


494 
607 


493 
724 
602 

494 
620 
618 
49 1 
475 

610 

728 
726 

481 

727 
602 
710 
493 
49 1 
718 

475 
724 
488 
466 
607 
604 
469 

796 
795 
493 
49 1 


236 


REDUCED  OBSERVATIONS  OF 


No. 


5^35 


5236 

5237 
5238 


5239 

524.0 
5241 
5242 
5H3 

5244 

5^45 
5246 


5247 

5248 

5249 
5250 

5252 
S2S3 
5^54 


5255 
5256 

5*57 
5258 

5*59 
5260 
5261 


5262 

5263 
5264 


R  A.  1880.0. 
h.  m.   s.  d. 


20  44  44.0 

45  3i-6 
45  36-9 


20  46  56.8 
57.0 
20  48  18.2 
20  49  34.3 
20  49  35.2 

20  51  31.3 

33-i 

20  53  5.0 
20  54  18.3 
20  54  47.3 
20  54  49.5 
20  55  32.3 
20  55  43.9 
20  56  — 
20  57  58.5 


20  58  22.7 

26.5 

21  o  53.7 
21  1  17.3 
21    1  20.7 

21.9 
21    1  44.7 

47.2 
21  2  — 
21  3  29.3 
214  — 


21    4  48.5 


6  42.3 

6  52.2 

7  13-4 
7  41-9 

7  56-2 

8  51. 1 
8  56.3 


21  10  13.9 
23.7 
21  10  46.4 
21  11  51.4 


N  P  D.  1830.0. 


174  59  36 

58  34 

59  20 


0  5 
128  21  25 
23  29 
163  56  28 

135  3  13 
133  39  14 

i«  59  38 
59  5 
157  42  39 

146  9  12 
123    o  40 

147  42  26 
115  25  24 

95  9  33 
175  17  19 

J45  J5  4 


139  32  20 

138  31  39 

121  21  59 

128  51  21 
154  23  o 

22  52 

113  47  23 

48  o 

105  43  _ 

129  16  13 

130  16  — 
116  36  26 


157  37  12 

151  02 

141  24  29 

144  9  31 

>37  45  49 

162  31  1 

176  35  16 


170  45  58 
46  40 
121  37  35 
125  42  40 


Position. 


Di»t. 


92.0 
92.1 
90.5 


91.3 
301.8 
306.9 
274.6 

14.0 

75-i 
73.8 
210.7 

213-3 
26.1 
39.8 
265+ 
96.0 
216. 1 
138.8 
195.0 
116.8 


186.9 
189.5 
324± 
331-3 
302.7 

3°4-3 
308.2 
305.2 
328.0 
183. 1 

3°4± 


153-3 
269.8 
296.2 
138.7 

270.3 
203.7 

205.6 

96.4 
94.4 
91.9 
73-7 


20 
25 
4 
10 
12 
10 
7 
4 
2.1 
10 


Magnitude. 


1  =  T 
8  8 


10=10 

10  10 
10'  12 

9  =  9 
6'=  6' 
6  =  6' 

9'=  9' 
9'  10 
9'  12 

11  11  + 

8  12 

9'=  9 
10  =  10 

9  10 


Remarks. 


»  9 

9  9 

11'  12 

8'  14 

8  9 

0  II 


8  9 
7  8 
9'=  9 


9  12 

8  8+ 

9'  10 

6  10 

7  11 

6'  12 


7  11 
7 

8  13 

9  12 


An  ill  denned  elongation.    A  bad  night   

A  fine  double  star  

Fine  star.    Good  measures   

A  fine  double  star.  Taken  in  a  widely  extrameridian 
reviewing  sweep,  but  readily  identified  by  a  rough 
place  obtained  by  mixed  estimation  and  measure- 
ment with  the  foregoing. 

Ill  seen  but  double  

Neat  double  # ,  3    

[A  mistaken  wire  assumed  and  corrected]   

Viewed  and  measured  

Neat  star  

Dist  by  oblique  transit  =  n*.52  

Pos  195.7,  194-3.    A  fine  D  star  

Pos  116. 3,  117. 1,  117. 1.  Close  as  this  star  is,  the 
night  is  so  perfect  that  it  needs  no  higher  than  the 
usual  sweeping  power  for  its  measurement  being 
most  beautifully  divided. 

[One  or  other  degree  of  P  D  wrong]   

Dist  by  oblique  transit  -  -  i6"4.o  

Excellent  measure  

Mean  epoch,  1836.127   

Neat  star  

5  th  or  6th  class.  Reviewed  

Very  neat  double  Hs.  [R  A  by  obs  e=  5  m,  but  the 
obs  in  my  5th  Catal  makes  the  minute  4.  Both 
being  found  correctly  reduced,  the  earlier  minute 
is  preferred. 

Dist  by  oblique  transit  =  34".  3  3  

(0  Indi).  Beautiful   

A  third  near   

Large  star  single  

Pos  203.8,  203.7,  203.5,  201.7  

Very  much  past  mer.  No  good  place  or  exact 
measure  attainable. 

A  R  A  =  12.' 5   


Synon. 


L.  8511 


M.  9689 
A.  236 


M.  9741 


h.  3007 


B.  6980 


Sweep. 


B.  6995 
h.  3014 


B.  7003 
M.  9S60 
B.  7006 


B.  7009 


800 
799 
795 

797 


796 
483 

724 
625 
463 

489 
728 
469 
710 
610 
710 
618 
470 
474 
739 
799 
710 


496 
467 
620 
718 

727 
602 

473 
474 
E 

718 
E 

474 


610 
613 
498 
468 
490 
625 
800 

797 

796 
623 
477 
49 1 


DOUBLE  STARS. 


237 


No. 


5265 
5266 


5267 

5268 
5269 
5270 
5271 
5272 
S273 
5274 

5275 
5276 

5277 
5278 


5*79 
5280 

5281 

5282 

S283 
3284 
5285 


5286 
5287 
5288 
5289 
5290 
5291 
5292 

5293 

5294 
5295 


5296 


5297 
5298 


R 

A.  1830.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

h. 

m.  s.  d. 

0 

il 

21 

12  17.6 

113 

5 

48 

196.7 

20 

9 

9' 

21 

14  32.2 

121 

49 

J3 

279.5 

15 

8 

11 

33-3 

49 

38 

275-5 

10 

9' 

1 1 

34.6 

5° 

17 

280.7 

10 

/ 

9 

11 

21 

15  - 

135 

47 

56.7 
183.4 

5 

7 
7 

11 

9' 

21 

15  48.8 

164 

15 

10 

233.0 

12 

11 

11' 

21 

16  20.6 

II4 

7 

5s 

342.6 

4 

21 

17  29.1 

150 

55 

37 

56.4 

18 

7' 

12 

21 

*7  49-7 

115 

37 

7 

40.7 

15 

10 

11' 

21 

18  24.4 

I32 

9 

H 

200-4- 

20 

8 

13 

21 

19  32.1 

I39 

6 

102.5 

3 

10 

11 

2 1 

20  5*i 

"5 

32 

58 

100.0 

20 

9' 

=  9' 

9.0 

32 

25 

158.9 

25 

9 

9' 

2 1 

20  27.O 

127 

16 

44 

199.5 

45 

7' 

12 

21 

23   21. 1 

146 

8 

56 

*3-3 

4 

II: 

=n 

23  25.6 

144 

3 

2 

3  5-5 

g 

IO' 

13 

23  48.7 

173 

29 

5 

0 1.0 

3 

5' 

9' 

21 

*3  55-9 

123 

6 

288.2 

5 

II: 

=  11 

21 

25  5.8 

121 

17 

45 

349± 

7 

IO 

10' 

21 

26  37.3 

158  18 

48  \ 

217.3 
213.4 

30 
3 

9' 

I  3  = 

13 
—  11 

21 

28  — 

107 

10 

80.3 

18.0 

9' 

10 

21 

28  45.1 

129 

13 

20 

84.1 

2 

II  : 

=n 

21 

28  - 

107 

4 

- 

268.9 

52.2 

8 

10 

21 

29  26.4 

120 

13 

28 

290.5 

10 

9 

10 

30.9 

12 

24 

292.4 

12 

8' 

9' 

31.3 

J3 

59 

294.1 

8 

9 

10 

21 

31  8.9 

148  39 

11 

91.7 

6 

9 

10 

21 

3i  154 

165 

1 

4 

319.6 

3 

10' 

11 

21 

32  5.6 

128 

42 

2 

56.1 

15 

8 

10 

21 

32  29.5 

171 

22 

51 

46.8 

10 

10' 

12 

21 

32  41. 1 

144 

54 

15 

287.0 

10 

9' 

11 

21 

32  45 

104  59 

8' 

9 

21 

33  34-5 

i75 

32 

19 

130-4- 


3 

7' 

10 

21 

35  8-8 

122 

25 

44 

252.9 

15 

8' 

J3 

9.8 

*5 

J3 

252.1 

15 

9 

12 

21 

35  45-5 

150 

59 

7 

193.2 

4 

9' 

=  9' 

35  5s-5 

165  41 

4 

204.7 

9 

10 

21 

36  12.1 

117 

29 

27 

188.7 

16 

9' 

=  9' 

21 

37  9-4 

138 

4 

0 

13.7 

20 

5' 

10 

9.9 

4 

18 

'3-5 

20 

7 

11 

21 

37  44-6 

121 

40 

54 

335-7 

30 

5' 

10 

45.0 

40 

43 

336.0 

30 

5' 

10 

46.2 

4i 

2 

333-9 

25 

5 

13 

21 

40  57.1 

118 

43 

37 

256.6 

20 

8' 

11 

21 

41  48.0 

163 

22 

3 

304.5 

5 

11 

13 

21 

43  49 

106 

39 

8 

9 

Remarks. 


Synon. 


L  red,  S  blue  

£  ^}  Epoch  1834.479   

Very  ill  defined   

Pos  unsatisfactory  

Pos  estimated  from  diagram  

(\  Octantis)  not  noticed  as  double   

Viewed  to  verify  an  obs  with  the  equatorial.  It  is  a 
fine  double  star.  The  equatorial  observation  was 
no  illusion.    Pos  79.6,  82.3. 

AB  ) 

Epoch  1836.641  ;  Nisi  P  D  =  1070  5'  

Epoch  1836.641  

Neat  star  

Class  3.    Zone  review   

Too  ill  defined  for  measure.  Pos  from  diagram .... 
Seen  double,  but  night  too  bad  for  measure   

Pos  204.1,  205.3  

Pos  13.5,  14.0 ;  "  double  "  in  the  B.  catal.,  but  it  is 
there  stated  that  the  chief  is  the  following, 
which  is  an  error. 

(9  Piscis  Australis)   

Large  star  single  with  320  

Class  4.    Zone  review   

_____ 


B.  7019 


L.8829 
B.7042 


L.8887 


h.3054 
B.7080 


A.2587 
h.  3059 


238 


REDUCED  OBSERVATIONS  OF 


No. 


5299 

5300 
53OI 

5302 

S3°3 

53°4 
53°S 
5306 

5307 

5308 
S3°9 

53i° 
S3n 
5312 
S3I3 
S3i4 
53!5 
5316 

53i7 
5318 

5319 


5320 
5321 
5322 
53*3 
53*4 

53*5 
5326 

5327 
5328 

5329 
533° 
533i 
5332 


R  A.  1880.0. 
h.  m.    s.  d. 


21  43  49-5 
51.0 

55-2 
21  44  8.7 

21  44  37.3 
38.6 

21  44  59.6 
62.5 
63.0 
68.6: 

21  45  28.2 
28.7 
21  45  38.2 

21  45  57-7 
21  46  3.3 

21  46  6.0 

9.9 

21  46  29.3 
21  46  56.6 

21  47  54-3 
21  49  8.6 

21  49  41.9 

21  50  1.6 
21  53  3.9 

21  53  5i-4 
21  55  33.2 

21  55  - 

22  o  58.4 
22    1  13.3 

25-9 
22  1  53.8 
55.2 
58.7 
22  2  16.5 
22  2  40.6 
22  7  12.8 
22  7  42-3 
22  7  58-3 
22    9  28.7 

22  9  52.3 

22  10  43.6 

22  10  46.3 

22  11  58.5 

22  12  11. o 

22  14  0.6 

22  14  20.2 

22  14  51.9 

56.1 


X  PD.  1830.0. 


150 
168 


130  44  IO 
44  28 
44  35 

7  56  5 

7  5 
6  49 

H3  50  55 
51  11 

5i  47 

49  55  : 

133  22  7 

21  32 

121  32  13 

131  50  21 

166  55  44 

121  43  24 

43  27 
136  12  13 
141  52  39 

118  34  27 
168  32  10 

119  52  37 
161  51  22  - 

144  4°  4 
133  32  10 

128  31  8 
149  54  - 
149  39  41 
171  17  38 

18  10 

129  9  o 
9  10 

8  9 
146  17  40 

167  30  44 

93  44  2 

151  39  36 
114  33  22 

163  39  24 1 

127  32  24 
160  51  44 

»55  59  49 
155  58  44 

94  25  3 

130  34  33 

152  49  9 

132  53  3 

53  3 


242.1 

242.0 

240.8 

7.2 
273.0 

203.7 

206.1 

349.2 

347-3 
348.6 

347-3 

44.1 

45-5 
253.9 
244.3 

71.3 

161. 1  I 
161. 3 

3I5-3 
169.2 
295.8 
2511b 

298.2  I 

359-3 
87.7 
56.8 

149.5 

142.2 
98.3 

123.9 

118.9 
109.2 
in. 9 
105.3 
264.1 

97-5 
203.3 
23.5 

357-3 
270.0 

98.9 
302.0 

83.9 
307.9 
116. 3 

97.6 
275.9 
9.8 
244.4 

250.9 


Dist. 

Magnitude. 

30 

8 

8 

30 

8 

=  8 

10 

8' 

=  8' 

30 

8' 

J  T 

25 

11 

12 

12 

9 

10 

8 

5 

IO 

12 

5 

1 1 

10 

8 

I  I 

12 

8' 

12 

8 

8 

II' 

25 

9 

IO' 

15 

9 

II 

8 

10 

IO 

20 

9 

9 

30 
ju 

/- 
0 

1 1 

25 

10 

9 

1*3 

18 

9 

9' 

5 

9' 

=  9' 

c 

9' 

10' 

A 

1 1 

12 

1  n 
3U 

8 

11 

3° 

30 

10 

3 

12 

8' 

1 1 

20 

9 

9  + 

*i 

8 

10 

15 

9 

9' 

12 

9 

=  9 

12 

2 

8' 

=  8' 

2 

g 

=  8 

2 

8 

=  8 

12 

9 

12 

12 

10 

=  10 

20 

8' 

=  8' 

10 

8 

12 

25 

9 

30 

9 

12 

5 

9 

9' 

25 

6' 

9\ 

30 

9 

9 

5 

1 1 

11' 

6 

10 

10 

3 

1 1 

11 

12 

10 

10 

10 

9' 

1 1 

10 

9 

11 

Remarks. 


Synon. 


Pos  242.6,  241.6 . 


4  R  A  =  3  .0.    R  A  unsatisfactory  in  this  f 
A  B  > 
BC  J 

Pos  203.9,  203.5. 
Pos  207.0,  205.3. 


Neat  if. 
Neat  * 


{The  reductions  of  this  sweep  are  very  precarious 
for  want  of  good  fiducial  stars.] 


L.  8955 


B-7°98 


Triple.    All  3  exactly  in  a  line  

Triple.    One  L,  2  small  in  one  line 


The  former  obs  makes  pos  =  287.0 
111  denned   


h.  3068 


Very  nearly  an  equilateral  triangle 


Pos.  55.3,  58.3   

Epoch,  1834.6  +  the  northern  of  two. 


Points  a  little  north  of  e  Octantis,  which  is  very 
near  it  

Points  a  little  n  <•!'  a  *  5  m  which  precedes  it  .... 

Very  fine  double  *   

Pos  in. 8,  112. 8,  in. 2,  excellent  measures   

A  fine  double  star   

Difficult  to  measure   


M.  10234 


L.9047 


R  A  somewhat  uncertain   

R  A  somewhat  uncertain   

AB) 

AC|  ARA  =  5.o   

?  Position  ;  micrometer  deranged 
Pos  83.4,  83.3,  84.9  (A  238)  


B.7154 


Neat  star  

Pos  243.4,  245.5. 


DOUBLE  STARS. 


239 


No. 


R  A.  1830.0. 
h.  m.    s.  d. 


N  PD.  1830.0. 


Position. 


Dist. 


Magnitude. 


Remarks. 


Synon. 


Sweep. 


5333 
5334 
5335 
5336 
5337 
5338 


5339 

534° 
534i 


22  15  6.0 

22  15  8.5 

22  15  18. 1 

22  16  35.2 

22  16  58.3 

22  17  48.6 

22  19  35+ 

22  20  24.5 
38.8 
22  20  54.3 
22  21  32.5 
22  21  47.3 
47.8 

47-9 
49.0 

49-3 


49.4 

5342 

22 

23 

25.5 

5343 

22 

25 

26.1 

5344 

22 

25 

43-7 

5345 

22 

26 

4.9 

5346 

22 

26 

59-9 

61.4 

5347 

22 

27  48.9 

49.6 

5348 

22 

28 

0.3 

5349 

22 

28  38.0 

535° 

22 

28 

45-8 

535i 

22 

29 

4.2 

5352 

22 

29 

1 1.4 

5353 

22 

29 

14.7 

5354 

22 

29 

29.9 

5355 

22 

29 

30 

5356 

22 

30 

17.6 

5357 

22 

3i 

53-4 

5358 

22 

33 

30.9 

5359 

22 

35 

59.0 

5360 

22 

36 

0.0 

0.1 

536i 

22 

36 

2.0 

5362 

22 

36  35-7 

5363 

22 

38 

12. 1 

22 

39 

4.I 

5364 

22 

39 

52.O 

5365 

22 

42 

6.4 

152  25  54 

155  49  52 

136  9  1 
164  44  50 
135  45  12 

142  39  7 

134  37  ± 

164  45  44 
46  47 
152  16  1 

137  10  28 
123  12  23 

12  26 
12  44 

11  ± 
9  ± 

12  29 

156  55  30 
132  38  51 
129  35  57 

95  55  17 
122  32  56 

32  13 
125  14  21 

14  49 
149  41  25 

143  34  6 
178  51  36 

138  29  40  j 

135  54  35  \ 

170  44  35  [ 
148  42  41 
104  59  - 
119  J3  32 

148  43  6 
151    1  4 

94  52  25 [ 

149  36  41 

37  27 
156  26  39 

137  49  40 

125  56  34 

95  6  20 
147  24  14 

126  47  1 

46  ± 


236.6 
282.8 
85.5 
24.4 
21.7 
190.7 
225+ 

131.4 
134.2 

3°4-3 
94.0 
171. 1 
169.3 
170.0 
170.9 
173-5 

169.9 

73-3 
52.7 
173,1 
207+ 
32.4 
290+ 
28.4 
27.2 
273.2 
117.3 
120+ 

34°-3 
209.8 

272.3 
253.1 

119.9 
240.8 
76.4 

59.2 


143.2 
89.8 
68.3 

336± 
90.0 


140.2 
285.9 
245.3 
98.0 
270+ 

272.8 


2 
2 
30 

*5 
30 

*5 
25 

30 
5 
3 
4 
10 
100 
12 
10 
7 
3 
30 
20 

5 
3 


10  11 

5  11 

10  =  10 
10'  13 
10' =  10' 
/  12 
5'  9 


9 
10 

10 


10' =  10' 
5  9 


4  7 
io'  =  io' 
10  10'+ 


6'  12 


10 
10 


S  13 
9  i  ' 
y    I  9 

9  10 

9  10' 

8'  9 
8,  8',  9 
8  10 


9+ 
12 

10 

12 


9  10 

7=7 
10  10' 
6'  13 

7  14 


(8  Tucani)  283.3,  282.3 


L  yell,  S  bluish.    Pos  est  by  diagram  (o2  Gruis) 


Pos  300.3  ;  304.3  better  

Neat  star  

(|3  Piscis  Australis)  fine  D>|{   

Pos  169.3,  169.4  

Pos  170.7,  169.4   

Pos  172. 1,  170.5,  170.0  

Pos  173.7,  173.8,  172.9;  PD  rude,  being  beyond 
the  sweep  more  than  a  degree. 


Dist  by  oblique  transit=  8". 67. 

Neat  

Very  neat  star  


A  fine  object   

The  preceding  of  two  bright  st,  very  difficult 


Pos  273.8,  272.6;  very  neat 


M. 10473 


Excessively  ill  defined 


Triple 


^Triple   

A  R  A  =  4'.o  

Class  4,  zone  review  

Elegant ;  has  a  ^  6  m  2\5  p,  and  about  100"  n, 
which  with  this  constitutes  the  coarse  double  star 
A.  242. 


AEA  =  fj, 


A  B  ) 
A  C  5 


Triple 


Exactly  in  the  parallel 


Class  6  

Pos.  141.4,  139.0 


A  third  ion,  dist  about  60" 


Very  delicate   

Pos  271.4,  274.3,   difficult,  and  not  well  defined 
(past  merid.) 


A.2760 


L.9133 

A.  239 

B.  7173 


B.7176 
A.  240 


L.9177 

B.7185 
A.  241 


B.7187 


B.7190 
+  7191 


L.  9217 
2937 

L.  9227 
B.  7208 

2.  2944 

L.  92S2 


501 

602 

49° 
625 
490 
730 
728 

627 
625 

501 
490 

494 
495 
492 
620 
619 

493 
610 
728 
737 
739 
495 
494 
493 
49  2 
735 
500 
8co 

496 
490 

623 

470 
E 

475 

47o 
501 

739 
47o 

735 
731 

49  6 
493 
739 
735 
484 

637 


240 


REDUCED  OBSERVATIONS  OF 


No. 

R  A.  1830.0. 
h.  m.    s.  d. 

N  P  D.  1830.0. 
0       /  // 

Position. 

I 

Dist. 

Magnitude 

Remarks. 

| 

Synon. 

Sweep. 

5366 

AH    A  C  Ci 
TJ'T 

133  41  36 
4'  19 

254.0 
254.I 

15 
IO 

g 

9 

1 

728 
489 

g 

8' 

A  D  _J    »    «     .                  ,    -  .              .         -  .       ,  . 

1 14. 1 

10 

15= 

=  15 

5367 

22 

43  2-i 

123  46  35 

275.O 

2j 

5 

9 

.  Pos  274.-3,  276.3,  ^74"4-»  the  last  with  320^  and  A. 

A. 2728 

493 

which  it  does  not  bear  being  tremulous. 

4-9 

46  22 
175  25  46 
26  — 

265+ 
126.5 
125.9 

2j 

5 

8 

(22  Piscis  Australis)  too  ill  defined  for  measurement 

i 

492 
800 
796 

5368 

22 

43  55-8 

8 

9 

9 

=  9' 

IO 

9' 

5369 

22 

46  55.6 

163  12  26 

11. 8 

20 

10' 

11 

625 

537° 

22 

47  38-9 

152    5  30 

136.8 

15 

IO 

1 1 

726 

537i 

22 

48  32.5 

117    0  17 

346.4 

5 

9 

IO 

474 



537* 

22 

49  9-4 

144  16  27 

301.9 

15 

9 

1 1 

500 

5373 

22 

5°  ± 

155  11  ± 

99.6 

48-9 

7' 

IO 

B  72-32 

7Z3 

E 

22 

50  52.4 

95  15  55 

288.7 

8 

9' 

IO 

2.  2964 

739 

C  1 1A 

i  3/4- 

22 

5i  0.4 

164  12  1 

58.1 

IO 

10' 

=  10' 

•••»«• 

625 

5375 

22 

5 1  27-1 

167  14  4 

121. 7 

A 
*t 

11: 

=  11 

627 

c  1 76 

22 

52  39.6 

162  17  47 

351.0 

C 

3 

IO 

II 

625 

5377 

22 

52  39.9 

158  22  49 

270.8 

6 

IO 

II 

610 

5378 

22 

52  49.2 

173  18  50 

343 -1 

35 

-/ 
9 

9' 

633 

5379 

22 

S3  17.0 

147  11  6 

33°-5 

8 

9' 

9' 

470 

22.5 

12  33 

329.5 

12 

9 

IO 

500 

24.8 

12  24 

325.6 

20 

9' 

IO 

Pos  326.0,  325.2;  330.5  tried,  but  declared  unbear- 

735 

able. 

538o 

22 

54  2-9 

158  21  46 

93.1 

12 

10' 

1 1 

731 

538i 

22 

54  5°-7 

ifi5  55  39 

48.8 

3 

IO 

10' 

Tl  • 

027 

5382 

22 

55  2-5 

142  16  2 

5i-5 

7 

0' 

y 

=  9' 

XT 

730 

3.8 

16  15 

45.2 

8 

9'- 

=  9' 

498 

5383 

22 

55  55-3 

125  28  10 

128.2 

8 

9' 

IO 

Til    .1 /'  1 

492 

22 

C-7  fl 

J  /  -^-v 

23.7 

141  36  6 
36  7 

259.4 
264.5 

IO 

g 

15.7240 

=A246 

49» 
730 

IO 

/ 

6' 

7 

Pos  264.4,  264.7.    [N.B.  Examined  the  adjustment 

of  the  micrometer  and  found  all  right.    The  star 
has  surely  changed  if  my  former  position  was  at 
all  correct.] 

22 

57  55- 

105  53  — 

8' 

9 

E 

22 

58  17-9 

150  38  48 

2Q2.I 

12 

8 

11 

A.  245 

726 

28C  •! 

12 

8 

IO 

L.Q372 

501 

5385 

23 

0  1 1.9 

169  15  40 

337-9 

25 

8' 

11 

623 

23 

1  41.2 

116  13  45 

8o± 

IO 

IO 

IO 

733 

53»7 

23 

4  °-9 

131  52  14 

277.9 

12 

8' 

IO 

B  7260 

7  t  7 

737 

6-3 

278.3 

0 
5 

8 

IO 

A  8(1 

4°9 

88 
53°° 

23 

4  4.9 

171   20   ■3  7 

1 2  ^  .2 

IO 

8 

12 

B.72CQ 

6-t-i 

5389 

23 

5  2.2 

158    6  6 

253-5 

8 

8' 

12 

Dist  by  obi  trans  =  7"-34 — Pos  misread  1800  giving 

610 

73.5,  which  the  diagram  contradicts.    A  mean  pos 
used  in  calculating  the  oblique  transit. 

3.0 

5  4° 

246.1 

8 

13 

731 

9 

23 

99  51  26 

1 76. 1 

30 

8' 

2.2993 

740 

5  IO-7 

9 

23 

6  58.5 

100    1  10 

310.7 

60 

5' 

IO 

<r.  776 

740 

539° 

23 

7  9-2 

135  24  24 

12.8 

15 

6 

12 

L.9419 

490 

23 
23 

7  55-8 

8  34-4 

151  55  5° 
126  59  14 

8 

8 

Class  5.                                               A.  247  = 

L.9423 

726 

5391 

341.0 

12 

IO 

484 

9' 

42.1 

58  7 

339-4 

IO 

10' 

The  R  A  not  to  be  relied  on,  as  this  f  cannot  be 

637 

15 

exactly  reduced  for  want  of  zero  stars. 

5392 

23 

8  35-7 

149  13  52 

17-3 

12 

8 

IO 

B.7270 

735 

38.0 

14  11 
115  56  50 

19.4 
312-7 

8 

8' 

IO 
10 

1 

504 
733 

5393 

23 

15 

9  18.8 

9 

DOUBLE  STARS. 


241 


No. 


5394 


5395 


5396 

5397 
5398 

5399 
5400 
5401 

5402 
54°3 
5404 
5405 
54o6 


5407 
5408 

54°9 

5410 
541 1 


5412 
54i3 
54i4 
5415 
5416 

5417 
5418 

54i9 


5420 
5421 


R  A.  1830.0. 
h.  m.  s.d. 


23  10  35.7 
23  II  II. 7 
14.8 

15-3 
15.4 


23  II  40.3 
41.9 
42-3 

23  13  II. I 

23  14  55-3 
23  15  - 
23  16  25 
23  17  28.3 
23  20  9.9 
23  20  28.5 
23  20  50 — 
23  22  16.9 
23  25  - 
23  25  56.3 
23  26  22.5 

23  26  22.8 

25.4 

23  26  45.6 
23  27  19.7 
23  27  25.3 
26.2 
23  30  11.4 
23  30  12.6 

23  30  20.4 

23  30  31.9 

23  32  55+ 

23  33  7-7 

23  33  26.7 

23  34  0.7 

23  35  32.3 

23  36  42.5 

23  36  50.4 

23  37  11. 1 


23  37  1 1.4 
23  38  18.2 


NPD.  1880.0.  i  Position. 


96    3  6 
141  14  25 
14  2 
14  15 
13  37 


128  37  58 

36  25 

37  2 

137  56  45 
99  23  46 
105  25  - 
108  10  — 
172  3  1 
165    4  5 

145  14  52 
108  11  — 

160  o  12 

155  38  - 

120  17  23 
127  48  32 

170  58  59 

59  10 

155  1  47 
140  35  40 

161  45  2 

45  '7 
114  39  15 

93    1  58 

'37  34  44 

121  34  38 

108  43  ± 
168  44  40 

161  46  14 
137  15  28 
117  11  55 
135  35  29 

162  54  42 

109  37  43 


'44  13  7 
145  32  12 


26.3 
209.3 
206.6 
209.5 
207.4 


222.3 
219.0 

153-5 
90.5 
330.0 

90.8 
179.3 
40.0 

199.8 
48.4 

304.7 
80.7 

5  34-8 
(  351-3 
S  38-2 
1 3531 

24.6 

313. 1 

323.3 
325-3 

7Q~I~ 
32.7 

270.O 

57-2 

262.7 
II7. 3 
217.7 
326.9 
I34-I 

95-9 
138.2 


45.0 
49-3 


3 
3 

6 
8 

61.8 

12 
18 


35 

42.3 
15 
5 

15 

20 

18 

20 

n 

3 

7 
5 
8 

15 
3 
16 


Magnitude. 


8'  10 


10  11 
9  =  9 
7  9 

11=11 

7'  13 

10  10 

10  10 

8'  10 

7  10 
io'=io' 

10  11 


9  12 
9  12 

9  9 
12=12 


1 1 

10' 
10 
9' 
8' 

9 
5' 
8' 
6 
6 
6' 


10=10 
6  8 


9  11 
11  11 


Remarks. 


(96  Aquarii),  very  delicate   

Pos  210.3,  208.3  

Pos  207.3,  205.9  

Pos  208.9,  2 10. 1.    Fine  H<   

Pos  207.1,  207.7.  Dist  by  oblique  transits  = 
I3"-°3-  [N.B.  The  obs  of  this  oblique  transit  is 
irregularly  entered ;  there  is  either  some  mistake 
in  the  setting  of  the  wire,  or  it  had  been  moved  in 
the  act  of  observing.] 

Very  elegant  j|e .  ?  Position,  the  micrometer  being 
deranged. 

Pos  226.5  (rejected)  222.8,  221.8;  a  very  elegant 
double  star. 

Pos  219.9,  218  8,  218.3.  Tried  226.5  the  first 
measure  of  f  636.  It  is  evidently  a  mistake  of  50 
in  the  reading  of  the  micrometer. 

Neat  star  

Epoch,  1835.761   

Class  3.    Zone  review   

A  R  A  =  6  .5   

Class  2.    Zone  review   

Mean  epoch,  1836.017  

Micrometer  derangement  corrected  

I  Triple  

I  Triple  

Extremely  ill  defined  

In  a  very  poor  region  

Beautifully  defined  and  tranquil   

The  following  and  less  of  2   

(9  Phoenicia  =  A  251  =  R  27)  

Class  5.    Zone  review   

Points  exactly  toa3d  =  n'm  

Fine  H:  >  and  good  measure  

Pos  95.1,  96.7  ;  A  R  A  =  5%o   

107  Aquarii.  A  fine  double  ^ .  but  ill  defined. 
Measured  after  meridian  by  recalling  the  star  by 
the  collimating  screws  and  reins,  a  great  con- 
venience. 


Sjnon. 


A.  2783 

B.  7276 
A.  248 


2.3008 

L.9487 
h. 3197 
B.  7301 


B.7314 


L.9562 
L.9565 
M. 10865 


A.2836 
a.  786 


Sweep. 


739 
497 
498 
496 
730 


484 
636 
637 

490 
740 
E 
E 

633 
622 
629 
E 

616 
E 

494 
484 

633 
623 

5°5 
497 
616 

5i3 
733 
739 
497 
494 
E 

623 
625 
490 

733 
490 
482 
74» 


629 
629 


242 


REDUCED  OBSERVATIONS  OF  DOUBLE  STARS. 


No. 


S4.22 


K  A.  1880.0. 
b.  m.   s.  d. 


5423 
54.24 


542  5 
5426 

5427 
5428 

5429 
543° 
543i 
5432 


5433 
S434 
5435 
5436 
5437 


5438 
5439 

5440 

5441 
5442 


23  40  32.7 


33.2 


23  41  0.2 
23  41  11. 2 
11.4 

23  41  16.0 

23  43  41.7 

23  44  13. 1 

23  44  32.7 

a3  44  55-7 

23  45  29.5 

23  45  41. 1 

23  46  17.4 

21.2 

2  3  46  57- 
23  47  1 1.2 
23  48  - 
23  50  27.7 
23  51  42-3 

47-7 

23  5i  56-3 
23  53  25-6 
25.9 

23  54  - 
23  57  10.1 
23  58  58.1 
60.6 


N  P  D.  1830  0. 


134  24  27 


24  47 


116  17  o 
146  49  26 
49  23 

152  3  16 
135  26  1 
163    7  31 

i56  53  54 
120  20  43 
167  44  36 
142  30  45 
149  40  58 

4i  55 
108  42  — 
161  48  21 
107  6  — 
152  o  23 
144    2  17 

2  28 


148  10  18 

163  34  31 

34  12 

118    4  - 

112  36  6 

168  25  55 

26  25 


Position. 


349-7 


35'-7 


313.8 
50.7 

57-4 
56.3 
275.1 
317.7 
64.0 
115.5 
221.3 

49-3 
146.6 
32.6 

41.4 

47-9 
2.7 
274.8 
297.6 

293.6 


322.7 
86.3 
87.1 
285.1 
223+ 
63.9 
60.4 


DM. 


Magnitude 


9  =  9 


6' 

9 

9' 
1 1 
11 

9 


9  =  9 
7  14 

7'  10 
9'  io 
9 
9 


Remarks. 


Synon. 


9 
10 
8' 
9 
9' 
5' 


10 
9' 

9' 
10 
12 

9' 
12 
1 1 

*4 


9  H 
10  13 


Nisi  R  A  =  23  41  16. 1 ;  Pos  349-8,  349  7.  The 
last  measure  taken  with  power  1200  with  12 
inches  aperture,  with  which  power  it  is  seen  with 
perfect  distinctness  and  well  denned. 

Nisi  R  A  =  23  41  16.7  ;  Pos  352.7,  350.8.  [N.B. 
In  one  or  other  observation  the  wire  has  been 
■mistaken,  and  on  reducing  both  on  either  sup- 
position, the  point  remains  equivocal.  The 
earliest  R  A  is  therefore  set  down,  as  usual  in 
such  cases.'} 

Very  delicate  ,  good  measure   

Viewed  and  measured  

A  star  7' m  4' s  p   

Pos  63.5,  64.5;  elegant  star  

Very  delicate   

L  yell,  S  blue  

ARA=4%5   

R  A  unsatisfactory  for  want  of  sufficient  fiducial  stars 
in  this  f. 

Pos  40.7,  42.1  T  

Class  3.  A  star  7  m  precedes   

Epoch,  1835.761.    Nisi  PD  =  1070  1'  

Very  difficult.  Seen  only  by  glimpses,  being  ill 
defined.    Must  be  re-examined. 

A  most  delicate  and  beautiful  object.  The  night  will 
not  bear  magnifying,  but  the  small  star  perfectly 
well  seen,  and  no  doubt  remaining. 

Very  delicate   

Epoch,  1834.780   


B.7341 


DOUBLE  STARS  ACCIDENTALLY  OMITTED  PREVIOUS  TO  NUMBERING  THE  GENERAL  CATALOGUE. 


5443 

6  36  — 

130 

11 

104.5 

17.2 

9' 

10 

B.1318 

E 

5444 

10  32  44.3 

171 

2 

8 

230.3 

40 

6 

8 

B.3137 

549 

5445 

14  29  - 

144 

1 2 

70.1 

20 

9 

10' 

E 

5446 

17  20  44.1 

98 

16 

9 

91.3 

15 

9 

10 

609 

5447 

19  42  52.6 

144 

31 

56 

273.6 

5 

10 

1 1 

710 

5448 

22  38  29.9 

128 

55 

2 

205.1 

10 

9 

'3 

637 

5449 

23  46  9.0 

160 

16 

37 

349.6 

4 

10' 

1 1 

510 

INTRODUCTION  TO  THE  MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


(156)  The  instrument  with  which  these  measures  were  executed  was  the  same  with  that 
employed  in  all  my  previous  measures  of  the  same  nature  at  Slough  ;  nor,  excepting  a  change 
in  the  length  of  its  polar  axis  necessary  to  adapt  it  for  a  different  latitude,  was  any  alteration 
introduced  in  the  mode  of  mounting  it.  The  elevated  extremity  of  the  axis  rested,  as  formerly, 
in  a  strong  iron  Y,  projecting  as  an  arm  somewhat  curved  from  the  summit  of  a  wooden  post 
very  firmly  planted  in  the  ground,  so  as  to  allow  room  for  the  person  of  the  observer  between 
it  and  the  eye-piece  when  the  telescope  was  directed  horizontally.  The  lower  end,  carrying 
the  hour  circle,  with  the  necessary  sliders  for  adjusting  the  axis  in  altitude  and  azimuth, 
rested  on  a  wooden  block  bedded  on  a  pier  of  brickwork  laid  in  cement.  The  movement 
necessary  for  following  a  star  in  the  act  of  measurement  was  communicated  as  previously, 
not  by  a  clock-work  mechanism,  but  by  a  screw  movement  worked  by  a  long  handle  and 
Hook's  joint. 

(157)  The  building  in  which  this  instrument  was  placed  was  circular,  consisting  of  a  wall 
seven  feet  eight  inches  high  from  the  floor,  with  a  recess  on  the  north  side  for  receiving 
the  pier,  and  a  door-way  on  the  west.  Its  internal  diameter  was  9  feet  4  inches,  and  on  the 
top  was  bedded  a  wooden  circle  of  4|  inches  in  thickness  by  7  in  breadth,  supporting  and 
held  together  (so  as  to  break  joints)  by  a  cast-iron  circular  rail  whose  section  is  represented 
in  fig.  5,  PL  XII.,  the  projection  being  destined  to  carry  the  rollers  of  the  revolving  roof ; 
and  forming,  when  laid  down  and  screwed  fast  on  its  bed,  a  circle  of  10  feet  6  in.  diameter 
from  summit  to  summit  of  the  projecting  part. 

(158)  The  revolving  roof  itself  consisted  of  a  square  horizontal  frame  of  fir  timber,  five 
inches  in  thickness  and  breadth,  mitre-cut,  and  joggled  together  at  the  angles,  and  bolted 
firmly  together  by  stout  iron  screw-bolts,  which,  besides  drawing  the  joggles  into  close  fitting, 
served  another  purpose  in  reference  to  the  connection  of  the  frame  with  the  superstructure, 
to  be  more  fully  explained  further  on.  On  the  under  side  of  each  of  the  four  beams  composing 
this  frame  and  in  the  middle  of  its  length  was  fixed  a  cast-iron  shoe,  carrying  an  axle  and 
roller,  as  seen  in  section  in  fig.  4,  PI.  XII.  The  form  of  the  shoe  is  shown  in  perspective 
in  fig.  6,  and  in  lateral  projection  in  fig.  2.  The  construction  of  the  axle  is  shown  more 
particularly  in  fig.  8.  The  portion  C  is  squared,  to  prevent  its  turning  in  the  corresponding 
square  aperture  of  the  shoe,  wherein  it  is  secured  by  the  screw  D,  and  the  cylindrical  portion 


244 


MICROMETRICAL  MEASURES  OF 


A,  outside  of  the  shoe,  which  carries  the  roller,  is  somewhat  larger  in  diameter  than  the 
inner  portion  B,  abutting  with  a  shoulder  on  the  outer  face  of  the  shoe.  These  figures 
sufficiently  explain  the  structure  and  adaptation  of  the  parts ;  and  it  is  only  necessary  to 
mention,  that  the  rollers  are  all  situated  on  the  inside  of  the  frame,  which  in  consequeuce 
overhangs  and  entirely  includes  the  circular  rail-way,  as  shown  in  fig.  1. 

(159)  It  is  manifest  that  a  square  frame  simply  so  constructed  and  supported  would  not 
maintain  itself  with  any  constancy  in  one  plane.  Two  of  its  opposite  corners  would  inevitably 
rise,  and  the  other  two  sagg  down  with  every  accidental  inequality  of  pressure.  Stiffness 
must  therefore  be  given  by  the  superstructure.  The  mode  in  which  this  is  effected  will  be 
best  understood  by  inspection  of  fig.  1,  PI.  XII.,  which  is  a  perspective  representation  of  the 
framing  of  the  roof,  supported  on  its  rollers  on  the  railway.  From  the  corners  of  the 
horizontal  frame  rise  four  "  hips"  or  planks  of  deal  somewhat  tapering  upwards,  and  at 
their  lower  ends  cut  so  as  partly  to  rest  upon,  partly  to  abut  into  the  corners  of  the  frame, 
as  shown  in  fig.  7.  These  hips  meet  at  the  top,  where  they  are  all  four  connected  together 
by  a  cross  of  iron,  whose  arms  are  bent  down  and  run  along  their  under  edges,  to  which 
they  are  strongly  screwed.  They  form,  therefore,  the  four  oblique  edges  of  a  quadrangular 
pyramid,  resting  on  and  abutting  into  the  corners  of  the  square  base.  It  follows,  then,  that 
no  two  opposite  corners  of  that  square  can  rise  without  forcing  up  the  vertex  of  the  pyramid 
by  the  hips  resting  upon  them,  and  thus  carrying  up  the  alternate  ones  off  their  bearings. 
To  counteract  this  effect,  and  to  prevent  the  rising  of  these  latter,  or,  which  comes  to  the 
same  thing,  the  relative  sagging  down  of  the  corresponding  corners  of  the  frame,  a  strap 
of  iron,  turned  up  at  its  lower  end  into  a  hook,  is  made  to  seize  the  cross-bolt  uniting  the 
beams  at  the  corner,  and  is  then  screwed  firmly  along  the  under  side  of  the  hip,  as  seen  in 
fig.  7  ;  which  done  at  all  the  corners,  a  pushing  and  pulling  connection  of  the  square  base 
with  the  oblique  sides  and  vertex  of  the  pyramid  is  effectually  established,  and  the  whole 
pyramid  rendered  perfectly  stiff  and  unchangeable  in  form.* 

(160)  The  vertex  of  the  pyramid  is  purposely  made  to  correspond  perpendicularly  over 
a  point  not  in  the  centre  of  the  square  base,  but  20  inches  nearer  one  side  of  the  frame 
than  the  other,  without  which  it  would  be  impracticable  to  observe  in  the  zenith.  In 
consequence,  one  of  the  faces  of  the  pyramid  slopes  materially  more  than  the  other  ;  and 
in  this  more  sloping  face  is  the  opening,  18  inches  wide,  closed  by  two  doors  folding  back  on 
hinges,  and  overlapping  each  other  with  grooves  and  splash-boards  to  carry  off  rain.  The 
rest  of  the  framing  of  the  roof  is  sufficiently  shown  without  further  explanation,  in  the 
perspective  view,  fig.  1,  and  in  projection  in  fig.  3,  where  the  dotted  circle  represents  the 
projection  of  the  spherical  surface  described  by  the  eye-piece  of  the  telescope  when  directed 
to  every  point  of  the  heavens  in  succession,  that  being  rather  the  longer  end  of  the  tube 
when  mounted  in  its  bearings. 

(161)  A  light  boarding  and  painted  canvass  completes  the  covering  of  the  pyramid. 


*  In  the  whole  structure  of  this  roof  the  object  has  been  to  avoid  crippling  and  destroying  the  strength 
of  the  timbers  and  planks  by  cross  cutting  and  mortising,  a  practice  in  carpentry  which  (in  its  lavish  and  too 
common  use)  cannot  be  too  strongly  reprobated.  With  exception  of  the  four  corner  bolts  which  are  indis- 
pensable, small  wood  screws  alone  interrupt  the  continuity  of  the  woody  fibre  throughout  the  whole  structure, 


DOUBLE  STARS.  245 

Beneath  the  square  frame,  the  corners  also,  where  they  project  beyond  the  wall,  are  boarded  ; 
and  a  circular  skirt  board  carried  down  below  the  level  of  the  iron  rail-way,  but  not  quite 
into  contact  with  the  wall,  and  outside  of  the  wooden  ring  on  which  the  rail- way  is  bedded, 
excludes  both  wind  and  rain  beneath.  The  whole  structure  is  so  light  that  it  might  be 
apprehended  that  the  violent  winds  prevalent  at  the  Cape  would  carry  it  away,  especially 
if  gaining  admittance  beneath  it.  But  the  pressure  downwards,  arising  from  the  slope  of 
its  exposed  surface,  more  than  suffices  to  counteract  any  such  lifting  tendency  ;  nor  in  point 
of  fact  did  any  accident  of  the  kind  happen  even  during  the  most  violent  gales,  after  a 
precaution  at  first  employed  of  tying  down  the  corners  by  ropes  to  posts  fixed  in  the  ground 
had  fallen  into  habitual  neglect  from  experience  of  its  needlessness.  The  ropes  were  therefore 
removed  all  but  one,  which  served  to  drag  round  the  roof  into  its  proper  situation,  no 
provision  having  been  made  for  turning  it  from  within. 

(162)  In  the  measurements  executed  with  this  instrument,  the  same  micrometer  (a 
parallel  thread  revolving  micrometer  by  Troughton  and  Simms)  which  had  served  for  my 
former  measures  was  retained,  and  the  same  set  of  eye-pieces  as  heretofore  (of  79,  179,  273, 
and  400  magnifying  powers).  A  "  macro-micrometer"  eye-piece,  by  Dollond,  was  provided, 
and  a  few  measures  taken  with  it ;  but  its  performance,  though  satisfactory,  was  not  so 
decidedly  superior  to  that  of  the  ordinary  double  eye-pieces  as  to  induce  me  to  persevere  in 
its  use  to  their  exclusion  ;  and  no  table  for  the  reduction  of  its  measures  having  been  formed, 
the  few  measures  in  which  it  was  employed  have  remained  unreduced.  As  respects  the 
micrometer  itself  (which  remained  unchanged,  whatever  eye-piece  was  used),  its  readings 
of  position  are  and  always  have  been  unexceptionable,  and  on  the  positions  measured  with 
it  I  have  the  fullest  reliance.  But  as  regards  the  distances,  I  lament  to  be  compelled  to 
state  that  the  case  is  far  otherwise.  The  inherent  defect  of  the  instrument  (a  very  costly 
one),  that  of  the  hitching  of  the  parallel  spider's  threads  in  the  act  of  crossing,  could  never  be 
fairly  overcome.  It  was  in  vain  that,  previous  to  quitting  England,  it  was  placed  in  the 
maker's  hands  for  the  express  purpose  of  remedying  this  annoying  evil.  For  a  while, 
indeed,  it  performed  satisfactorily,  but  the  mischief  soon  recurred,  and  grew  at  length  so 
obvious  a  source  of  error  that  already  in  October,  1834,  I  began  occasionally  to  substitute 
for  the  system  of  measures  by  cross  zeros,  with  the  spider  lines,  that  of  an  absolute  zero, 
with  one-sided  measures  between  the  inner  edges  of  two  thick  parallel  wires  which  had 
been  added  to  the  system  of  wires  in  the  micrometer,  and  which  could  be  brought  into  the 
centre  of  the  field  by  the  screws,  to  the  exclusion  of  the  spider  threads.  This,  it  is  obvious, 
is  a  far  less  eligible  mode  of  measurement  —  the  thickness  of  the  wires  precluding  all 
certainty  of  the  bisection  of  the  stars  by  their  edges,  and  introducing  a  difference  between 
the  measures  of  large  and  small  stars  depending  on  their  brightness ;  add  to  which,  a 
parallactic  error  is  introduced,  which  can  only  be  eliminated  by  empirical  processes,  and  which, 
in  fact,  proved  the  source  of  a  vast  deal  of  trouble  and  of  much  and  obvious  error.  Still 
the  evil  increasing  with  the  spider  threads,  after  vainly  attempting  to  correct  it  myself,  on 
the  9th  April,  1835,  they  were  condemned  as  useless,  and  soon  afterwards  removed  (April  13). 
From  this  time  until  June  3,  1836,  the  thick  wires  alone  were  used  in  the  measurement 
of  distances.  Then,  however,  by  the  kindness  of  Mr.  Maclear,  the  micrometer  was  refitted 
with  a  pair  of  beautifully  even  and  delicate  threads  of  the  Bermuda  spider,  which  he  was 

3  R 


246 


MICROMETRICAL  MEASURES  OF 


so  good  as  to  fix  and  adjust  with  his  own  hands  ;  but  the  hitching  being  thus  only  partially 
remedied,  on  the  27th  June,  1836,  these  were  again  removed  by  him,  and  their  places 
supplied  with  another  pair  more  cautiously  applied.  These  went  on  very  well  for  some 
time ;  but  on  April  27,  1837,  the  hitching  was  again  remarked,  and  from  this  time  to  the 
conclusion  of  my  observations  continued  a  more  or  less  frequent  source  of  annoyance.  So 
long  as  the  evil  in  question  is  confined  (as  it  usually  was)  to  a  mere  temporary  adhesion 
of  the  threads  in  the  act  of  crossing,  it  may  be  presumed  indeed  that  their  elasticity  will 
at  once  restore  them  to  their  right  places,  and  that  no  material  change  of  zero  would  arise  ; 
and  this  really  does  appear  to  have  been  the  case,  on  examining  the  +  and  —  readings  in 
a  great  many  instances.  There  is,  however,  no  security  that  it  shall  be  so  ;  and  where,  as 
has  occasionally  happened,  the  wires  drag  in  their  motion,  though  not  crossing,  and  move 
by  visible  jerks,  all  confidence  is  destroyed,  and  error  to  an  unknown  amount  must  be 
expected  to  arise. 

(163)  The  measurements  of  distance  taken  with  the  thick  wires,  when  compared  with 
those  observed  with  the  spider  lines,  exhihit  a  disagreement  evidently  systematic,  and  one 
which  it  is  of  the  utmost  consequence  to  eliminate,  in  order  that  measures  of  the  same 
double  star  taken  by  both  methods  shall  become  comparable  with  each  other,  and  admit 
of  a  mean  being  taken.  To  this  end  all  the  cases  in  which  measures  of  the  same  star  have 
been  actually  taken  have  been  collated,  and  the  differences  of  the  mean  results  of  both 
methods  being  tabulated,  an  interpolating  curve  was  constructed  by  the  projection  of  the 
results  on  a  chart  of  engraved  squares,  taking  the  distance  as  measured  by  the  thick  wires 
for  the  horizontal  co-ordinate  x,  so  that  the  vertical  co-ordinate  (y)  shall  represent  the 
correction  to  be  applied  to  reduce  that  measure  to  what  it  would  have  been  had  the  spider 
lines  been  used.  It  is  needless  to  give  at  length  the  details  of  this  process,  which  is  one 
purely  mechanical ;  but  the  final  result  of  reading  off  and  tabulating  the  interpolating  curve 
is  presented  in  the  following  table : — 


TABLE  OF  CORRECTIONS 

To  be  applied  to  the  Measures  of  Distance  taken  with  the  thick  wires  and  a  fixed  zero,  to  reduce  them  to  comparison 

with  those  obtained  with  the  spider  lines  and  cross  zeros. 


Dist. 
Meas. 

Correc- 
tion. 

// 

Dist. 

Corr. 

Dist. 

Corr. 

Dist. 

Corr. 
a 

Dist. 
a 

Corr. 

Dist. 
m 

Corr. 
' 

Dist. 
0 

Corr. 
# 

2 

0.0 

18 

+  2.0 

34 

+  3.0 

5° 

+  3-3 

66 

+  3-4 

82 

+  3-4 

98 

+  3-i 

3 

+0.1 

19 

+  2.1 

35 

+  3.0 

51 

+3-3 

67 

+  3-4 

S3 

+3-4 

99 

+  3-' 

4 

+0.3 

20 

+  2.2 

36 

+  3.0 

52 

+  3-3 

68 

+  3-4 

84 

+  3-4 

100 

+  3-' 

5 

+  0.5 

21 

+  2.2 

37 

+  3-i 

53 

+  3-3 

69 

+  3-4 

85 

+  3-4 

101 

+  3-i 

6 

+0.6 

22 

+2.3 

38 

+  3-i 

54 

+  3-3 

70 

+  3-4 

86 

+3-4 

102 

+  3-i 

7 

+0.7 

23 

+  2.4 

39 

+  3-i 

55 

+  3-4 

71 

+3-4 

87 

+  3-3 

103 

+3-1 

8 

+  0.9 

24 

+2.4 

40 

+  3.2 

56 

+  3-4 

72 

+  3-4 

88 

+  3-3 

104 

+  3-i 

9 

+  1.0 

25 

+  2.S 

41 

+  3-2 

57 

+  3-4 

73 

+  3-4 

89 

+  3-3 

i°5 

+  3.0 

IO 

+  1.1 

26 

+  2.5 

42 

+  3.2 

58 

+  3-4 

74 

+  3-4 

90 

+  3-3 

106 

+  3.0 

ii 

+  1-3 

27 

+  2.6 

43 

+  3-2 

59 

+  3-4 

75 

+  3-4 

91 

+  3-3 

107 

+  3.0 

12 

+  1.4 

28 

+2.7 

44 

+3.2 

60 

+  3-4 

76 

+  3-4 

92 

+  3-3 

108 

+  3.0 

!3 

+  i-5 

29 

+2.7 

45 

+  3-3 

61 

+  3-4 

77 

+  3-4 

93 

+  3.2 

109 

+  3.0 

14 

+  1.6 

30 

+  2.8 

46 

+  3-3 

62 

+  3-4 

78 

+  3-4 

9+ 

+  3-2 

110 

+  3.0 

15 

+  1.7 

31 

+  2.8 

47 

+  3-3 

63 

+  3-4 

79 

+  3-4 

95 

+  3-2 

16 

+  i.g 

32 

+2.9 

48 

+  3-3 

64 

+  3-4 

80 

+  3-4 

96 

+  3-* 

»7 

+  1.9 

33 

+2.9 

49 

+  3-3 

65 

+  3-4 

81 

+  3-4 

97 

+  3-2 

DOUBLE  STARS. 


247 


The  corrections  thus  obtained  have  been  applied  to  all  the  distances  measured  with 
the  thick  wires,  as  part  of  the  process  of  their  reduction ;  so  that  the  results  presented  in 
the  following  measures  are,  so  far  as  is  possible,  cleared  of  the  peculiar  sources  of  error 
which  the  use  of  this  method  introduces. 

(164)  The  method  of  oblique  transits*  is  altogether  free  from  this  and  from  every  other 
source  of  systematic  error;  and,  except  that  it  is  liable  to  be  occasionally  defeated  by  the 
accidents  of  variable  refraction,  is  wholly  unexceptionable.  A  great  many  of  the  distances 
have  been  obtained  by  this  method ;  and  when  this  has  been  the  case  it  is  noted  in  the 
appended  notes,  which  contain,  besides,  a  variety  of  miscellaneous  remarks  on  circumstances 
affecting  the  probable  exactness  of  the  measures  both  of  position  and  distance — on  the 
distinctness  of  vision  and  performance  of  the  telescope  as  affected  by  atmospheric  changes, 
and  a  number  of  other  particulars — all  noted  at  the  time  of  observation  (except  in  a  few 
cases  where  the  contrary  is  expressed). 

(165)  In  the  measures  as  originally  set  down,  every  individual  measure,  whether  of 
position  or  distance,  has  a  weight  attached  indicative  of  the  estimated  reliance  to  be  placed 
on  the  measure.  These  weights  vary  from  1  to  10  to  each  measure.  In  my  former  published 
measures  the  sums  of  these  weights  have  been  set  down,  with  the  mean  results.  But  as,  in 
taking  the  mean  results  of  several  sets  of  measures,  the  use  of  these  weights  entails  a  vast 
amount  of  arithmetical  computation,  without  the  advantage  of  any  really  increased  precision 
in  the  result  sufficient  to  repay  the  trouble  thus  caused,  I  have  thought  it  advisable,  in 
presenting  these  observations  to  the  public,  to  adopt  a  system,  intrinsically  quite  as  good, 
and  greatly  facilitating  the  calculation  of  general  means.  It  consists  in  substituting  for  the 
total  or  joint  weights  of  each  night's  observations,  classificatory  numbers  or  simple  numerical 
values  expressed  in  lower  numbers,  1,  2,  3,  4,  and  in  a  few  rare  cases  5.  The  system  on 
which  these  are  assigned  is  this : — If  the  sum  of  the  weights  in  a  set  of  measures  be  below  15, 
the  result  is  considered  as  entitled  only  to  the  lowest  unit  of  value — as  decidedly  an  inferior 
and  unsatisfactory  result.  If  15,  and  below  35,  the  value  2  (expressive  of  a  fair  and  average 
degree  of  reliance)  is  assigned  ;  if  35  and  below  55,  it  is  classed  as  decidedly  good,  and  valued 
as  3 ;  above  55  and  below  85  (cases  occurring  usually  in  favourable  conjunctures,  and  not 
frequent),  the  value  assigned  is  4 ;  while  to  the  very  few  sets  in  which  the  total  weight 
exceeds  this  limit,  and  on  which  particular  pains  had  been  bestowed,  and  a  greater  than 
usual  number  of  measurements  made,  the  value  allowed  is  5.    This  done,  the  operation  of 

*  Let  p  be  the  polar  distance  of  a  double  star  ;  9  its  measured  angle  of  position  reckoned  as  usual  from  0°  to 
360°  in  the  direction  nfsp;  a  the  angle  of  position  of  an  oblique  wire  across  which  both  the  stars  are  allowed  to 
transit  by  their  diurnal  motion;  A  the  interval  of  their  transits  across  it  in  seconds  of  time.  Then  will  the 
distance  of  the  stars  from  each  other  be  given  by  the  formula 

^  _  15".  A.  sin  p.  cos  a 
sin  (a  —  6) 

Convenient  valves  of  o  are  100°  or  110°,  or  (on  the  other  side  of  the  vertical)  260°  or  250°.  Those  most 
commonly  used  were  100°  and  260°.  The  inclination  of  the  oblique  wire  ought  to  be  towards  the  opposite  side  of 
the  meridian  to  that  of  the  line  joining  the  two  stars.  In  situations  not  remote  from  the  pole,  a  high  degree  of 
precision  is  attainable  by  this  method. 


•24S 


MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


taking  the  general  mean  of  several  nights'  measures  is  reduced  to  involve  only  multiplications 
by  a  single  figure,  and  therefore  most  materially  alleviated  ;  while,  from  the  extreme  vagueness 
which  necessarily  attaches  to  such  numerical  estimates  of  the  weight  or  value  of  any  indi- 
vidual observation  or  any  assemblage  of  such,  it  is  obvious  that  no  sacrifice  of  ultimate 
numerical  precision  at  all  worth  considering  is  induced ;  or  rather,  that  the  one  process  is 
quite  as  well  calculated  to  lead  to  final  accuracy  of  determination  as  the  other.  Individual 
measures  are  in  no  case  given,  except  under  some  remarkable  circumstance,  or  if,  as 
sometimes  happens,  only  a  single  measure  was  procured.  To  have  done  so  would  have 
entailed  an  immense  mass  of  printing  without  any  corresponding  advantage. 

(166)  Appended  to  the  micrometrical  measures  here  registered  as  the  results  of  single 
night's  observations,  is  a  synoptic  view  of  their  general  mean  results  reduced  to  mean  epochs. 
In  calculating  these,  not  only  the  positions  and  distances,  but  also  the  epochs  of  each,  are 
derived  from  the  use  of  the  assigned  values  attached  to  them  in  the  general  register,  and 
the  sums  of  these  values  are  appended  in  columns  of  their  own  to  both  the  elements,  as  the 
representatives  of  the  relative  values  of  the  several  results.  In  the  case  of  stars  of  whose 
binary  connection  there  can  be  no  doubt,  not  only  the  general  mean  angle  of  position  with 
its  mean  epoch  is  stated,  but,  for  convenience  of  future  reference,  sub-epochs  are  calculated 
for  each  year  of  the  interval  over  which  the  observations  extended.  The  same  has  also  been 
done  in  the  case  of  one  remarkably  close  double  star  (y  Lupi),  whose  binary  character  is  not 
apparent,  by  reason  of  the  great  discordance  of  its  measures  (arising  from  its  closeness).  In 
the  case  of  y  Virginis  the  general  epoch  has  not  been  calculated,  owing  to  the  extraordinary 
velocity  and  excessive  inecpaality  of  its  angular  motion  in  perihelio,  which  make  such  a  calcula- 
tion useless. 


249 


Micrometrical  Measures  of  Double  Stars  with  the  Seven-feet  Equatorial,  taken  at  Feld- 
hausen,  Cape  of  Good  Hope,  in  the  Years  1834,  1835,  1S36,  1837,  and  1838. 


ndex 
So.  for 
Eefe- 

ence. 


Synonyms. 


1944   

A.  1.    /3  Toucani  . .  .  . 

?  Apparatus  

h.  3376  =  B.  64  

h.  3395   

A.  2  ;  \  Toucani ;  R.  i 


«■  17   

h.  3416  

B.  156.  £  Phoenicis ;  R.  2 

2.  no  

B.  178  ;  k  Toucani  

h.  3426  =  B.  180   

h.  2036  

h.  3437  =  X.  2690  

h.  3447  =  B.  227   

A.  4  =  L  489  

A.  5  =  p,  6,  Eridani 

2.  147  

h.  3461.  —  t  Sculptoris.  . 

h.  3469  =  B.  260   

&•  3475  

h-  3484   

h.  3488   

35°4   


R  A. 

1830.0. 


°  5 


o  24 


o  25 

o  26 

o  38 

o  46 


o  50 
o  56 


9 

10 
1 1 
12 

20 
28 
32 
33 


33 
38 

42 
5° 


2  7 
2  23 


N  P  D. 

1830.0. 


108  6 


153  54 


"5  55 

146  16 
132  50 

160  26 


106  34 

151  o 

146  9 

103  12 

*59  47 

157  18 

106  41 

108  9 

120  47 

144  18 

147  3 


102  7 

115  54 

129  12 

151  8 

120  27 

152  27 

121  7 


Position 
with  Meri- 
dian from 
N  by  W. 


346  24 

344  59 

345  45 

346  3 

173  44 

171  15 

172  8 

172  4 
164  33 
164  31 
163  8 
247  21 

247  53 
62  40 

62  50 

63  25 

78  30 

79  33 

80  51 


80  35 
32  42 

31  35 

32  43 
126  17 

126  38 

127  23 
244  o 

243  58 
352  42 
17  50 
14  20 
346  8 
348  15 
45  o 
38  3 
243  56 
246  24 

75  49 
75  8 
103  57 
105  17 
122  20 
124  12 
122  20 
120  25 

86  55 
69  13 
69  45 

7°  53 
38  47 
36  31 
63  32 
134  56 

"34  43 
267  52 
269  28 
267  20 


Dist. 


68.25 

67.65 
66.21 
68.24 
28.25 
27.12 
29.43 
26.27 
27.31 
7.04 
6.23 
6.30 
7-74 

7-  45 

10.46 

8-  45 
20.46 
19.50 
22.65 
20.97 
21.89 
23.51 
20.94 

6.27 
7.06 
6.65 
5.26 
4.63 
5.26 
5-58 
6.73 
5.81 
8.05 
5.78 
4.24 

2"± 
2.52 

J* 

1.82 
14.24 
I2.58 

3.65 

3.04 
IO.50 
IO.42 

3-39 

3.92 

3-75 
4.65 
5.82 
5-43 

3-37 

3-  32 
89.16 

4-  93 
6.28 
6.49 

8-34 

7.09 


Magnitude. 


5 

5 

5 

=  5 

4' 

=  4' 

6 

9 

6' 

8 

7 

10 

6 

1 1 

7 

1 1 

9 

9 

»  9 
6'  7 


6'  8 
7'=  7' 
7  7 
7'  7' 


7  =  7 

5  1° 

6  11 

8'  9 

5'  11 

6'  10 

7  11 
6  9' 

8'  9 

8'  8' 

7,  9 

7'  10 

6'  7' 

5'  7 

7'  8 

7'  8' 
7=7 


7=7 
6=6 
6  8 


Date  of 
Observa- 
tion. 
1800+ 


35-832 
36.830 
36.895 
36.914 
36.914 
34.849 
34.928 
35-583 
35-583 
37.739 

34-  717 

35-  58o 
35-9I7 
36.958 

37-739 
34.693 

35-583 
37.739 
35.920 
36.711 
36.711 
36.750 

do 

do 
37.739 
35-717 
35-832 
37.797 

34-  772 
36.711 

do 
36.958 
34.772 
36.641 

37-797 
36.641 
36.914 

35-  583 
37.739 

35-717 
36.958 
35-772 
36.925 
36.641 
37.802 

35-9I4 
36.646 

34-  772 
34.849 
34.928 

35-  583 
37-797 
35.906 
36.958 
37.808 

36-  958 
37.802 
37.01 1 
34-772 
36.914 
35.906 
36.958 
37.802 


250 


MICROMETRICAL  MEASURES  OF 


Index 
Ko.  for 
Hefe- 

Synonyms. 

R  A. 
1830.0. 

N  PD. 
1830.11. 

Position 
with  Meri- 
dian from 

N  by  W« 

j 

0  S 
> 

Dist. 

0  s 
3  - 

Magnitude. 

Date  of 
Observa- 
tion. 
1800-)- 

1176 

2 

/- 
20 

118  59 

244  8 

2 

9-75 

- 

2 

6 

9 



34.780 

"77 

241  8 

3 

11.95 

3 

5 

_/ 
7 

35.906 

1178 

240  40 

3 

1 1. 16 

3 

5 

8 

37.802 

1179 

t-  351°   

2 

28 

133  44 

10  55 

2 

4-33 

0 

9 

10 

36.641 

1 1 80 

7  12 

1 

4± 

0 

9 

_  / 
10 

36.958 

1181 

B.  379  +  380  

32 

135  27 

7  35 

3 

97.26 

3 

7  = 

=  7 

36.841 

1182 

h.  35*3   

2 

3S 

120  17 

94  44 

2 

61.55 

3 

0 
0 

8 

37.01 1 

1 183 

66.32 

1 

do 

1 184 

2 

36 

121  48 

56  35 

1 

i5± 

0 

7 

1 1 

34.780 

1185 

2 

37 

131  15 

41  56 

2 

1.90 

1 

7'  = 

=  7' 

35.920 

1186 

46  7 

2 

1.41 

2 

8  = 

=  8 

36.841 

1 187 

42  18 

3 

1.39 

4 

7 

7 

37.019 

1 1 88 

2 

37 

116  15 

184  55 

2 

10.39 

2 

6' 

9 

34.780 

1 189 

185  23 

2 

11.68 

3 

6 

9, 

37.802 

1 1 90 

2 

5i 

115  40 

221  27 

3 

28.62 

2 

7 

7 

35-9°3 

1 191 

2 

130  59 

81  19 

3 

8.27 

3 

4' 

6 

34.928 

1 192 

80  53 

3 

8.96 

1 

35.903 

1193 

82  42 

2 

5 

6 

35.911 

1 194 

81  39 

2 

9.16 

2 

4 

6 

36.841 

1195 

2 

58 

141  59 

70  42 

2 

37-3' 

2 

7 

8 

37-945 

1196 

3 

5 

1 19  40 

310  4 

3 

5.19 

2 

3 

7 

35.870 

1 197 

307  25 

1 

5 

10 

35.903 

1198 

311  15 

2 

5.42 

2 

3' 

9 

36.925 

1199 

3 

9 

154  57 

328  47 

3 

48.38 

2 

8' 

9 

36.901 

1200 

3 

1 1 

IOQ  6 

109  27 

2 

c.77 

1 

_/ 

5 

9 

35-758 

1201 

111  27 

2 

5 

9 

35.870 

1202 

3 

12 

*55  4 

101  49 

3 

18.09 

1 

7 

9' 

3  5-9 '4 

1203 

102  53 

3 

20.5 1 

2 

7 

9' 

36.901 

1204 

$  3576   

3 

136  14 

341  30 

2 

4-75 

1 

7' 

9 

36.006 

1205 

333  25 

1 

4.25 

3 

7 

10 

36.901 

1206 

34°  25 

3 

3.61 

4 

7 

9 

37.019 

1207 

3 

20 

141  40 

42  22 

3 

36.91 

0 

34-772 

1208 

B.  583  =  A.  1 5  =  184  (Bode)  End  

4i  45 

3 

31-55 

1 

7 

10' 

35-9H 

1209 

3 

34 

130  55 

326  53 

2 

8.58 

2 

8 

9 

34.928 

1210 

325  42 

3 

8.74 

2 

7 

8 

35-9°3 

1211 

326  23 

2 

8.59 

1 

6' 

i 

36.003 

1212 

A.  14  =  B.  586   

327  29 

3 

9-54 

1 

7' 

8' 

36.865 

1213 

3 

35 

150  20 

270  33 

2 

54.89 

0 

7' 

8 

34-772 

1214 

269  25 

3 

59.28 

1 

7' 

8' 

36.83S 

1215 

h-3589  

3 

38 

131  12 

344  48 

2 

6.58 

2 

7 

1 1 

37.068 

1216 

h-  3592   

3 

40 

144  48 

11  24 

3 

5.58 

2 

6 

10' 

36.958 

1217 

11  8 

3 

6.38 

2 

6' 

10' 

37.019 

1218 

42 

128  9 

9.06 

2 

35.906 

3 

199  17 

3 

1219 

200  3 

4 

8.29 

4 

5 

5' 

36.914 

1220 

3 

42 

122  18 

136  8 

2 

10.32 

1 

8 

=  8 

35.906 

1221 

136  30 

3 

10.11 

4 

36.925 

1222 

3 

59 

126  18 

"3  45 

2 

10.25 

2 

8 

9 

37-843 

1223 

"°  55 

1 

10.52 

1 

9 

9 

38.082 

1224 

♦ 

6 

124  12 

3°4  25 

2 

30.05 

2 

8 

10 

37-843 

1225 

302  15 

1 

29.26 

1 

8 

10 

3S.082 

1226 

h.  3628   

4 

6 

126  36 

50  3 

2 

50.51 

2 

7 

7 

38.082 

1227 

4 

8 

120  30 

160  37 

9-73 

I 

7' 

9' 

35.906 

1228 

163  15 

2 

1 1.64 

2 

8 

10 

36.988 

1229 

4 

10 

i35  3 

148  25 

3 

12.90 

I 

8' 

8' 

36.006 

1230 

148  5 

2 

12.86 

2 

10 

10 

36.838 

1231 

4 

152  37 

289  37 

1 

6.90 

I 

5' 

12 

36.958 

1232 

4 

13 

124  17 

157  55 

2 

6.52 

2 

7 

10 

37-843 

^33 

157  20 

2 

5.29 

3 

6' 

10 

37-945 

1234 

R.  3  ;  0  Reticuli  

4 

16 

153  4° 

6  5 

3 

5-53 

1 

5' 

9 

34-772 

1235 

B.  713 ;  —  R.4  

6  2 

2 

6.85 

6 

9 

36.S38 

1236 

4 

21 

147  28 

231  28 

3 

7-59 

2 

7' 

8 

36.914 

1237 

232  8 

3 

6.86 

4 

7' 

8' 

36.942 

1238 

4 

2 1 

130  55 

184  9 

2 

4.76 

2 

7 

9 

36.901 

1239 

183  58 

2 

5.14 

2 

7 

10 

36.914 

1240 

4 

28 

115  23 

189  41 

2 

22.42 

1 

7 

11 

37-953 

1241 

4 

30 

145  24 

108  33 

2 

82.29 

1 

3 

1 1 

36.006 

1242 

h.  3677  

4 

34 

119  54 

170  51 

2 

9-94 

1 

9 

=  9 

35.906 

1243 

170  54 

2 

12.56 

9 

=  9 

36.925 

1244 

4 

34 

135  22 

327  15 

2 

40.55 

1 

8 

10 

36.006 

124s 

327  6 

2 

42.79 

2 

8 

10 

36-953 

DOUBLE  STARS. 


251 


Index 
No.  for 
Refe- 
rence. 


1246 
1247 
1248 
1249 
1250 
1251 
1252 
1253 
1254 

I255 
1256 
1257 
1258 
1259 
1260 
1261 
1262 
1263 
1264 
1265 
1266 
1267 
1268 
1269 
1270 
1271 
1272 
1273 
1274 
1275 
1276 
1277 
1278 
1279 
1280 
1281 
1282 
1283 
1284 
1285 
1286 
1287 
1288 
1289 
1290 
1291 
1292 
1293 
1294 
1295 
1296 
1297 
1298 
1299 
1300 
1301 
1302 
1303 
1304 

!3°5 
1306 
1307 
1308 
1309 
13 10 
131 1 
1312 
1313 
1314 
1315 


Synonyms. 


h.3683. 
h.  3694. 


h.  3702  

One  or  other  P  D  io°  wrong  

A.  18  =B.  810  +  811  ;  1  Pictoris. 


h.  3735. 
Rigel  . 


h.  3741  =  B.  905   

h-  374-5  

IT.  I7O  

M751  

h.  3752  =  A.  641  A.  and  B. 

  A.  and  C. 


h-  3759 


h.  376c  

A.  20  ;  B.  961  +  962  ;  6  Pictoris 
h.  3767  =  B.  973   


A.  21   

A.  22  =  B.  976 


h.  3777  =  B.  994 

£  Orionis  

h-  3797  


h.  3803  . 
h.3823. 


A.  23  

B.  1201  "  double." 


B.  1210  +  1211  =  A.  27  ? 

h.3849  

h.  3857  =  B.  1229  


B.  1254  +  1256 
B.  1267  ;  A. 30 


B.  1320  +  1321  ;  A.  31  ;  V.  Puppis  . 


h.  5443  =  B.  1328 
B.  1335;  A.  32.  .. 


R  A. 
1B30.0. 

N  P  D. 
1880.0. 

Position 
with  Meri- 
dian from 
N  by  W. 

Value  attri- 
buted. 

Dist. 

Value  attri- 
buted. 

4 

3s 

149 

I7 

82 

30 

3 

3.25 

2 

79 

58 

3 

4.20 

3 

4 

44 

J35 

27 

63 

12 

1 

?.7Q 

j#/y 

1 

61 

25 

2 

4 

47 

ll5 

26 

222 

35 

2 

21.61 

2 

105 

26 

219 

23 

2 

20. 37 

2 

4 

47 

H3 

45 

56 

57 

3 

12.3  I 

3 

58 

47 

3 

1 2. ill 

4 

5 

7 

122 

7 

150 

19 

3 

7.84 

1 

'51 

27 

2 

7.47 

2 

5 

7 

98 

24 

200 

7 

3 

O.40 

2 

198 

30 

4 

8.96 

4 

200 

43 

3 

9.89 

y  y 

4 

5 

9 

168 

32 

116 

30 

2 

4.2.08 

1 

1 10 

35 

2 

42 .4  C 

1 

5 

12 

124 

12 

168 

18 

1 

15.63 

0 

165 

8 

2 

1 1.4.2 

1 

5 

12 

108 

42 

17 

57 

3 

•38.00 
j"  yy 

3 

18 

0 

3 

jy'  1 

4 

5 

*4 

123 

34 

319 

44 

3 

24.72 

2 

319 

36 

2 

21.46 

2 

5 

15 

114 

57 

hi 

32 

3 

3.27 

5 

108 

25 

2 

"2.  .43 

2 

106 

2 

56.22 

1 

49 

107 

27 

2 

59.87 

2 

106 

58 

2 

Co  28 

1 

5 

y 

109 

50 

316 

15 

2 

27  Q  C 

/  y  j 

2 

314 

35 

3 

20. 6-: 

j 

3 

315 

0 

2 

28.O7 

2 

5 

20 

125 

30 

222 

18 

1 

"t  on 

1 

220 

57 

3 

/  j  j 

1 

5 

21 

142 

28 

285 

5' 

3 

■?  n  1  (S 
iy*iu 

1 

286 

2 

3 

■17  Ci 

3 

s 

25 

137 

!3 

223 

26 

2 

26.44 

0 

23245+ 

1 

I  8.00 

0 

c 

J 

2  c 

1 37 

1 3 

264 

5 

1 

197.15 

1 

5 

26 

132 

26 

171 

35 

3 

/.yo 

2 

172 

1 

•3 

8.78 

•? 

5 

30 

145 

1 

349 

20 

1 

51.82 

1 

e 

j 

32 

Q2 
J 

1 
j 

147 

55 

1 
j 

2.76 

t 

5 

40 

136 

22 

176 

0 

% 

50.40 

1 

174 

52 

2 

1 

5 

42 

134 

55 

114  45 

3 

T  1  O 

1 

116 

8 

1 

109 

30 

1 

iZ"43 

1 

5 

54 

121 

4 

129 

35 

2 

5»°4- 

1 

128 

33 

3 

5.00 

2 

133 

8 

2 

4.66 

4 

131 

18 

•5 

2 

6 

0 

138 

26 

162 

27 

2 

3.86 

2 

163  27 

3 

22.66 

6 

12 

155 

29 

114 

6 

2 

2 

116 

5i 

2 

20.51 

1 

114 

16 

3 

21.21 

4 

6 

149 

8 

223 

24 

3 

cc  66 
55. uu 

1 

224 

54 

3 

55.02 

4 

6 

14 

I29 

25 

5i 

20 

2 

38.59 

2 

53 

13 

2 

40.27 

2 

6 

18 

126 

38 

66 

2 

3 

70.27 

3 

16 

66 

32 

2 

68.45 

2 

6 

24 

I30 

1 10 

12 

2 

71.00 

2 

6 

26 

140 

7 

3J7 

8 

3 

13.83 

2 

318 

5i 

2 

13.24 

1 

6 

34 

I38 

4 

318 

45 

3 

13.87 

2 

3 '4  49 

3 

12.30 

1 

36 

317 

45 

2 

13.19 

4 

6 

130 

11 

105 

2 

3 

17.42 

1 

104 

9 

2 

17.09 

1 

6 

36 

128 

14 

276  45 

3 

8.97 

2 

275 

3 

2 

7.36 

1 

Magnitude. 


Date  of 
Observa- 
tion. 
1800  + 


9  10 
6'  8' 
6'  8 


35-925 
36.884 
36.008 
36.958 
36.925 
36.988 

34-931 
35.016 
36.008 
36.988 
35.049 
36.958 
37.088 

34-  945 
37.019 

37-945 
38.036 
37.107 
37.903 
37.077 
37.110 
37.110 
37.942 
36.925 
37.1 10 
37.942 
37.942 
37-945 
37-953 
35.022 
35.906 

35-  9H 
36.884 

35-911 
37.920 
37.920 

34-931 
35.016 

34-  947 
36.958 

35-  936 
36.082 
35-936 
37.068 
37.920 
36.082 
36.988 
37.071 
37.110 
35.016 
36.878 

34-  947 
36.082 
37.019 

35-  923 
37.068 
37.942 
38.036 

37-945 
38.082 
38.090 

34-  945 

35-  923 
35.016 
36.082 
37.019 

35-936 
36.082 
35.016 
36.008 


•252 


MICR0METR1CAL  MEASURES  OF 


Index 
No.  for 
Refe- 
rence. 


[316 
1317 
1318 
1319 
[320 
1321 
1322 
1323 
1324 
1325 
[326 
[327 
[328 
1329 
1330 
1331 
1332 
1333 
'334 
'335 
[336 

'337 
[338 

'339 
[340 
1341 
1342 
■3+3 
[344 
'345 
[346 
■347 
[348 

[349 
[350 

[35i 
'352 
'353 
'354 
■355 
1356 

'357 
'358 
'359 
[360 
1361 
[362 
1363 

[364 
1365 
1366 
1367 
[368 
[369 
1370 
1371 
1372 
'373 
'374 
'375 
'376 
"377 
1378 

'379 
[3S0 
.381 
[382 

'383 
(384 


Synonyms. 

h.  3889  =  B.  1340  

h.  3891  =  M.  2677  

B.  1464  +  1465  =  A.  38   

h.  3928  A.  and  B 

  A.  andC. 

B. 1475  ;  A.  39   

h.  3931  =  B.  1473  

A.  40  =  B.  1500 -|-  1501   

B.  1507  ;  A.  41 ;  R.  5  

h.  3941  =  B.  1508  

h.  3945  

B.  1523  "  double"  

B.  1529  4- 1530  =  A. 42   

■y  Volantis   

h.  3949  =  B-  >54*  

h.3958   

B.  1578.  R.6  

h.  3960  =  B.  1576  

B.  1582  +  1583  

h.  3966  

B.  1603  4-  1604   

A.  49  ;  B.  1622   

B.  1631  =  A.  51.    cr  Argus  

B.  1648  =  A.  52.  n  Puppis  

h.  3984=  B.  1661   

h.  3988  =  B.  1673  

B.  1679  4-  1680  ;  A.  53  ;  k  Puppis  .... 


Position 

R  A. 

N  P  D. 

with  Meri- 

-i 

1830.0. 

1830.0. 

dian  from 
N  by  W. 

<D  ^ 
3  3 
~  -° 

Dist. 

alue 
bute 

0 

39 

40 

'7 

265 

12 

3 

43-53 

I 

200 

57 

3 

42.  u 

3 

6 

39 

120 

47 

222 

J3 

2 

4.99 

3 

221 

4° 

2 

5.07 

2 

22 1 

55 
35 

1 

6 

59 

133 

23 

121 

3 

20.16 

1 

120 

-7  8 
—  0 

3 

20.62 

1 

£ 

0 

59 

124 

31 

1S7 

55 

3 

5.76 

1 

t  r  A 
156 

44 

2 

5.09 

2 

t  r  Q 

158 

17 

2 

5-5° 

2 

„  0/: 
2oO 

5° 

2 

37.87 

1 

0  9.  r 

205 

33 

2 

37-27 

1 

5° 

207 

10 

2 

36.56 

2 

7 

1 

T  1  9. 

140 

72 

43 

1 

3-49 

1 

74 

!9 

2 

2.09 

2 

74 

2 

3 

78 

6 

2 

2.06 

2 

7 

1 

132 

4 

40 

4i 

3 

72.46 

1 

146 

41 

5 

2 

73-38 

1 

7 

6 

5 

139 

3° 

2 

38.53 

3 

15 

140 

55 

2 

37-5' 

2 

7 

7 

J45 

223 

44 

3 

7.86 

2 

220 

18 

2 

7.29 

1 

7 

7 

150 

c. 
0 

322 

0 

0 

3 
<r 

0 

309 

58 

1 

1 

0 

3 10 

48 

1 

Si 

3 

0 

7 

9 

"3 

2 

67 

27 

3 

28.20 

3 

36 

67 

43 

2 

28.23 

3 

7 

9 

120 

IS  1 

1 1 

3 

38.03 

2 

IDO 

181 

30 

3 

37-15 

3 

7 

10 

13 

301 

12 

3 

12.82 

3 

301 

10 

3 

12.62 

3 

301 

10 

4 

12.86 

3 

301 

55 

3 

12.96 

3 

7 

12 

120 

30 

75 

20 

3 

4-74 

1 

71 

55 

3 

3.22 

4 

77 

12 

3 

2.79 

4 

7 

16 

141 

53 

281 

35 

3 

31.40 

1 

282 

1 

3 

33.23 

1 

282 

10 

2 

32.11 

4 

7 

16 

142 

0 

15 

57 

2 

10.99 

2 

16 

"5 

3 

9.98 

2 

7 

16 

138 

12 

163 

40 

3 

7.86 

1 

164 

5 

2 

7.71 

1 

138 

163 

57 

3 

9.42 

3 

7 

17 

'3 

157 

57 

3 

22.41 

2 

157 

5 

3 

23.72 

2 

157 

40 

3 

22.35 

4 

7 

J9 

126 

57 

141 

27 

2 

6.59 

1 

140 

33 

3 

7.48 

1 

7 

20 

151 

38 

209 

55 

2 

179.00 

1 

7 

22 

121 

30 

52 

37 

3 

9.10 

2 

53 

3 

3 

8-93 

1 

5° 

34 

3 

10.47 

4 

5i 

4' 

3 

9.04 

5 

5° 

57 

3 

9.99 

4 

7 

*4 

132 

58 

75 

33 

3 

21.77 

1 

74 

32 

3 

23.27 

1 

7 

27 

113 

7 

107 

15 

3 

9.52 

1 

106 

33 

4 

9.46 

4 

106 

37 

3 

9.25 

4 

7 

29 

144 

48 

258 

35 

2 

63-33 

1 

257 

0 

2 

64.67 

4 

138 

258 

45 

1 

64-75 

3 

7 

31 

28 

300 

54 

2 

18.01 

1 

298 

20 

2 

16. 1 5 

3 

7 

32 

Il6 

24 

138 

33 

3 

10.38 

4 

136 

38 

3 

11. 16 

2 

138 

13 

3 

9.69 

4 

Magnitude. 


7  7 

6'  7' 

7  8 

7'=  7' 

7  7' 

9'  9' 

8'  8' 


8 
9 
9' 
7 
7' 
10 
10 
10 
8' 


9 
9 
7 

7  8 
6'  8 
7'=  7 
7  =  7 
6'  8 

7  7 
6'  7 
7  8 


6' 
+ 
5' 
6 

7 
6' 

7 
7' 
7 


7 
10 
10 

6 

7 
6' 


10 


5  =  5 
5  =  5 
5'=  5' 


DOUBLE  STARS. 


253 


Index 

No.  for 
Refe- 
rence. 


1385 
1386 
1387 
1388 
1389 
1390 
1391 
1392 
1393 
J394 
!395 
1396 

J397 
1398 

r399 
1400 
140 1 
1402 
1403 
1404 
1405 
1406 
1407 
1408 
1409 
1410 
141 1 
1412 
1413 
1414 
1415 
1416 
1417 
1418 
1419 
1420 
142 1 
1422 
1423 
1424 
1425 
1426 
1427 
1428 
1429 
1430 
143 1 
1432 
1433 
i+34 
143  5 
1436 

1437 
1438 

H39 
1440 
1441 
1442 
1443 
1444 
1445 
1446 

1447 
1448 
1449 
1450 
1451 
1452 
H53 
1454 
H55 


Synonyms. 


h.  3994  =  B.  1702  A  B 

AC. 

h.  3997  =B.  1731  

B.  1740+  1741  =  A.  55   

h.  4005  =  B.  1762  

B.  1753  +  '754   

h.  4018  AB 

A  C. 

h.  4024  

h.  4027  

h.  4028  =  B.  1848  

h.  403 1  

h.  4032  =  B.  185 1  

h.4038  =B.  1872  

B.  1875  =  A.  60  

h.  4046  =  B.  1887  

B.  1903  4-  1906  =  A.  62   

B.  1914;  A.  63  

7  Argus.     B.  1916,  7,  8  ;  A.  64,5  (A  B) 

  (AC) 

  (B  C) 

h-4°SS  

h.  4057  =  B.  1929  

h.  4060  

B.  1940;  R.  7  ;  A.  66    (e  Volantis) .  .  . . 

B.  1941  -|-  1942  =  A.  67  

h.  4069  =  B.  1948  

B.  1974  "  double."  

h.  4087  

B.  2018  -j-  2022  4-  2023.  (A  B) 

 B  C. 

A.  70  : —  B.  2054  

h.  4104  =  B.  2056.  (A  B)   

  (AC) 

h.  4126  —  B. 2143  


R  A. 
1830.0. 


7  35 


N  P  D. 

1830.0. 


Position 
with  Meri- 
dian from 
N.  by  W. 


138  40 


7 

39 

163 

53 

7 

40 

140 

2 

7 

41 

146 

18 

7 

41 

131 

4 

7 

49 

149 

11 

7 

53 

119 

3 

7 

54 

150 

21 

7 

54 

139 

3i 

7 

56 

150 

24 

7 

56 

136 

5° 

7 

57 

130 

5° 

7 

57 

144 

3 

7 

59 

123 

5 

8 

2 

152 

21 

8 

4 

132 

8 

8 

4 

136 

5° 

8 

6 

•59 

23 

8 

7 

132 

29 

8 

7 

125 

56 

8 

7 

158 

7 

8 

8 

125 

49 

8 

9 

i35 

'9 

8 

13 

134 

30 

8 

16 

130 

27 

8 

20 

160 

58 

8 

24 

134 

10 

8 

24 

137 

21 

8  35 


142  29 


»7  7 
16  52 

'7  45 

216  19 

217  42 
101  46 

99  5° 
132  47 

*33  3 
220  23 

219  38 
176  52 

176  50 

325  35 
321  52 
258  45 
78  50 
82  41 

114  59 

115  28 

46  35 

47  13 
360  57 

357  57 
351  52 
351  2 

344  9 
346  40 
161  23 
159  28 
88  33 
88  25 
264  26 
264  30 
80  26 
80  38 

220  43 
219  38 
152  10 
151  9 
in  48 

8  27 
10  31 

297  45 
297  52 

177  2 
21  21 
24  1 1 

175  1 

175  27 
258  57 

254  33 
147  16 
146  20 
146  15 

146  37 

147  30 

55  2 
28  45 

349  42 

35°  5* 

349  2  3 

351  27 

242  41 

241  25 

242  45 
39  58 
39  49 

31  12 
30  34 

32  38 


14.91 
11.74 
14.07 
17.31 
20.62 
1.92 
1. 71 
50.64 
51.24 
39.31 
36.66 
48.21 
50.06 

6.06 
60.38 
10.75 
10.58 
9.13 
9.70 
17.89 
16.84 
6.01 
6.56 
31.85 
29.69 
29.50 
28.71 
40.78 
40.30 
22.84 
21.74 
88.12 
87.83 
5.76 
6.14 
41.19 
41.12 

62.40 

6.64 
6.88 
23.89 
23.68 
21.59 
7.67 
6.20 
68.86 
66.51 
33.25 
33.24 
5.66 
5.76 
4-33 


64.97 
34.16 

6.73 
4.27 
6.01 
4.48 
4-39 
4-33 
21.10 
19.03 
16.49 
14.92 
16.73 


as  t3 

S  3  [Magnitude, 


6'  10 

7'  10' 

7  n 

6'  11 

7  11 


r 

6' 
6 
6 
7 
7 
8 

7' 
7' 


7  =  7 


X  9 

7  9 

6'  10 

7  8' 


8+ 
9 
9' 
9 

10 

10 

10 

i 

6 


Date  of 
Observa- 
tion. 
1800+ 


3 


T 


254 


MICROMETRICAL  MEASURES  OF 


Index 
No.  for 
Refe- 
rence. 


I456 

1457 
1458 

H59 
1460 
146 1 

1462 
1463 
1464 
1465 
1466 
1467 
1468 
1469 
1470 
H7I 
1472 
1473 
1474 
H75 
1476 

1477 
1478 

H79 
1480 
148 1 
1482 
1483 
1484 
14S5 
i486 
1487 
1488 
1489 
1490 
149 1 
1492 

1493 
1494 

1495 
1496 

1497 
1498 
1499 
1500 
1501 
1502 
1503 
1504 
1505 
1506 
1507 
1508 
1509 
1510 
1511 
1512 

i5j3 
1514 

'5*5 
1516 

1517 
1518 
1519 
1520 
1521 
1522 
1523 
1524 


Synomms. 


h.  4128  =  B.  2153 
h.  4130  =  B.  2159 
B.2168  +  2169  . . 


h.  4133  =  B.  2179  =  d  Velorum 
B.  2206  "  double  ;"  R.  9  ;  (A  B) 


 4(A+B),C. 

  i  (A  +  B),  D. 

S.585  

B.  2283  +  2286.       A.  73?  


B.  2293  4-  2294.    A.  74  b'  Carina  . 

h.  4165  =  B. 2320  

h.  4172   

h.  4188  =  B.  2387  

B.  2452  ;  R.  10   

B.  294:  ;  l,  Octantis  

B.  2505  4-  2507  =  A.  76  

B.  2511  4-  2512.     A.  77  

B.  2515=  £Antliae.  A.  78... 

h. 4220  =  B.  2546  

B.  25444- 2547.  A.  79  ? ... . 

B.  2647.  A.  80  

h.  4249   

B.  2682  =  v  Argus  

h.  4252  

B.  2723.  A.  81  

h.  4272  =  A.  82  ?  

B.  2796  4-  2800.  A.  83  

h.  4282  

h.  4283  —  B.  2824  


R  A. 
1830.0. 

N  P  D. 
1830.0. 

Position 
vitli  Meri- 
dian from 
N.  by  W. 

Value  attri- 
buted. 

8 

36 

149  43 

218 

6 

1 

223 

53 

2 

8 

37 

146  57 

230 

5 

I 

222 

15 

I 

8 

38 

142  30 

309 

31 

3 

3  IO 

8 

3 

8 

38 

132  2 

60 

5i 

3 

8 

41 

148  6 

I  IO 

43 

1 

112 

49 

3 

108 

9 

3 

IO9 

36 

4 

IO9 

5^ 

2 

354 

15 

1 

217 

5 

1 

8 

47 

107  36 

H5 

29 

3 

8 

51 

144  53 

356 

0 

3 

357 

9 

3 

356  13 

3 

8 

53 

14.8  74 

73 

44 

3 

75 

35 

3 

75 

32 

2 

75 

26 

3 

8 

56 

141   1 1 

T  J 

88 

27 

3 

87  30 

1 

8 

59 

1 14-  4> 

216 

16 

2 

216 

49 

3 

9 

6 

1-32    C  C 

286  38 

3 

287 

14 

3 

9 

16 

T  CO  C 

18 

55 

2. 

17 

54 

3 

9 

20 

174  <;8 

108 

30 

1 

117 

59 

1 

9 

22 

134  45 

97 

51 

3 

9 

23 

1 1 1  a8 

257 

48 

2 

9 

23 

121  10 

210 

3 

3 

210 

45 

3 

212 

8 

2 

210 

6 

3 

9 

28 

138  15 

202 

25 

3 

201 

24 

3 

202 

20 

2 

9 

28 

1^8  CO 

30 

40 

3 

30 

30 

2 

31 

25 

3 

9 

39 

J  TJ 

67 

0 

3 

69  19 

3 

69 

r3 

3 

9 

42 

I2J.  Id. 

126 

37 

2 

125 

32 

3 

123 

48 

3 

9 

43 

154  17 

123 

31 

2 

126 

H 

3 

127 

40 

3 

9 

43 

154  18 

303 

28 

2 

300 

35 

3 

9 

48 

134  29 

240 

18 

3 

237 

52 

2 

238 

48 

3 

9 

51 

175  *3 

267 

21 

3 

267  58 

3 

267  49 

3 

56 

265  43 

3 

9 

144  10 

222 

55 

3 

222 

10 

1 

9 

57 

141  15 

204 

0 

2 

205  38 

3 

9 

58 

140  58 

181 

28 

2 

180 

34 

3 

Dist. 


2.92 

2.31 
4± 

3± 
76.57 
77-51 

nisi 
64.79 
47.20 

4.67 

4-59 
5.10 
4.92 


68.95 
66.64 
66.60 
66.27 
42.62 
38.80 
40.63 
40.39 
1.41 

it 
7.8, 
7.22 
2.43 
3.40 
11. 18 
1 1.62 

1.71 
59-57 
108.47 
8.91 
8.12 

7-97 
2.03 

3-  23 
3.23 

128.75 
130.26 
132.12 
18.48 
19.05 
17.27 
3.8, 
6.21 

4-  55 
6.29 

4-77 

4-  57 
13.46 
12.74 

6.18 
6.53 

5-  13 
16.32 
16.05 
17.46 
15.17 

1 10.33 
108.68 
71.56 
70.15 
7.23 
7-33 


11 
10 

7 
7' 
7 
7 
7 
7 


5'  7 

6  8 

6'  8 

9  10 

8'  9' 

6  7 


7  » 
6'  7 
6'  8 
7'  7' 
7  =  7 
7  7 
7'=  7' 


3  9 

I  7 
3  9 

9  9 
ic=io 
6  9' 
6  10 

6  11 

7  7 
7'  =  7' 
7  7 


DOUBLE  STARS 


255 


Index 
No.  for 
Refe- 
rence. 


!525 
I  526 
1527 
1528 
1529 
1530 
1531 
1532 
!533 
1534 
1535 
1536 

1537 
1538 

1539 
1540 
1541 
1542 
J543 
J544 
J545 
1546 

1547 
1548 

1549 
1550 

i55i 
1552 

1553 
1554 
1555 
1556 

J557 
1558 

»559 
1560 
1561 
1562 
1563 
1564 

J565 
1566 
1567 
1568 
1569 
1570 
1571 

1572 
1573 
1574 

r575 
1576 

1577 
1578 

J579 


1580 
1581 
1582 
1583 
1584 
1585 
1586 
1587 
1588 
1589 
1590 


Synonyms. 


h.  4289  

h.  4306  =  B.  2955  . 


B.  2972  =  T  Velorum  =  R.  13 ;  . .  A  B 

Do.  A  C 

h-4323  

B-  3°47  +  3048  =  A.  86  

°-4327  

B-  3°SS  +  3°57-  A.  87  

A.  88  =  S.  Velorum  


h.  4329  =  B.  3062  =  Y  Velorum  .... 
h.  4330  =  B.  3069  =  t  Velorum  

h-4332  

A.  89   

B.  3086  "double."  =  A.  91  

B.  3103  +  3104.  A.  93  

B.  3127  =  A.  94  

B.  3 125  =  A.  95  =  X  Velorum   

h-4346  

B.  3 18 1  "  double."  

h-4356  

h-4359  

B.  3194  "  double."  

h.  4360.    Triple   AB 

c(A±_B)=B.3.,o  

h-4364  

B.  3203=  A.  99.  A  B. 

A  C. 
B  C. 

h-4374  

h.  4378  =  B.  3252  

B.  3274+3276;  A.  IC2  ;    AB. 

Ditto  A.  103  ;    AC. 

h-4383   •  

h.  4393  =  B.  3314  

h.  4409  =  B.  3400  

h.  4423  =  B.  3501  


R  A. 
1830.0. 

N  P  D. 
1830.0. 

Position 
with  Meri- 
dian from 
N.  by  \V. 

Value  attri- 
buted. 

Dist. 

Value  attri- 
buted. 

Magnitude. 

Date  of 
Observa- 
tion. 
1800-)- 

IO 

3 

J53  46 

59 

44 

3 

9.78 

I 

10 

10 

37.151 

61 

38 

2 

13.82 

I 

11  = 

1 1 

37-375 

10 

13 

r53 

49 

141 

40 

1 

I* 

O 

7  = 

:  7 

36.175 

139 

39 

2 

1.60 

I 

7 

7 

36.178 

138 

J9 

3 

1.26 

3 

37-I51 

10 

15 

'45 

1 1 

102 

40 

2 

7-37 

2 

5' 

10 

35.120 

103 

54 

4 

6.82 

3 

5 

10 

37-375 

192 

0 

1 

37-15 

1 

35.120 

191 

10 

3 

36.28 

1 

*•;• 

10 

36.178 

10 

23 

'51 

43 

219 

9 

3 

21.78 

4 

8' 

8' 

37.099 

220 

8 

3 

22.98 

3 

8 

8' 

37.214 

10 

24 

131 

2 1 

29I 

5° 

3 

82.71 

2 

7 

8 

38.090 

10 

24 

H3 

38 

352 

15 

2 

JI3-73 

1 

8 

8 

37.099 

10 

25 

150 

29 

331 

40 

2 

85.03 

1 

7' 

i 

35.249 

33° 

15 

1 

82.76 

2 

6' 

7 

37.446 

10 

25 

'34 

12 

37 

29 

3 

12.65 

2 

6 

6 

36.003 

38 

6 

3 

14.46 

1 

7 

7 

36-r59 

38 

22 

3 

H-75 

2 

6' 

6' 

37.162 

37 

18 

2 

37-375 

10 

25 

142 

51 

17 

5 

3 

!7-59 

3 

5' 

9 

37.077 

17 

46 

3 

17.48 

3 

6 

9' 

37.162 

10 

26 

130 

8 

165 

47 

3 

40.65 

1 

6 

9 

36.159 

164 

4 

3 

40.66 

3 

6 

9 

37.214 

10 

26 

130 

c 
0 

165 

17 

3 

25-93 

1 

7 

10 

36-i59 

26 

164 

24 

3 

26.84 

1 

8 

10 

37.214 

10 

\  A  A 

■20 

30 

36 

3 

26.19 

2 

7' 

8' 

37.099 

30 

29 

2 

26.68 

2 

6 

6' 

37.162 

31 

5 

3 

26.38 

3 

•  • 

37.214 

10 

28 

w  C  - 

IOI 

14 

<;8 

A  A. 
TT 

■i 
j 

8.75 

2 

g 

8 

35.183 

59 

42 

3 

10.64 

3 

8' 

9 

37-183 

58 

52 

2 

10.82 

1 

9 

9  + 
8' 

38.090 

10 

29 

'53 

J5 

37 

43 

2 

25.32 

1 

8 

35.118 

37 

40 

3 

26.93 

2 

8 

9 

37.408 

10 

32 

148 

18 

20 

38 

3 

J5-74 

2 

6 

9' 

36.175 

22 

12 

3 

3 

5' 

10 

■3  7.1  C3 

10 

33 

144 

43 

105 

9 

3 

51.85 

2 

6 

8 

38.088 

10 

35 

150 

8 

82 

0 

1 

26.63 

1 

8 

9 

37-145 

80 

42 

2 

26.29 

1 

8' 

1 1 

37.408 

10 

37 

150 

17 

173 

40 

3 

12.84 

2 

7 

1 1 

37.1  IO 

173 

41 

3 

J3-34 

3 

7 

9 

37-H5 

172 

57 

3 

12.54 

2 

7' 

9 

37-153 

J73 

58 

2 

13.22 

2 

7 

9' 

37.381 

10 

37 

148 

39 

H7 

56 

3 

3.00 

1 

8 

10 

36.323 

10 

37 

149 

12 

234 

47 

2 

0 

8 

11 

37-3 

10 

38 

148 

5i 

214 

1 

3 

17.14 

1 

8' 

9' 

36.164 

214 

59 

3 

l  S.O5 

3 

8' 

9 

37-225 

10 

38 

148 

4i 

119 

13 

2 

3-43 

1 

a 

A+B 

=  8 

35.118 

•'•9 

=9 

36.323 

115 

13 

2 

2.38 

1 

9 

9 

1 14 

2 

0.82 

1 
2 

9 

9 

37.225 

109 

1 

8 

8 

35.118 

59 

14.29 

108 

16 

4 

13.16 

2 

8 

8 

36.315 

38 

108 

23 

3 

14.19 

2 

8 

8 

37.225 

10 

148 

28 

350 

45 

2 

8 

10 

36-3i5 

353 

56 

2 

O.D9 

3 

8 

9' 

37-225 

10 

39 

159  58 

75 

22 

3 

63.92 

1 

7 

7 

37-H5 

40 

1? 

7 

9 

do 

148 

285 

35 

2 

7 

9 

do 

10 

42 

33 

"5 

15 

1 

IO.I4 

0 

8 

10' 

36-3r5 

10 

45 

149 

3 

344 

27 

3 

30.89 

1 

7' 

10 

36.164 

10 

47 

147 

57 

'3 

0 

1 

65.28 

1 

4' 

8 

37-H5 

200 

10 

1 

i63± 

0 

4 

7 

37-H5 

10 

48 

r59 

5° 

285 

5° 

1 

1.42 

0 

7 

8' 

37.183 

10 

5i 

158 

8 

131 

0 

3 

7.10 

1 

7' 

10 

35.312 

10 

59 

131 

43 

276 

38 

2 

1.15 

6 

9 

37-153 

279 

23 

1.89 

1 

5' 

11 

37-444 

1 1 

9 

r34 

57 

270 

42 

2 

1.37 

3 

7- 

:  7' 

35.120 

265 

37 

2 

1. 15 

2 

7' 

7' 

37.183 

273 

1 1 

1 

6' 

7 

37-444 

256  MICROMETRICAL  MEASURES  OF 


I  ndex 
No.  for 
Refe- 
rence. 


Synonyms. 


1591 

1592 
1593 
!594 
1595 
1596 

J597 
1598 

!599 
1600 
1601 
1602 
1603 
1604 
1605 
1606 
1607 
1608 
1609 
1610 
161 1 
1612 
1613 
1614 
1615 
1616 
1617 
1618 
1619 
1620 
1621 
1622 
1623 
1624 
1625 
1626 
1627 
1628 
1629 
1630 
1631 
1632 
1633 
1634 
1635 
1636 
1637 
1638 
1639 
1640 
1641 
1642 
1643 
1644 
1645 
1646 
1647 
1648 
1649 
1650 
1651 
1652 
1653 
1654 
1655 
1656 
1657 
1658 
1659 


h.  4432  =  B.  3562  

B.  3574  "  double."   

B-  3594- +  359S  

17  Hydra.  H.  III.  96  . 
h-  4455  =  B.  3670  

B.  3706  "  double."   

h.  4478  =  /3.  Hydrse  Crater 


B.  3828  "double." 
B.  3836.       A.  116 


h.  4486  =  t .  Cfiamtpleontis 


h.4487  

B. 3904  +  3905  ;  A.  117 ; 


Ditto, 

h.  4495  =  B.  3918. 

h.  4522  

a  Cruris  =  A.  123. 


A  B. 
AC. 


AB. 


a.  Crucis  (A  C.)    A.  122 


R  A. 
830.0. 


I  24 
I  28 


I  32 
I  44 


II  47 

II  48 

II  5I 

1 1  52 

1 1  56 


11  57 

12  16 
12  17 


a.  415  =  c  Corvi 

h.  4539  =  y  Centauri. 


12  21 
12  32 


12  32 


N  P  D. 
1830.0. 


154  2 
150  43 
»31  44 

Il8  20 
122  38 


152  32 
122  58 


151  38 

121  19 

167  16 

I25  48 

151  3 


122  O 
I58  32 
IS2  9 


io5  34 
138  1 


102  5 


Position 
with  .Meri- 
dian from 
N.  by  W. 


Dist. 


287  3 
290  42 

296  10 

297  33 
167  20 

166  5 

167  o 

3°  13 
245  18 

244  45 
244  27 
275  42 

337  41 

338  50 
340  44 

337  53 

338  30 
342  24 
342  15 
265  48 

82  55 

83  17 
178  38 
178  o 
124  45 
150  10 
150  48 

19  40 
19  58 
315  21 
312  21 

65  34 
68  50 
122  57 

120  56 

121  1 

"9  55 

120  57 

121  42 

122  27 

119  38 

120  5 

121  13 

119  48 

122  19 

120  20 

119  19 

120  47 
120  3 
120  4 

34 
3° 
5 
3 

201  44 
198  2 
213  o 

354  5° 

360  20 
351  21 

346  47 
349  37 

355  20 

361  58 
355  25 

347  27 
3fii  55 
122  8 
122  26 


201 
201 
202 
202 


2.46 
2.32 
6.18 
6.58 
13.19 

12.43 
8.92 
4.25 
3.84 

25-97 
1.98 
1.71 
1.87 
2.50 
2.86 
1.78 
1.86 

17-73 
21.84 
20.06 
1.73 
1.51 
5.65 
23.68 
23.29 
26.96 
25.60 
7.10 
7.08 
13.12 
13.70 


5.26 
5-34 
5-53 

6.44 
5.70 

5-57 
6.3 1 
4.96 


5-83 
5.27 
6.62 
5.30 
92.89 
91.99 

89.60 
90.09 

23-44 
Z  1" 


1 

7.20 
7-57 


Magnitude. 


8  9 

8  9 

6  8 

6  8 

6  8 
6  =  6 

6  8' 


6' 
6 
/ 
4 
5 
5 
4 
5' 
5 
4 


4 
6 

5' 
4' 
6 

s 

5 

8  9' 
8  8 


6 

7 
10 


10 
1 1 

10 
10 
9 
9 


1'  6 
7**7 
3'  10 


7  7 
6'  6' 


DOUBLE  STARS.  257 


Index 
No.  for 
Refe- 
rence. 


Synonyms. 


R  A. 
1S30.0. 


NPD. 
1830.0. 


Position 
with  Meri 
dian  from 
N  by  W. 


Dist. 


Magnitude 


1660 
1661 
1662 
1663 
1664 
1665 
1666 
1667 

1668 
1669 
1670 
1671 
1672 
1673 
1674. 

1675 
1676 
1677 
1678 
1679 
1680 
1681 
1682 

1683 
1684 
1685 
1686 
1687 
1688 
1689 
1690 
1691 
1692 
1693 
1694 
1695 
1696 
1697 
1698 
1699 
1700 
1701 
1702 
1703 
1704 
1705 
1706 
1707 
1708 
1709 
1710 
1711 
1712 
1713 
1714 
1715 
1716 
1717 
1718 
1719 
1720 
1721 
1722 
1723 
1724 


(y  Virginis) . 


12  33 


90  31 


h-4556  

t.4SS8  

B.  4268  +  4271.      A.  127   , 

h-4S63  

A.  128  =  £2  Centauri  , 

B.  4323  =  11. 16;  A.  129  ;  9  Muscce  . 

B.  4367 -f  4369.    A.  131.    tj  Muscce  . 


h.  4580  =  B.  443 1  

h.  4586  —  B.  4460  

B.  4494 ;  R.  17  

A.  1552=  A.  138.  i.Hydrce  

B.  4582  ;  Q  Centauri;  A.  141  

B-4597  +  4598-    A.  J42  

h.  4607  

B.  4629  +  4630.       A.  143  

A.  144  

B.  4655  +  4656  ;  R.  18  ;  (N.  Centauri.) 


12  45 

12  47 

12  50 

12  52 

12  57 

12  57 

'3  4 


13  13 

13  16 

13  21 

13  27 


117  2 

119  13 

144  59 
122  42 
139  o 
154  24 

156  S8 


137  40 

156  59 

152  10 

115  37 


13  31 

143  42 

J3  32 

148  22 

13  32 

161  8 

13  37 

151  14 

J3  39 

136  31 

13  41 

141  58 

48  17 

48  20 

37  22 
39  45 
44  22 

38  33 

4i  59 
46  11 


46  53 
44  4° 
23  8 

34  16 
34  11 
32  24 

3i  27 


19  50 

21  57 

20  40 
17  56 
23  35 

22  55 

13  4° 

23  48 


237  28 
220  55 

80  20 

78  55 

81  25 

i79  5 
177  3° 
126  20 
126  o 
236  48 
236  45 
100  52 

99  59 
188  35 
188  24 

185  23 

186  33 
332  50 

331  53 

332  28 
331  17 

333  23 
10  15 

151  30 
147  18 
357  17 
359  5 
192  21 

190  13 

191  5° 
165  6 

ifi3  15 
90  10 
90  43 
76  18 
76  15 

35  3° 

36  4 
255  38 
257  14 
288  40 
280  6 


Contact 


1.51 


0.5 


0.67 

7-77 
6.76 
6.91 
25.40 
21.78 
16.35 
16.71 
6.33 
6.77 
26.48 

25-55 
5.12 

5-75 
6.12 

5-77 
58.32 

57-75 
60.99 
59.91 
61.83 
0.5 
3.67 

17.26 
16.30 
10.24 
9.86 

9-95 
5.23 
5.69 
30.99 
33.89 
11. 16 
11.83 
14.78 
12.22 

7-94 
9.69 
18.15 
18.48 


7,  9 
6'  10 


3 


u 


258 


MICROMETRICAL  MEASURES  OF 


Index 
Nil  for 
Refe- 
rence. 

Synonyms. 

R  A. 
1830.0. 

N  P  D. 
1880.0. 

Position 
with  Meri- 
dian from 

N  by  W. 

Value  attri- 
buted. 

Dist. 

Value  attri- 
buted. 

Magnitude. 

Date  of 
Observa- 
tion. 
1 800  — f— 

1725 

A.  145   

13 

42 

156  8 

50  21 

3 

23.06 

I 

7' 

8' 

36.567 

1726 

5i  3° 

3 

24.44 

4 

8 

9 

37-277 

1727 

49  J5 

3 

25-75 

3 

8 

9, 

37-37° 

1728 

B.  4662.    A.  148.    k.  Centauri  

13 

42 

122  8 

114  41 

2 

7.83 

1 

6 

7 

35-345 

1729 

in  59 

3 

IO.03 

1 

5' 

7' 

36.159 

1730 

in  2 

3 

8.40 

1 

36.162 

1731 

113  4 

3 

9.25 

4 

36.493 

1732 

113  30 

3 

8.32 

3 

6 

8 

38.110 

1733 

B.4669  "double.''  Asc.  1580.  h.  Centauri 

13 

43 

121  5 

185  20 

2 

13.14 

2 

5 

10' 

37-457 

1734 

185  53 

2 

14.39 

2 

5' 

10 

37.482 

1735 

13 

46 

145  12 

310  35 

2 

12.40 

1 

7 

8' 

35-345 

1736 

309  9 

3 

IO.64 

1 

7' 

9 

35-427 

1737 

310  32 

2 

1 1.40 

2 

7' 

9 

36.233 

1738 

13 

55 

125  43 

131  20 

3 

22.70 

1 

8 

9 

36.386 

J739 

130  45 

2 

20.61 

2 

8' 

9 

37-444 

1740 

r3 

56 

142  52 

27  42 

2 

24.00 

2 

7' 

8 

36.493 

1741 

27  51 

3 

24.85 

3 

8 

8 

37.370 

1742 

!3 

58 

140  42 

J33  56 

3 

62.17 

3 

6 

9 

36.567 

1743 

134  10 

2 

63.91 

2 

6 

I 

37.446 

J744 

14 

3 

92  31 

26  54 

3 

7-93 

3 

8'  = 

=  8' 

37-479 

1745 

«4 

9 

169  19 

128  44 

2 

6.27 

1 

8' 

9 

36.238 

1746 

126  3 

2 

5.6, 

2 

8' 

9 

37.446 

1747 

B.  4g64  +  4865  ;  R.  19  ;  A.  159  

'4 

11 

147  40 

164  21 

3 

10.04 

2 

6 

8 

36-233 

1748 

161  47 

3 

9.40 

3 

6' 

9 

36.610 

1749 

96  59 

163  40 

2 

9.56 

2 

6 

8 

37.446 

1750 

2-  1833  

14 

14 

163  59 

3 

6.25 

3 

7'= 

=  7' 

37-479 

1751 

2.1837   

14 

16 

100  49 

321  33 

2 

0 

7' 

9 

37.482 

1752 

14 

25 

125  49 

81  5 

1 

2.46 

1 

10= 

10 

36-377 

1753 

83  32 

3 

2.03 

2 

2/ 

9 

37.649 

1754 

H 

27 

J44  57 

270  5 

1 

9.56 

1 

8' 

9 

37.140 

1755 

269  2 

1 

1 1.06 

1 

9 

10 

37.446 

1756 

28 

150  8 

217  20 

17.83 

2 

34-331 

3 

1757 

B.  4990+4991.    A.  165  

218  27 

3 

17-59 

2 

1 

2' 

34-435 

1758 

219  7 

3 

17.41 

3 

34.468 

'759 

219  10 

2 

35.052 

1760 

218  26 

4 

17.33 

2 

I 

2 

35.107 

176 1 

218  53 

4 

17.02 

2 

1 

2' 

35.186 

1762 

218  36 

3 

35.271 

1763 

220  43 

4 

1 

2 

35-37° 

1764 

218  S3 

3 

1 

2' 

35-353 

1765 

219  17 

2 

1 

2' 

36.145 

1766 

218  58 

3 

1 

1' 

36.162 

1767 

217  51 

3 

1 

1' 

36.178 

1768 

219  43 

3 

2 

36.244 

1769 

221  31 

2 

36.258 

1770 

220  28 

2 

36.285 

1771 

220  36 

2 



36.394 

1772 

220  16 

3 

16.76 

4 

36.610 

1773 

219  38 

2 

15.71 

2 

37-153 

1774 

219  53 

2 

16.28 

4 

2 

37.183 

1775 

221  36 

3 

16.81 

3 

37.266 

1776 

221  29 

3 

16.77 

3 

2 

37.277 

1777 

220  32 

3 

15.44 

4 

38.082 

1778 

220  10 

2 

15-57 

3 

38.107 

1779 

*»■  5444  

221  55 

2 

15.09 

2 

38.110 

1780 

H 

29 

144  12 

70  8 

2 

20.23 

2 

9 

10' 

37-389 

1781 

A.  1655;  B.  4995;  A.  166  (0  Circini) 

H 

29 

154  14 

245  23 

2 

15.62 

1 

4 

10 

36.192 

1782 

242  59 

3 

15-55 

4 

4 

9 

36.567 

1783 

243  56 

3 

15.50 

3 

3' 

10 

37-277 

1784 

243  40 

3 

15.99 

4 

9 

38.107 

1785 

31 

144  27 

203  13 

2 

7.09 

1 

9  = 

=  9 

36.386 

1786 

203  24 

3 

6.93 

3 

8 

8' 

37.381 

1787 

205  15 

3 

6.16 

2 

7' 

8 

37-389 

1788 

14 

36 

114  43 

*33  38 

3 

8.94 

3 

6 

8 

34-3°7 

1789 

r35  4 

3 

9-35 

4 

5' 

8 

34.465 

1790 

J33  54 

3 

9.23 

4 

6 

9 

37-334 

1791 

14 

40 

136  42 

217  35 

2 

6.86 

2 

7' 

10 

36.490 

1792 

217  18 

3 

7.27 

4 

7' 

10 

37.329 

DOUBLE  STARS. 


259 


Index 
No.  for 
Refe- 
rence 


J793 
J794 
J795 
1796 
1797 
1798 

'799 

1800 

1801 

1802 

1803 

1804. 

1805 

1806 

1807 

1808 

1809 

1810 

1811 

1812 

18 1 3 

1814 

1815 

1816 

1817 

1818 

1819 

1820 

1821 

1822 

1823 

1824 

1825 

1826 

1827 

1828 

1829 

1830 

1831 

1832 

J833 
1834 
1835 
1836 
1837 
1838 
1839 
1840 


1843 
1844 
1845 
1846 
1847 
1848 
1849 
1850 
1851 
1852 
1853 
1854 
1855 
1856 
1857 
1858 
1859 
i860 


Synonyms. 
h.4707.    B.  5071  

B.  5089.       A.  171  

h.  4712   

h.  4715  =  B.  5 1 12  

A.  1690.  H.  145,  28  . 
h.  4728  (tt  Lupi)   


k  Lupi  =  A.  177  

B.  5223  =  A.  179   

h.  4753  =  fi'  Lupi  

{pf  +  ju2)  Lupi  =  A.  180  

h.  4757  =  y  Circini  

£  Lupi  =  A.  182  

A.  183?  B.  5313  AB 

 AC. 

h.  4766  

h.477l  



h.  4776  =  B.  5351  

h.  4777  =B.  5355   

A. 186   

^4784  

h.4783  

S.  673  


Position 

'u 

•g 

Date  of 

R  A. 

NPD. 

with  Men 

■  «T3 

Observa- 

1830.0. 

1830.0. 

dian  from 

oi  £ 

Dist. 

Magnitude 

tion. 

N  by  W. 

1 800  4- 

IA  AO 
't  t 

'33  t 

230  7 

I 

1 ,  CO 

O 

8  =  8 

j  /  j  y 

223  18 

J 

1.68 

I 

8  8' 

'T.7.4.5'2 

222  45 

I 

1.33 

O 

8  8' 

37.482 

228  18 

I 

1.32 

I 

8  8 

37.649 

14  42 

1^5  0 

224  5 

3 

16.39 

2 

7  IO 

37.329 

224  24 

3 

17.22 

2 

7  10' 

37.452 

IA  A3 
XT  Ti 

T  /I  A     A  A 

*tt  tt 

226  50 

2 

8  8' 

7  5.24.Q 

J  J  T7 

6.27 

227  35 

3 

I 

8  8' 

35-427 

14.  AC 

T  TJ 

137  II 

277  2 

3 

2.64 

3 

7  8 

35.l8l 

277  59 

3 

2.98 

2 

6'  7 

35.364 

278  32 

•5 
j 

1.^8 

4. 

T 

6'  7 

37.120 
J  /    J  J 

*t  t° 

I IO  38 

278  55 

2 

I 

c'  7 

X  5.4.52 

J  J  TJ  ~ 

276  20 

3 

12.26 

4 

6  9 

37.460 

IA  CA 

1  jt 

I  -7  6    2  1 

III  55 

1 

0.67 

■2 
j 

5=5 

35.l8l 

109  24 

2 

1. 01 

1 

j  j 

1  5-"!OI 
jj  j 

1 14  4 

A 

T 

0.72 

1 

5  =  5 

j  5 

%  5.-? 64. 

J  J    J  T 

115  35 

2 

35.424 

1 10  13 

I 

35.564 

109  45 

2 

0.67 

0 

6  =  6 

36.I78 

108  46 

■3 

0.67 

0 

6  =  6 

j  /  j  y 

108  30 

•2 
J 

0.67 

0 

•37. -7  -3.4. 
J  /    J  JT 

15  0 

138  5 

144  35 

3 

27.15 

4 

5  6 
4'  6 

36.500 

j    j  y 

145  20 

2 

27.2  c 

2 

37.444 

143  4 

•3 
j 

27.27 

•5 
j 

5'  7 

7'  Q 

/  " 

J  /  jj/ 

I  c  3 

132  A3 

46  4 

•3 
j 

I  I.  CO 

2 

■36.4.00 

J  T?w 

47  45 

3 

IO.I7 

4 

7  Q 

37444 

I  C  7 

j  / 

137    I  C 

172  39 

2 

5'=  5' 

15.567 

J  J  J  / 

174  5 

■3 
J 

3  5.  580 

172  46 

3 

I.8l 

1 

36.238 

174  16 

4 

2.33 

2 

6'=  6' 

36.4I9 

111  4.5 

■3 
j 

2.00 

•3 
i 

6  7 

•37  -300 

do 

do 

132  O 

2 

5  7 

3  5-58o 

131  34 

2 

22,85 

1 

36.238 

130  10 

2 

22.78 

2 

5  9 

16.4.10 

J     T  J 

131  20 

2 

23.02 

yl 
T 

6  8 

11 .  too 
j  /  -  j^y 

15  10 

148  42 

109  30 

3 

5'  6 

35.370 

109  21 

2 

I 

O 

5'  6 

j 

3  C.A2A 

J  J  *T**T 

102  56 

0 

I 

6  6' 

36.  I92 

107  7  7 

2 

1.80 

6  6' 

J  /•TUU 

IO7  1-5 

2 

O.QO 

2 

«'  6 
j  u 

37. C37 

11  11 

1 3A  A 

I78  40 

1 

27.87 

I 

4  10' 
3  10' 

3  C.l86 

111  4.6 
'  J  Tv 

i 

5  /•iuT 

17  5  4-1 

/  J  T 

j 

2C.8C 

2 

A.  O 

37.a6o 

J  /  T 

174.  Q 

/  t  y 

•3 
3 

26.27 

4. 

T 

1  a 
i  y 

3  7.6AQ 

I  C  IA 
J  *t 

128  6 

208  4  5 

I 

89.48 

I 

5  q' 
j  y 

5  o' 

8  10 

36.380 

45  5"? 

Tj      J  J 

I 

IAA.  CO 

I 

36.380 

J       J  7 

I  C  11 

j  j 

T  -22.    T  C 
J       1  J 

116  43 

•3 
J 

I  3. 1 A 

J  T 

2 

37.36A 

J  1    J  I 

119  48 

■3 
J 

I3.IO 

-7 
j 

8'  10 

37.AC2 

J'  TJ 

1 1  17 

j      *  / 

IA7  Id 

186  55 

jj 

■3 
J 

7.3  3 

I 

8  Q 

8  8' 

36.386 
J  J 

180  0 

2 

6.AQ 

2 

3  7.AC2 

J  /  TJ  ^ 

190  25 

2 

5.29 

2 

8  9 
8  9' 

37-545 

186  40 

2 

5-23 

2 

37.649 

15  17 

140  50 

249  37 

250  35 

2 
I 

12.60 

I 

7  12 

8  12 

36.643 
37-545 

15  19 

I3I  20 

222  57 

3 

5-'7 

7'  9' 

34-435 

225  31 

3 

6.73 

2 

7  IO 

37.446 

15  i9 

146  49 

302  48 

3 

6.23 

I 

7,'  9' 

36.643 

300  40 

3 

6.37 

3 

7  IO 

37-452 

15  20 

147  38 

114  7 

2 

39-25 

3 

8  8 

37-545 

15  22 

137  0 

237  30 

3 

34.28 

1 

7'  IO 

36.386 

238  52 

3 

34.12 

4 

37-537 

15  22 

109  35 

282  30 

2 

10.72 

1 

6  10 

3  5-45  2 

281  17 

4 

1 1.23 

2 

6  10 

37-471 

15  23 

"3  54 

123  57 

3 

7.92 

1 

8  8 

34-3°7 

121  18 

4 

9.04 

4 

7  =  7 

34-3°7 

120  18 

2 

11. 01 

2 

8'=  8' 

36.320 

118  5 

3 

9.86 

1 

8  =  8 

36-337 

118  43 

3 

9.83 

3 

8  8 

37-545 

260 


MICROMETRY CAL  MEASURES  OF 


Index 
Xi>.  for 
Refe- 
rence. 


1861 
1862 
1863 
1864. 
1865 
1866 
1867 
1868 
1869 
1870 
1871 
1872 
1873 
1874 
1875 
1876 
1877 
1878 
1879 
1880 
1881 
1882 
1883 


1886 

1887 

1888 

1889 

1890 

1891 

1892 

1893 

1894 

1895 

1896 

1897 

1898 

1899 

1900 

1901 

1902 

1903 

1904 

1905 

1906 

1907 

1908 

1909 

1910 

191 1 

1912 

i9I3 

19 14. 

1915 

1916 

1917 

1918 

1919 

1920 

1921 

1922 

1923 

1924 

1925 

1926 

1927 

1928 

1929 

1930 

1931 


Synonyms. 


h.  4786  =  y  Lupi 


h.  4788  =  B.  5384.    f.  Lupi  

A.  190  

2.  1962  

b-4796  

B.  5442.    R.  20  

h.  4805  =  B.  5484  

B.  5486  =  A.  193   

h.  4809  A  B. 

 AC. 

B.  5515  "double."    A.  195  

B-  5535  +  5536-    A.  196.    ?  Lupi  

h.  4.821  

B.  5554.  R.  21.    tj  Lupi  

h.  4825  =B.  5559  

2. 1998  =  51  Libra  AB, 


  AC. 

0-.  506  =  (3  Scorpii  

h.4830  

 A.  199 

M837  

h.  4839.   12  Scorpii  

h.4840  

B.  5699  —  A.  200  

h.4845  =  B.  5708  


R  A. 
1880.0. 


15  24 


15  24 


15  26 
15  29 
15  31 


15  32 

15  37 

15  38 

15  39 

15  42 

15  46 

15  48 

15  49 

15  50 

15  55 


15  56 

15  56 

15  58 

16  1 
16  2 
16  6 
16  1 1 
16  12 


N  P  D. 
1830.0. 


13°  35 


134  23 


147  33 
98  13 

148  9 


!54  54 

142  41 
144  32 
150  10 
139  49 

123  28 

121  32 
127  54 

147  17 
100  54 


Position 
with  Meri- 
dian from 
N  by  W. 


109  20 

132  32 
128  39 

133  12 
117  58 
124  23 

133  30 
130  50 


104  30 

95  23 
95  35 
100  34 

97  4 

93  2 
95  0 

91  1 

92  8 

94  43 
91  20 

95  36 

96  6 

97  J3 
90  10 

347  58 
344  3° 
350  48 
350  49 
94  4° 
7  57 
116  18 

116  12 

117  16 

i53  35 
157  18 

155  11 
129  33 
135  10 

22  26 
21  23 
5°  55 

257  2 
11  59 

10  31 

9  3i 
50  2 

48  5 

49  27 
H5  31 
144  39 

21  50 

23  28 
20  53 

251  41 
251  56 
9  3 

7  34 

11  40 

10  56 

1 1  19 

8  39 
11  9 
11  24 
77  12 
25  28 


25 
232 
,85 
185 


76  21 

74  33 
82  17 
80  55 
293  o 
292  41 
198  32 

!97  45 
136  38 
133  22 


Dist. 


3 
4 

0 

do 

0 

2 
I 

0 

0.74 

1 

0.95 

1 

1 

0 

2 
3 

0 

2 
3 

0 

3.06 

1 

2.99 

1 

3-37 

1 

33-n 

35-23 
2.65 
2.26 

2-34 
33.32 
32.70 
23.99 
22.66 

43-47 
49.30 
11.77 
12.84 
12.24 
10.79 
9.70 
11. 71 
17.30 
21.15 

15.12 
14.92 

9.21 
10.58 

1.24 


1.58 


13. 1 1 
13.86 
13.70 
21.21 
46.26 
44.41 

9-73 
10.60 
4.13 
5-59 
5-79 
4-59 
43.50 
42.53 


Magnitude. 


4  =  4 


8  8' 
7  =  7 
7  =  7 
7  =  7 
6  11 
6'  12 
6  10 


=  8 


Date  of 
Observa- 
tion. 
1800+ 


9  =  9 
9,  9 

6  10 

7  10 


10 
10 
10 


34-  435 
34.465 
34.611 
35.120 
35.181 

35-  353 
35-364 
35-424 
35-567 
36.178 
36.386 
37-14° 
37-277 
37.309 

37-334 
35-567 
36.386 
36.490 
37-329 

34-  3°7 
37-545 
36.304 
36.419 
37.326 

35-  3°7 
35-353 
35-364 
36.419 

37-342 
35-367 
37.329 
36.244 
36.244 

35-427 
36.490 
37.326 

34-  3°4 
3  5-424 
37-318 

35-  452 
37-323 
34.285 
34.304 
35-452 
35-427 
37.326 

34348 
3455° 
35-345 
35-364 
35-375 
35400 
35.424 

37-334 
34.348 

35-452 
36.422 
37.476 

34348 
34.304 

37-537 
34-435 
36.416 

34-348 

35364 
36.320 
37.318 
36487 
37-38I 
36.416 

36487 


DOUBLE  STARS.  261 


Index 
No.  for 
Refe- 
rence. 


1932 
1933 
1934 
!935 
1936 
1937 
1938 
1939 
1940 
1941 
1942 

!943 
1944 

J945 
1946 

1947 
1948 
1949 
1950 
1951 
1952 
r953 
*954 
1955 
1956 

!957 
1958 

!959 
i960 
1961 
1962 
1963 
1964 
1965 
1966 
1967 
196S 
1969 
1970 

1971 
1972 

1973 
1974 
J975 
1976 

1977 
1978 
1979 

1980 

1981 
1982 
1983 
1984 
1985 
1986 
1987 


1990 
1991 
1992 
1993 
1994 

J995 
1996 
1997 
1998 
1999 
2000 
2001 


Synonyms. 


R  A. 
1880.0. 


B.  5709  ;  1  Triang  Aus.    A.  201  

h.4848  

h.  4850  

h.  4853  (e  Norma)  

5  Ophiuchi  A  B 

AC 
AD 

B.  5741  "double."    A.  203  ?  

A.  202  ?   

h.  4866  =  B.  5770  

h.4871  =B.  5781  

b-  4873  •  

h.  4876  =  B.  5792  

h.4880  

h.  4883  — :  A. 207   

A.  210  

B.  5841  —  A.  209  

h.4889  

h.  4890  

h.4896  

h.4909  =  B.  5931  

A.  213   

B.  6009  (doubtful)  

36  Ophiuchi  —  Sh.  243  

h.4938  

h.4939  

h.  4947  

h.  4949.    B.  2072  =  L.  1432.    A  B. 

AC.    (=A.  216) 


16  12 

16  13 

16  14 

16  15 

16  15 

16  18 

16  20 

16  26 

16  27 

16  27 

16  28 

16  30 

16  33 

16  34 

16  37 

16  40 

16  41 

16  44 

16  51 

16  58 

17  4 
17  5 

17  8 

17  9 

17  14 

17  14 


N  P  D. 
1830.0. 


Position 
with  Meri- 
dian from 
N.  by  W. 


153  39 
122  48 

119  18 

137  10 

"3  3 

150  30 

131  28 
146  39 

137  26 

139  1 

138  25 

136  3 

132  4 

145  3 

126  34 

127  12 

136  37 
136  34 

140  50 

136  31 

132  8 
116  21 

146  16 
146  17 
171  47 
I3S  4i 


26  41 

27  55 

155  28 
152  51 

156  24 

348  14 

349  20 
347  26 
334  29 
336  52 

334  37 
2  34 

1  42 

2  10 
286  35 
250  5 
247  42 
180  25 

126  32 
123  34 

127  32 

46  55 

47  32 
47  25 

46  45 

47  38 
71  23 
71  38 

73  17 

264  38 

265  25 
151  o 

185  53 
184  56 

!73  53 

148  o 

147  18 
146  10 

148  30 

5  3 

3  25 

6  37 
146  35 
148  58 

26  35 

28  25 

29  22 
284  13 

284  36 
164  36 
167  35 
159  4° 
43  43 
43  34 
45  43 
43  7 
41  25 
109  51 
107  o 
224  25 
224  18 

74  57 

75  59 

266  34 

267  7 

265  59 
267  6 

313  55 
313  23 
313  20 


15  -° 


Dist. 


24.66 

"s'7V 
6.62 

5-55 
7.38 
9.20 
7.29 
24.32 
23.61 
23.80 
4.11 


36-5i 
35.86 
58.48 

3-51 
3.91 
4.11 

26.88 
30.48 
27.18 
27.08 
28.90 
32.01 
31.80 
31.74 
9-34 
9-95 
31.86 
10.63 
1 1.30 

25.96 
28.90 
23.56 
22.18 
7.86 

6.73 
32.14 
30.71 


4-39 
16.55 

S  17.66 
\  15-72 

9-37 
7-94 

2 
5.19 
4.80 

3.66 
5.00 
23.88 
25.25 
29.98 

3J-57 
10.76 
10.38 
3.25 
4.01 
3.26 
2.75 

!°4-57 
102.64 
106.21 


3  x 


Date  of 

Observa- 

Magnitude. 

tion. 

t> 

I  8 OO-j- 

I 

(.1 
0 

12 

36.487 

5' 

1 1 

37-545 

I 

7 

7 

35424 

3 

37.323 

3 

7 

7( 

37.663 

4 

7 

7' 

34-348 

1 

7 

8 

36.320 

4 

O 

7 

37.663 

1 

5' 

8 

35.370 

1 

5 

0 

35-427 

3 

5 

8 

37.460 

4 

0 

6 

c 

D 

0 

8 
8 

34.348 
35-433 
35-433 
3  5-433 

1 

8 

8 

36.389 

1 

7' 

8 

37-381 

1 

6 

1 1 

36.643 

1 

5 

5 

35-37° 

1 

7' 

0 
5 

35-58o 

4 

_/ 
7 

9 

37-334 

1 

7 

9 

34-479 

1 

7 

1 1 

37.381 

2 

7 
7' 

1 1 

37-457 

2 

10' 

37.482 

1 

7' 

10 

37-521 

1 

8 

8 

35-427 

2 

8 

8' 
0 

37-348 

3 

8' 

9 
7' 

37.381 

1 

6 

36.389 

4 

6 

7 

37.381 

2 

8 

1 1 

37-348 

1 

8' 

9 
9' 

35-427 

1 

8' 

37.608 

36.389 

•• 

1 

7' 

8 

36.315 

0 

8 

8' 

36.320 

1 

8 

7' 

8' 

37.646 

■3 
J 

8' 

37.663 

I 

6' 

10' 

35.320 

6' 

10 

35-37° 

I 

6 

9 

35-452 

I 

8  . 

=  8 

36.315 

3 

7' 

7' 

9' 

37-348 

7' 

36.238 

7' 

10 

36.301 

4 

8 

10 

36.487 

1 

00  00  00 

8 

36.386 

1 

2 

9 

36.64.6 

1 

10 

36.301 

1 

7' 

9 

36.646 

0 

7 

1 1 

37-539 

4 

6: 

=  6 

34-3°7 

4 

6 

6 

34-348 

34-55° 

1 

6' 

=  6' 

35-375 

2 

6 

6 

37.608 

1 

8' 

8' 

34.309 

1 

9 

9 

37.482 

2 

8 

9 

34.309 

2 

8' 

10 

37.482 

2 

9 

9' 
9' 

36.487 

1 

9' 

36.556 

1 

6 

7 

35.424 

1 

6' 

7 

36.315 

4 

6 

7 

36.487 

4 

6 

7 

37-38i 

1 

6' 

7 

36-3i5 

2 

6 

T 

36.487 

1 

6 

7 

37.381 

262 


MICROMETRICAL  MEASURES  OF 


Index 

Position 

•~ 

♦|  . 

2  . 

Date  of 

No*  for 

R  A. 

N  PD. 

with  Meri- 

Observa- 

Refe- 

Synonyms. 

1S80.0. 

1830.0. 

dian  from 

Dist. 

Z  | 

Magnitude 

tion. 

rence. 

N.  by  W. 

"3-= 

1800+ 

20O2 

W     h\r\9  f           A  itt 

17 

J7 

*33  49 

I7l  45 

1 3-59 

1 

7,  9 

34-435 

170  16 

3 

14.79 

4 

6  9 

37-453 

200^. 

17 

34 

145 

115  42 

* 

2 

0 

7  11 

35-3^7 

2OO5 

8l  21 

1. 51 

■ 

6  10 

37.663 

2006 

"7 

37 

H3  32 

9  3 

2 

I  Z.Os 

O  II 

34-4^5 

2007 

fi'       T  T 

35.370 

li       «  „  O  ^             T>      £  -  -  — 

17 

3* 

I3X  13 

ou  23 

43.(39 

1 

7,  9 

37-35° 

200 

59  J7 

3 

42.52 

7  10 

37.460 

2010 

\      _  _  _     ,  .      TJ  /'_/'_ 

'7 

47 

120  50 

265  45 

47.64 

1 

0  5 

n(\  1  8£ 

20  I  I 

2 

46.55 

1 

5  7 

37-35° 

2012 

r»      F  f~*r\c\             Tl  hini 

17 

48 

I2D  55 

106  28 

2 

5-73 

7  11 

-6  186 
30.300 

20  I  3 

107  52 

■a 

7-39 

2 

8  in 
0  IU 

37-35° 

20  14 

r»      ^         «  TV'T  Qi^/~i 

'7 

48 

120  14 

]°Z  1Z. 

j 

0.55 

4 

6'  8 
u  0 

36.422 

20  I  5 

107  3 

2 

5-49 

2 

5  7 

37.400 

17 

49 

135  45 

29  3 

3 

27-34 

3 

n'  8 

7  5 

34-479 

28  0 

26.34 

2 

7  9' 

37-35° 

20l8 

27  30 

i 

26.57 

2 

•7'  to' 

7  10 

37-452 

20  I  p 

17 

55 

133  24 

62  t8 
Do    1 0 

0.07 

2 

O  D 

36.422 

2020 

6 1  4- 

j 

1" 

0 

0=0 

A  2^ 

30-457 

76  43 

1" 

0 

O  O 

36.663 

2022 

70  3 

Z  1" 

0 

O  U 

37-3b4 

2023 

4             O                     A     X"  1* 

•7 

57 

57  27 

132  29 

3 

•  • 

34.61 1 

2024 

129  30 

3 

7.19 

2 

e  8 

5  » 

5  u.  040 

An 

202| 

7.24 

3 

2020 

129  0 

3 

6.51 

2 

5  » 

36.663 

2027 

6.93 

3 

UO 

202  8 

I2? 

1 

*  * 

r'  8 
5  8 

37-47^ 

2029 

17 

59 

130  37 

27 

3 

IO.35 

1 

8  8' 
5  5 

36.3OI 

203O 

275  34 

3 

9.17 

1 

8  2' 

36.71  I 

203I 

276  30 

3 

X.99 

3 

9  =  9 

37-537 

2032 

h-  5025  

17 

59 

130  39 

100  5 

2 

48.74 

1 

9  9 

36.30 1 

2O3  3 

100  40 

3 

47-13 

1 

9  9 

36.711 

2O34 

- 

18 

2 

*33  H 

335  49 

2 

'i 

0 

7  10 

37.663 

2035 

18 

4 

136  4 

9 1  20 

3 

1.92 

2 

*  9 

36.501 

ftr.  rr\ 
89  50 

1 

0 

ft  T/-. 
O  IO 

37-452 

2037 

86  49 

1 

Ji 

0 

ft  n 

8  9 

37.482 

203  8 

18 

6 

1 0 1  51 

300  28 

2 

10.26 

1 

_  _/ 

9,  9 

36.490 

2039 

300  17 

2 

10.66 

1 

8'  TO 

36.504 

2040 

8 

300  20 

3 

13.10 

2 

0  IO 

37-348 

2041 

18 

145  38 

1 80  1 3 

2 

28.95 

1 

7  » 

35-433 

2042 

179  5° 

3 

32-57 

2 

7  7 

35.580 

2043 

179  37 

3 

31.51 

4 

8  8' 

36.501 

2044 

18 

178  50 

3 

32.06 

1 

0  0/ 
a  5 

36.71 1 

2045 

12 

134  11 

1 64  30 

2 

76.94 

1 

_ 

3,  9 

36.501 

2046 

164  30 

3 

75-74 

1 

5  11 

37-457 

2047 

18 

105  1 1 

35  3° 

3 

13.00 

3 

37-479 

2048 

18 

16 

96  41 

195  20 

1 

5.25 

1 

8  9 

30.040 

2049 

18 

198  47 

2 

7  10 

37-479 

2050 

22 

128  50 

359  45 

3 

22. 16 

2 

6  7 

35-433 

205 1 

359 16 

3 

22.26 

2 

0  0 

36.709 

2052 

18 

358  45 

3 

21.49 

0 

6  7 

37-537 

2053 

30 

143  I 

75  32 

1 

7-39 

2 

8  2 

37.665 

2054 

18 

31 

145  50: 

198  58 

3 

3 1.26 

1 

7  10 

34.309 

2055 

198  44 

3 

33.02 

2 

7  10' 

37-523 

"R    nf  Til     1    n"ic  A 

18 

41 

137  28 

63  53 

3 

0  2  .OO 

7  7 

34-479 

2057 

64  3 

2 

81.55 

1 

7  =  7 

35-433 

2058 

63  28 

5 

84.28 

1 

7  =  7 

36-457 

2059 

18 

48 

154  I 

108  15 

2 

1.86 

1 

8'  8' 

35-454 

2060 

108  56 

2 

1* 

0 

8'  8' 

35.580 

2061 

18 

50 

127  17 

282  30 

3 

12. 98 

3 

7  7 

37.663 

2062 

18 

55 

I27  l8 

37  6 

3 

1.23 

0 

7  =  7 

34.468 

2063 

37  2 

2 

6  =  6 

35-433 

2064 

36  42 

35.561 

3 

2065 

34  28 

3 

3.67 

2 

6  =  6 

36.427 

2066 

32  2 

3 

3-63 

1 

5'=  5' 

37-348 

2067 

33  55 

3 

2.76 

2 

37-444 

2068 

32  10 

4 

2.04 

1 

6=6 

37-45* 

2069 

32  41 

4 

2.40 

3 

5'  5' 

37-457 

2070 

18 

59 

142  4 

252  30 

2 

68.75 

1 

7  « 

35-433 

2071 

253  23 

2 

70.00 

2 

7  8 

37-444 

DOUBLE  STARS. 


263 


Index 

Position 

s 

Date  of 

No.  for 

R 

A. 

N  P  D. 

with  Meri- 

03 *o 

S3  -O 

Observa- 

Refe- 

Synonyms. 

1830.0. 

1830.0. 

dian  from 

V  ^ 
3  3 

Dist. 

3  3 

Magnitude. 

tion. 

rence. 

N.  by  W. 

*«  -° 
> 

73  a 

1800+ 

2072 

'9 

I 

107 

43 

58 

48 

2 

15.67 

I 

8 

9 

35.616 

2073 

63 

44 

3 

14.69 

2 

8' 

IO 

37.526 

2074 

l9 

IO 

134  46 

78 

3 

2 

*9-55 

2 

5 

9 

34.465 

2075 

79 

»3 

1 

28.62 

4 

7 

34-556 

2076 

79 

3 

1 

2 

5 

8 

36-553 

2077 

 A  B. 

!9 

H 

I AA. 

130 

57 

1 

if 

O 

6 

1 1 

37.663 

2078 

AC. 

270 

40 

1 

69.43 

I 

6 

7 

37.663 

2079 

l9 

16 

134 

'3 

264  49 

2 

5.11 

I 

8' 

9 

35.580 

2080 

266 

44 

1 

4.63 

I 

8 

IO 

36.504 

208 1 

264  30 

2 

6.61 

8 

10' 

37-539 

2082 

l9 

34 

*55 

J9 

94 

5 

2 

2.24 

I 

8': 

=  8' 

36.556 

2083 

86 

35 

2 

I.24 

I 

9 
8' 

9 

36.715 

2084 

88 

!3 

2 

I.82 

8' 

37-539 

2085 

19 

39 

'45 

24 

150  29 

3 

22.24 

I 

5' 

6 

34.548 

2086 

151 

10 

3 

24.38 

I 

7' 

8 

34-55° 

2087 

150 

27 

2 

22.93 

6' 

7 

35-433 

2088 

J9 

45 

142 

21 

243 

27 

2 

8l.  QQ 

j 

7' 

8 
7' 

34.479 

2089 

244 

l9 

2 

83-39 

I 

7 

36.504 

2090 

20 

1 

!47 

20 

29 

5i 

3 

6.87 

I 

8' 

9 

34.548 

2091 

29 

23 

3 

8.39 

I 

8  = 

=  8 

35.580 

2092 

28 

28 

2 

8.9O 

3 

8 

8 

37-539 

2093 

20 

6 

130 

42 

115 

26 

3 

II.85 

4 

7' 

8 

36.504 

2094 

114 

30 

3 

IO.34 

2 

36-7i5 

2095 

20 

l7 

IOI 

45 

65 

0 

2 

II6.98 

2 

7' 

8 

36.504 

2096 

20 

17 

IO5 

55 

17 

23 

3 

I8.69 

1 

6' 

7 

35.608 

2097 

17 

35 

z 

I8.9O 

3 

36.504 

2098 

17 

0 

2 

i8.ii 

1 

6' 

7 

36.594 

2099 

A.  2404.      jo  Capricomi  = 

H.n.5i  = 

20 

19 

105 

22 

177 

20 

2 

4-39 

3 

5' 

8 

35-534 

2100 

Sh.  323. 

177 

38 

3 

3.91 

3 

5' 

8 

37.526 

2101 

20 

20 

109 

9 

239 

23 

2 

21.35 

3 

7 

7 

35-534 

2102 

239 

18 

2 

22.82 

5 

7 

8 

36.646 

2IO3 

20 

20 

J35 

55 

34 

20 

3 

7.08 

1 

8 

9 

35.608 

2IO4 

34  47 

3 

6.07 

5 

8 
6' 

IO 

36.715 

2IO5 

20 

37 

J53 

3 

IOI 

28 

2 

7 

34.638 

2I06 

IOI 

17 

2 

3.23 

1 

7  = 

=  7 

35-556 

2IO7 

20 

39 

1 24 

23 

164  31 

2 

21.71 

1 

5 

1 1 

35.608 

2  I08 

20 

42 

IOI 

4 

no 

42 

2 

7.09 

1 

9 

9' 

36-5  53 

2IO9 

109 

55 

3 

7.88 

4 

8 

8 

36.567 

21  IO 

112 

14 

3 

7.14 

1 

7' 

8' 

36-7i5 

211  J 

20 

49 

!33 

39 

*55 

10 

2 

59-79 

2 

8  = 

=  8 

36556 

21  12 

254  40 

3 

60.10 

4 

7 

7 

36.646 

2II3 

21 

2 

105 

43 

328 

5° 

1 

2 

0 

8 

8' 

35-6i3 

21 14 

327 

6 

1 

2.12 

1 

8 

8 

36.641 

2II5 



21 

8 

144 

9 

307 

3i 

2 

3-65 

2 

5 

10 

34.468 

21  16 

306 

53 

2 

5 

IO 

34-479 

21 17 

302 

27 

2 

3.71 

1 

5' 

9' 

34.548 

2Il8 

46 

309 

42 

3 

5' 

IO 

34-55° 

21 19 

h.  5262  =  B.  7009  

•  •  •  •  •••••• 

21 

10 

170 

92 

53 

1 

33-34 

0 

6 

1 1 

34-775 

2I20 

92 

0 

1 

24.22 

1 

6 

12 

37-526 

2121 

 AB. 

21 

15 

136 

47 

56  45 

1 

5 

0 

7 

I  I 

34-479 

2122 

AC. 

183  25 

1 

7 

9' 

34-479 

2123 

21 

23 

i73 

29 

83 

28 

3 

3.00 

4 

5' 

9 

34-7I7 

2124 

80 

37 

2 

4-55 

1 

6 

9 

35-583 

2125 

83 

55 

3 

3-57 

2 

6 

9 

36.422 

2126 

2 1 

28 

107 

10 

80 

18 

2 

17.99 

i 

9' 

IO 

36.641 

2127 

2 1 

28 

107 

4 

268 

55 

2 

5 1.02 

1 

8 

IO 

36.641 

2128 

21 

37 

138 

4 

1 1 

35 

1 

29.69 

1 

6' 

IO 

36-556 

2129 

15 

3 

3 

3°-5i 

3 

6' 

9 

36.690 

2130 

h.  S3°9  

21 

47 

141 

53 

169 

10 

1 

10.14 

1 

IO 

IO 

34.548 

213I 

21 

48 

105 

56 

3i8 

30 

1 

19.79 

1 

7 

IO 

35.613 

2132 

 AB. 

320 

33 

2 

17.30 

0 

6 

II 

37.797 

2133 

2 1 

55 

149 

54 

142 

J5 

1 

2 

0 

8 

IO 

34-55° 

2134 

142 

!3 

1 

7' 

10 

34-643 

2135 

154 

25 

0 

8' 

IO 

35.608 

2136 

AC. 

190 

5° 

1 

7' 

7' 

34.643 

2137 

22 

1 

149 

40 

99 

5° 

2 

15.20 

1 

9 

IO 

34-548 

2138 

100 

30 

3 

15.86 

1 

8' 

9' 

35.608 

2139 

h.S3!9  

22 

2 

129 

9 

1 1 1 

31 

2 

1.87 

2 

8  = 

=  8 

34.693 

2140 

108 

4i 

2 

1.98 

1 

8  = 

=  8 

35-5°4 

214I 

1 10 

10 

1 

8'= 

=  8' 

35-58° 

2142 

1 10 

48 

3 

1.54 

3 

8  = 

=  8 

37.660 

264 


MICROMETRICAL  MEASURES  OF 


Index 
No.  for 
Refe- 

1'flKV. 


2  143 
2144 
2145 
2I46 
2147 

2  148 
2149 
2150 
2151 
2152 
2153 
2154 
2I55 
2156 
2157 
2158 
2159 
2l6o 
2l6l 
2l62 
2163 
2164 
2165 
2l66 
2167 
2168 
2169 
217O 
2I7I 
2172 
2173 
2174 
2175 
2176 
2177 
2178 
2179 
2l8o 
2l8l 
2l82 
2183 
2184 
2185 
2l86 
2187 
2l88 
2189 
2190 
2191 
2192 
2193 
2194 


Synonyms. 


B?7i54  +  7iS5-    A.  238  

h.  5334=  8  Toucani  

B.  7173  S  3  Grids.    A.  239   

,'  Aquarii   

B.  7176  "  double."     A.  240  

(3.  Pise.  Austr. 

A.  241  

h.5354  

B.  7190  +  719I  =  A.  242  A  B. 

h.  5 3 56=  do.  the  smaller  star  double;  BC 


2.2943   

h.  5367  =  B.  7218. 
22  Pise.  Austr.  . . . 

h-  5373  

2.  2970   

B.  7246  =  A.  246  . 

A.  24S  

2.  2988  

2-  2993  

<>•  776  

h.  5392  =  B.  7270. 

2.2998   

B.  7276.     A. 248  . 


B.  7280  4-  7281.    A.  249.    \p  Gruis 

2.  3008   

h-  5397   

h.  5403  =  B.  7301   


B.  73J4  +  73I5;  R'27;  A. 251 
9  Phcenicis. 

B.  7342  "  double."  

h-5435  

h.  544°  


R  A. 
1830.0. 

N  PD. 
1830.0. 

Position 
with  Meri- 
dian from 
N.  by  W. 

Value  attri- 
buted. 

Dist. 

Value  attri- 
buted. 

22 

1 1 

IDS 

52 

°3 

43 

3 

18.44 

2 

82 

8 

0 

J7-39 

1 

22 

15 

'55 

5° 

282 

3 

6.78 

2 

282 

00 

A 

6.97 

22 

20 

T  0 A. 

1 J4 

0 H 

2 1  c 

j 

"3  C 
4  J 

0 

61.46 

I 

2 1  c 

C  T 

J  1 

0 

61.20 

0 
5 

22 

20 

90 

53 

0  C2 

JJ 

20 

0. 
J 

3-55 

0  C2 

O 

0 
J 

3-42 

0  C.  I 

J  J 

0 
3 

4.18 

5 

22 

22 

123 

'3 

'73 

3 

3°-33 

1  /  3 

2 1 

0 

5 

28.27 

0 
3 

22 

0  7 

33 

O  d 

40 

3 

87.01 

29 

140 

43 

71 

40 

43.64 

1 

22 

30 

1 19 

:4 

160 

20 

85.31 

0 

J59 

'5 

T  cn 
'59 

cn 

21 

39 

4.30 

5° 

9 

3 

4.61 

2 

c8 

4 

2 

4.13 

22 

on 

jy 

104 

55 

1  jfl 
113 

40 

3 

30.86 

22 

43 

123 

47 

276 

5° 

3 

3-59 

1 

27 

3° 

2 

22 

5° 

T55 

99 

35 

3 

48.89 

2 

22 

J4 

02 

12 

06 
3° 

18 

8.87 

3 

2 

57 

141 

3° 

260 

!5 

3 

200 

5° 

3 

7.96 

1 

5s 

260 

24 

3 

8.17 

3 

150 

39 

290 

4 

3 

15.62 

1 

292 

16 

3 

14.93 

4 

23 

2 

102 

5° 

100 

15 

2 

3-43 

2 

23 

5 

99 

5i 

356 

44 

3 

25.74 

3 

23 

7 

100 

0 

311 

28 

3 

49.29 

3 

23 

9 

149 

H 

17 

57 

2 

21 

30 

2 

6.96 

1 

23 

1 1 

104 

22 

343 

37 

2 

H-75 

2 

23 

1 1 

141 

14 

210 

7 

3 

I  7.OO 

2 

212 

14 

3 

I6.64 

3 

212 

27 

2 

l6.42 

2 

23 

14 

144 

45 

213 

18 

3 

26.81 

2 

213 

45 

4 

27.45 

23 

14 

99 

24 

90 

'5 

2 

6.88 

2 

23 

15 

105 

25 

329 

57 

2 

61.76 

1 

23 

25 

155 

38 

47 

1 1 

3 

43.09 

2 

49 

17 

3 

41.48 

1 

48 

46 

3 

42.34 

2 

23 

30 

137 

35 

268 

16 

3 

4.30 

1 

269 

33 

4 

4.72 

1 

46 

268 

7 

2 

4-44 

3 

23 

117 

59 

267 

45 

2 

6.92 

2 

267 

20 

a 

6.79 

1 

23 

48 

107 

6 

2 

45 

1 

12  ± 

0 

23 

54 

118 

4 

285 

5 

3.63 

2 

Magnitude. 


Date  of 
Observa- 
tion. 
1800+ 


9 
10 


9 

10 


7' 
6' 

7  • 
6 

4' 

5 

7' 

8' 

6 

7 
6' 


5 

7 

9 

7 

9' 

7 

6' 

9 

9 

9 

9' 
10 
11 
10 

9 
6' 


7 

7'  9' 
7  10 

7'=/ 
7  7' 


1 0 


5 
7 
9 

6  9 
6'  10 
6  9 


10 
6' 


9 
10 


6'  10 


35-  9 '4 

36-  567 
35.608 
36.711 
36.567 
36.646 

35-55° 
36.564 
36.646 
35.761 
36.646 
34.780 

34-  548 
36.641 
37.652 
37.660 
36.641 
37.660 
37.797 
35.761 

35-  55° 
35556 
36.567 

37-  797 
34.638 

34-  772 
37.663 
35.608 
36.711 
37.797 
37-797 

37-791 
34.643 

35-  9'4 
37.791 
36.567 
36.646 
37.808 
34.641 
35.580 

37-797 
35.761 

34-693 
36.646 
36.711 
34-717 
34-772 
37.660 
34.780 
35  556 
35.761 
34.780 


265 


NOTES  TO  ACCOMPANY  THE  MICROMETRICAL  MEASURES 
OF  DOUBLE  STARS. 


1 1 1 3  Distance  by  thick  wires  without  cross  zeros,  cor- 
rected as  per  table. 

1 1 14.  An  oblique  transit  (in  which  there  must  have  been 
some  error  in  setting  the  micrometer  wire)  gave 
by  4  transits  74".8o  for  the  distance,  which  is 
rejected. 

1 1 15  Distance  by  6  oblique  transits  taken  with  great 
care. 

1 1 17    Distance  by  5  oblique  transits,  great  care  taken. 

1 12 1  Distance  by  4  oblique  transits  over  a  wire  50  in- 

clined to  the  parallel,  which  is  too  small  an  angle 
for  the  purpose,  the  zero  uncertainty  having  too 
much  influence.  In  consequence  the  observation 
is  allowed  only  half  its  value. 

1122  All  possible  care  taken  with  the  distances,  and  by 

nice  management  of  the  micrometer  screwhead, 
all  hitching  of  the  threads  avoid  in  the  crossing. 
(The  screwhead  being  drawn  towards  the  eye.) 

1 123  The  wires  were  purposely  set  to  1700  (the  mean 

angle  of  sweep  484)  but  it  proved  intolerable. 

1 126  Distance  scarcely  obtainable,  but  a  little  illumination 

improves  the  object. 

1 127  Very  difficult,  especially  in  distance. 

1 1 28  Bad  night,  will  not  bear  the  le  1st  illumination.  No 

distances  could  be  procured. 

1 129  Distance  between  thin  wires  and  the  screwhead  of  the 

micrometer  being  drawn  tc  vards  the  eye  in  cross- 
ing, no  hitching  of  the  threads  took  place. 

1 1 3  3    Distance  by  7  oblique  transits. 

1 1 34  Micrometer  set  to  780  30',  the  mean  measure  of 

1835.920:  it  is  now  cert -inly  no  measure.  The 
star  has  surely  changed.  Distances  close  clipped 
between  the  thick  wires. 

1 1 35  Distance  by  5  differences  of  R  A. 

1136  Distances  by  9  oblique  transits  over  a  wire  io° 

inclined. 

1 139  Stars  excessively  furred  but  with  distinct  centres. 
At  least  half  the  light  goes  to  the  furring. 

1 143  Distance  by  3  oblique  transits. 

1 144  Very  strong  S.E.  wind,  steadiness  and  definition 

perfect.    No  fiddling  of  wires,  but  all  excellent. 

1 145  Grew  unsteady  before  measures  could  be  com- 

pleted. Distance  a  mere  guess — one  measure 
only  on  either  side  of  the  zero. 

1 146  Extremely  delicate,  but  bears  a  fair  illumination. 

1 148  A  very  delicate  and  beautiful  object.  Definition 

good  but  creeping. 

1 149  Definition  blurred,  but  the  threads  do  not  fiddle. 
1 1 52    Very  close,  distance  estimated  at 

1 1 54  Thick  hazy  sky,  but  good  definition. 

1 155  Strong  S.  E.  wind  but  steady  and  well  defined. 

1 1 56  Will  not  bear  power  No.  3,  though  near  the  zenith. 

1 158    Micrometer  set  to  Mr.  Dunlop's  measure  I5".8. 

Both  discs  are  broadly  included  between  the  wires 
with  an  interval  on  either  side. 


1 161  Very  bad  definition,  stars  furry  with  tolerable 
glimpses,  perfectly  steady  however. 

1 1 64  Well  defined,  perfectly  steady — a  fine  double  star; 

excellent  measures  of  position. 

1 165  Delicate.    Tremulous  and  furred. 

1 167  The  star  will  not  remain  quiet.  This  star  must  be 
verified,  though  after  nearly  three-quarters  of  an 
hour's  attention  I  feel  assured  the  small  star  is  no 
illusion.  The  power  No.  4,  leaves  hardly  a 
doubt,  and  admits  of  measure  in  position,  but  the 
night  is  not  good  enough  for  such  delicate  work. 
[N.B.  Brisb.  makes  PD  =  1290  16'.] 

1 1 69  Very  good  definition  and  perfectly  steady.  The 

position  must  be  within  a  degree  of  the  truth. 

1 170  Good  and  steady  definition.    Distance  by  6  diffe- 

rences of  R  A. 

1171  Very  difficult,  too  faint  for  the  instrument.  Dis- 

tances quite  rough. 

1 173  A  faint  object,  but  in  a  good  night  not  difficult. 

Not  well  defined. 

1 1 74  Perfectly  steady,  tolerably  defined. 

1 1 79  Too  difficult  for  the  instrument,  especially  in  dis- 
tance. 

1 1 82  }  One  hundred  parts  error  being  suspected  in  the 

1 183  S     micrometer  reading,  (which  being  supposed)  gave 

6 1"-5 5  for  the  distance,  3  differences  of  R  A  were 
taken,  not  very  satisfactory,  whose  mean  gave 
66.32,  thus  establishing  the  supposed  omission  of 
1  Rev. 

1 184  Extremely  difficult,  a  20-feet  object. 

1 1 86  Definition  confused,  star  not  very  steady. 

1 187  Definition  perfect,  stars  very  steady,  and  both  posi- 

tion and  distance  noted  as  excellent. 

1 19 1  Definition  wonderfully  fine.  Distance  difficult,  the 
position  being  so  near  the  parallel. 

1 193  After  taking  the  position,  it  grew  ill-defined,  and  no 
distance  could  be  got. 

1 196  Delicate.    Requires  the  strongest  illumination  the 

lamp  will  give  to  see  the  small  star.  Some  sus- 
picion of  elongation  in  the  large  star. 

1 197  Dense  haze  and  cirro-cumuli,  which  evidently  affect 

the  estimations  of  magnitude,  which  must  be  re- 
jected in  taking  means. 

1 199  Distance  by  4  oblique  transits  over  wire  io°  inclined 
to  parallel. 

1201  Well  seen  by  very  short  glimpses  in  the  drift  of  a 
black  south-easter.    Clouds  thickening. 

1203  Distance  by  two  sets  of  oblique  transits,  3  each  over 

wire,  inclined  respectively  io°  and  200  to  the 
parallel  —  the  former  giving  2i".20,  the  latter 
i9".82  ;  mean  2o"-5i. 

1204  Full  moon.    Superb  and  cloudless,  not  a  trace  of  a 

cloud  on  the  mountain.  (N.B.  How  often  the 
full  moon  nights  are  so  !) 

1206    All  excellent. 

3  Y 


266 


NOTES  TO  ACCOMPANY  THE 


1207  The  distance  irregularly  taken  by  using  the  left  hand 
edges  of  each  of  the  thick  wires,  a  method  ad- 
mitting of  no  satisfactory  zero  being  applied. 
The  result  is  of  course  of  no  value. 

1212  Distance  by  2  oblique  transits  over  a  wire  io° 

inclined. 

12 13  Distance  by  the  faulty  method  noticed  in  No.  1207  ; 

no  value. 

12 14.    Distance  by  4  differences  of  R  A. 

12 1 5  Excessively  difficult  in  distance. 

12 16  Perfect  definition  and  steadiness,  rather  difficult  in 

distance,  but  bears  illumination  pretty  well. 

1217  Steady,  and  definition  superb,  distance  difficult,  and 

a  tendency  to  cloud  to  westward. 

1228  Distance  by  6  oblique  transits  over  a  wire  io°  in- 

clined. No  other  mode  of  measurement  would 
give  a  satisfactory  distance  of  such  a  star. 

1229  Difficult  in  distance ;  very  steady,  pretty  well  de- 

fined. 

1230  Extremely  difficult  in  distance,  but  great  pains 

taken. 

123 1  Small  star  certainly  seen,  but  far  too  difficult. 

Distance  by  5  unsatisfactory  differences  of  R  A. 
Requires  illumination. 
1234    Bad  definition,  came  on  before  the  distances  could 
be  completed. 

1239  Measured  with  the  lowest  power.    Will  not  bear 

magnifying. 

1240  111  defined,  and  in  consequence  not  bearing  illumi- 

nation— therefore  difficult  in  distance. 

1242  Very  difficult  in  distance  for  want  of  light. 

1243  Ditto. 

1244  A  difficult  star,  especially  in  distance.    Very  steady. 

1245  Distance  by  4  oblique  transits  over  wire  io°  in- 

clined. 

1247  Glimmering,   but  perfectly  steady.     No  sign  of 

fiddling  in  the  threads  or  crossing. 

1248  Too  difficult.    The  night  will  not  permit  the  use  of 

higher  power  than  No.  2. 

1249  Very  difficult.    Power  No.  1  (the  lowest)  used. 

1250  The  polar  distances  of  this  star  disagree  io°,  1150  is 

probably  the  right. 

125 1  Distance  by  5  unsatisfactory  oblique  transits. 

1253  Very  steady,  but  glimmering. 

1254  Steady,  but  glimmering.    A  superb  sky  and  full 

moon,  but  the  night  is  not  good  enough  for  this 
star. 

1259    Difficult.    Perfectly  steady,  but  not  well  defined. 

1261  In  a  cirrous  haze,  of  which  two  systems  at  right 
angles  to  each  other  have  come  on. 

1264  A  third  star  C,  2'  +  distant  is  situated  a  very  little 
following  the  line  A  B  prolonged. — C  =  9  m. 

1268  Full  moon  very  troublesome. 

1269  Very  bad  definition,  the  large  star  not  separated. 

1275  Much  of  the  object  glass  cut  off,  being  past  me- 

ridian, and  near  the  zenith.  A  third  star  9  m 
seen  making  nearly  an  isosceles  triangle  with  the 
other  two,  and  preceding  both. 

1276  Clouded  densely  over  before  more  than  a  single 

distance  could  be  taken. 

1278  Three  oblique  transits  gave  dist  =  43".i3,  but 
there  must  have  been  some  mistake  in  setting  the 
wire. 


1279  Distance  not  measurable  to-night.     A  single  rough 

measure  only,  of  no  value,  procured. 

1280  26".    The  measure  of  1279  is  certainly  too  much — 

no  measure  is  possible,  but  18°  is  the  outside 
allowable. 

128 1  Distance  by  two  differences  of  R  A. 

1287  Violent  gusts  of  wind  from  S.  E.  or  S.  Steadiness 
and  definition  (with  the  lowest  power)  perfect. 

1290  Too  difficult. 

1 29 1  Wind  gusty ;  definition  not  good. 

1292  Both  stars,  perhaps,  ruddy,  but  too  faint  to  see  the 

colour  well,  yet  I  do  think  they  are  redder  than 
ordinary. 

1293  Both  stars  pale  pink,  bearing  good  illumination, 

and  improved  by  it.  Definition  glimmering, 
and  will  not  bear  No.  2  ;  blurred  and  moulding. 

1294  Wants  light. 

1305  Sky  clouding  and  clearing  alternately.  Perfectly 

steady,  and  well  defined. 

1306  Well  defined,  and  perfectly  steady. 

1307  Much  improved  by  a  pretty  strong  illumination. 

13 1 1  Distance  by  two  distinct  series  of  measures  with 

powers  No.  3  and  No.  4. 

1 3 12  Two  other  stars  C  =  10  m  and  D  =  9  m  near. 

Distance  of  D  =  3'  26".8.  That  of  C  about  one- 
third  of  this. 

1320    Too  ill  defined  for  any  measure  of  distance. 

1322  Full  moon.  Superb  sky  ;  a  N.  W.  cloud  over  Table 

Bay. 

1323  Triple.    The  nearer  star  B  bears  great  illumination, 

the  farther  C  does  not. 

1324  Sky  alternately  clearing  and  clouding,  —  at  last 

clouded  over. 

1330    Dancing,  trembling,  and  glimmering. 

1332    Position  wire  set  to  720  40',  but  it  cannot  be  borne. 

The  star  has  certainly  changed.  [Mr.  Dunlop's 
position  is  n°  12',  which  is  probably  a  mistake  of 
reading.] 

1336  Moon  apparently  full  (it  was  full  yesterday  at 
2  p.  m.)    A  superb  sky — not  a  trace  of  cloud. 

1339  Certainly  divided,  but  far  too  difficult  a  star  for 

this  instrument  except  in  the  very  choicest  oppor- 
tunities. Position  almost  conjectural — a  single 
measure.    Distance  estimated. 

1340  Extremely  close.     Unmanageable  from  bad  de- 

finition. 

1341  Measures  obtained  with  the  utmost  difficulty,  two 

only  got,  which  cost  upwards  of  half  an  hour. 
Obliged  to  use  the  left  eye,  which  in  moments 
divided  it.    The  right  of  no  use  at  all. 

1342  Orange  and  green,  fine  contrast  of  colours. 

1343  Ditto  ditto. 

1346    y  Pise.  Volantis.    A  high  yellow.    B  pale  blue. 

1350  Does  not  bear  magnifying.    No.  2  allows  the  stars 

to  be  sharply  seen,  but  is  barely  sufficient  to 
divide  them.    With  No.  3,  furred. 

1 35 1  Stars  glimmering  and  "crabby."    Does  not  bear 

No.  2  well. 

1352  At  first  very  ill  seen,  but  by  degrees  better,  at  last 

pretty  well.  A  distance  of  5"  is  out  of  the 
question. 

1360  Difficult.  Required  extreme  patience  and  frequent 
re-examination  of  measures.  The  preceding  of 
two  double  stars  nearly  on  the  same  parallel. 


MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


267 


1372  The  small  star  bears  a  reasonable  illumination. 

Steady,  but  ill  denned. 

1373  Difficult  in  distance. 

1 38 1  Distance  by  6  oblique  transits  over  a  wire  io° 

inclined. 

1382  Definition  the  finest  imaginable. 

1386  Distance  by  5  oblique  transits. 

1387  Far  too  difficult  in  distance,  and  liable  to  great 

error. 

1389  Distance  by  3  oblique  transits. 

1390  Patience  and  perseverance  required.    Star  moulding, 

but  good  glimpses. 

1392    Found  in  sweeping  unsuccessfully  for  A.  59. 

1395  Distance  quite  impracticable,  even  with  power  No.  1, 
even  with  the  thick  wires,  as  it  bears  no  illu- 
mination. With  No.  2  and  the  thick  wires  it 
succeeds  better. 

1398  Far  too  difficult  for  this  instrument.  A  3d  star  C 
seen  at  about  40",  10  m. 

14.01  Found  in  sweeping  for  A.  61,  which  this  assuredly 
is  not. 

1402  In  a  very  rich  part  of  the  heavens.  Many  more 
stars  in  the  field. 

1404    In  the  preceding  part  of  a  great  cluster. 

1407    In  a  fine  cluster. 

1412  Clouded  suddenly,  and  cleared  again.  It  is  the 
following  of  two  stars  B  1884  and  1887. 

141 8  Distance  by  8  differences  of  R  A. 

141 9  In  strong  morning  twilight,  and  excessively  fatigued 

with  7  hours'  work. 

1427    Distance  by  5  oblique  transits,  taking  alternately 
the  disappearances  and  re-appearances   of  the 
stars  behind  the  two  thick  wires  placed  close 
■  together.    A  very  satisfactory  procedure,  the  field 
being  perfectly  dark. 

1429  Bears  an  illumination  sufficient  for  measurement  of 

the  position,  but  is  too  difficult  in  distance. 

1430  Besides  the  two  double  stars  (A  B  and  E  F)  mea- 

sured in  this  and  No.  1433,  there  is  another  pair, 
C  D,  whose  position  (by  a  single  measure)  = 
2060  30'  and  whose  distance  is  considerably 
greater  than  that  of  A  B.  A  B  C  D  together 
make  up  the  group  A.  67,  which  he  describes  as 
four  stars  "  forming  a  parallelogram."  It  is  in 
fact  a  very  irregular  trapezium.  Distances  by 
oblique  transits  over  wires  included  io°  and  450. 

143 1  Requires  pretty  strong  illumination. 

1432  Bears  and  requires  a  full  illumination. 

1438  Taken  in  broad  morning  twilight ;  no  lamp-light 

required. 

1439  The  line  of  junction  prolonged  passes  through  a  3d 

star  8' m. 

1440  Very  close,  and  extremely  difficult.     Great  patience 

required  for  procuring  the  angles,  but  no  distance 
can  be  had.    Estimated  at  1". 

1444  Too   ill  defined  for   any   measure   of  distance. 

Roughly  estimated  at  6". 

1445  Distance  of  no  value  ;  cloud  rising  and  obscuring 

the  small  star  before  the  bisection  was  complete. 

1450  Clouds  prevented  measures  of  distance.  Only  one 
obtained. 

1454  The  s  p  of  two  stars  forming  a  coarse  double  star  in 
the  finder. 

1456    A  close  and  difficult  star,  being  ill  defined. 


1457  If  there  be  any  reliance  to  be  placed  on  the  mea- 

sures of  1456,  this  star  must  have  changed  con- 
siderably. 

1458  Too  difficult  for  to-night. 

1459  111  defined,  and  unsteady. 

146 1  Distance  by  3  oblique  transits  over  a  wire  io° 

inclined  to  parallel. 

1462  An  error  of  io°  obviously  committed  in  one  of  the 

micrometer  readings ;  corrected  before  taking 
their  mean.  I  cannot  explain  the  great  dis- 
cordance of  the  measures  of  distance,  unless 
another  pair  of  stars  near  it  has  been  measured 
by  mistake. 

1464  Too  close  for  the  low  power,  and  will  not  bear  a 

higher — all  confusion. 

1465  Definition  much  improved,  and  in  consequence  the 

measure  of  this  star  repeated. 

1466  This  star  must  have  changed,  and  the  measures 

must  be  repeated. 

1473    Deep  red  illumination  resumed  after  long  disuse. 

1475    In  strong  morning  twilight,  just  before  sunrise. 

1477  Full  moon  (at  7  a.m.  this  morning).  Sky  perfectly 
cloudless  to-night  (with  exception  of  the  usual 
covering  of  the  table  mountain),  after  a  fortnight 
of  calm  cloudy  weather,  with  rain. 

1480    Will  not  bear  the  necessary  magnifying  power. 

Only  a  single  measure  of  position  and  an  esti- 
mated distance. 

1484  Excellent  views  obtained  by  long  and  patient  wait- 
ing. 

1487  Extremely  close  and  difficult.     Hardly  a  doubt, 

but  it  requires  to  be  most  scrupulously  verified. 
It  is  an  object  for  the  20  feet. 

1488  £  Octantis.    I  can  hardly  believe  the  companion 

star  to  be  an  object-glass  illusion.  Diagrams 
and  measures  taken  with  the  object-glass  in  its 
usual  position,  and  turned  900  round.  Both 
agree  in  placing  the  small  star  s  f,  and  though 
the  measures  differ  90,  it  is  not  more  than  the 
closeness  and  inequality  of  the  stars  will  admit  of. 

1490  Not  the  smallest  occasion  to  re-measure  this  star. 
Distance  by  8  differences  of  R  A. 

1493  Measured  in  company  with  Mr.  Smyth,  but  his 

measures  not  used  in  casting  up  the  mean. 

1494  Another  set  of  measures  taken  alone. 

1496  Night  growing  bad,  good  views  growing  short  and 
rare. 

1499  Several  other  stars  in  the  field.  Too  coarse  and 
on  that  account  difficult  in  dist. 

1 504  Will  not  bear  the  illumination  necessary  for  procuring 

a  good  distance. 

1505  Will  not  bear  magnifying  beyond  No.  2. 

1507  Too  difficult  in  distance,  as  it  becomes  violently 
agitated. 

1 5 12  Difficult  both  in  pos  and  distance,  owing  to  the 
great  difference  of  magnitudes. 

1 5 14  Position  is  better  measured  than  dist,  the  definition 

growing  worse. 

1 5 15  Dist  by  6  differences  of  R  A,  and  4  measures  with 

cross  zeros. 

15 16  Dist  by  5  differences  of  R  A,  which  for  a  star  so 

near  the  pole  is  the  best  mode  of  measurement 
for  such  an  angle  of  position. 

1 5 17  Dist  by  3  differences  of  R  A. 

1 5 18  Dist  by  3  very  doubtful  differences  of  R  A. 


268 


NOTES  TO  ACCOMPANY  THE 


1 5 19    Dist  by  8  differences  of  R  A. 

1 52 1  Dist  by  a  single  measure,  and  that  misread  by 

1  revolution  (corrected  in  reduction). 

1522  Distance  most  careful,  after  many  trials  and  rejec- 

tions. 

1523  Not  very  easy,  but  bears  illumination. 

1525  Distance  by  two  oblique  transits,  but  too  difficult. 

1526  Distance  by  four  oblique  transits,  but  no  sort  of 

confidence  in  them.  The  star  is  excessively 
difficult. 

1527  Too  ill  denned  for  any  good  measure. 

1528  Well  divided  in  good  glimpses,  but  difficult. 

1531    Most   beautifully  defined.     The  small  star  con- 
spicuous in  a  fully  illuminated  field. 

1535  Will  not  bear  sufficient  illumination. 

1536  Distance  rough,  the  lamp  being  almost  out. 
1543  Clouded  thickly  before  distances  could  be  taken. 
1547  Stars  burred,  and  not  very  steady. 

1549  Burred.    Too  difficult  in  distance  to-night. 

1550  A  calm,  hot  night.    Tolerably  defined,  but  catching. 

1 55 1  The  larger  of  these  two  stars  seen  with  the  right 

eye  through  the  telescope,  is  equal  to  n  Argus 
seen  with  the  left  eye  directly. 

1553    Bears  illumination,  but  is  difficult. 

1555  Morning  twilight  coming  on. 

1556  Another  double  star  seen  south  of  this. 

1 561  Found  in  a  fruitless  search  for  A.  92.    It  is  the 

nearest  to  his  place  and  description  I  can  find. 
[It  cannot  be  A.  92.] 

1562  Distance  by  6  differences  of  R  A. 

1563  A  close  star  suspected  3"  dist,  pos  8i°.o,  11  m. 

[But  this  cannot  be  Mr.  Dunlop's  star  (A.  97), 
as  he  makes  both  magnitudes  7.]  This  com- 
panion was  evidently  an  illusion,  as  it  was  not 
seen  in  the  20  feet,  nor  in  any  of  the  subsequent 
equatorial  observations. 

1 566  The  chief  star  of  a  cluster  of  large  stars. 

1567  The  star  O  in  the  monograph  of  n  Argus,  which 

see.    Very  difficult. 

1569    No  measure  of  distance  possible,   but  estimated 
at  1  J". 

1 57 1  Distance  assuredly  too  great. 

1572  Distance  fair  enough. 

1573  Distance  certainly  too  small.     Very  close,  how- 

ever, and  a  difficult  star.  [N.B.  The  mean  of 
the  distances  of  1571  and  1573,  which  are  faulty 
opposite  ways,  gives  very  nearly  that  of  1572.] 

1574  )  These  measures  are  reduced  to  the  middle  point  of 

1576  \     A  and  B,  by  applying  to  the  measured  positions 

of  A  B  the  correction  +  o°  44',  and  to  the 
measured  distance  +  i"-i2,  which  results  from 
a  collation  of  all  the  measures.  In  obs  1575, 
the  measures  were  taken  at  once  from  C  to  the 
middle  point  of  A,  B  seen  as  one  star. 

1577  Distance  impossible;  a  rough  and  conjectural  mea- 

sure of  35  Hh  micrometer  parts  was  declared  not 
worth  casting  up. 

1578  Distance  by  9  oblique  transits. 

1580    Too  difficult  for  any  measure  of  distance. 

1583    The  star  is  coarsely  triple.    C  estimated  to  be  2J 
times  farther  from  A  than  B  is. 


1584  Too  close  for  No.  3  power,  and  too  faint  for  No.  4, 
and  not  well  enough  defined.  Belongs  to  the 
pervicinse.  The  measured  distance  i".42  is  too 
large. 

1586  Very  delicate.  Requires  great  patience  and  strong 
illumination.    Definition  perfect. 

1588  An  extremely  close  double  star,  and  almost  exactly 
on  the  parallel,  which  makes  it  difficult  to  mea- 
sure. 

1590  Definition  at  first  tolerable,  but  rapidly  growing 
worse.    Too  difficult  for  a  measure  of  distance. 

1593  Both  stars  decidedly  red. 

1594  Both  ruddy. 

1595  This  star  is  beautifully  triple,  a  very  good  resem- 

blance of  what  £  Cancri  one  day  was,  and  one 
other  day  will  be.  Came  on  suddenly  ill  defined, 
and  no  measures  of  the  close  star  could  be 
obtained.  On  the  back  of  the  paper  stands  the 
following  memorandum  : — "  If  ever  I  saw  a  close 
double  star  in  my  life,  I  saw  this  as  one.    I  went 

in  and  mentioned  it  to   ,  and  then  came 

out  to  measure  it.  It  was  then  most  beautifully 
distinct  (i.  e  ,  after  I  returned).  I  got  my 
pencil  ready,  and  laid  out  the  lens  to  read  off, 
and,  looking  again  —  the  close  st.ir  was  gone. 
After  this  it  grew  rapidly  ill  defined,  and  i  lost 
a  full  hour  in  working  against  the  faults  of  the 
atmosphere  in  vain  to  recover  my  lost  star.  At 
last  it  grew  all  confusion,  and  I  gave  it  up.  This 
must  be  re-examined  with  all  possible  care,  as  it 
is  quite  unaccountable." 

The  diagram  makes  the  position  of  the  illusory 
star  about  3320.  I  have  often  exan  laed  it  since. 
There  is  no  close  star.  It  must  i.^ve  besn  an 
illusion,  but  a  very  odd  one. 

1596  The  supposed  triplicity  of  this  star  is.  I  believe,  an 

illusion.  It  wants  the  20  feet  to  decide.  [The 
star  has  occurred  twice,  in  f  542  and  554,  but 
in  neither  observation  is  any  close  star  men- 
tioned.   See  Catal.~\ 

1 60 1  A  single  measure,  got  by  great  patience.  The  small 
star  is  certainly  s  p. 

1605  A  beautiful  object  ((3  Hyd.  Crat),  very  like  ?  Ursae, 
but  closer  and  a  little  more  unequal. 

1609  Set  micrometer  (with  all  due  attention  to  the  zero) 

to  pos  3370  45'.  It  cannot  pass.  If  the  angle 
ever  was  3370  45',  the  star  must  have  changed. 

1610  Morning  twilight  coming  on. 

1613    Clouding  and  clearing  during  the  measures. 

16 1 5    Far  too  difficult  for  this  instrument  in  distance. 

16 19  Difficult  in  position.  In  distance  hardly  prac- 
ticable. 

1622    Wants  light.    The  distance  very  precarious. 

1624  \  Elaborate  sets  of  distances  taken,  but  an  eye-piece 

1625  S     used  for  which  I  have  no  data  for  casting  up  the 

measures. 

1627  Beautiful  discs,  but  trembling  like  drops  of  mer- 
cury. 

1629  The  small  inequality  of  the  discs  increases  the  diffi- 
culty of  getting  correct  measures. 

1635  Taken  while  the  discs  were  dwindling  under  the 
influence  of  a  black  south-east  cloud,  which  at 
length  reduced  them  to  nothing  and  extinguished 
the  stars. 

1637  Working  vehemently,  but  good  centres  which  keep 

their  places. 

1638  Extremely  agitated. 


MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


269 


I  Morning  twilight. 

645  Quiet  at  first,  but  at  the  end  of  the  measures  very 
bad,  working,  fluctuating,  and  confused. 

648  y  Centauri.    Extremely  close  and  very  difficult,  at 

least  as  close  as  y  Virginis;  273  barely  elon- 
gates it. 

649  Certainly  double,  but  far  too  difficult  for  this  tele- 

scope. Distinctly  elongated,  but  the  measures  of 
no  dependence. 

650  Far  too  difficult  for  satisfactory  measures ;  yet  I 

must  believe  these  to  be  somewhere  about  the 
truth. 

651  A  better  set  of  measures  than  hitherto  got  with  the 

equatorial,  but  it  is  too  difficult  for  this  object- 
glass. 

652  Certainly  seen  double,  i.  e.  elongated  with  parallel 

fringes. 

1654  Excessively  close  and  difficult,  but  the  power  No.  4 
will  act  to-night,  though  not  quite  so  well  as  I 
could  wish.    Field  strongly  illuminated. 

1656  Tolerably  elongated  with  No.  4.  Brandishes, 
dances,  and  spreads,  yet  occasionally  an  elongated 
centre  caught. 

1660  Measured  with  Dollond's  new  compound  achromatic 

eyepiece.  Dreadfully  ill-defined,  spreading  and 
agitated.    (Nine  measures  taken.) 

1 66 1  The  utmost  patience  required,  as  the  star  will  not 

keep  a  moment  still ;  moulds,  twirls,  dilates,  and 
all  that  is  horrible.  At  times  becomes  a  diffused 
mass— a  mere  nebula.    (Ten  measures  taken.) 

1662  Tolerably  defined.    Discs  in  contact.    (Nine  mea- 

sures taken.) 

1663  Excessively  ill-defined.    (Two  measures  taken.) 

1664  Definition  bad.    (Six  measures  taken.) 

1665  Pretty  well  defined.    (Ten  satisfactory  measures  of 

position,  and  8  tolerably  so  of  distance.) 

1666  Very  ill  defined,  dancing  violently.    (Seven  mea- 

sures.) 

1667  Passable  definition.    In  twilight.    (Eight  satisfac- 

tory measures.) 

1668  Definition  generally  bad — but  in  good  glimpses  6 

tolerable  measures. 

1669  111  defined,  among  clouds,  but  with  great  patience 

got  5  tolerable  measures. 

1670  111  defined — excessively  difficult — yet  I  feel  assured 

that  pos  400  (500  microm  reading)  is  too  large 
(small  on  micr)  an  angle,  and  300  (=  60°  micr) 
nearly  right. 

1671  Not  well  defined,  and  unsteady.    (Five  measures.) 

1672  In  broad  daylight,  just  after  sunset.    Definition  bad 

and  exceedingly  unsteady.  Glimpses  interrupted 
by  total  confusion. 

1673  These  are  by  far  the  best  measures  (of  this  star)  I 

have  had  at  the  Cape.  Their  discordance  arises 
not  from  atmospheric  influence  as  in  all  the 
former  measures,  but  from  the  exceeding  close- 
ness which  renders  the  oval  of  elongation  (power 
400)  too  nearly  a  circle  to  admit  of  a  good  judg- 
ment of  the  direction  of  the  axis.  Good  defini- 
tion, perfect  steadiness  of  centres  ;  10  measures 
taken,  difference  of  greatest  and  least  =  n°  35'. 

1674  Four  measures  taken,  3  of  which  (allowed  double 

weight)  were  made  when  the  star  was  very  tran- 
quil and  quietly  contemplated,  the  only  time  I 
have  even  seen  it  thus  here. 


1675  Firm  good  glimpses.    Discs  very  small  and  fairly 

divided,  (in  the  midst  of  much  flare)  [caused  by 
throwing  the  eyepiece  a  trifle  out  of  focus']  (2 
measures.) 

1676  Fairly  seen,  and  a  real  set  of  measures.  (Five 

measures  taken.) 

1678  The  utmost  patience  necessary  to  procure  these 

measures  [5  in  number]  and  they  are  extremely 
unsatisfactory.    Definition  very  bad. 

1679  A  wedge.    Bad  definition,  but  glimpses  obtained  [5 

measures] . 

1680  Two  measures.    The  last  decidedly  a  good  one. 

[Difference  o°  20'.] 

1 68 1  Two  bad  measures.      Quite  unmanageable;  yet 

taken  ih  past  merid  at  3h  a.m.,  thinking  it  a 
peculiarly  favourable  opportunity — but  it  dances, 
twirls,  and  makes  all  manner  of  distortions. 

1682  The  best  set  of  y  Virginis  I  have  got  since  my 

residence  at  the  Cape,  and  deserving  confidence. 
Six  measures.  Very  fair  definition  and  steadiness. 
The  distance  is  less  than  1". 

1683  Very  conspicuously  wedge-formed.  Unequivocally 

elongated.  Twirls,  moulds,  dances,  and  wriggles 
in  a  most  violent  manner,  but  preserves  an  elon- 
gated disc.  [Three  tolerably  good  measures 
taken.]  There  is  no  doubt  or  hesitation  now 
about  the  star  being  double.  Estimated  distance 
of  centres  two-thirds  of  a  second. 

1684  Quiet,  but  furry,  and  not  worth  measuring.  Only 

a  single  measure,  and  that  of  no  value,  procured. 

1686  Night  after  the  full  moon.  Not  a  cloud  to  be 
seen.  Calm.  Steadiness  perfect,  but  the  star 
glimmers. 

1688  Very  difficult. 

1689  Too  faint  for  direct  measures  of  distance.  Three 

good  oblique  transits  by  disappearances  and  re- 
appearances. 

1690  Steadiness  and  definition  perfect. 

1699  111  defined  and  unsteady. 

1700  Perfect  definition  and  steadiness. 

1705  By  far  the  closest  double  star  I  have  seen  double  in 

this  instrument.  I  have  no  doubt,  but  should 
like  to  see  it  in  the  20  feet.  Night  perfect. 
Power  No.  4,  perfect  in  its  action. 

1706  Found  in  a  fruitless  search  (for  the  third  time)  for 

A.  132. 

1707  Distance  impracticable,  owing  to  bad  definition. 

17 13    Glimmering,  but  steady.    Good  measures. 

17 1 5  The  two  stars  run  along  so  nearly  bisected  by  the 
true  parallel,  that  it  is  hardly  possible  to  say  which 
is  the  northern  or  southern. 

1717  Faint,  and  difficult  in  distance. 

1718  Rather  too  faint  for  measures.    Difficult  in  distance. 

Glimmers. 

17 19  Observation  interrupted  by  clouds. 

1723  It  makes  a  moderately  small  angle  with  the  parallel 

(19°+)-  Mr.  Dunlop's  angle  is  quite  erroneous. 
All  carefully  re-examined  before  unsettling  the 
instrument. 

1724  Very  bad  definition,  working,  a  N.W.  wind  begin- 

ning to  stir. 

1726    Distance  by  patience,  in  intervals  of  clear  sky. 

growing  murky.  Definition  and  steadiness  per- 
fect. 

1729  k  Centauri.  Halley's  comet  close  to  the  star,  and 
almost  in  contact  with  it. 

3  z 


270 


NOTES  TO  ACCOMPANY  THE 


1 73 1  Perfect  steadiness  and  definition. 

1732  Superb  sky,  but  the  stars  furred. 

1735  Found  in  looking  for  A.  151,  which  could  not  be 
found  ;  but  this  star  [which  cannot  be  A.  151] 
stands  very  nearly  in  the  place  assigned  to  that 
object,  and  must  have  been  in  Mr.  Dunlop's  field 
of  view  had  his  instrument  been  really  pointed  to 
that  place. 

1737  Mr.  Dunlop's  position  for  A.  151  is  900  north  from 
parallel,  I  can  find  no  other  double  star  here- 
abouts. 

1740    Bears  a  pretty  strong  illumination. 

1746  Difficult. 

1747  Distance  by  3  oblique  transits. 

1748  Carefully  examined  the  thin  wires.     They  pass 

freely. 

1750  Wolves  howling  very  near,  at  the  end  of  the  south 

avenue  or  in  the  grounds. 

175 1  Excessively  difficult  for  want  of  light   and  the 

necessity  of  magnifying.  Telescope  left  long  at 
rest. 

1752  Very  close — too  difficult  for  this  instrument. 

1754  Found  in  a  fruitless  search  for  A.  170  which  does 

not  exist. 

1755  Distance  too  difficult.     Object-glass  dewed  cer- 

tainly. 

1756  a  Centauri.    The  first  trial  of  the  7-feet  equatorial 

in  its  new  situation  at  Feldhausen.  Tolerably 
steady,  but  ill  defined  ;  between  clouds. 

1757  Well  defined,  but  working  and  not  quite  steady.  B 

is  certainly  greater  than  4  m. 

1758  Fine  definitions  but  tremulous.    A  pale  yellow,  B 

higher  yellow. 

1759  Very  well  defined,  but  unsteady. 

1760  Both  superb  yellow,  inclining  to  orange.  There  is  a 

shade  of  difference.  The  smaller  star  has  cer- 
tainly a  higher  colour  than  the  larger.  Fine 
definition,  but  very  tremulous. 

1761  A  pale  yellow.    B  rather  a  deeper  shade  of  yellow. 

Fine  discs,  but  shuddering. 

i-jbz  The  distances  with  the  inner  edges  of  the  thick 
wires,  the  thin  ones  being  now  utterlg  deranged 
and  useless. 

1763    A  yellow,  B  yellow  inclining  to  brownish  or  orange. 

I  cannot  imagine  finer  measures.  [Inner  edges 
of  the  thick  wires  used,  and  so  continued.  N.B. 
Till  and  inclusive  of  No.  1770.] 

1765  A  yellow,  B  deeper  yellow.    Tremulous  and  bran- 

dishing. 

1766  Working  and  furred. 

1767  Four  oblique  transits  over  a  wire  50  inclined  gave 

1 5  ".8 1  for  the  distance.  But  this  inclination  is 
too  small  for  practical  use. 

1768  A  yellow,  B  pale  orange.    Working  violently,  but 

good  centres. 

1769  The  stars  are  balls,  not  discs,  yet  small  and  well 

concentred,  but  furiously  working  within  then- 
own  limits. 

1770  The  stars  reduced  to  7th,  8th,  &c,  magnitudes, 

until  extinguished  by  dense  cloud. 

1771  The  centres  not  seen,  but  the  stars  work  inwardly 

in  close  rapid  vibrations,  giving  fuzzy  or  bushy 
pellets. 

1772  The  thin  wires  and  cross  zeros  for  distance  resumed. 

Working  and  brandishing. 


1773  A  yellow,  B  brownish-yellow,  a  dull  yellow  inclining 
to  orange.  Very  difficult  to  measure  by  reason  of 
the  great  size  and  brandishing  of  the  discs. 

1777  Fine  definition.  Tremulous,  but  the  measures  ex- 
cellent. 

1779  A  fine  yellow,  B  brownish-yellow.    Working  furi- 

ously and  dilating.  [N.B.  General  note  on  the 
measures  of  a  Centauri  from  No.  1762  to  1770 
inclusive.  The  distances  are  peculiarly  affected 
by  the  change  of  th*  micrometer  ic ires  from  the 
thin  ones  with  cross  zeros,  to  the  thick  with 
inner  contacts,  and  require  a  special  discussion, 
which  see  further  on.~] 

1780  Too  faint  for  good  measures. 
1782    Requires  strong  illumination. 

1786  Full  moon  at  7  a.  m.  this  morning.  Not  a  trace  of 
cloud  in  any  part  of  the  sky,  after  a  fortnight 
calm  cloudy  weather. 

1788  At  first  clear,  but  a  fog  or  light  cloud-drift  from 
S.W.  came  on  after  the  first  2  or  3  measures  of 
position.  A  bright  halo  about  the  full  moon.  It 
cleared  off  and  the  measures  were  completed 
satisfactorily. 

1790  Steadiness  and  definition  perfect. 

1791  Found  while  searching  in  vain  for  A.  174.  Distance 

extremely  difficult  with  the  thin  wires. 

1793  Far  too  difficult  with  this  instrument,  but  certainly 

divided  in  momentary  glimpses. 

1794  Very  difficult  in  distance. 

1795  Barely  discernible  as  a  separated  double  star  with 

No.  2.  Hardly  better  seen  with  No.  3  for  want 
of  light.    Came  on  ill  defined. 

1804    Large  star  ruddy,  small  also  reddish. 

1806  tt  Lupi.    Suspected  with  273,  verified  with  No.  4. 

A  hair-breadth  division,  or  at  least  a  deeply- 
notched  disc  by  glimpses.  Is  of  the  order 
pervicince. 

1807  Excessively  close  and  difficult  star,  but  well  seen 

double. 

1808  I  do  not  think  better  measures  will  be  got  of  this 

star  with  this  instrument.  Disc  distinctly,  in  best 
moments  deeply,  notched. 

1809  Excessively  difficult.    It  is  closer  than  y  Lupi,  for 

the  discs  are  smaller,  and  yet  it  is  not  even  so 
much  divided. 

18 10  Not  sufficiently  well  defined.     Too  early  in  the 

night. 

18 1 1  it  Lupi  is  certainly  far  more  difficult  than  last  year. 

It  was  by  no  means  a  very  difficult  star  when  first 
discovered.  Now  it  is  barely,  but  certainly, 
elongated  "  ex  sequalibus."  [N.B.  However,  in 
this  obs.  the  power  No.  3  =  273  was  used.] 

18 12  Excessively  close,  but  well  separated  with  No.  4, 

and  the  measures  very  satisfactory. 

18 1 3  I  am  not  sure  that  this  star  is  not  closer  than 

y  Lupi.  The  discs  are  smaller,  yet  not  (I  think) 
proportionately  more  separated.  Altogether  it  is 
quite  as  difficult.  A  black  line  of  separation 
seen.    Definition  very  fine,  and  steadiness  perfect. 

18 16  Moon  to  the  eye  full.    (Is  full  by  almanac  at  10 

p.m.  to-morroiv.)    Night  calm,  serene,  and  per- 
fectly cloudless. 

1 8 1 7  Glimmering,  difficult  in  distance  with  thin  wires. 

1 8 1 8  Capital  measures. 


MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


271 


1819  n  Lupi.  No.  3  elongates  it  decisively,  No.  4 
divides  the  discs  clearly  by  a  perceptible  black 
line.  It  is  not  so  close  as  it  or  y  Lupi,  and  is 
much  wider  than  y  Centauri.  Attempted  dis- 
tance by  transits  over  a  wire  8°  inclined,  but 
variable  refraction,  and  the  closeness  of  the  stars, 
rendered  the  result  (3  ".5)  not  worth  registering, 

1824  Pos  of  C  taken  from  the  middle  of  A  +  B. 

1825  Pos  of  C  from  the  middle  of  A,  B.    Distance  from 

A,  reduced  to  middle  by  calculation. 

1826  Pos  and  dist  of  C  from  the  middle. 

1827  Pos  and  distance  both  measured  from  A  (reduced  to 

middle)  so  as  to  render  all  the  measures  compar- 
able inter  se.  [N.B.  The  reduction  to  the  middle 
point  of  A  +  B,  has  been  made  where  needed  in 
the  series  1824,  5,  6,  7,  by  applying  to  distances 
measured  from  A,  the  correction  — o".68,  and  to 
positions  so  measured  the  correction  —  i°  42' 
derived  from  a  general  collection  of  the  whole 
series  of  angles  1819 . .  . .  1827.] 

1828  An  attempt  made  to  measure  the  distance  by  a  pro- 

cess of  repetition,  reading  off  at  once  the  sum  of 
several  distances  between  the  edges  of  the  thick 
wires,  but  it  proved  unavailing. 

1829  Three  measures  of  position  taken,  good,  but  as  they 

went  on  the  star  became  unsteady,  and  I  desisted 
rather  than  spoil  excellent  measures.  Distance 
estimated  at  1  . 

1830  Very  close  and  difficult.    The  4  angles  taken  differ 

inter  se  by  io°  50',  [and  the  diagram  contradicts 
the  mean  102°  56'  so  very  much  that  it  is  impos- 
sible to  allow  any  value  to  the  series,  when 
placed  in  comparison  with  the  other  4  sets.] 

1835  Full  moon  night,  and  (as  usual)  not  a  trace  of 

cloud  in  any  part  of  the  horizon.  A  perfect 
calm.    Steady,  and  well  defined. 

1836  This  may  be  the  star  intended  by  A.  183,  but  I 

cannot  see  his  two  close  stars.  However,  the 
night  is  hazy,  and  definition  bad,  therefore  they 
may  exist. 

1839  Not  seen  triple  ;  but  the  night  is  dull,  and  some- 
times the  ^  Bis  hardly  visible.  If  this  be  not 
A.  184,  that  double  ^  is  not  to  be  found.  [It 
cannot  be  A.  184.    See  f  454.] 

1 84 1  Taken  for  A.  186,  which  it  cannot  be.  Very  dif- 
ficult in  dist. 

1845  Excessively  difficult.    A  distant  star  C  follows,  a 

good  deal  to  the  south. 

1846  Too  difficult.    A  star  8  m  south,  and  5  more,  9  and 

10  m  north. 

1847  Before  the  distances  could  be  completed  a  haze 

came  over  which  put  out  the  small  star. 
1849    Confused  definition. 

1851  I  suppose  this  must  be  A.  186,  if  not,  I  cannot  find 

it.  There  is  a  first  class  double  star  pre- 
ceding this,  and  somewhat  north  of  it,  but  that 
cannot  be  A.  186.  [The  D.  star  alluded  to  is  h. 
477I-] 

1852  Very  difficult  in  distance. 

1853  Distance  by  6  satisfactory  oblique  transits  over  a 

wire  10°  inclined. 

1854  Difficult  in  distance,  owing  to  wind. 

1856    Glimmering.    Very  difficult  in  distance. 

1858  Besides  the  measures  obtained  with  the  thick  wires, 
which  are  always  precarious  (and  which  in  this 
case  gave  n".99  for  the  distance,  certainly  too 
great),  3  oblique  transits  were  procured  over  a 
wire  50  inclined  (too  small  an  inclination"),  which 
gave  10.03.  The  mean  of  both  sets  is  allowed  a 
value  =  2  in  the  reduced  measures. 


186 1  y  Lupi.    No  doubt  remains  as  to  the  elongation 

with  the  highest  power  and  single  eyepiece.  Yet 
the  star  should  be  re-examined.  Unsteady.  Bad 
position. 

1862  A  most  beautiful   double   star,    but  excessively 

close.  However,  perfectly  sure.  A  notched 
disc.    More  separated  than  y  Virginis  now  is. 

1863  Definition  perfect.     More  separated  than  y  Vir- 

ginis. [The  diagram  represents  two  discs  in  close 
contact.] 

1865  No  confidence  in  the  measures.    Elongated,  but  no 

firm  glimpse  to  be  had. 

1866  Being   nearly   in   zenith,    and    tolerably  defined 

(though  restless)  the  measures  are  not  very  bad. 
Much  patience. 

1867  Deeply  notched — all  but  separated,  perfectly  well 

measurable. 

1869  Too  low. 

1870  Deeply  notched.    Will  not  bear  No.  4. 

1871  Too  unsteady.    Almost  exactly  in  the  parallel. 

1872  After  sunrise.      Disc  deeply  cleft,   not  merely 

notched. 

1873  The  direction  is  decidedly  oblique  to  the  parallel. 

1875  A  blank  division  well  and  steadily  seen  with  power 
No.  4,  the  measures  quite  to  be  relied  on.  The 
discs  are  all  but  points,  with  a  division  equal  to 
half  or  one-third  of  a  disc  of  each  star.  Alto- 
gether so  close  that  measures  of  this  star  when 
only  seen  elongated  must  be  very  precarious. 

1877  Certainly  double,  but  very  difficult.  Best  seen 
with  No.  4. 

1880  Too  difficult.  Will  not  bear  illumination  enough 
to  see  the  wire. 

1882  Found  in  looking  for  A.  191,  which  star  it  cannot 
be.  [N.  B.  on  this  (the  south)  side  of  the 
zenith,  the  stars  are  tranquil,  and  steadiness 
perfect.  On  the  other,  variable  refraction  is 
very  troublesome.  The  distance,  as  measured  by 
5  oblique  transits,  and  also  by  the  thick  wires, 
differ  by  no  less  than  7". 2,  whence  it  is  clear  that 
some  great  mistake  must  have  been  made,  and 
both  are  accordingly  rejected. 

1884  Distance  by  3  oblique  transits  over  a  wire  io° 

inclined. 

1885  Too  ill  defined  for  good  measurement  to-night. 

1887  Perfectly  steady  and  well  defined. 

1888  Very  difficult  (<rNormse).  [Another  star  having  by 

mistake  been  taken  for  a  Norma,  some  confusion 
appears  to  have  arisen,  occasioning  a  suspicion 
of  the  zero  having  sustained  some  violent 
change,  but  on  collating  the  other  observations, 
this  is  not  borne  out,  and  the  difference  though 
large,  is  not  more  than  the  excessive  inequality 
of  the  stars  and  feebleness  of  the  companion 
might  well  give  rise  to.] 

1889  No  distance    measurable   by  the   wires.  Four 

oblique  transits  gave  32"-70. 

1895  Mr.  Dunlop's  polar  distance  is  io'  +  in  error. 

1896  Distance  a  mean  of  ii"io  given  by  8  measures  with 

cross  zeros,  and  1 3"-39  by  6  oblique  transits  over 
a  wire  io°  inclined — neither  set  being  good. 

1898  Steadiness  and  definition  perfect.     Measures  ex- 

cellent, but  the  use  of  the  thick  wires  has 
vitiated  the  distance. 

1899  Perfect  steadiness  and  definition.    Distance  by  cross 

zeros  with  the  thin  wires. 

1900  Possibly  NPD  =  1220  32',  in  which  case  the 

star  is  B  5550. 


272 


NOTES  TO  ACCOMPANY  THE 


1901  Distance  by  5  oblique  transits  over  a  wire  io° 

inclined.  Much  fatigued  by  7  hours  uninter- 
rupted work,  and,  in  fact,  unable  to  keep  longer 
awake.  [In  consequence  I  presume  the  oblique 
transits,  which  are  delicate,  and  require  especial 
attention,  to  be  less  dependable  than  usual,  they 
are  accordingly  allotred  only  half  their  value."] 

1902  A  set  of  distances  procured  with  Dollond's  concave 

achromatic  eyepiece,  but  for  want  of  data  they 
cannot  be  reduced. 

1905    Small  star,  ruddy,  and  bears  good  illumination. 

1908  5  Librae  (51  PL)  will  not  bear  No.  4  (400),  but  with 

power  273  it  is  very  well  defined  and  cleanly 
divided. 

1909  Bad  measures  got  by  long  and  patient  attention,  in  a 

sweeping  S.  E.  blast,  allowing  but  very  imperfect 
and  momentary  glimpses. 

19 10  Measured  quite  easily  with  the  highest  power  and  a 

perfectly  satisfactory  set  of  positions. 

19 1 3    Not  the  least  difficulty  to-night  of  getting  the  finest 
measure  the  instrument  is  capable  of. 

19 19  Too  difficult  in  distance.    Requires  the  thick  wires. 

Cross  zeros  used. 

1920  Perfect  calm.  Full  moon  after  rain  the  day  before 

yesterday,  and  a  cloudy  sky  all  to-day.  At  pre- 
sent, sky  cloudless. 

1922  Rather  too  faint  for  good  measures,  especially  in 

distance.    Perfectly  steady,  and  well  defined. 

1923  June  1,  184.6.      New  spider  lines  of  Bermuda 

spiders  put  into  the  micrometer  for  me  by  Mr. 
Maclear. 

1924  Steadiness  and  definition  perfect.    The  small  star  at 

the  end  of  the  measures  had  a  minute  disc  quite 
visible  in  good  illuminations,  though  at  the  begin- 
ning it  was  hardly  more  than  a  sensible  point. 

1926  Wants  light  for  No.  3,  and  is  too  close  for  No.  2. 

Distance  very  rough. 

1927  The  spider  threads  have  relapsed  into  their  old  habit 

of  hitching  in  the  act  of  crossing. 

1929  Distance  by  5  oblique  transits.    Full  moon.  Sky 

perfectly  clear  and  cloud  less.  I  read  small  print 
with  ease  by  its  light.  No  lamp  needed  for  the 
measures.    Definition  good;  steadiness  perfect. 

1930  Extremely  close,    and  will  not  bear  magnifying. 

Distance  too  difficult. 

1931  Excessively  difficult.    Divided,  but  almost  no  in- 

terval with  No.  2.  The  discs  are  points.  Wants 
light  for  No.  3.    Far  too  difficult  for  distance. 

1934  No  measures  of  position  can  be  more  perfectly 

satisfactory.    Double  value  allowed  them. 

1935  Distance  by  8  oblique  transits. 

1937  Steadiness  perfect ;  definition  very  good. 

1938  Steadiness  and  definition  perfect. 
1929    Perfectly  steady  and  well  defined. 

1942  Excellent  definition.     Distance  by  5  very  good 

oblique  transits. 

1943  p  Ophiuchi.    [g  of  former  catalogttcs,  altered  to 

p  by  Mr.  Baily  in  the  Catalogue  of  the  British 
Association.]  Most  beautifully  defined,  and  the 
measures  excellent. 

1947  A  hot  north  wind  suddenly  come  on  has  greatly 

improved  the  definition  of  the  stars,  which  re- 
main  perfectly  steady. 

1948  Perfect  measures. 

1949  The  distance  easy  (in  spite  of  the  faintness  of  the 

small  star)  by  reason  of  its  situation,  exactly  in 
the  meridian. 


1950  Perfectly  steady,  but  glimmering,  and  difficult  in 

distances,  for  want  of  light. 

195 1  Distance  between  thick  wires.    Tried  oblique  tran- 

sits, but  variable  refraction  proved  too  trouble- 
some, and  defeated  the  attempt. 

1952  In  taking  the  set  of  distances,  found  the  right  hand 

thread  to  move  by  visible  jerks.  Altered  the  zero 
40  divisions,  and  worked  with  the  other  wire. 
The  jerks  were  thus  obviated,  and  a  dependable 
set  of  distances  procured  with  cross  zeros. 

1953  Well  defined  and  perfectly  steady,  but  bears  no 

illumination,  and  is  excessively  difficult  in  distance. 
1 9  54  Distance  by  five  oblique  transits  over  one  of  the  thick 
wires,  while  the  other  was  so  placed  as  just  to 
obscure  the  large  star  at  the  moment  of  the  small 
one  emerging  from  behind  the  transit  wire  (the 
emergences  being  noted).  [Tt  would  appear  that 
this  method,  as  might  indeed  be  expected,  gives 
results  in  excess.] 

1955  Three  oblique  transits  taken,  but  too  difficult ;  the 

moon  being  too  bright.  Moon  nearly  full,  and 
a  lunar  rainbow  seen  on  the  dewed  herbage. 

1956  Five  oblique  transits.     A  third  star  much  closer 

violently  suspected,  nearly  south. 

1957  Three  not  very  satisfactory  oblique  transits. 

1958  Found  in  looking  for  A.  205  (which  it  cannot  be). 

There  is  no  double  star  in  Mr.  Dunlop's  place. 

1959  No  star  near  answering  the  description  of  A.  205. 

Steady  and  well  defined. 

196 1  Hot  north  wind  with  occasional  cold  blasts — and 

the  definition  of  the  star  alternately  good  and  bad, 
but  not  unsteady. 

1962  The  chief  star  of  a  cluster. 

1963  Found  in  looking  for  A.  208,  which  does  not  exist, 

unless  this  be  it ;  but  the  descriptions  disagree, 
and  it  cannot  be  the  same.  Distance  by  three  ob- 
lique transits.    Very  difficult. 

1965  Too  faint  and  difficult  for  a  good  determination  of 

distance. 

1966  Very  coarse.     Sixth  class.    Stars  perfectly  steady 

under  the  healing  influence  of  a  hot  north  wind 
which  has  just  set  in. 

1968  The  measures  taken  with  the  lowest  power  No.  1 

(=  79).  [N.B.  This  is  too  low  for  measure- 
ments of  distance  by  the  thick  wires  without 
cross  zeros,  and  accounts  for  the  enormous 
excess  in  the  reduced  distance.  The  observa- 
tions must  be  rejected.] 

1969  Clouded  before  the  measures  of  distance  could  be 

finished,  and  those  obtained  too  imperfectly  seen 
to  have  any  value. 

1970  Surely  this  star  must  have  changed  in  distance. 

197 1  Stars  superbly  defined  and  steady,  rendering  the 

measures  easy,  in  spite  of  the  great  difference  of 
magnitudes. 

1972  Imperfect  measure,  owing  to  flitting  cloud  and  in- 

distinctness. 

1975  Distance  by  five  very  good  oblique  transits. 

1976  Too  difficult  for  measures  of  distance. 

1977  Distance  too  difficult  for  this  instrument. 

1978  A  new  set  of  spider  lines  adapted  to  the  micrometer 

by  Mr.  Maclear  which  do  not  hitch.  [  The  first 
set  applied  by  him,  June  3,  did  not  prove  quite 
satisfactory.] 

1979  A  very  symmetrical  little  constellation  of  two  large 

and  three  very  minute  stars,  12  m,  forming  a 
pentagon  somewhat  elongated  in  a  direction  per- 
pendicular to  the  two  large  stars  at  its  base. 


MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


273 


1983 


1985 


1987 


1989 

1990 

1991 

1992 
1993 
1994 

«995 


Two  sets  of  distances  obtained,  one  with  the  thick 
wires  and  without  cross  zeros,  and  therefore  pre- 
carious (i7".66);  and  one  by  5  oblique  transits 
(i5".72)  much  more  to  be  relied  on. 

Though  I  have  scarcely  a  doubt  about  the  existence 
of  the  companion,  it  is  far  too  difficult  to  get 
measures  with  this  instrument.  [N.B.  This  ob- 
servation was  never  verified,  and  from  subse- 
quent consideration  of  several  similar  cases 
there  is  reason  to  believe  the  small  star  to  have 
been  an  illusion,  for  which  reason  I  have  not 
entered  it  in  the  general  catalogue. 

As  perfectly  denned  and  as  good  measures  as  it  is 
possible  to  get.    This  star  has  changed. 

I  do  not  suppose  finer  measures  can  be  had.  The 
stars  heave  together  by  refraction  without  relative 
motion. 

Not  far  from  the  moon,  and  an  oceultation  ex- 
pected. The  threads  hitch  abominably.  Zero 
changed  one  revolution,  but  still  has  same  fault. 
[In  consequence  only  one  half  the  registered 
weight  allowed  to  the  distance.) 

The  preceding  of  two  double  stars  in  the  field 
together. 


Very  difficult, 
favourable. 


yet   all  circumstances  perfectly 


The  following  of  two  double  stars  ;  all  circumstances 
perfect. 

All  circumstances  perfect. 

Very  difficult  in  distance  with  the  thin  wires. 

Object  glass  much  dewed  internally.  Very  difficult 
in  dist. 

A  very  coarse  double  star,  of  which  the  place  agrees 
with  A.  216,  but  the  other  particulars  differ  com- 
pletely. The  large  star  is  a  close  double  star, 
hitherto  undescribed. 

2001  Distance  of  A  C  by  5  differences  of  R  A,  mean  = 
7s-37.  Mr.  Dunlop  makes  the  diff.  of  R  A  in  his 
star  No.  216  to  be  1 5 5 .  [Yet  the  places  agree, 
and  there  is  no  other  near.'] 

2003  Bears  strong  illumination. 

2004  One  of  the  most  difficult  double  stars  [for  this 

instrument]  in  the  heavens.  Certain  of  its  being 
double.  The  definition  is  perfectly  beautiful.  No 
rings  or  appendages  whatever — a  mere  lambent 
quiet  disc,  with  a  point  beside  it. 

2005  Seen  double  with  No.  2 ;  better  with  No.  3  ;  best 

with  No.  4.  Well  separated,  and  quite  sure. 
No  doubt  whatever.    Extremely  difficult. 

2007  Very  difficult.    [N.  B.    The  thick  wires  are  ad- 

mirable for  these  difficult,  distant  stars.  The 
distance  was  obtained  with  more  ease  than  the 
position. 

2008  Distance  by  6  differences  of  R  A. 

2009  Very  difficult  in  distance.    Thin  wires  and  cross 

zeros. 

201 1    Distance  by  5  differences  of  R  A. 

20 14  }  The  R  A  and  P  D  of  this  star  as  read  off  and  set 

2015  i    down  in  this  obs  are  16'' 48™'  39s  and  i2o°3i'. 

But  the  star  has  been  repeatedly  looked  for  since 
in  that  place,  without  success.  A  mistake  of  20' 
in  declination  (easily  committed)  and  i'1  in  R  A 
brings  it  to  coincidence  with  No.  450  of  John- 
son's Catal.,  in  a  review  of  which  Catal.  the 
latter  was  seen  double,  and  measured  June  18, 
1837  (No.  2015.)  On  a  collation  of  all  the 
observations,  the  identity  of  both  with  h.  5003 
can  admit  of  no  doubt. 


2016  Every  circumstance  eminently  favourable. 

2017  Do.  Dist  by  thin  wires  and  cross  zeros,  but  the  illu- 

mination is  not  sufficient  to  give  perfect  mea- 
sures of  distance. 

2019  Discovered  in  a  review  of  large  stars.  Distance 

certainly  below  1",  but  seen  double  with  279. 

2020  Fairly  elongated,  but  not  divided  with  279.  No 

dependence  on  the  measures,  —  the  night  be- 
coming bad. 

2021  Elongated  with   No.  3,  but  hardly  measurable. 

With  No.  4,  a  black  division  like  a  train  is  seen 
in  momentary  glimpses. 

2022  Excessively  close  and  difficult. 

2023  A  superb  observing  night  after  three  days'  rain. 

Every  condition  of  observing  perfect. 

2024  Excellent  definition,  but  tremulous. 

2025  Distance  by  10  oblique  transits. 

2026  Well  defined,  but  refraction  variable. 

2127  Distance  by  11  oblique  transits. 

2028  111  defined.  Before  the  distances  were  taken  it 
suddenly  grew  so  furred  that  I  could  no  longer 
distinguish  the  two  stars. 

2031  All  conditions  perfect. 

2032  Very  difficult  in  distance. 

2034  Vicinse,  difficillima.    Discovered  with  No.  3,  but 

only  a  violent  suspicion,  which  No.  4  positively 
verified,  showing  the  small  star  well  separated, 
but  it  requires  a  capital  night.  The  larger  and 
most  southern  of  two. 

2035  Bears  some  illumination.    Small  threads  used  for 

distance  ;  large  ones  for  position. 

2037  No.  2  not  powerful  enough.    No.  3  wants  light. 

Not  well  defined. 

2038  Pos  between  the  thick  wires.    Three  measures  of 

pos  procured  by  the  horizontal  wire  alone  gave  a 
mean  3030  57',  but  this  I  reject,  as  the  stars  are 
too  minute  to  be  brought  into  comparison  with  a 
single  spider  line. 

2039  111  defined  ;  a  south-easter  having  most  unexpectedly 

and  suddenly  come  on  (after  a  very  short  lull) 
upon  the  shoulders  of  a  warm  north  wind,  con- 
tradicting all  expectations. 

2040  Distance  by  4  oblique  transits. 

2042  All  conditions  favourable. 

2043  Dunlop's  R  A  is  18  4  46.   There  is  no  other  double 

star  preceding  in  R  A.    Well  examined. 

2045  Examined  the  revolutions  of  the  screw  in  distance, 

as  Mr.  Dunlop  makes  the  distance  40".  Found 
all  right. 

2046  Used  the  thin  wires  and  an  adjusted  zero  without 

crossing. 

2047  Good  definition  and  perfect  steadiness.    Nine  dis- 

tances taken. 

2048  Over  the  Table  Mountain.    Blotted  and  dim,  so  as 

sometimes  hardly  to  be  seen. 

2049  Dull  cirro-cumular  streaks  on  star.    No  getting  a 

distance. 

2050  Distance  particularly  good,  owing  to  the  very  fa- 

vourable angle  of  position. 

2052  Distance  by  two  excellent  series,  viz.,  2i".22  by 
cross  zeros  by  motion  of  a  single  wire  in  decli- 
nation— (the  small  star  being  nearly  in  meridian) 
the  single  thread  being  set  to  zero — and  21.76  by 
the  usual  method  of  cross  zeros. 

2054    All  conditions  perfect,  vet  difficult  in  distance. 

4  A 


274 


NOTES  TO  ACCOMPANY  THE 


2055  Distance  by  3  oblique  transits. 

2056  The  wires  hitching  in  the  measures  of  distance 

(mean  =  82"-33)  a  set  of  differences  of  R  A,  three 
in  number,  whose  mean  are  83".oo.  The  mean  of 
both  sets  adopted. 

2057  A.  224.    N.  B.  Looked  well  for  A.  223,  all  round 

2  fields  +  and  —  in  R  A  and  declination.  No 
such  stars  to  be  found.  [Dist  83.56  by  A.  RA 
7  9".  54  was  obtained  by  3  measures  with  the  thick 
wires.  The  star  being  very  coarse,  it  is  probable 
that  the  measures  were  somewhat  roughly  taken, 
and  their  mean  is  accordingly  unscrupulously 
adopted.] 

2059  Extremely  close  and  difficult.    In  a  worse  night 

measures  would  be  impracticable.  At  present 
every  condition  is  perfect. 

2060  Very  close;  273  is  hardly  power  enough,  but  the 

night  will  not  bear  power.  Tried  No.  4.  Worse 
defined,  but  better  separated,  and  measures 
better. 

2062  Detected  in  a  review  of  ASC.    The  hitching  of  the 

threads  very  bad  in  distance.  Obliged  in  conse- 
quence to  reject  the  result. 

2063  Unsteady,  and  at  length  growing  ill  defined. 

2064  Position  excellent,  but  grew  very  ill  defined  before 

distances  could  be  got. 

2066  Threads  move  by  jerks. 

2067  Very  doubtful  measures  ;  stars  convulsed,  and  discs 

dancing  in  flare. 

2069    The  northern  star  of  y  Corona;  Aus,  is  a  mere  trifle 
the  smaller  of  the  two. 

2075  Most  dreadfully  ill  defined,  a  violent  struggle  going 

forward  between  the  regular  S.  E.  wind  and  a 
hot  north-wester  which  is  coming  on. 

2076  Very  ill  defined  and  tremulous.     The  first  fine 

night  after  several  days'  rain.  Calm  and  clear. 
Therm.  470  Fahr. 

2077  Excessively  difficult,  yet  I  feel  convinced  it  is 

double.  [N.  B.  After  all,  there  remains  some 
degree  of  suspicion  attached  to  this  star,  the 
quadrant  being  s  f  in  which  an  illusory  appendage 
has  been  frequently  observed.] 

2078  No  appendage  observed  to  the  distant  star  C,  7  m. 

Distance  by  a  single  difference  of  R  A,  pos  by  a 
single  measure. 

2079  Glimmering ;  will  not  bear  high  powers  ;  No.  2 

answers  best. 

2081  Full  moon  at  10  p.m.  Calm,  serene,  and  per- 
fectly cloudless.  The  distance  is  assuredly 
greater  than  4".    I  should  estimate  it  at  6". 

2083  Too  close  and  faint  for  the  power  used,  No.  2,  but 
will  not  bear  No.  3. 

2085  Large  star,  pale  yellow  ;  small  one,  pale  blue. 

2086  Dist  by  5  differences  of  R  A.    Yellow  and  pale 

blue. 

2087  Distance  by  7  oblique  transits  as  a  trial  of  the 

method  [since  so  often  used] .  The  calculation  is 
troublesome,  but  the  method  seems  to  be  beau- 
tifully exact,  provided  the  zero  of  the  micro- 
meter be  well  secured.  Result  =  22".63  (4). 
Ditto  by  3  measures  between  the  thick  wires 
24.15  (1).  —  mean  22.93  (5). 

2088  No  dependence  on  the  distance,  as  the  threads 

drag — an  evil  which  must  be  cured.  All  other 
conditions  perfect. 


2090  The  fine  threads  being  now  quite  deranged,  the 
system  of  measurement  by  interior  bisections  and 
contacts  of  the  coarse  ones  was  commenced 
(July  20,  1834).  The  place  agrees  nearly  with 
that  of  R.  25,  but  it  is  not  the  same  double 
star. 

2092  At  first  well  defined,  but  grew  faint  and  so  con- 
fused that  dew  was  suspected  on  the  object  glass — 
and  so  it  proved. 

2094  Distance  by  10  oblique  transits  io".35.  By  5  direct 
measures  between  the  thick  wires  (duly  cor- 
rected) io".33. 

2096    Mr.  Dunlop's  place  is  a  degree  erroneous  in  P  D. 

2099  Distance  by  a  mean  of  5  oblique  transits  over  a 
wire  4°  55'  inclined,  carefully  observed  —4". 3 7  ; 
by  two  measures  between  thin  wires  duly  cor- 
rected 4".44. 

2 io  1  Distance  by  6  oblique  transits  over  a  wire  50  9' 
inclined  =  21". 24.  By  2  measures  with  thick 
wires  2i".58. 

2102  Distance  by  10  oblique  transits  over  a  wire  10°  in- 

clined =  22".43.  By  5  measures  with  thick 
wires  23'  .8o. 

2103  All  conditions  excellent. 

2104  Dist  by  7  oblique  transits  at  io°  inclin.  =  6".07  ; 

by  a  single  measure  with  thick  wires  6".o8. 

2105  Measured  with  the  "  macro-micrometer." 

2107  Distances  taken  with  half  the  object  glass  inter- 
cepted by  the  roof. 

2109  While  taking  the  distances,  detected  again  the 
spider-lines  hitching  in  the  act  of  crossing.  In 
consequence  took  10  measures,  crossing  each  time 
to  observe  and  destroy  the  effect.  On  the  whole 
they  were  found  to  return  by  their  elasticity  very 
nearly  to  the  same  places,  so  that  the  effect  on 
the  distance  is  not  formidable.  Mean  8".04  (2). 
Dist  by  4  oblique  transits  at  io°  =  7 ".72  (2). 

2112  Dist  by  4  measures  with  thick  wires  =  58".86  (1)  by 
10  oblique  transits  6o".5i  (3)  the  stars  not  lying 
favourably. 

2 1 14  The  threads  still  hitch,  and  as  they  now  affect  the 

zero  when  they  cross,  no  reliance  can  be  placed  on 
the  distance. 

21 15  9  Indi.    Detected  in  the  course  of  renew.     [N.  B. 

This  *  is  not  in  AS.  Cat.  thoughNo.  2533,  which 
is  not  5  m,  but  7.8,  is  very  near  it,  and  in  the 
field  of  the  finder.] 

21 16  Growing  unsteady,  and  reeling.    No  distance  could 

be  got. 

21 17  Difficult;  but  the  small  star  certain!//  seen  and 

measured.  In  a  perfectly  good  night  this  would 
be  a  very  elegant  object. 

2118  Bears  illuminating.    Sometimes  finely  seen. 

2119  Excessively  difficult;  a  20-feet  object.     Only  a 

single  rude  measure  of  distance,  of  no  sort  of 
value. 

2120  Distance  by  5  differences  of  R  A. 

2 12 1  Extremely  difficult.    The  small  star  not  to  be  seen 

with  179,  and  barely  with  273.  Measured  with 
400,  which  shows  it  certainly,  but  no  measure  of 
distance  could  be  got. 

2123  Detected  in  a  review  (\  Octant  is).    Bears  strong 

illumination.    Unsteady,  twirling. 

2124  No  doubt  about  the  star  being  double,  but  it  is 

difficult  and  delicate,  and  the  low  situation  makes 
it  hard  to  see  and  measure,  but  it  bears  a  good 
illumination.    Twitching.    Tolerably  defined. 


♦ 


MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


275 


2125  A  difficult  star,  from  the  low  situation  and  atmo- 

spheric affections.  To-night  well  seen,  though 
a  good  deal  plagued  with  appendages. 

2126  A  third  star  Cum  near.— [  ?  if  P  D  he  not  rather 

1070  5'.] 

2127  Distance  by  4.  measures  with  thick  wires  52.21  (1)  ; 

by  6  differences  of  R  A  49.83  (1). 

2129  All  circumstances  favourable.     Distance  by  5  good 

measures  with  thick  wires  i<)"-77  (2)  ;  by  5  ditto 
oblique  transits  at  io°  inclination  =  3o".67  (3). 

2130  Very  difficult. 

2132  Will  bear  no  illumination.    One  rough  reading  of 

distance  only  got. 

2133  Extremely  difficult.    A  3rd  9  m  or  8.9  about  2' 

distant.    105  shows  it  nicely  double. 

2134  Extremely  difficult.    An  object  for  20-feet.  Want- 

ing light.    Ill  denned. 

2135  Too  difficult.    A  20-feet  object.    Only  seen  double 

by  momentary  ghost-like  glimpses.  Only  a  single 
reading  [it  cannot  be  called  a  measure]  of  posi- 
tion obtained  [of  no  value']. 

2139  Close  and  difficult.    Distance  excessively  so. 

2140  Twirling  and  ill  denned. 

2142  Measures  perfectly  satisfactory. 

2143  A  good  star  for  No.  1.    (Power  105),  and  easily 

measured.    All  good. 

2144  Oblique  transits  attempted,  but  spoiled  by  variable 

refraction. 


2145 


2146 


2148 


2151 


2153 


May  be  pretty  well  measured  with  patience,  but 
requires  a  perfect  night,  considerable  power  (as 
273)  and  light  in  field. 

Stars  ill  defined  and  unsteady,  generally,  but  with 
perfect  intervals.  Waiting  patiently  for  these 
the  measures  are  not  difficult. 


Distance  by  3  measures  with  thick  wires  60.63(1)  ; 
by  3  oblique  transits  at  io°,  6i".49(2). 

2 149  A  rare  opportunity  and  perfectly  taken  advantage  of. 

2150  The  wires  hitch  in  crossing,  [but  return  to  their 

places  by  elasticity,  as  is  evident  on  comparing 
the  +  and  —  readings.] 


Distance  by  6  measures  between  thick  wires  4.88(1), 
by  16  oblique  transits  at  inclination  5°,  4.01(4). 

Distance  by  3  thick  wire  measures  30.23(1)  ;  by  4 
oblique  transits  over  the  thick  wire  27.29(2). 


2154    Most  wonderful  definition  and  perfect  steadiness. 

21^ 

2158  j 


156  ^Some  great  confusion  about  the  measures  in  distance 

157  J-    ofAB.    2156  by  2  oblique  transits  gave  8  5".  3 1. 
No.  2157  by  a  single  A  R  A  3'.o  =  116.69,  but  it  is 


remarked  that  the  definition  was  very  bad  ;  while 
again,  No.  2158  by  6  differences  of  R  A  (2'. 65) 
gave  98".28.  The  great  angle  of  position  (830 
with  the  parallel),  however,  renders  the  method 
of  differences  of  R  A  liable  to  enormous  errors, 
while  it  favours  the  oblique  transits.  Both  the 
former  are  therefore  rejected.  Yet  I  cannot  help 
suspecting  some  mistake  in  setting  the  wire  for 
the  latter,  and  in  consequence  attribute  no  value 
to  the  result. 

2162  All  conditions  perfectly  good. 

2163  Detected  in  a  review.    Tangibly  certain,  but  would 

be  impossible  to  measure  under  less  favourable 
circumstances  of  sky,  steadiness,  and  definition. 
Bears  strong  illumination.  The  small  star  is 
quite  beyond  the  rings. 

2164  The  smallest  point  imaginable. 

2165  The  description  of  A.  244  might  suit  this  star,  but 

there  are  18'  of  difference  in  declination. 

2167  Measured  with  Dollond's  macro-micrometer  eye- 

piece. Threads  hitch  in  crossing.  The  measures 
of  distance  not  reducible  for  want  of  data. 

2168  Irregular  motion  of  the  thin  threads  in  measures  of 

distance  avoided  by  a  peculiar  management  of  the 
micrometer. 

2169  All  conditions  of  good  observing  perfectly  satisfied. 

2171  Distance  5  by  thick  wire  measures  =  i5".5o(i),  by 
7  oblique  transits  at  io°  —  14.74(3). 

2176  y  Tucanse  precedes  69'.$  ;  position  of  the  double 
star  from  y  =  in0  15'.  A  star  10  m  nearly  in 
the  line  B  A  prolonged. 

2179  Distance  by  4  thick  wire  measures  i6".8i(i);  by  5 
oblique  transits  at  io°,  i6".56(2). 

2 1 3 1    All  conditions  of  observation  perfect. 

2182  A  violent  suspicion  that  the  large  star  is  close 

double.  In  good  glimpses  I  can  hardly  doubt  it. 
[The  companion,  if  it  exist,  is  8' m,  and  almost 
exactly  following  by  diagram.] 

2183  Exactly  in  the  parallel,  so  as  to  allow  no  motion  of 

the  wire  without  destroying  the  measure.  Most 
carefully  examined  in  every  way. 

2184  All  conditions  satisfied. 

2185  Measures  of  distance  by  the  thick  wires  but  with 

cross  zeros.  It  will  not  bear  illumination  enough 
for  the  spider  thread. 

2186  Moon  approaching  the  full.    A  very  fine  calm  clear 

night. 

2188    Distances  good  for  little  as  the  wires  jerk. 
2191    All  conditions  perfect. 

2193  Moonlight  too  strong  for  the  measures. 

2194  Extremely  difficult  except  in  so  fine  a  night  as  this. 


276 


SYNOPSIS  OF  THE  RESULTS  OF  THE  MICROMETPJCAL  MEASURES 

OF  DOUBLE  STARS. 


No. 

Name  of  Star. 

R  A. 
1830.0. 
h.  m. 

N  P  D. 
1830.0. 

0  / 

Magni- 
tudes. 

Anfjte  of 
Position. 

Epoch 

1810+ 

Value. 

Distance. 

Epoch 

Value. 

I 

0 

5 

108  6 

7'  8 

345-8 

6.56 

10 

67.59 

6.64 

8 

2 

0 

24 

*53  54 

5  =  5 

172.2 

5-71 

13 

27.72 

5-79 

15 

3 

O 

25 

Iz5  55 

6'  9 

164.2 

5.22 

8 

6.45 

545 

4 

4 

0 

26 

146  16 

6'  11 

247.6 

7.27 

5 

7.60 

7-35 

4 

5 

0 

38 

132  50 

8'  9 

63.0 

6.01 

6 

8.95 

7.20 

4 

6 

0 

46 

160  26 

7  8 

79.2 

6.78 

13 

21.25 

6.83 

14 

7 

O 

5° 

106  34 

7  —  7' 

32.0 

5.81 

9 

6.65 

6.99 

5 

8 

0 

5° 

151  0 

8  =  8 

126.8 

6.15 

9 

5-33 

6.40 

9 

9 

I 

1 

146  9 

5'  10 

244.0 

5.89 

5 

6.27 

5-7i 

2 

10 

I 

9 

103  12 

8'  9 

352.7 

7.80 

2 

8.05 

7.80 

2 

ii 

I 

10 

'59  47 

6  10 

16.4 

6.75 

5 

4-75 

6.82 

3 

12 

I 

11 

157  18 

6'  10 

347-5 

7.02 

3 

2.52 

7-74 

1 

l3 

I 

12 

106  41 

8'  9 

40.4 

6.54 

3 

1.82 

6.96 

2 

14 

I 

20 

108  9 

7  9 

245.2 

6.35 

4 

13.00 

6.64 

4 

15 

I 

28 

120  47 

6  7 

75-5 

7.11 

5 

3.12 

7-51 

4 

16 

I 

32 

144  18 

7'  8 

104.6 

6.28 

6 

10.46 

6.28 

2 

l7 

I 

33 

'47  3 

6'=  6' 

122.3 

5.00 

10 

3-65 

5.00 

10 

18 

I 

33 

102  7 

6  8 

86.9 

7.80 

3 

4.65 

7.80 

2 

19 

I 

38 

ri5  54 

6  10 

69.6 

6.54 

5 

5-53 

6.70 

4 

20 

I 

42 

129  12 

6  10 

70.9 

7.81 

1 

2.25 

7.81 

0 

21 

I 

5° 

151  8 

7  7 

37-6 

7.38 

6 

3-35 

7.24 

6 

22 

2 

2 

120  27 

8  9' 

63.5 

7.01 

2 

89.16 

7.01 

1 

23 

2 

7 

152  27 

9  9' 

134.8 

5.84 

4 

5-83 

6.20 

3 

24 

2 

*3 

121  7 

8  9 

268.5 

6.91 

4 

747 

7.09 

5 

25 

2 

26 

118  59 

5'  8 

241.7 

6.34 

8 

11. 15 

6.34 

8 

26 

2 

28 

133  44 

9'  10 

9.7 

6.75 

3 

4.33 

6.64 

0 

27 

2 

32 

135  27 

7'=  7' 

7.6 

6.84 

3 

97.26 

6.84 

3 

28 

2 

35 

120  17 

8  8 

94-7 

7.01 

2 

62.74 

7.01 

4 

29 

2 

36 

121  48 

7  11 

56.6 

4.78 

1 

15.— 

4.78 

0 

30 

2 

37 

'31  15 

7'=  7' 

43.2 

6.65 

7 

1.47 

6.81 

7 

31 

2 

37 

116  15 

6'  9 

185.1 

6.29 

4 

1 1. 16 

6.59 

5 

32 

2 

51 

115  40 

7  7' 

221.4 

5.90 

3 

28.62 

5.90 

2 

11 
j  j 

2 

5* 

130  59 

5  6 

81.5 

5.80 

10 

8.68 

5.73 

6 

^4 

2 

58 

141  59 

7  8 

70.7 

7.94 

2 

37.31 

7.94 

2 

3 

5 

119  40 

3'  8 

310.0 

6.23 

6 

5.30 

6.40 

4 

■36 

J 

3 

9 

154  57 

8'  9 

328.8 

6.90 

3 

48.38 

6.90 

2 

J  / 

3 

11 

log  6 

5  9 

1 10.4 

5.81 

4 

5.77 

5.76 

1 

38 

3 

12 

155  4 

7  9' 

102.3 

6.41 

6 

19.70 

6.57 

3 

iy 

3 

J9 

I16  14. 

7  0 

j  j  j 

6.66 

6 

4.00 

6.85 

8 

3 

20 

141  40 

7  10' 

42.1 

5-34 

6 

31.55 

5.91 

1 

41 

a.  is   

3 

34 

130  55 

7  8 

326.6 

6.02 

10 

8.81 

5-75 

6 

42 

3 

35 

150  20 

7'  8 

269.9 

6.01 

5 

59.28 

6.84 

1 

43 

3 

38 

131  12 

7  11 

344-8 

7.07 

2 

6.58 

7.07 

44 

3 

40 

144  48 

6  10 

"•3 

6.99 

6 

5.98 

6.99 

4 

45 

3 

42 

128  9 

5  5' 

199.7 

6.48 

7 

8.55 

6.57 

6 

46 

3 

42 

122  18 

8  =  8 

136.3 

6-54 

5 

10.15 

6.72 

5 

47 

3 

59 

126  18 

I'  9 

112. 8 

7.92 

3 

10.34 

7.92 

3 

48 

4 

6 

I24  12 

8  10 

3°3-7 

7.92 

3 

29.79 

7.92 

3 

49 

4 

6 

126  36 

7  7 

50.0 

8.08 

2 

5o-5i 

8.08 

2 

5° 

4 

8 

I20  30 

8  10 

161. 9 

6.45 

4 

11.00 

6.63 

3 

5i 

4 

10 

'35  3 

9,  9 

148.3 

6.36 

5 

12.87 

6.56 

3 

52 

4 

13 

152  37 

5  12 

289.6 

6.96 

1 

6.90 

6.96 

1 

53 

4 

13 

124  17 

7  10 

157.6 

7.89 

4 

5.78 

7.90 

5 

54 

4 

16 

153  40 

5'  9 

6.1 

5.60 

5 

6.40 

6.15 

3 

55 

4 

21 

147  28 

7'  8 

231.8 

6.93 

6 

7.10 

6.93 

6 

56 

4 

21 

130  55 

7  9' 

1 84. 1 

6.91 

4 

4-95 

6.91 

4 

57 

4 

28 

115  23 

7  11 

189.7 

7-95 

2 

22.42 

7-95 

1 

58 

4 

3° 

145  24 

3  11 

108.5 

6.01 

2 

82.29 

6.01 

1 

59 

4 

34 

119  54 

9  =  9 

170.9 

6.42 

4 

11.75 

6.59 

3 

60 

4 

34 

135  22 

8  10 

327.2 

6.48 

4 

42.04 

6.64 

3 

61 

4 

38 

149  17 

8  =  8 

81.2 

6.40 

6 

3. 82 

6.50 

5 

62 

4 

44 

135  27 

8  10 

62.0 

6.63 

3 

5-79 

6.01 

1 

63 

4 

47 

115  26 

9  10 

22 1. 0 

6.96 

4 

20.99 

6.96 

4 

64 

4 

47 

143  45 

5'  6' 

57-9 

4-97 

6 

12.3S 

4.98 

7 

65 

5 

7 

122  7 

8  =  8 

150.8 

6.40 

5 

7-59 

6.61 

3 

SYNOPSIS  OF  RESULTS  OF  MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


277 


R  A. 

NP  D. 

Magni- 

Angle of 
f  osi  t  ion. 

Epoch 

Epoch 

a? 

No. 

Name  of  Star. 

1830.0. 
h.  m. 

1830.0. 
0  / 

tudes. 

18304- 

*> 

Di  E  tatice. 

18304- 

"5 
f» 

65 

Ri<rpl 

5 

7 

98  24 

I 

8 

6  AZ 

IO 

9-4- 

6.63 

*° 

6-7 

5 

9 

103 

32 

6 

10 

I  I  7  .  C 

<  08 

A 
4" 

4.2  7 1 

c  08 
3-y° 

68 

5 

12 

124 

12 

i 

10 

1 66.2 

8.01 

7 
3 

11^2 

8.04 

6n 

°9 

,  7 

5 

12 

IOS 

42 

7 

7' 

18.0 

7.  CO 

6 

3y,w3 

7  c6 

7 

7° 

5 

14 

123 

34 

9 

10 

1  t  n  7 

7  Oft 

C 

J 

23.09 

7.09 

4 

7i 

5 

15 

114 

57 

6 

9' 

I  10.3 

7  ^  /I 
/  TT 

C 

J 

3-5  3 

7-35 

7 

Do  AC   

6 

9 

106. 1 

7.33 

I    J  3 

6 

58.81 

7.27 

4 

72 

5 

J9 

109 

5° 

6 

9 

3  I  C..2 

7.0  C 

/  -y  3 

7 

28.70 

70c 

/ 

1  3 

5 

20 

125 

30 

7 

7' 
6' 

22  1.3 

5.68 

4- 

7.32 
/  3 

3  4-^ 

74 

5 

21 

142 

28 

6' 

28 c  0 

6 

3  8.20 

6.64 

4 

75 

5 

25 

137 

r3 

g 

I  I 

226.5 

6.58 

1 

i 

20.  — 

76 

5 

25 

J37 

'3 

6 

7 

264. 1 

7. 02 

1 

IQ7. 1  C 

y  /  *  3 

6.92 

1 

77 

5 

26 

132 

20 

7 

8 
9' 

171. 8 

6 

8.46 

A  08 

5 

7° 

5 

30 

x45 

I 

6' 

3AO  1 

A  O  C 
T"'7  J 

J 

51.82 

/I  n  c 

/y 

5 

32 

92 

3 

2 

6 

IJ.7.Q 

T*  /  y 

6.96 

2.76 

6.96 

A 
T 

80 

5 

40 

136 

22 

8 

9 

1  7  C  A 
1  /  3"+ 

6.OI 

co  co 

81 

5 

42 

J34 

55 

7' 

10 

I  I4.O 

6.c6 

C 
J 

IQ.08 

6.0  3 

-y  3 

82 

5 

54 

121 

4 

9  : 

=  9 

I  30.  C 

6.86 

IO 

4-84. 

6.o  c 

y  3 

y 

8? 
°3 

6 

0 

138 

26 

8  : 

=  8 

I63.O 

6  I  "3 

c 

J 

3.86 

5 .02 

84. 

6 

12 

'55 

29 

7' 

8' 

I  I  A..Q 

6.l6 

7 

2I.52 

62c 

1 

8c 

6 

149 

8 

6 

7' 

224.  I 

6.50 

6 

C  C  7  C 

6 

5 

86 

6 

14 

129 

*5 

6' 

7 

C2.  3 

7.70 

A 

T" 

7  O  A 1 

7  7n 

4 

87 
88 

Vi  i%ci   

6 

18 

126 

38 

5' 

7 

66.2 

8.00 

f 

J 

6n  C/l 

8.00 

5 

6 

24 

130 

16 

6' 

6' 

1 10.2 

8.09 

2 

7 1. 00 

8.09 

8q 

6 

26 

140 

7 

6 

8' 

■3  17  8 

3-v* 

C 
J 

7  7  67 
1  3-u  3 

5-27 

3 

90 

6 

34 

138 

4 

5' 

7' 

inn 

5.92 

8 

7  7  /i  n 

6.3 1 

7 

91 

6 

36 

130 

1 1 

9' 
6' 

10 

104.7 

5-99 

c 
5 

17.25 

.01 

2 

92 

6 

36 

128 

H 

8 

5.41 

r 
3 

847 
0.43 

5-35 

3 

93 

h  3889 

6 

39 

140 

17 

6' 

8' 

266.1 

6, 50 

6 

^c'02 

6.78 

4 

94 

h  389 1 

6 

39 

120 

47 

6 

10 

222.0 

8.00 

c 

7-97 

5 

95 

A  78 

6 

59 

'33 

23 

6 

7' 

5.96 

20.39 

5-9^ 

2 

ofi 
9° 

6 

59 

124 

31 

6' 

8' 

1 57-7 

6.60 

7 

5-39 

6.84 

5 

■  c 

Z00.5 

6.70 

g 

37.04 

A  8^ 
O.oO 

4 

6' 

97 

7 

1 

148 

56 

7' 

74-9 

.19 

g 

2.40 

6.26 

5 

9» 

7 

1 

132 

4 

6' 

7' 

40.0 

5-99 

5 

72.92 

6.00 

2 

99 

7 

6 

146 

5 

6' 

7 

8.10 

4 

3  0. 1  z 

8  70 

0.10 

5 

100 

A  AT 

7 

7 

145 

18 

7 

7' 

zz4>o 

5.41 

5 

7.67 

5-35 

3 

IOI 

7 

7 

150 

6 

9 

9 
7' 

3 IO-4 

7.09 

2 

r>  8  t 
O.o  I 

6.75 

0 

7 

0 
j 

113 

12 

6' 

67.6 

7.21 

5 

28.2  I 

7.22 

g 

103 

7 

9 

120 

36 

6' 

8 

181. 3 

8.20 

g 

37-5° 

7.10 

5 

104 

7 

10 

160 

13 

5 

7 

301.3 

6.40 

'3 

77  87 
12.01 

6.34 

12 

105 

7 

12 

120 

30 

8 

8 

74.6 

7.05 

9 

-r  7  8 
7.3S 

9 

106 

7 

16 

141 

53 

7' 

9 

7  8  7  n 
201.9 

0.20 

0 

77  t8 
32. 1 0 

6.73 

O 

107 

7 

16 

142 

0 

6' 

7 

1 0. 1 

4.99 

5 

IO.48 

4.98 

4 

108 

7 

16 

138 

12 

9 

10 

163.9 

f\  7  8 
U.Z  0 

Q 
0 

8  nn 
°-77 

0.04 

5 

109 

B  1582 

7 

17 

138 

13 

7 

8 

157.6 

6.36 

9 

22.71 

6.54 

8 
0 

7 

19 

126 

57 

7  • 
6' 

=  7 

140.9 

5-97 

5 

7.O3 

5.96 

2 

hi 

7 

20 

151 

38 

8 

6.99 

I79.OO 

6.99 

112 

7 

22 

121 

30 

6' 

7' 

CT  8 
51.0 

6.84 

'5 

9.03 

6.99 

7  fi 

1 1 7 
1 1  3 

7 

24 

132 

58 

5 

10 

7  C  O 
/  3-u 

6 

22.52 

.00 

2 

T  Tyl 

A  52 

7 

27 

113 

7 

6' 

6' 

106.8 

6.69 

° 

9-37 

9 

T  7  C 
1  *3 

7 

29 

144 

48 

7 

Q 
O 

258.O 

7.27 

5 

*>4-53 

7.82 

8 
0 

Il6 

h  3988 

7 

31 

138 

28 

8 

IO 

4 

7fi  fi  7 
1  U.O  1 

6.77 

4 

T  T7 
1  1  / 

7 

32 

116 

24 

5  : 

=  5 

777  8 

6.67 

9 

Il8 

7 

35 

138 

40 

7 

10' 

17. 1 

6.25 

6 

13. II 

6.81 

4 

7 

1 1 

216.9 

5.88 

5 

19.51 

6.39 

3 

119 

7 

39 

163  53 

8  : 

=  8 

IOO.8 

6.56 

4 

6.83 

5 

I20 

A- 55   

7 

40 

140 

2 

7 

8 

I32.9 

7-53 

4 

50.94 

7-53 

6 

121 

7 

4i 

146 

18 

6 

1 1 

220.0 

6.55 

2 

37-98 

6.55 

2 

122 

B. 1753   

7 

41 

'3i 

4 

7 

i 

I76.8 

6.82 

5 

49- 1 3 

6.51 

4 

I23 

7 

49 

149 

1 1 

;: 

1 1 

323.I 

7-74 

3 

6.06 

8.08 

1 

Do.  AC  

1 1 

258.7 

8.08 

1 

60.38 

8.08 

1 

124 

7 

53 

119 

3 

8 

9' 

8l.I 

7.04 

5 

10.65 

7.04 

5 

125 

7 

54 

150 

21 

8' 

9 

I  15.2 

5.91 

5 

9.41 

6.11 

6 

126 

h.  4028  

7 

54 

139 

31 

7  : 

=  7 

46.9 

6.61 

6 

17.05 

6.88 

5 

I27 

7 

56 

150 

24 

8 

9 
% 

359-7 

5.91 

5 

6-34 

6.3 1 

5 

128 

7 

56 

136  50 

7 

351-4 

6.55 

4 

30.41 

7.06 

3 

I29 

7 

57 

130 

5° 

7 

345-4 

7.04 

4 

29.10 

7.04 

6 

130 

7 

57 

144 

3 

7 

9 

8' 

160.4 

7.00 

4 

40.42 

7-54 

4 

I3I 

7 

59 

123 

5 

6 

88.5 

8.00 

4 

22.29 

8.00 

4 

132 

8 

2 

152 

21 

6 

7 

264.5 

6.71 

4 

87.90 

6.71 

4 

133 

A.  63   

8 

4 

132 

8 

7 

8' 

80.5 

6.02 

7 

5-95 

6.04 

2 

4  B 


278  SYNOPSIS  OF  THE  RESULTS  OF  THE 


R  A. 

rs  p  D. 

Magni- 

Angle  of 

Epoch 

» 

Epoch 

No. 

Name  of  Star. 

183U.0. 
h.  m. 

1830.0. 
0  / 

tudi 

Position. 

t9-7o_1- 

t> 

Distance. 

1°3°+ 

> 

1  j4 

8 

4 

116  SO 

J  J 

2 

6 

220.2 

C.I  I 

J 

6 

41 16 

5.C9 

7 

AC  

2 

8 

151. 6 

5.I4 

c 

62.4.0 

T 

c.18 

2 

BC  

6 

8 

in. 8 

5.02 
7.08 

z 

13  ^ 

j  j 

8 

6 

159  23 

8' 

8' 

9.5 

6 

6.76 

7.08 

6 

1 16 

j 

8 

7 

132  29 

6 

9 

297.8 

6.0'2 
7  J 

c 

j 

2  "3  .7  C 

7.44 
/  TT 

1 
J 

1  3/ 

\i    4060.  ■ 

8 

7 

121:  c6 

9 

10 

177.0 

6  00 
"■yy 

1 

7  T  tn 

6.99 

1  3° 

8 

7 

1  c8  7 

5' 

10 

2-3.2 
j 

CO  I 

6 

6.69 

coi 

4 

8 

8 

125  49 

6 

7 

175.2 

7.  C4 

/  JT 

A 
T 

67.4  C 

/  T  J 

7  8c 
/,dj 

c 
j 

J4O 

h  4069  f 

8 

9 

I  7  C  TO 

Mj  *y 

6 

2' 

2  C6.7 

6  io 

6 

33.24 

6.84 

c 
^) 

141 

8 

13 

1 14  10 

8' 

8 

146.6 

6.22 

6 

C.  I  c 

J  J 

6.05 

c 

14-2 

8 

16 

130  27 

8 

8 

146.8 

A 

0.83 

7.62 

0 

14.3 

8 

20 

160  58 

6 

6' 

55.0 

C.Q2 

2 

64.07 

vt  y  / 

C.Q2 

I 

B  C 

6' 

7 

28.7 

C  02 

2 

1A.  l6 

C  n7 

I 

TAA 

8 

24 

I  14  IO 

6 

9 

J  J  J 

C.4Q 

8 

c  c8 

671 

A_ 

J<+3 

8 

24 

T  -3  7  21 

6 

9 

242. 1 

6. ci 

0 

y 

7L  ylO 
T  T 

6  ci 

AC   

6 

10 

3Q.Q 

c.81 

> 

20.06 

C  7? 

2 

I4.6 

ll    4I26  . 

8 

35 

I42  29 

6 

10 

31.3 

c  06 

3'7 

g 

l6.22 

6.28 

T/1  *7 

h  4128 

8 

36 

*4y  43 

7' 

8 

22 1.9 

6.66 

3 

2.51 

6.66 

3 

I48 

4  3 

8 

37 

I46  57 

7 

jo' 

226. 1 

6.68 

3.5O 

6.68 

149 

B.  2168  %   

0 
a 

38 

I42  30 

6 

6' 

309.8 

6.62 

6 

j  77-20 
J  64.79 

6.17 
7.07 

"3 
i 

3 

I  CO 

Yl    A  T  -7  1 

8 

38 

I32  2 

5 

11 

60.8 

c  12 

7 

3 

/i  7  7  n 

c  1 2 

1 

I  C  I 

J 

R  9 

8 

41 

148  6 

8 

8 

1 10. 1 

T  7 

'3 

/l  87 
4.0  / 

7.03 

1      4-  T?"!  r. 

8 

1 1 

1  C4.2 

COT 

1  CA  -4-  V>\   D  . 

8 

10 

2  17. 1 

COI 

j-y 1 

j 

107  '26 

I  C2 

S  c8c 

8 

47 

5' 

7 

I4.C.C 

TJ'  J 

7  2  1 

3 

68  oc 

7  2  T 

I  C*2 

B  2286  . 

8 

51 

•\  A  A     f  1 
T"T    j  3 

7 

7 

3  <;6.  c 

6  C  *2 

3  3 

9 

66.46 

601 

"•y  3 

•7 

T  CA 

8 

53 

148  34 

6 

7 

7  c  0 
/3*u 

4°-59 

6.98 

g 

ICC 
J33 

5 

50 

141  31 

6 

8 

88.2 

7—5 

4 

1.41 

7.23 

i  c6 

h  4172 

8 

59 

1 14  43 

9 

IO 

2 16.6 

7.2 1 

5 

7-51 

7.19 

4 

Tt'7 

*57 

h  4188 

9 

6 

132  55 

6' 

7' 

286.9 

C  7  T 

i-7 1 

g 

3.07 

5-°4 

3 

1  3° 

R  10 

9 

16 

J59  5 

8 

8 

18  1 
10.  j 

8.10 

5 

1 1.44 

8.10 

5 

9 

20 

174  58 

5' 

9' 

1 1 3.2 

5.08 

1.7 1 

5  - 1 3 

160 

A  76 

9 

22 

J34  43 

6' 

7 

07  8 

8.09 

3 

59-57 

8.09 

3 

161 

9 

23 

133  48 

8 

8 

2C7  8 

7. 10 

7.10 

-> 

162 

£  AntliiE  . 

9 

23 

12  1  10 

6 

7 

2 10.6 

6.32 

1 1 

8.38 

6, 12 

10 

1 6? 

9 

28 

130  15 

6' 

7' 

202.0 

u,x3 

g 

2.99 

"•45 

c 

3 

1 64 

9 

28 

'38  59 

7 

7 

■jo  n 

5.88 

g 

130.70 

5-95 

r 

3 

16? 

A  80 

9 

39 

■3°  43 

8  = 

:  8 

68.5 

6.09 

9 

18.27 

6.09 

j 

166 

9 

42 

124  14 

8 

8 

6  "?  T 

*  3 

g 

4-93 

6.60 

5 

167 

9 

43 

x54  J7 

3 

9'= 

8 

126  I 

6.83 

g 

4.90 

6.92 

7 

168 

9 

43 

T  CA  t2 

154  ia 

=  9' 

3OI.7 

6.71 

5 

12.98 

0.77 

3 

!^ 

A  8 1 

9 

48 

134  29 

6 

10 

239.I 

6  ic 

g 

5-95 

6  tc 
0.15 

3 

170 

9 

51 

J75  '3 

7 

7 

7.30 

7.23 

g 

T  7  T 

1  / 1 

A  83 

9 

56 

144  IO 

7 

7' 

222.6 

7  T  7 

4 

OQ  CO 

7.24 

172 

h  4"1 82 

9 

57 

141  15 

7 

8 

6.64 

5 

70.43 

6.86 

c 
3 

'73 

V>    An  %1 

9 

58 

140  58 

8 

9 

l8  I. O 

6.I7 

5 

6.16 

3 

*74 

10 

j 

'53  4° 

10' 

10' 

60.  ^ 

7.24 

5 

1 1.80 

7.26 

*75 

10 

13 

*53  49 

7  — 

/ 

1 39*3 

6.66 

6 

1.34 

6.91 

4 

176 

R.  13   

10 

15 

145  1 1 

f 

3 

10 

y  j 

5 

7-u4 

"•47 

3 

_  A  P 

5 

10 

19  1.4 

5.91 

4 

36.71 

6.18 

" 

177 

10 

23 

'51  43 

8 

8' 

7.16 

6 

7-J5 

7 

178 

10 

24 

131  21 

7 

8 

29I.5 

8.09 

3 

a2-7 1 

8.09 

179 

10 

24 

143  38 

g 

g 

352.2 

7.10 

2 

1 13.73 

7  TO 
7. 1U 

1 

ISO 

A.  87   

10 

25 

150  29 

7 

7' 

331.2 

5.98 

3 

83.52 

6.7I 

3 

l8l 

A.  88   

10 

25 

134  12 

6' 

6' 

37.8 

6.61 

11 

13.85 

6.5O 

5 

182 

10 

25 

142  51 

5' 

9 

17.4 

7.12 

6 

17-53 

7.12 

6 

I83 

h-433°  

10 

26 

136  8 

6 

9 

164.4 

6.61 

6 

40.66 

6.95 

4 

I84 

10 

26 

136  6 

7' 

10 

164.8 

6.61 

6 

26.38 

6.6l 

2 

185 

A.  89   

10 

26 

144  30 

7 
8' 

7' 

30.7 

7.16 

8 

26.41 

7.17 

7 

186 

10 

28 

161  14 

9 

59.1 

6.74 

8 

10.04 

6.67 

6 

I87 

A-  93   

10 

29 

153  x5 

8 

9 

37-7 

6.49 

5 

26.39 

6.62 

3 

188 

A-  94-   

10 

32 

148  18 

6 

10 

21.4 

6.66 

6 

15.25 

6.76 

5 

I89 

A-  95   

10 

33 

J44  43 

6 

8 

105. 1 

8.09 

3 

51.85 

8.09 

2 

190 

h.  4346  

10 

35 

150  8 

8 

10 

81. 1 

7.46 

3 

26.46 

7.28 

2 

B.  3181   

191 

10 

37 

150  17 

7 

9' 

173-5 

7.18 

1 1 

13.02 

7.19 

9 

192 

10 

37 

148  39 

3 

10 

147.9 

6.32 

6.32 

1 

3 

3.00 

J93 

10 

37 

149  12 

8 

1 1 

234.8 

7-3- 

2 

1.50 

7-3- 

0 

194 

B-  3»94   

10 

38 

148  51 

8' 

214.5 

6.69 

6 

18.27 

6.96 

4 

9 

195 

10 

38 

148  41 

117. 2 

5.72 

4 

2.24 

6.25 

C,  i  (A  -f  B)  ) 

9 

9 

8 

8 

108.7 

6.35 

9 

13.80 

7.88 

5 

=  B.  3190  S 

MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


279 


No. 


Name  of  Star. 


196 
J97 


198 
199 

200 

201 
202 
203 
204. 
205 
206 
207 
208 
209 
210 
211 


Do. 


212 
213 
214 
215 
216 


217 
218 
219 


220 
221 


222 
223 


224 
225 
226 
227 
228 
229 
230 
231 
232 
233 
234 
235 
236 
237 
238 
239 
240 
241 
242 
243 
244 
245 
246 
247 
248 


L.4364. 
A.  99  . 


h-4374  

h-4378  

A.  102,  A  B . . 

A.  103,  AC. 

h.4383  

h-  4393  

h.  4409  

b-  4423  

h.  4432  

B.  3574 

B.  3594  .... 
17  Hydrse    . . 

h-4455  

B.  3706  . . . . 

/3.  Hyd.  Crat. 


Sub-epochs 


B.  3828   

A.  n6  

£.  Chamaleontis 

h-4487  

B-  39°4   

AC  .... 

h-  4495  

h.  4522  

a  Cruris   


Sub-epochs 


Do.  A  C. 

S  Corvi    . . 
y  Centauri 
Sub -epochs 


2.  1669   . .  . 
y  Virginis 
2d  epoch 

3d  „ 

4th 
h.  4556.... 
h.4558.... 
A.  127  .... 

h.4563  

£2  Centauri 
0  Muscse  . . 
r\  Muscse  . . 
h.  4580. .  . . 

h.  4586  

R.  17   

f  Hydrae  . . 
Q  Centauri 
A.  142  .... 
h.  4607 .... 
A.  143  ... . 

A.  144   

R.  18   

A.  145  .... 
k  Centauri 
h  Centauri 

h.  4634  

A.  154  .... 
A.  155  ...  . 
h.  4651 
2.  1807.. 


R  A. 

N  P  D. 

Magni- 

Angle of 

Epoch 

CO 

Epoch 

6 

1880.0. 

1830.0. 

tudes. 

Position. 

TJ},n  1 
I83°T 

3 

Distance. 

1530-f- 

3 

h. 

m. 

0  / 

i> 

"3 

10 

38 

I40  28 

8 

10 

352.3 

O.77 

4 

6.69 

7.22 

3 

10 

39 

159  58 

7 

7 

75-4 

7.I4 

3 

63.92 

7.14 

1 

7 

9 

40.2 

7.14 

2 

7 

9 

10' 

285.6 

7.I4 

10 

42 

I48  33 

8 
7' 

1 15.2 

6.3  I 

1 

10.14 

6.3  I 

0 

10 

45 

r49  3 

10 

344-4 

6.16 

3 

30.89 

O.JO 

1 

10 

47 

J47  57 

4 

8 

13.0 

7.14 

1 

05.28 

7.14 

1 

4 

7 

200.2 

7.I4 

1 

103^^ 

7.14 

0 

10 

48 

159  50 

7 

8' 

7. IS 

1 

I.42 

7. 18 

0 

10 

5i 

..9  q 
I55  0 

7' 

10 

131. O 

5-31 

3 

7.IO 

5-3 1 

1 

10 

59 

J3J  43 

5' 

9 

7.30 

4 

7.25 

3 

1 1 

9 

J34  57 

7 

7 

269  2 

6.41 

5 

1.2  8 

5-95 

5 

1 1 

J7 

154  2 

6 

8 

0.03 

5 

2.37 

O.5I 

3 

1 1 

17 

150  43 

8 

9 

296.7 

8  in 
0. 1  (J 

5 

£  .9 
u.  3  0 

8.  IO 

O 

1 1 

20 

131  44 

6 

8 

166.9 

5.27 

7 

12.93 

5.24 

3 

1 1 

24 

118  20 

6  : 

=  6 

30.2 

5.11 

3 

8.92 

5.II 

4 

1 1 

28 

122  38 

6 

9 

8' 

244.9 

6.92 

7 

3-98 

6.96 

6 

1 1 

32 

152  32 

7' 

275.6 

8.09 

2 

25.97 

8.O9 

2 

1 1 

44 

122  58 

5 

5 

339.6 
338.3 

339-3 
340.4 
342.2 

5-78 
4-47 
5.23 
6.68 
8.09 

20 
6 

0 

£ 
D 

2 

2.03 

5.92 

15 

1 1 

47 

151  38 

8 

9' 

205.b 

2 

17.73 

O.O9 

2 

1 1 

48 

121  19 

8 

8 

83.1 

6.4. 1 

£ 
U 

2O.98 

6^ 

3 

1 1 

5i 

167  16 

6 

6' 

178.4 

5-93 

5 

I.5S 

3 

11 

52 

125  48 

10 

10 

124.7 

6.49 

2 

5.65 

6.49 

1 

1 1 

56 

151  3 

8 

8 

150.4 

7.27 

5 

23.48 

7.30 

6 

8 

10 

19.7 

7.23 

4 

26.62 

7.23 

4 

11 

57 

122  0 

7 

10 

313.8 

0.21 

0 

7.O9 

0.2  I 

4 

12 

16 

158  32 

8 

9 

07.2 

7.30 

0 

I3.4I 

7-3° 

4 

12 

17 

152  9 

2 

2' 

I20.6 
121. 5 
I20.9 
I20.6 
I  I9.9 
I20.0 

5-33 

4-  39 

5-  J7 
6.18 
7.18 

0.O5 

5° 
1 1 

J5 
•3 

5 

0 

5.65 

0.30 

_  /- 

20 

2OI.5 

6.43 

r3 

90.09 

6.75 

7 

. 

12 

21 

105  34 

3' 

10 

2I3.O 

7.48 

3 

23.44 

7.48 

2 

12 

32 

138  1 

4 

4 

354-3 
351.6 

5.89 

5-32 

13 

7 

0.75 

5.90 

0 

357-3 

0.3a 

6 

7.2s 

12 

32 

102  5 

7 

7 

122.3 

7.31 

6 

7.32 

0 

12 

33 

90  31 

4' 

4' 

43.1 

34-9 
21.5 

237-5 

4-37 
4-54 
5. 11 

8.00 

16 
16 
12 
2 

1. 51 

4-39 

3 

12 

45 

117  2 

8 

10 

O-  . 
OO.4. 

O.98 

0 

8 

7.05 

7.04 

5 

12 

47 

119  13 

9' 

9' 

178.3 

0.80 

4 

22.99 

7.03 

3 

12 

5° 

!44  59 

8 

9 

I20. I 

7-34 

5 

io-57 

7-34 

5 

12 

52 

122  42 

7 

9 

23O.5 

7-35 

0 

O.55 

7-35 

0 

12 

57 

139  0 

5 

10 

IOO.3 

6.51 

5 

6.0  I 

0.28 

4 

12 

C  7 

154  24 

6' 

0 
y 

187.5 

6.38 

10 

5.82 

O.07 

7 

13 

4 

156  58 

5' 

8 

332.2 

0. 12 

12 

59-86 

O.27 

9 

13 

13 

137  40 

8 

8 

10.2 

6.I9 

1 

0.50 

6.I9 

0 

13 

16 

156  59 

7' 

10 

150.1 

7-45 

3 

3-67 

7-44 

2 

!3 

21 

152  10 

7' 

8' 

358.2 

7.28 

6 

16.94 

7.25 

6 

13 

27 

115  37 

6 

7 
7' 

191. 5 

4.71 

9 

10.04 

4-49 

9 

13 

31 

143  42 

6 

164.0 

5-4° 

7 

5.38 

5.38 

3 

13 

33 

148  22 

7 

8' 

90.4 

6.37 

4 

32.92 

6.72 

3 

*3 

32 

161  8 

8' 

i 

76.3 

7.29 

6 

11.40 

7.31 

5 

13 

37 

151  14 

8 

35-8 

6.88 

5 

12.73 

7.08 

5 

!3 

39 

136  31 

8 

9' 

256.4 

6.92 

6 

9.25 

7.10 

4 

13 

41 

141  58 

6 

8 

288.9 

7-32 

6 

18.26 

7.31 

6 

J3 

42 

156  8 

8 

9 

50.4 

7.07 

9 

24.51 

7.22 

8 

!3 

42 

122  8 

6 

7' 

112. 7 

6.57 

14 

8.82 

6.90 

10 

13 

43 

121  5 

5 

10 

185.6 

7-47 

4 

13.76 

7-47 

4 

«3 

46 

145  12 

7' 

9 

310.0 

5.63 

7 

1 1.46 

5.81 

4 

55 

125  43 

8 

9 

131. 1 

6.81 

5 

2 1.64 

7.09 

3 

!3 

56 

142  52 

7' 

8 

27.7 

7.02 

5 

24.51 

7.02 

5 

13 

58 

140  42 

6 

134.0 

7.12 

5 

62.67 

7.12 

5 

14 

3 

92  31 

8' 

=!< 

26.9 

7.48 

3 

7-93 

748 

3 

280 


SYNOPSIS  OF  THE  RESULTS  OF  THE 


No. 


249 
250 
251 
252 
253 
2  54 

-55 


256 
257 
258 
259 
260 
261 
262 
263 
264 
265 
266 


267 
268 
269 
270 
271 
272 
273 

274 

275 
276 
277 
278 
279 
280 
281 
282 
283 


284 
285 
286 
287 
288 
289 
290 
291 

292 
293 
294 
295 
296 
297 


298 
299 
300 
301 
302 
303 
304 

3°5 
306 
307 


Name  of  Star. 


h.  4671 .... 
Y  Centauri 
2.  1833  .. 
2.  1837  .. 

h.4687  

h.  4691 . . . . 
a  Centauri 


Sub-epochs 

h.  5444.... 
a  Cireini 
A 

54 
h. 
h. 

A. 

h. 
h. 
11 

7T 


,  28 


168  .. 

Hydra? 
4706. . . , 
4707..., 
171  ... 
4712.. . , 
47I5- 
•  145. 
Lupi. . . . 

Sub-epochs 
k  Lupi  .... 

A-  179   

n'  Lupi    . . 

A.  180   

y  Cireini  . . , 

t  Lupi 

A.  183?  .. 

A  C 
h.  4766 .... 

h-4771  

h.4772  

h.  4776.... 

h.4777  

A.  186   

h.  4784  

h.  4783.... 

S-  673   

y  Lupi .... 

Sub-epochs 

4788  

190 

1962   . . . 

4796  

20   

4805  

193  ..... 

4809. 
A  C 


i95  

Lupi  

4821  

Lupi  

4825  

51.  Librae 


Sub -epochs 


AC... 

/3  Scorpii  

h.  4830  

A-  199   

h-4837-v.  

12.  Scorpii 

h.  4840  , 

A.  200  

h-  4845  

1  Triang.  Austr. 
h.4848  


R  A. 

N  P  D. 

Magni- 

Allele of 
Position. 

Kpoch 

a! 

Epoch 

18S0.0. 

1830.0.' 

tudes. 

1830+ 

3 
09 

Distance. 

18304- 

h. 

m 

»> 

14 

9 

169  19 

8' 

9 

127.4 

6.84 

4 

5-83 

7.04 

3 

14 

11 

147  40 

6 

8' 

163.2 

6.55 

8 

9.63 

6.74 

7 

J4 

14 

96  59 

_/. 
7  • 



—  7 

164.0 

7.48 

3 

6.25 

748 

3 

!4 

_  r 
ID 

IOO  49 

7; 

321-5 

7.48 

2 

I.25 

7.48 

0 

14 

25 

125  49 

9' 

-0' 

82.5 

7.32 

4 

2.17 

7.21 

3 

!4 

27 

144  57 

9 

9 

269.3 

7.29 

2 

10.3 1 

7.29 

2 

'4 

25 

150  8 

1 

2 

219.6 

6.05 

66 

16.52 

6.60 

36 

218.5 

4-79 

19 

17.43 

4.68 

11 

219.5 

5.86 

25 

* 

* 

* 

220.7 

7-34 

22 

16.12 

7.44 

25 

!4 

29 

144  12 

9 

10' 

70.I 

7-39 

2 

20.23 

7-39 

2 

'4 

29 

154  14 

4 

9 

243.8 

7. 11 

11 

15.63 

7.05 

IO 

'4 

31 

154  27 

g 

8' 

204.1 

7.14 

8 

6.70 

7.22 

6 

J4 

oft 

114  43 

g 

8' 
0 

134.2 

5-37 

9 

9.19 

547 

I  I 

40 

136  42 

7 

217.4 

6.99 

5 

7-13 

7.05 

6 

!4 

40 

155  42 

0 
0 

0 
0 

225.2 

7-47 

3 

1.50 

7-55 

2 

!4 

42 

'35  9 

7 

10 

224.2 

7-39 

6 

16.80 

7-39 

4 

14 

43 

114  44 

8 

8' 

227.3 

5-39 

5 

6.27 

543 

1 

14 

45 

137  11 

£/ 
0 

7 

277.8 

5.96 

9 

3.04 

6.18 

9 

14 

48 

110  38 

.1 

5 

7 

2774 

6.66 

5 

12.08 

7.06 

5 

14 

54 

176  23 

5' 

=  5' 

in. 1 
112.8 
108.6 

6.11 

5-37 
7.04 

18 

IO 

8 

0.7  c 

5.24 

c 

■ 

15 

0 

138  5 

5 
7 

0 

144.2 

7.13 

8 

27.21 

7.06 

9 

'5 

3 

132  43 

9 

46.9 

6.97 

6 

10.64 

7.13 

6 

15 

7 

117  11; 

6  : 

=  6 

173.6 

6.28 

1  c 

j 

2.08 

6.83 

6 

'5 

7 

137  15 

5; 
5' 

Q 
O 

131. 3 

6.39 

8 

22.93 

6.96 

7 

'5 

10 

148  42 

O 

108.5 

6.33 

9 

1.26 

7-77 

3 

!5 

1 1 

134.  A 

4 

9' 

174.0 

7.26 

IO 

26.35 

7.27 

Q 

I5 

14 

128  6 

5 

9' 

298.7 

6.39 

1 

89.48 

6.39 

I 

5 

9 

45.9 

6.39 

1 

144.50 

6.39 

I 

J5 

132  15 

0' 

6 

10 

118.3 

7.41 

6 

13.12 

7.42 

5 

15 

17 

147  30 

8 

9 

188.1 

7.16 

9 

5.91 

7.38 

7 

17 

140  50 

8 

12 

249.9 

6.94 

3 

12.60 

7.54 

1 

19 

131  20 

7 

9 

224.2 

5.94 

6 

5.95 

5.94 

4 

'5 

!9 

14.6  40 

_/ 
7 

9' 

301.7 

7.10 

6 

6.33 

7.27 

4 

20 

147  ^8 

Q 

8 

1 14. 1 

7.54 

2 

39.25 

7.54 

3 

15 

22 

137  O 

7' 

10 

238.2 

6.96 

6 

34.15 

7.31 

5 

15 

22 

109  35 

6 

10 

281.7 

6.80 

6 

1 1.06 

6.78 

3 

I5 

23 

113  54 

Q/  _ 
0  - 

—  q' 

—  a 

120.5 

5.60 

15 

9-55 

5.78 

11 

15 

24 

130  35 

4; 

=  4 

94.1 

94-3 
93.8 

5.86 
5.05 
7.04 

3* 
J9 
13 

0.84 

5.24 

2 

15 

24 

134  23 

5 

9 

349.0 

6.62 

5 

3.14 

6.42 

3 

26 

14-7  7  3 

7' 

io' 

94.7 

4.3 1 

1 

15 

29 

98  13 

7' 

7' 

7.9 

7.54 

3 

12.20 

7.54 

3 

15 

31 

148  q 

8 

8' 

116.6 

6.65 

Q 

34.18 

6.87 

4 

15 

32 

154  54 

7  = 

=  7 

155.9 

5.35 

7 

2.42 

5.34 

3 

15 

37 

14.2  4. 1 

6 

11 

172.3 

6.88 

4. 

32.0 1 

7.03 

3 

15 

38 

144.  32 

6 

10 

21.9 

6.35 

6 

23.17 

6.67 

3 

15 

39 

1 50  IO 

7 

9 

6.24. 
— ( 

2 

4.3.4.7 

6.24. 

1 

7 

9 

2C7.0 

6.24 

1 

40.30 

6.24 

1 

J5 

42 

T  "2  f>  An 

7 

6' 

10.7 

6.3  I 

0 

I2.38 

6.6l 

j 

15 

46 

123  28 

6 

49.3 

C.  CJ. 

J  JT 

IO 

I  I.O3 

5.76 

7 

15 

48 

121:  32 

8 

8 

145. 1 

6.38 

6 

19.22 

6.38 

2 

IS 

49 

127  54 

4 

8' 

22.2 

4.68 

9 

15.07 

4-59 

4 

15 

5° 

147  17 

6 

10 

251.6 

6-37 

6 

I0.24 

6.85 

4 

'5 

55 

100  54 

5' 

5' 

IO.I 
8.3 
IO.6 

5-4° 
445 
5-39 

22 
6 
13 

I.4I 

4.85 

2 

5' 

1 1.4 

7-33 

3 

9 
5' 

77.2 

4-35 

2 

15 

56 

109  20 

3 

25.6 

6.63 

5 

I3.65 

6.79 

6 

'5 

5fi 

132  32 

9 

10 

232.7 

4-35 

3 

21.21 

4-35 

1 

15 

58 

128  39 

7 

7' 

185.2 

5.92 

6 

45.03 

6.46 

6 

16 

1 

133  12 

* 

9 

75-4 

543 

6 

I0.02 

5.10 

3 

16 

2 

117  58 

10 

81.7 

4.78 

7 

4.62 

4.69 

3 

16 

6 

124  23 

9 

10 

292.8 

6.82 

4 

5.I4 

7.07 

4 

16 

1 1 

133  30 

6 

10 

198. 1 

6.93 

4 

42.85 

7.08 

3 

16 

12 

130  50 

8 

9 

135.0 

6.45 

2 

I.20 

6.49 

1 

16 

12 

!53  39 

6 

11 

27.2 

6.9 1 

5 

24.66 

6.49 

1 

16 

r3 

122  48  j 

7 

7 

155.0 

6.55 

1 1 

6.O4 

7.20 

7 

MICROMETRICAL 


MEASURES  OF 


DOUBLE  STARS. 


281 


No. 


308 
309 
310 


3H 
312 
313 
31+ 
315 
316 

3*7 
318 

3J9 
320 
321 
322 

323 
324 

3*5 
326 
327 
328 
329 
330 

331 
332 

333 
33+ 
335 
336 
337 
338 
339 
340 

34i 
342 

343 
344 
345 
346 
347 
348 

349 
350 

35i 

352 

353 
354 
355 
356 


357 
358 

359 
360 

361 
362 
363 
364 

365 
366 
367 
368 
369 
370 


Name  of  Star. 


h.  4850  

t  Normse  

5  Ophiuchi 

AC.  .. 

AD.  ... 

A. 203   

A.  202  ?   

h.  4866  

h.  4871  

h-  4873  

h.  4876  

h.  4880  

h.4883  

A.  210  ........ 

A.  209   

h.  4889  

h.  4890  

h.  4896  

h.  4909  

A.  213   

36  Ophiuchi   . . 

b-  4938  

h-4939  

h.  4947  

h-  4949  

A.  216  =  AC. 
A. 217   

h-4975  

2d  epoch  . .  . . 

h-  4978  

h.  4982  

A.  219   

h.  5000  

h.  5003  

h.  5005  

h.  5013  

70  Ophiuchi 
2d  epoch 

h.  5023  

h.  5025  

h.  5032  

h-  5034  

h.  5038  

A.  220   

A.  221   

2.  2306   

2.  2313   

ic  Coronse  Austr. 

h-  5055  

h.  5056  

A.  224  

h.  5°75  

B.  6556   

y.  Coron.  Austr. 

2d  epoch  . . . . 

3d  ,  

4th    „  .... 

A.  225  

h.  1367  

/3  Sagittarii 

h.  5114  

A  C  

h.  5"7  

h.  5 140  

A.  227   

A.  229   

h-  5177  

A.  230  

A.  231   

A.  232   

p  Capricorni  .. 
0  Capricorni    . . 


R 

A. 

N  P  D. 

Magni- 

Angle of 

Epoch 

03 

Epoch 

1830.0. 

1830.0. 

tudes. 

Position. 

1830  + 

3 

Distance. 

1830  + 

3 

"3 

h. 

□  / 



(2 

> 

16 

14. 

119  18 

6' 

7' 

348-3 

5-93 

IO 

7-54 

6.04 

9 

16 

I  c 

j 

137  IO 

5' 

7' 

335-2 

6.01 

IO 

23.87 

6.64 

5 

16 

I  c 

J 

113  3 

6 

6 

1.9 

4.78 

5 

4.1 1 

4-35 

4 

6 

8 

2.2 

5-43 

1 

6 

8 

286.6 

5-43 

1 

.... 

10 

18 

150  30 

8 

8 

248.9 

6.88 

4 

36.18 

6.88 

2 

16 

20 

131  28 

6 

1 1 

180.4 

6.64 

2 

52.48 

6.64 

I 

16 

26 

146  39 

7' 

8' 

125.8 

6.14 

8 

3.98 

6.70 

6 

16 

27 

17  7  26 

7 

10 

47-3 

6.87 

IO 

27.82 

7.04 

7 

16 

27 

139  1 

8 

8' 

72.0 

6.81 

7 

31.80 

7.04 

6 

16 

28 

138  25 

6 

7 

265.1 

6.98 

5 

9.83 

7.18 

5 

16 

3^ 

176  7 

1 3"  3 

8 

1 1 

151.0 

7-35 

31.86 

77c 

16 

33 

132  4 

8' 

Q 

185.4 

6.88 

3 

10.96 

6.52 

z 

16 

7  A 

H5  3 

J73-9 

6.39 

2 

.... 

.. 

16 

7  7 

5 1 

126  34 

7' 

8' 

H7-3 

6.82 

8 

23.21 

7-39 

5 

16 

A.O 

127  12 

6 

10 

5.0 

5.36 

5 

7.24 

5-39 

2 

16 

4.1 

7- 1 

J36  37 

7' 

 :  7' 

147.6 

6-73 

5 

31.07 

7.09 

4 

16 

44- 
Tr 

136  34 

7' 

IO 

28.0 

6-35 

7 

4-39 

6.49 

4 

16 

51 

140  50 

8 

8' 

284.4 

6.52 

6 

16.46 

6.33 

4 

16 

58 

136  31 

7' 

9' 

166. 1 

6.47 

6 

8.65 

6.47 

2 

17 

c 

j 

116  21 

6 

-  6 

43-5 

5.19 

17 

4-97 

5.02 

11 

1 7 

8 

146  16 

8' 

8' 

108.4 

5.89 

6 

24.56 

5.89 

2 

17 

0 
y 

146  17 

8 

Q 

y 

224.4 

5.89 

6 

30.77 

5.89 

4 

17 

171  47 

9 

q' 

y 

75-5 

6.52 

4 

10.63 

6.5, 

3 

1 7 

IA 

*35  41 

6 

7 

267.4 

6.40 

12 

3-23 

6.72 

3 

6 

7 

3I3-5 

6.81 

5 

104.01 

6.66 

4 

6' 

T  7 

133  49 

n 

y 

i7i-3 

6.25 

5 

H-55 

6.85 

5 

1 7 

74. 

145  20 

6' 

1 0 

1 1 5.7 
81.3 

5-37 
7.66 

2 
2 

1    I  CI 

\  1,51 

7.66 

1 

*7 

37 

143  32 

6 

J  I 

269.5 

4.92 

4 

12.14 

4-77 

3 

J7 

78 
3s 

138  13 

7 

r' 
3 

59-7 

7.42 

5 

42.91 

7.42 

3 

J7 

47 

126  50 

7' 

265.1 

6.87 

4 

47.10 

6.87 

2 

T  7 

a8 
40 

126  55 

n! 
1 

IO 

107.3 

6.96 

5 

6.84 

7.03 

3 

J7 

4s 

120  14 

6 

7 

107. 1 

6.84 

5 

6.20 

6.68 

6 

17 

49 

135  48 

7' 

9 

28.2 

7.23 

8 

26.83 

6.15 

7 

T  7 

r  r 

33 

133  24 

6' 

6' 

69.0 

6.67 

5 

0.67 

6.42 

2 

l7 

57 

87  27 

5 

g 

132.5 

4.61 

3 

129.3 

6.77 

7 

6.98 

6.65 

10 

1 7 

59 

130  37 

8' 

8' 

276.1 

6.85 

9 

9.30 

7.12 

5 

1 7 

59 

130  39 

9 

9 

100.5 

6.55 

5 

47-93 

6.51 

2 

1  0 

2 

133  14 

7 

10 

335-8 

7.66 

2 

1.50 

7.66 

0 

1 8 
1 0 

4 

136  4 

g 

9 

90.1 

6.89 

5 

1.92 

6.50 

2 

18 

5 

161  51 

8' 

300.4 

6.87 

7 

11.78 

6.92 

4 

18 

8 

145  38 

/ 
5 

8 

179.6 

6.11 

1 1 

31.52 

6.16 

8 

18 

12 

134  11 

164.5 

7.07 

5 

76.34 

6.98 

1 0 

J3 

105  11 

8  ; 

—  g 

35-5 

7.48 

3 

13.06 

7.48 

3 

18 

16 

96  41 

,' 

/ 

9 

197.6 

7.20 

3 

5-25 

6.65 

1 

1  0 

22 

128  50 

5 

7 

359-3 

6.56 

9 

21.78 

6.95 

5 

1  0 

3° 

143  1 

8 

g 

75-5 

7.66 

1 

7-39 

7.67 

2 

18 

3 1 

145  50: 

7 

10 

198.8 

5.92 

6 

32-43 

6.45 

3 

18 

41 

137  28 

7  : 

7 

—  / 

63.7 

5.66 

10 

82.12 

5.21 

4 

18 

48 

154  1 

8' 

8' 

108.6 

5.52 

4 

1.86 

5-45 

1 

18 

5° 

127  17 

7 

7 

282.5 

7.66 

3 

12.98 

7.66 

3 

18 

55 

127  18 

6  : 

=  6 

37-i 

4-47 

3 

] 

36.8 

5-55 
6.43 

5 

!>  2.66 

7.21 

9 

34-5 

3 

1 

j 

32.7 

7-43 

!4 

18* 

59 

142  4 

7 

8 
9' 

252.9 

6.44 

4 

69.58 

6.77 

3 

19 

1 

107  43 

8 

61.8 

6.76 

5 

15.02 

6.89 

3 

'9 

10 

134  46 

4' 

8 

78.6 

5.01 

4 

29.09 

5-5i 

4 

*9 

J4 

144  39 

6 

1 1 

13 1. 0 

7.66 

1 

'•75 

7.66 

0 

6 

7 

270.7 

7.66 

1 

69.43 

7.66 

1 

J9 

16 

!34  13 

8 

10 

265.1 

6.55 

5 

6.03 

7.04 

6 

!9 

34 

155  >9 

8' 

8' 

89.6 

6.94 

6 

1.78 

7.09 

4 

r9 

39 

145  24 

6' 

7 

150.7 

4-77 

8 

23.04 

5.18 

7 

'9 

45 

142  21 

7 

7' 

243.9 

5-49 

4 

82.69 

5-49 

2 

20 

1 

147  28 

8 

8 

29.3 

5.68 

8 

8.39 

6.55 

5 

20 

6 

130  42 

7' 

8 

115. 0 

6.61 

6 

11.35 

6.57 

6 

20 

!7 

161  45 

7' 

8 

65.0 

6.50 

2 

116.98 

6.50 

2 

20 

17 

165  55 

6' 

7 

17.2 

6.16 

7 

18.70 

6.34 

5 

20 

*9 

108  22 

5' 

8 

177-5 

6.73 

5 

4.15 

6-53 

6 

20 

20 

109  9 

7 

7' 

239-3 

6.09 

4 

22.27 

6.23 

8 

4  c 


282 


SYNOPSIS  OF  RESULTS  OF  MICROMETRICAL  MEASURES  OF  DOUBLE  STARS. 


No. 

Name  of  Star. 

R  A. 
1830.0. 
b.  m. 

N  P  D. 
1830.0. 

0  / 

Masni- 
tudes. 

Angle  of 
Position. 

Epoch 
1830  + 

Value. 

Distance. 

Epoch 
1830  + 

'a 
> 

3/  1 

20 

20 

Q 
0 

9 

34.6 

6.16 

0 

6.24 

6.c  \ 

j  j 

6 

372 

20 

37 

r53  3 

7 

7 

101.4 

5.IO 

4 

3.23 

5.56 

1 

373 

20 

39 

124  23 

5 

1 1 

164.5 

5.61 

2 

21.71 

5.61 

1 

37+ 

20 

42 

161  4 

0 
5 

8' 
0 

1 10.8 

6.62 

Q 
O 

7.62 

6.59 

6 

375 

20 

+9 

133  39 

7 

7 

254.9 

6.61 

5 

60.00 

6.62 

6 

376 

105  43 

g 

0 

328.0 

6.13 

2 

2.12 

6.64 

1 

377 

21 

9 
0 

144  9 

5 

10 

307.O 

4.52 

9 

3.67 

4.49 

3 

378 

2 1 

10 

170  46 

0 

1 1 

92.4 

6.16 

2 

24.22 

7-53 

1 

379 
— 

2 1 

*5 

136  47 

7 

1 1 

56.7 

4.48 

1 

5.OO 

4.48 

0 

7 

9' 

183.4 

4.48 

1 

380 

2 1 

23 

173  a9 

g 

9 

82.9 

5-57 

s 
0 

3.38 

5-i3 

7 

381 

2 1 

25 

107  10 

9' 

10 

80.3 

6.64 

2 

17.99 

6.64 

1 

382 

2  I 

25 

107  4 

Q 
0 

D 

10 

268.9 

6.64 

2 

5 1.02 

6.64 

1 

383 

2  I 

37 

138  4 

9 

14.2 

6.65 

4 

30.30 

6.65 

+ 

384 

2 1 

47 

1+1  53 

IO 

IO 

169.2 

+•55 

1 

10.14 

+•55 

1 

38S 

2 1 

48 

105  56 

O 

10 

319.9 

7.07 

3 

19.79 

5.61 

1 

386 
— 

2 1 

55 

H9  5+ 

Q 

IO 

142.2 

4.60 

2 

2.00 

+■55 

0 

AC   

0 
0 

0 
5 

190.8 

4.64 

1 



387 

22 

1 

149  40 

9 

IO 

100.2 

5.18 

5 

15-53 

5.08 

2 

388 

22 

2 

129  9 

Q  _ 
O  - 

—  5 

1 10.4 

6.12 

Q 
O 

1.72 

5.41 

6 

389 

22 

1 1 

165  52 

D 

1 

82.9 

6.24 

O 

18.09 

6.13 

3 

390 

22 

J5 

i55  5° 

./ 

4 

,0' 
10 

282.3 

6.16 

0 

6.84 

5.98 

3 

391 

22 

20 

13+  37 

5 

9' 

215.7 

6.66 

0 

61.26 

6.63 

+ 

392 

22 

20 

90  53 

_^ 

5 

5 

352.O 

6.25 

9 

3.91 

6.61 

8 

393 

22 

22 

123  13 

+' 

J73-3 

6.20 

0 

29.09 

6.29 

5 

39+ 

22 

27 

122  33 

0 

7 

30.7 

4.78 

3 

87.01 

4.78 

1 

395 

22 

29 

148  43 

9 

9' 

7i-7 

+•55 

1 

43.64 

+•55 

1 

396 

22 

30 

119  14 

6 

7 

159-7 

7.25 

5 

85.31 

6.64 

0 

397 

22 

30 

119  15 

7 

9 

57.6 

7.41 

7 

4.36 

7.50 

5 

398 

22 

39 

104  55 

6 

9' 

113.7 

5.76 

3 

30.86 

5.76 

1 

399 

22 

+3 

123  47 

+' 

10 

276.8 

5-55 

5 

3-59 

5-55 

1 

400 

h-  5373  

22 

5° 

155  11 

7' 

10 

99.6 

6.57 

3 

48.89 

6.57 

2 

401 

22 

5+ 

102  12 

8' 

9' 

3>3 

7.80 

2 

8.87 

7.80 

3 

402 

22 

57 

141  36 

6' 

7 

5.69 

9 

8.12 

6.94 

+ 

403 

22 

58 

150  39 

7' 

10 

291.2 

6.16 

6 

15.07 

6.49 

5 

404 

23 

2 

102  50 

7'= 

=  7' 

100.2 

7.80 

2 

3-+3 

7.80 

2 

405 

2- 2993   

23 

5 

99  51 

7 

7' 

176.7 

7.80 

3 

25.74 

7.80 

3 

406 

23 

7 

100  0 

5' 

10 

3"-5 

7.80 

3 

49.29 

7.80 

3 

407 

23 

9 

149  14 

8 

9' 

19.7 

5.28 

4 

6.96 

5.91 

1 

408 

23 

1 1 

104  22 

6 

9 

343.6 

7-79 

2 

14-75 

7-79 

1 

409 

23 

1 1 

141  14 

6 

9' 

211. 5 

6.91 

8 

16.87 

6.96 

7 

410 

23 

1+ 

1++  +5 

6 

7' 

213.5 

5.18 

7 

27.13 

5.11 

+ 

411 

23 

1+ 

99  2+ 

7' 

8 

90.2 

7.80 

2 

6.88 

7.80 

2 

412 

23 

15 

105  25 

7 

9 

330.0 

5.76 

2 

61.76 

5.76 

1 

+13 

23 

*5 

155  38 

7 

10 

48.4 

6.02 

9 

42.47 

5.89 

5 

414 

23 

3° 

137  35 

6 

7 

268.8 

5.40 

9 

+•+7 

6.50 

5 

+15 

23 

46 

117  59 

6' 

7 

267.5 

5-s7 

+ 

6.88 

5.04 

3 

416 

23 

48 

107  6 

9 

9' 

2.7 

5.76 

1 

12.00 

5.76 

0 

+  J7 

h-  5++°  

23 

5+ 

118  4 

8' 

9 

285.1 

4.78 

2 

3-63 

4.78 

2 

COMPARISON  OF  ANGLES  OF  POSITION  OF  DOUBLE  STAES, 

MEASURED  WITH 

THE  SEVEN-FEET  EQUATORIAL  AND  THE  TWENTY-FEET  REFLECTOR. 


(167)  When  we  compare  the  results  of  micrometric  measurement,  as  respects  the  angles  of 
position,  given  in  the  above  synoptic  table,  with  the  mean  results  of  the  angles  for  the  same  stars, 
afforded  by  the  twenty-feet  position  micrometer  in  the  ordinary  course  of  sweeping,  material  dis- 
cordances will  be  found  in  a  great  many  instances,  such  as  cannot  wholly  be  accounted  for,  either 
by  the  comparatively  greater  attention  to  precision  in  this  respect  in  the  equatorial  measures,  and 
the  greater  time  and  care  bestowed  on  them,  or  on  the  greater  number  of  measures  usually  taken 
with  the  latter  instrument.    It  is  true  that  several  cases  of  great  disagreement  may  be  perfectly 
well  accounted  for  in  this  way,  when  the  closeness  of  the  stars  measured,  their  inequality,  and 
even  the  difficulty  of  seeing  them  at  all  with  the  smaller  instrument  are  taken  into  the  account. 
But  on  subjecting  the  matter  to  a  more  particular  examination,  it  becomes  very  evident  that 
these  causes  alone  are  not  sufficient  to  account  for  the  discordances — and  that  there  exists  a 
systematic  bias,  from  whatever  cause  arising,  which  has  affected  all  the  twenty-feet  measurements 
(as  compared  with  the  equatorial) — and  that  differently,  according  tu  the  different  direction  of  the 
small  star  with  respect  to  the  large  one.    What  is  more  singular,  and,  indeed,  so  far  as  I  see,  unac- 
countable, is,  that  neither  the  amount  nor  direction  of  this  bias  is  the  same  for  all  the  four 
quadrants  of  position,  nor  is  it  even  the  same  in  the  same  direction  for  positions  differing  by 
180°.    That  the  eyes  of  different  persons  do  not  judge  with  equal  certainty  of  parallelism,  is 
notorious — as  well  as  that  the  two  images  of  one  and  the  same  straight  line,  seen  with  the  right  and 
left  eye,  are  not  parallel.    If  we  attempt  to  place  a  ruler  parallel  to  the  edge  of  a  paper,  we  shall 
find  that  a  material  difference  in  the  accuracy  with  which  we  shall  do  it  by  the  judgment  of  the 
eye  alone  is  made  by  the  situation  of  the  paper  with  respect  to  the  vertical  or  principal  section  of 
the  eye — and  it  would  appear  from  the  facts  in  question,  that  our  judgment  of  parallelism  is 
liable  to  be  greatly  affected  also  by  the  different  attitude  of  the  person  generally,  and  especially 
by  the  difference  between  looking  up  and  down.    Such  at  least  is  the  best  account  I  have  been 
able  to  give  to  myself  of  the  cause  of  the  systematic  discrepances  alluded  to.     Their  law  and 
amount  can  only  be  made  out  inductively,  by  the  assemblage  of  the  totality  of  instances,*  where 
stars  have  been  measured  with  both  instruments,  such  as  is  presented  in  the  following  table : — 


*  Quick  moving  Binary  Stars  are  excluded  from  this  comparison,  so  are  Rough  Measures  and  Estimates. 


284  COMPARISON  OF  ANGLES  OF  POSITION 


Th?  numbers  in  column  1,  are  those  of  the  Synoptic  Catalogue  of  Measured  Double  Stars. 


No. 

Equ. 

Refl. 

— E. 

No 

•qu. 

Refl. 

— E. 

No. 

Refl. 

 £# 

0 

0 

0 

O 

0 

0 

0 

0 

0 

1 72. 2 

T  70.  C 

1.7 

118 

I  7. 1 

12. 1 

CO 

2  IQ 

120.6 

1 17.8 

2.8 

7 
3 

j  64.2 

1 60. a 
± wy  t 

j 

2  l6.Q 

206.8 

1 0.1 

221 

7  CA.  1 

7A0  8 

I  7  c 
1 3-5 

A 

2A7.2 

O.4. 

HQ 

100.8 

100.0 

0.8 

222 

I22.3 

12  C  7 

4 

7  0 

C 

63,0 

6l.6 

1.4- 

I20 

I  "32. Q 
*  j  7 

I  2A.7 

4. 

1.4. 

224. 

X 

80.4 

83.6 

4 

2  2 

3-^ 

6 

70  2, 

76.8 

2. A 

121 

220.0 

2  I  C.7 
J  j 

4.-7 

22  s 

178  7 

/  °-  3 

182.0 

7  7 
3-/ 

8 

126.8 

127.8 

4 

I.O 

I23 

'32'? .  I 
j  j 

72  C.2 
J  J 

4- 

2.2 

226 

I26. 1 

128.8 

4 

2.7 

Q 

244.0 

27Q.  I 

4-.Q 

I24 

8 1. 1 

82.6 

4 

I.< 

j 

22Q 

187. c 

186.0 

T  C 

1 1 

1 6.4. 

1 1.7 

4..  7 

I2C 

J 

I  I  C.2 

3 

I  IO.9 

4..1 

2 14- 

IOI  c 

*y  i-3 

IQ7  I 

*y  3-A 

4 

1.6 

12 

3A7.  C 

7AI  .7 

5.8 

I26 

4.6.  Q 

A2.2 

TJ 

■?.7 
j  / 

"j" 

90.0 

89.8 

0.2 

16 

6 

103.7 

u.y 

7  7  7 

359*7 

3  54-4 

5*3 

237 

-6  7 
/  °-3 

76. 1 

T  7 

122.3 

1 20.0 

2.7 
3 

12  1 

88.5 

84.6 

"2.0 

238 

7C  8 
35-° 

7C  8 

0.0 

T  n 

69.6 

72  C 

X 

2  Q 

12  7 

80.5 

86.3 

_l_ 

2  c  6  /i 

7  Cn  6 

4. 

V 

3-2 

* 

37.6 

3O.3 

7-3 

7  7  A 
1  34 

218.5 

288.9 

285.8 

3-1 

23 

727  X 
13/. O 

X 

3.0 

I  7  C 

1  33 

9-5 

6  7 
u-3 

3*2 

242 

0.5 

24 

268.5 

27I.3 

X 

2.8 

776 

297.8 

292.1 

3-7 

243 

185.6 

183.6 

0  c 

24I.7 

0.6 

777 

1  3  / 

17-5 

r  t 

W 

24-4- 

X 

0.6 

26 

9*7 

1 0.6 

4 
X 

IAI 

14.6.6 

7  a6  1 

O  -3 
u*3 

TOT 

1 3 1. 1 

7  7  r»  c 

1.6 

1 1 
3 1 

185. 1 

183.8 

I  7. 

I42 

14.6.8 

14 1.0 

c8 

24.6 

27  7 

It 

777 

0.6 

"2  2 
3  3 

81  c 

81.8 

-L 

1 

O  "3 
J 

IA7 

ceo 

3  3 

C2  7 

i.t 

D 

I-*  7  A 

128.5 

4. 
X 

1. 1 

34 

70.7 

68.7 

144 

35°-3 

7/1  7  8 

347. 8 

2.5 

X 

1  c 

j  j 

3 1 0.0 

306.  i 

3-y 

IAC 
*t5 

24.2  "3 

7776 

^3  /•" 

4..  7 

2^1 

I  64.O 

I  6  C  A 

4. 

I  A 

•58 
5° 

102. 3 

yy-3 

2.8 

2  7  2 

3  / 

2.7 

8->  c 
oi-5 

80.8 

7  7 
*"/ 

40 

4-2..  I 

41.5 

0.6 

147 

220.2 

x-7 

254 

269.3 

270.0 

X 

O.7 

41 

327.1 

X 

0.5 

I48 

226  1 

"  't 

9*7 

'ire 
z3  3 

215.3 

4-3 

43 

44-+*° 

7a6  8 

_1_ 
X 

2.0 

I  AO 

700  S 
juy.o 

309.3 

u*3 

2  C7 

"A 7  8 

-4.3.0 

244-3 

4 

0  c 
u-5 

AA 

TT  n 
11.3 

A  1 

4-3 

7  0 

I  CO 

60.8 

_|_ 

0.6 

~3y 

T  7  /*  7 

136.8 

4 
X 

2.6 

a  r 

199.7 

I99.9 

4_ 

1 

0.2 

I  C  I 

'5 1 

1 10. 1 

108. 1 

2.0 

260 

2 1 7.4 

* 1 7-4 

0.0 

4U 

I36.3 

136.7 

X 

0.4 

354-3 

357-3 

T 

3.0 

225.2 

2  I9.7 

5-5 

47 

1 12.8 

113. 5 

X 

0.7 

217.6 

1 

X 

0.5 

262 

*,* 

224.5 

X 

0.3 

C  1 

14.0.3 

7  C  7  7 

X 

4-y 

I  C2 

J 

7  A  C  C 

'45-5 

144.0 

'•5 

263 

227.3 

222.9 

4-4 

C2 

289.6 

28c  c 

4-1 

7  C  7 

'53 

35^-5 

35  !-4 

5-i 

2^f 

277  8 
277.0 

273.I 

4-7 

C  r 

_  }  1  -  0 

6 

5-7 

154 

75-° 

71.7 

3-3 

205 

277-4 

279.7 

4 

2-3 

5" 

1 84. 1 

178.0 

6.1 

1  c6 

213.6 

3.0 

266 

f 

i-3 

Co 

5y 

I7O.9 

7  7  7  n 

1  /  3-y 

X 

7  n 

ic8 

18  7 
10.3 

9.4 

8  0 

o.y 

267 

T 

144.2 

144.2 

0.0 

6] 

8l.2 

81. 1 

162 

210.6 

209.9 

0.7 

270 

I3I-3 

136.5 

4 
1 

5.2 

D4 

57-9 

C/i  R 
54.8 

3-1 

163 

202.0 

197-7 

4-3 

271 

IO8.5 

110-1 

X 

1.6 

°5 

1  ^u.o 

1 

X 

1.8 

166 

125.2 

124.0 

o'2 

272 

J74-9 

J73-3 

1.6 

67 

1 1 5.8 

1 

X 

2.3 

239. 1 

238.9 

■ 

274 

1 18.3 

128.5 

4 
1 

10.2 

60 

18.0 

17.2 

0.8 

170 

263.7 

3-5 

z/3 

188. 1 

187. 1 

" 

70 

3*9-7 

3 19.4 

0.3 

173 

181. 0 

180  1 

0.9 

277 

224.2 

225.2 

_L 
X 

72 

3J5-2 

3  !5-3 

l 

X 

0.1 

174 

60.5 

57-3 

3.2 

278 

301.7 

297.1 

A  (l 
4.O 

73 

22 1.3 

221.0 

0.3 

176 

103.5 

104.4 

+ 

0.9 

2o  2 

120.5 

12 1 .2 

X 

O.7 

74 

285.9 

285.8 

- 

0.1 

191.4 

188. 1 

3-3 

283 

94.1 

95-5 

+ 

1-4 

7  c 

/  5 

222.8 

7  7 

3-/ 

177 

*  /  / 

2I9.6 

215.2 

A  A 

3-4 

285 

y*r*  / 

94-3 

O  A 

77 

171. 8 

173.2 

X 

1.4 

l8l 

37-8 

35-5 

2.3 

286 

7-9 

6.9 

I.O 

82 

130.5 

13 1.6 

+ 

1.1 

183 

164.4 

160.7 

3-7 

288 

155-9 

156.7 

+ 

0.8 

83 

163.0 

163-5 

+ 

0.5 

I84 

164.8 

160.3 

4-5 

290 

21.9 

18.6 

2.3 

85 

224.1 

223.6 

0.5 

187 

37-7 

36.3 

i-4 

292 

10.7 

10.3 

0.4 

86 

52.3 

5i-5 

0.8 

I89 

105. 1 

105. 1 

0.0 

293 

49-3 

47.2 

2.1 

90 

3'7-° 

319.8 

+ 

2.8 

I9I 

173-5 

176.2 

+ 

2.7 

295 

22.2 

22.0 

0.2 

92 

276.1 

276.9 

+ 

0.8 

194 

214.5 

206.1 

8.4 

296 

251.6 

25 1.2 

0.4 

96 

IS7-7 

156.6 

1.1 

195 

108.7 

104.7 

4.0 

297 

77.2 

80.5 

+ 

3-3 

97 

74-9 

77-3 

X 

2.4 

197 

40.2 

38.8 

1.4 

298 

25.6 

27.5 

X 

1.9 

100 

224.8 

221.7 

3-i 

285.6 

282.1 

3-5 

301 

75-4 

78.2 

+ 

2.8 

IOI 

310.4 

3 1 1.9 

+ 

i-5 

20I 

285.8 

275.8 

1 0.0 

302 

81.7 

84.5 

+ 

2.8 

102 

67.6 

63.0 

4.6 

202 

1 3 1.0 

130.5 

0.5 

303 

292.8 

293.3 

+ 

0.5 

104 

301.3 

298.5 

2.8 

204 

269.2 

278.0 

+ 

8.8 

305 

135.0 

140.5 

+ 

S-5 

105 

74.6 

79-9 

+ 

5-3 

205 

288.5 

280.0 

8.5 

306 

27.2 

22.4 

4.8 

107 

16.1 

13-5 

2.6 

206 

296.7 

292.2 

4-5 

307 

155.0 

156.5 

+ 

i-5 

109 

157.6 

157-3 

0.3 

207 

166.9 

168.4 

+ 

i-5 

308 

348-3 

352.1 

+ 

3-8 

110 

140.9 

139.2 

i-7 

208 

30.2 

29.9 

°-3 

309 

335-2 

336.8 

+ 

1.6 

112 

51.8 

50.4 

1.4 

212 

265.8 

263.7 

2.1 

310 

1.9 

2.1 

X 

0.2 

I13 

75.0 

74-9 

0.1 

213 

83.! 

80.4 

2.7 

3»3 

125.8 

128.2 

+ 

2.4 

US 

258.0 

255-9 

2.1 

215 

124.7 

127.4 

+ 

2.7 

316 

265.1 

265.9 

+ 

0.8 

116 

200. 6 

298.1 

i-5 

2l8 

67.2 

61.8 

5-4 

318 

185.4 

183.4 

2.0 

OF  DOUBLE  STARS. 


285 


No. 

Equ. 

Refl. 

R — E. 

No. 

Equ. 

in  n . 

IV — I .  . 

No. 

£.0,11. 

1  1  '  1 1  . 

0 

0 

0 

0 

0 

O 

0 

0 

O 

320 

H7-3 

149.8 

4-  2.6 

361 

265.1 

267.7 

+  2.6 

388 

1 10.4 

108.8 

-  1.6 

32! 

5.0 

7-i 

+  2.1 

362 

89.6 

89-3 

-  0.3 

389 

82.9 

83.9 

4-  1.0 

322 

147.6 

149.3 

+  i-7 

363 

150.7 

148.3 

-  2.4 

390 

282.3 

282.8 

+  0.5 

323 

28.0 

24.8 

-  3-i 

365 

29.3 

23.2 

-  6.1 

393 

173-3 

171. 0 

-  2-3 

326 

43-5 

41.3 

—  2.2 

366 

115. 0 

H8.7 

+  3-7 

394 

30.7 

32.4 

+  1.7 

329 

75-5 

75-3 

—  0.2 

368 

17.2 

12.2 

-  5-° 

395 

71.7 

76.4 

+  4-7 

330 

267.4 

268.0 

+  0.6 

371 

34.6 

3 1.2 

-  3-4 

397 

57.6 

59.2 

+  1.6 

33* 

171-3 

169.9 

-  i-4 

372 

101.4 

98.9 

-  2-5 

399 

276.8 

275.0 

-  1.8 

333 

269.5 

267.0 

-  2.5 

373 

164.5 

168.O 

+  3-5 

402 

260.5 

262.0 

+  i-5 

336 

107.3 

1 17.4 

4- 10. 1 

374 

110.8 

1 1 1.5 

+  0.7 

403 

291.2 

288.7 

-  2.5 

341 

276.1 

275.9 

—  0.2 

375 

254.9 

254-5 

—  0.4 

405 

176.7 

176. 1 

-  0.6 

344 

90.1 

93.0 

+  2.9 

377 

307.0 

296.2 

—  10.8 

406 

311. 5 

310.7 

-  0.8 

345 

300.4 

302.1 

+  i-7 

378 

92.4 

94.4 

+  2.0 

407 

19.7 

18.3 

-  1-4 

346 

179.6 

178.7 

-  0.9 

380 

82.9 

8l.O 

-  1.9 

409 

211. 5 

208.2 

-  3-3 

350 

359-3 

359.8 

+  0.5 

383 

14.2 

13-7 

-  o-5 

411 

90.2 

90.5 

-  °-3 

3Si 

75-5 

79.0 

+  3-5 

384 

169.2 

169.2 

0.0 

414 

268.8 

270.0 

+  1.2 

359 

78.6 

77-4 

—  1.2 

387 

100.2 

98.2 

—  2.0 

(168)  These  differences  being  projected  on  a  chart  of  engraved  squares,  an  interpolating  curve 
was  constructed  and  read  off,  when  the  following  table  of  reductions  resulted. 


R. 

E  — 

R. 

R. 

E  — 

R. 

R. 

E  — 

R. 

R. 

E  — 

R. 

R. 

E  — 

R. 

R. 

E  — 

R. 

0 

0 

0 

0 

0 

0 

0 

0 

0 

0 

0 

0 

0 

+2 

.  5 

60 

+  1 

.  0 

120 

-0 

.  9 

180 

+0 

.  8 

240 

+  1 

.  9 

300 

+  1 

.  4 

10 

+2 

.  5 

70 

+0 

.  6 

130 

-1 

.  1 

190 

+1 

.  5 

250 

+  1 

.  6 

310 

+  1 

.  6 

20 

+2 

.  4 

80 

+0 

.  3 

140 

-1 

.  1 

200 

+2 

2 
•  * 

260 

+  1 

.  3 

320 

+  1 

.  9 

30 

+  2 

.2 

90 

0 

.  0 

150 

-0 

.  9 

210 

+2 

.  6 

270 

4-1 

.  2 

330 

+2 

.  1 

40 

+  1 

.  9 

100 

-0 

.  3 

160 

-0 

.  6 

220 

+2 

.  5 

280 

+  1 

.  2 

340 

+2 

.  3 

50 

+  1 

.  5 

110 

-0 

.  6 

170 

+0 

.  1 

230 

+2 

.  3 

290 

+  1 

.  3 

350 

+2 

.  4 

60 

+  1 

.  0 

120 

-0 

.  9 

180 

+0 

.  8 

240 

+  1 

.  9 

300 

+  1 

.  4 

360 

4-2 

.  5 

(169)  This  table  exhibits  what  may  be  called  the  Bias-correction  to  be  applied  to  the 
20-feet  positions ;  and  the  effect  of  this  correction  when  so  applied  is  to  produce  a  much  better 
general  accordance,  and  an  even  distribution  of  positive  and  negative  errors.  In  any  case,  then, 
where  it  may  become  necessary  to  call  in  the  evidence  of  the  20-feet  measured  positions  (which, 
be  it  observed,  I  do  not  recommend  to  be  done  in  any  case  where  deliberate  and  careful 
measures  with  an  equatorially  mounted  instrument  can  be  had),  I  consider  it  necessary  to  apply 
this  correction.  As  an  example,  I  shall  take  the  20-feet  measures  of  the  position  of  a  Centauri, 
the  mean  of  which  for  the  mean  epoch  1835.791  is  215°  16'.  Now,  when  it  is  considered  that  in 
this  instance  none  of  the  five  20-feet  results  obtained  rest  on  single  measures,  and  that,  of  all  the 
eighteen  individual  measures  concerned  in  producing  it,  the  highest  (217°  18')  falls  materially 
short  of  the  lowest  of  the  mean  epochal  results  of  the  equatorial  measures,  it  will  hardly  be 
denied,  1st,  that  some  distinct  biassing  cause  must  have  existed  to  produce  such  a  disagree- 
ment ;  and  2dly,  that  the  tabular  correction  (  +  2°  33')  which  brings  up  the  deficient  result  to 
217°  49',  if  shown  to  rest  on  a  large  induction  of  instances  extending  over  all  kinds  of  stars, 
presented  in  all  sorts  of  positions,  is  not  only  admissible,  but  essential.  The  result  so  corrected 
still  falls  short  of  the  equatorial  result  for  the  same  epoch  (1835.791),  viz.,  219°  12'  by  1°  23' 

4  D 


'286 


COMPARISON  OF  ANGLES  OF  POSITION  OF  DOUBLE  STARS. 


which  seems  to  indicate  that  the  bias  in  question  acted  in  the  case  of  this  fine  star  in  a  more 
positive  and  efficacious  manner  than  in  those  of  less  conspicuous  and  closer  objects.  I  should 
observe,  however,  that,  in  examining  with  care  all  the  cases  of  comparison  presented  in  the  table, 
Art.  167,  I  have  not  found  any  distinct  ground  for  concluding  either  the  magnitudes  of  the  stars 
or  their  distance  (when  well  seen  and  well  separated),  to  have  exercised  any  systematic  influence 
on  the  angles,  or  on  the  amount  of  the  Bias  correction. 

(170)  As  it  may  fairly  enough  be  presumed  that  this  Bias,  whatever  its  cause  may  be,  acts 
equally  on  all  angles  of  position  measured  in  the  same  way,  the  positions  of  Saturn's  satellites 
measured  with  the  20-feet  will  also  stand  in  need  of  the  same  tabular  correction  to  render  them 
comparable  with  the  measures  which  have  been  obtained  with  the  equatorial,  or  which  would 
have  been  obtained  (in  the  case  of  the  satellites  not  being  visible  in  that  instrument)  had  its 
optical  powers  been  sufficient  to  show  them.  As  the  correction  in  the  north  preceding  quadrant 
amounts  at  its  maximum  to  +  2°.6,  and  in  the  south  following  to  —  l°.l,  the  total  effect  of  the 
Bias  in  a  whole  revolution  of  a  satellite  is  equivalent  to  a  periodical  inequality  influencing  the 
position  to  a  total  amount  =  3°  42' :  the  correction  therefore  becomes  theoretically  important,  as 
indeed  it  would  be  in  the  rotatory  movement  of  a  double  star  if  it  continued  to  be  so  observed 
during  a  whole  revolution. 


SPECIAL  REMARKS 

ON  THE 

MEASURES  OF  PARTICULAR  DOUBLE  STARS 
IN  THE  FOREGOING  CATALOGUES. 


(171)  A  Toucani.  RA0h46m;  NPD160°26/.  The  mean  results  of  the  measures  for 
1835,  6,  7,  are  as  follows  : — 

1835.92  — Pos  =  78  30 
1836.73  "  80  18 
1837-74       "      80  35 

These  angles  indicate  a  direct  movement.  Mr.  Dunlop  states  the  quadrant  in  1 826  to  have 
been  s  f,  with  a  difference  of  declination  of  6". 62.  The  actual  difference  of  declination  at  the 
mean  epoch  1836.78  is  3'/.74  by  calculation  from  the  mean  distance  and  position  here  given.  As 
I  can  fully  rely  on  my  angles,  I  have  no  hesitation  in  supposing  the  quadrant  for  1826  to  have 
been  mistaken.  In  that  case,  if  the  difference  of  declinations  6V.62  can  be  depended  on,  and  the 
distance  be  supposed  unaltered,  the  position  in  1826  must  have  been  somewhere  about  71°  37', 
which  agrees  well  with  the  presumed  direct  motion.  This  star,  therefore,  deserves  further 
attention  as  an  instance  of  pretty  rapid  angular  rotation.  There  are  two  20-feet  measures  of  this 
6tar  which  (corrected  for  Bias  as  per  table  p.  285)  give  for  the  epoch  1834.836  the  angle  of 
position  76°  51',  which  agrees  exceedingly  well,  both  as  regards  direction  and  velocity,  with  the 
progress  of  the  movements  in  the  succeeding  years,  as  above  stated. 

(172)  h.  2036.  RA  lh  12™ ;  NPD  106°  41'.  The  change  of  angle  in  a  single  year,  if 
both  my  equatorial  measures  be  correct,  is  so  very  great  as  to  render  it  certain  that  this  star  is  in 
a  state  of  rapid  rotation.  The  place  being  such  as  to  admit  of  its  being  pretty  well  observed  in 
northern  latitudes,  I  have  consulted  former  catalogues  for  observations  of  it.  Struve's  does  not 
contain  it ;  but  in  my  5th  catalogue  of  double  stars  it  occurs,  with  a  mistaken  degree  in  N  P  D, 
as  h,  No.  2036.  Referring  to  the  original  sweep,  the  degree  appears  to  have  been  erroneously 
cast  up,  and  instead  of  105  (as  printed),  should  be  106.  There  can  be,  therefore,  no 
doubt  of  the  identity  of  the  object— as  the  description  (dist  =  2",  magnitudes  8=8)  agrees 
sufficiently  well.  The  angle  there  assigned  (53°.0)  by  a  mean  of  two  measures,  corroborates 
the  great  angular  movement,  and  agrees  in  direction.  The  observations  collected  run  as 
follows : — 


288 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


h.  2036.  —  1830.786  —  Pos  =  53°.00  —  Sweep  307. 
1835.717      "       45  .00 
1836.958      "       38  .05 

giving  an  angular  motion  of  14°.95  in  6.172  years,  or  —  2°.422  per  annum.  The  faintness  of 
the  small  star  (9  m)  renders  the  equatorial  measures  difficult,  so  that  the  angles  are  not  to  be 
considered  as  normal,  but  no  doubt  can  remain  as  to  a  rapid  rotation,  and  hardly  any  as  to  its 
being  on  the  increase. 

(173)  p.  Eridani.  R  A  lh  33m ;  N  P  D  147°  3'.  The  measures  of  1834  give  for  their  mean 
result  a  position  of  122°  48' for  the  mean  epoch  1834.841,  which,  compared  with  the  single  night's 
measure  of  1835  (1835.583  — Pos  =  120°  25'),  would  indicate  a  considerable  orbitual  motion. 
Without  desiring  to  attribute  too  much  weight  to  this  conclusion,  I  would  remark  that  the 
tendency  of  the  20-feet  measures  lies  in  the  same  direction.    They  run  as  follows : — 

Sweep  500.  —  1834.758  —  Pos  120°.8  > 

504         34.821  120  .1  }  ^U  1834-8°°  ~  P°S  12°°  2T 

732         36.693  119 .5  > 

735         36.753  119 .5 1  1836723  119  30 

These  results  are  uncorrected  for  Bias  (see  p.  285),  and  the  correction  when  applied  tend 
rather  to  increase  the  disagreement  of  the  absolute  positions  given  by  the  two  instruments.  But, 
so  far  as  any  value  at  all  can  be  attributed  to  them,  they  corroborate  the  orbitual  motion  con- 
tended for. 

Mr.  Dunlop  has  given  measures  of  this  star.  His  mean  result  for  1826  is  73°  6'nf  (=  16° 
54'),  which  must  surely  indicate  some  great  mistake.  Were  the  measure  really  73°  6' s  f  (corre- 
sponding to  a  position  =  163°  6'),  a  rotation  in  the  same  direction,  but  much  more  rapid  in  the 
interval,  would  account  for  it.    But  it  is  useless  reasoning  on  such  hypothetical  data. 

(174)  h.  3823.  R  A  5h  54m;  N  P  D  121°  4'.  The  mean  positions  and  epochs  for  1836  and 
1837  are  :— 

1836.626.  —  Pos  =  128°  58'  —  (5) 
1837.094  132°  2'  (5) 

The  star,  however,  appears  to  have  been  somewhat  too  faint  for  exact  measurement  with  the 
equatorial,  and  the  great  difference  of  the  measured  angles  for  epochs,  so  near  as  1836.988  and 
1837.071  (Equatorial  Measures  Nos.  1292,  1293),  throws  a  doubt  upon  the  orbitual  motion, 
which  would  otherwise  seem  to  be  very  great.  Still,  I  cannot  but  think  that  some  such  motion, 
and  in  this  direction,  must  exist,  the  more  especially  as  the  20-feet  angles  indicate  a  slight 
change  in  the  same  direction.  The  mean  result  of  the  20-feet  measures  (when  the  Bias 
correction  is  applied)  is  130°  30',  coinciding  precisely  with  the  mean  equatorial  result.  This 
star  belongs  to  that  interesting  class  of  objects  whose  colour  deviates  the  same  way  from  white- 
ness, like  61  Cygni  and  a  Centauri. 

(175)  A.  70.  R  A  8h  24m;  N  P  D  134°  10'.  If  any  confidence  can  be  placed  in  Mr.  Dunlop's 
measure,  this  star  must  be  in  a  state  of  rapid  rotation,  the  difference  of  his  position  for  1826 
(320°  18')  and  mine  for  the  mean  epoch  1835.49  (350°  18')  amounting  to  30°.  For  so  distant  a 
double  star,  this  would,  however,  be  an  extraordinary  rapidity  of  motion,  and  my  measures,  taken 
seriatim  (1833.273  —  350°  1',  and  1836.994  —  351°  27')>  though  indicating  a  change  in  the  same 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


289 


direction,  afford  no  corroboration  of  so  remarkable  an  angular  velocity.  The  20-feet  measures 
are  too  close  together  in  date  to  be  taken  as  evidence  of  change  in  their  interval,  and  their  actual 
difference  lies  the  opposite  way.  Their  mean  (corrected  for  bias)  is  350°  6'  for  1836.230,  agree- 
ing extremely  well  with  the  mean  equatorial  epoch  1835.49  —  350°  18'. 

(176)  A.  4128.  R  A  8h  36ra;  N  P  D  149°  43'.  The  measures  of  1835  and  1837  differ  by 
5°  47',  but  unfortunately  they  rely,  each  on  only  a  single  night's  measure,  and  those  of  1835  not 
good  ones.  Still  some  degree  of  direct  orbitual  motion,  though  perhaps  not  so  considerable  in 
amount,  seems  strongly  indicated. 

There  is  but  one  20-feet  observation  of  this  star  (in  sweep  764).  The  position  given  by 
it  (corrected  for  bias)  is  222°  42',  differing  only  0°  48'  from  the  mean  equatorial  result  221°  54'. 

(177)  h.  4130.  R  A  8h  37m;  N  P  D  146°  57'.  The  difference  of  the  measures  of  1835  and 
1837  is  no  less  than  7°  50',  but  the  measure  of  1835  is  especially  reprobated  as  too  difficult,  and 
in  1837  the  star  was  not  well  seen.  In  fact,  the  object  is  beyond  the  fair  reach  of  the  equatorial, 
and  from  the  20-feet  measure,  which  (corrected  for  bias)  comes  out  218°  54',  it  is  certain  that 
the  equatorial  measure  No.  1458  is  entirely  erroneous,  and  must  be  rejected. 

(178)  R.  9 ;  R  A  8h  41m;  IN  P  D  148°  6'.  The  comparison  of  the  mean  results  for  1835 
and  1837  indicate,  with  some  certainty,  a  considerable  angular  motion. 

1835.914  — Pos  =  112°  18'  (4) 
1837.128  109  11  (9) 

+  1.214  —3°  7' 

The  20-feet  measures,  it  is  true,  indicate  an  opposite  movement,  but  their  evidence  is 
not  to  be  taken  as  destroying  the  weight  of  the  above  conclusion,  though  it  renders  it  probable 
that  the  angular  motion  —  3°  1f  errs  in  excess.  Meanwhile  their  mean  (corrected  for  bias) 
comes  out  289°  27',  which  agrees  within  40'  of  our  mean  equatorial  result,  110°  6'  =  290°  6'. 

(179)  h.  4249.  R  A  9h  42™ ;  N  P  D  124°  14'.  Here  again  the  20-feet  measures  of 
Sweeps  541  and  809  oppose  the  conclusion  of  angular  movement,  which  else,  from  the  conse- 
cutive progression  of  the  results  (Nos.  1504,  1505,  1506,  equ.  meas.)  would  appear  satisfactorily 
enough  made  out.  Probably  all  the  measures  are  in  error,  and  in  such  a  case  it  is  satisfactory  at 
least  to  find  the  mean  of  the  20-feet  results  (corrected  for  bias  as  per  table),  viz. :  124°  57' — 
epoch  1836*54,  agreeing  within  a  quarter  of  a  degree  with  that  of  the  equatorial  measures 
125°  12'  — 1836.31. 

(180)  v  Argus  R  A  9h  43m;  N  P  D  154°  17'.  The  difference  of  3°  26m,  between  the 
measure  of  1836  and  the  mean  result  for  1837,  would  indicate,  with  considerable  certainty,  a 
direct  angular  motion  to  a  large  amount,  but  that  the  former  rests  only  on  a  single  night's  obser- 
vations. 

(181)  p  Hydra  and  Crateris.  R  A  llh  44m ;  N  P  D  122°  58'.  The  series  of  angles  of 
position  of  this  fine  double  star,  for  the  sub-epochs,  calculated  in  the  Synoptic  Table  for  1834.47, 
1835.23,  1836.68,  and  1838.09— which  are  respectively  338°.3,  339.3,  340.4,  and  342.2,  place 
the  binary  nature  and  direct  movement  of  this  system  beyond  a  doubt ;  the  amount  of  motion 
being  +3°. 9  in  3.62  years,  or  +1°.077  per  annum. 

The  20-feet  measures  of  this  star  run  quite  irregularly,  and  are  evidently  entitled  to  no 
reliance. 

4  E 


290 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


(182)  h.  4495.  R  A  llh  57m ;  N  P  D  122°  0'.  The  mean  equatorial  angle  differs  nearly 
7°  from  the  20-feet  result  (duly  corrected  for  bias).  But  the  small  star,  in  both  the  equa- 
torial sets  of  measures,  is  noted  as  10  m,  a  sufficient  indication  of  the  impracticability  of  measur- 
ing it  in  that  instrument  with  any  degree  of  certainty.  It  is  probable  that  errors  (arising  from 
the  inequality  of  these  stars)  exist  in  all  the  results. 

(183)  a  Cruets  R  A  12h  17m;  N  PD  152°  9'.  This  beautiful  double  star  has  attracted  the 
attention  of  all  the  more  recent  southern  observers.  Lacaille  does  not  notice,  however,  the  fact 
of  its  being  double,  from  which  Mr.  Riimker  surmises  that  it  may  have  been  closer  in  his  time 
than  at  present,  which  is  rendered  not  improbable  by  a  comparison  of  measures  of  its  distance 
taken  within  the  last  twenty  years.  Mr.  Riimker  describes  it  as  involved  in  a  milk-white 
nebulosity  (Preliminary  Catalogue,  pp.  15,  17),  a  description  which  I  am  at  a  loss  to  understand, 
unless  it  refer  to  the  bright  surrounding  light  of  the  Milky  Way.  At  least  I  have  never  noticed 
any  nebulous  accompaniment  to  this  star,  on  any  of  the  very  frequent  occasions  on  which  I  have 
viewed  it,  or  shown  it  to  others. 

(184)  In  attempting  to  trace  the  orbitual  motion  of  the  individuals  of  which  this  double 
star  consists  about  their  centre  of  gravity,  we  are  deprived  of  any  assistance  from  their 
catalogued  differences  of  R  A  and  N  P  D,  by  the  absence  of  any  such  differences  in  Lacaille's 
catalogue,  and  by  their  precariousness  in  more  recent  ones.  In  such  a  case,  micrometrical 
measurements  only  can  be  relied  on,  and  of  these  I  am  not  aware  of  the  existence  of  any  prior 
to  those  recorded  by  Mr.  Dunlop  in  1826.  (Mem.  Art.  Soc.  vol.  iii.)  Mr.  Riimker,  it  is  true, 
assigns  12'/.3  as  the  A.  R  A  in  arc,  and  4".45  as  their  A.  P  D,  but  he  does  not  state  how  these 
quantities  were  obtained,  and  it  is  to  be  presumed  that  they  result  from  independent  places  of 
the  stars.  Comparing  therefore  only  Mr.  Dunlop's  measures  (their  mean  result  and  epoch)  with 
my  own,  taken  with  the  equatorial,  we  have  as  follows : 


Authority. 

Epoch. 

Position. 

Epoch. 

Distance. 

Dunlop, 

1826.45 

114°  24' 

1826.23 

5".29 

Herschel, 

1835.33 

120  36 

1836.36 

5  .65 

8.88 

+6°  12' 

(185)  If  the  position  assigned  by  Mr.  Dunlop  can  be  entirely  relied  on,  this  comparison 
indicates  an  orbitual  motion  at  the  rate  of  +  0.698  per  annum.  This  conclusion,  however,  is 
not  reconcilable  with  the  series  of  sub-epochs  computed  from  the  measures  of  the  successive 
years  1834,  5,  6,  7,  8,  as  stated  in  the  foregoing  synopsis  of  my  measures,  which  indicate  with 
considerable  decision,  a  much  slower  orbitual  motion  (—  0°.478  per  annum),  and  in  the  opposite 
or  retrograde  direction. 

(186)  a  Crucis  is  accompanied  by  five  small  stars  to  the  southward,  arranged  in  an  irregular 
line  concave  towards  the  large  stars.  Of  these,  the  principal  and  the  most  distant  has  been 
observed  by  Lacaille,  and  by  most  subsequent  astronomers.  Respecting  the  magnitude  of  this 
star  there  is  a  good  deal  of  difference  of  statement.    Lacaille  calls  it  7  m,  Johnson  5,  Fallows 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


291 


and  Taylor  4,  Dunlop  6  or  6.7.  In  my  equatorial  observations  it  is  marked  6  and  7,  while  (as 
might  be  expected),  in  the  20-feet  it  has  been  estimated  at  5  m.  Probably,  therefore,  5.6  m  is 
about  the  truth.  It  is  its  proximity  to  so  bright  a  star  as  a  Crucis  which  makes  the  estimation 
difficult.  From  the  differences  of  the  catalogued  places  by  Lacaille,  Fallows,  Johnson,  and 
Taylor,  and  from  the  micrometrical  measurements  of  Mr.  Dunlop  and  my  own,  the  following 
may  be  stated  as  a  synopsis  of  its  computed,  or  measured  position  and  distance.  The  micro- 
metrically  measured  elements  reckon  from  the  larger  star  of  the  double  star ;  those  computed 
from  the  catalogued  differences,  from  the  middle  between  the  two  constituents. 


Authority. 

Epoch. 

Position. 

Distance. 

Lacaille, 

1750 

215°  48' 

92".45 

Fallows, 

1824 

203  12 

92  .47 

Dunlop, 

1826 

200  0 

87  .29 

Johnson, 

1830 

202  18 

87  .99 

Herschel, 

1836.43 

201  30 

Ditto, 

1836.75 

90  .69 

On  the  whole  of  this  evidence  it  may  be  probably  concluded  that  the  small  star  in  question 
has  not  materially  changed  its  relative  situation  with  respect  to  the  large  one,  since  there  is 
reason  to  suppose  that  Lacaille's  difference  of  Right  Ascensions  ( — 7.60),  from  which  the 
results  for  1750  are  calculated  is  too  large.  If  this,  however,  be  not  the  case,  a  difference  of 
proper  motions  exists  which  carries  the  small  star  relatively  in  a  direction  nearly  at  right  angles 
to  the  line  connecting  it  with  the  great  one. 

(187)  y  Centauri.  R  A.  12  32  NP  D  138°.l'.  The  extreme  closeness  of  the  individuals 
of  this  remarkably  fine,  but  difficult  double  star,  which  are  equal,  and  each  of  the  4th  magnitude, 
necessarily  renders  the  positions  precarious.  Nevertheless,  their  assemblage  in  two  sub-epochs, 
1835.32  and  1836.63,  so  chosen  as  to  divide  the  total  value  (13)  of  the  whole  series  of  measures 
equally  between  them,  leaves  no  room  to  doubt  of  a  very  rapid  direct  angular  movement,  for  we 
thus  obtain  the  following  data  : 

Sub-Epoch  —  1835.32  —  Pos  351°  35'  (7) 
1836.38  357  21  (6) 

Interval,  1.06  Motion,  +5°  46' 

which  is  at  the  rate  of  +  5°.440  per  annum. 

(188)  y  Virginis.  R  A  12h  33m  N  P  D  90°  31'.  The  apparent  perihelion  passage  of  this 
interesting  double  star  took  place  in  the  first  half  of  1836,  and  the  appulse  of  the  two  stars 
proved  (as  predicted)  so  very  close  as  to  cause  it  to  appear  as  a  single  star  to  all  but  the  most 
powerful  and  perfect  existing  telescopes  under  the  most  favourable  circumstances.  In  no  part  of 
the  interval  from  1835.971  to  1837.545,  both  dates  inclusive,  was  it  possible  to  observe  any 
certain  elongation  of  the  united  discs  with  the  7-fcet  equatorial,  capable  of  being  in  the  smallest 
degree  relied  on  for  a  measure.  It  should  be  observed,  however,  that  owing  to  the  influence  of 
the  arid  and  heated  sandy  tract  intervening  between  Feldhausen  and  Table  Bay,  to  the  north- 


292 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


ward  of  the  former  station,  it  was  rare  to  procure  even  moderately  tranquil  images  of  stars 
situated  so  near  the  equator.  In  consequence,  almost  all  the  measures  obtained  of  this  star  were 
procured  only  by  the  most  obstinate  patience  and  perseverance  in  waiting  for  favourable 
glimpses,  occurring  among  long  intervals  of  confused  and  agitated  definition,  as  the  notes 
appended  to  the  individual  night's  results  sufficiently  show. 

(189)  During  the  interval  between  the  dates  above  mentioned,  the  star  was  frequently 
examined.  On  the  night  of  the  21st  Dec.  1835,  it  was  kept  in  view  nearly  an  hour,  trying  all 
sorts  of  methods  to  divide  it,  but  in  vain. 

"  I  see  the  disc  round  and  sharp,  though  tremulous,  and  the  rings  &c.  all  in  motion ; — no  power  I  can  apply 
gives  me  the  least  certainty  of  an  elongation.  To  this  telescope,  with  its  highest  power  and  in  good  action,  the 
star  is  single.  (7  feet  Equ.)" 

Again,  on  the  23rd  December,  1835,  it  was  examined  with  all  the  usual  powers  up  to  400. 

"  Definition  very  far  superior  to  any  I  have  ever  had  of  this  star  since  I  have  been  at  the  Cape.  Its  disc,  at 
the  best  moments,  is  seen  steadily  round.  I  can  no  way  succeed  in  dividing  it.  When  the  focus  is  over-urged, 
to  give  the  smallest  disc,  it  was  seen  a  little  wedge-formed  downwards,  but  turning  the  telescope  in  that  state  on 
Spica  the  same  appearance  was  seen.  This  observation  was  made  just  before  and  during  the  morning  twilight, 
and  as  the  star  gained  altitude  the  definition  continued  improving." 

"  January  10,  1836.  In  the  best  moments  I  fancy  I  see  a  very  trifling  elongation — roughly  about  the  direc- 
tion of  the  meridian  with  279  and  300."  [400]  "  Worked  at  it  a  full  hour,  turned  the  object-glass  and  its  cell  in 
the  tube  half  a  turn  round  with  remarkably  good  effect." 

"  February  9,  1836.  In  the  commencement  of  twilight,  in  the  thin  scud  of  a  black  south-easter,  which  is 
beginning  to  bring  up  its  cloud  after  a  cloudless  night,  I  feel  pretty  sure  that  there  is  an  elongation  as  indicated. 
Pos  13°  50'  a  single  measure,  with  the  lowest  weight  a  measure  can  have." 

February  18,  1836, — 20-feet  reflector.  "  Viewed  y  Virginis  with  powers  320  and  480  which  gave  round  discs 
and  very  good  definition  ;  but  could  get  no  indication  of  its  being  double.  Far  better  defined  than  y  Centauri." 
which  had  just  before  been  viewed  with  the  same  instrument,  and  which  was  seen  well  elongated,  and  in 
momentary  glimpses  separated  with  320  and  a  triangular  aperture. 

May  3,  1836.  "  With  the  utmost  patience  and  the  greatest  difficulty,  from  the  violent  agitation  of  the  star,  I 
think  I  have  a  measurable  elongation.    Pos  =  5°  30'"  (by  a  single  measure). 

May  12,  1836.  "  y  bears  No.  4  better  than  usually  No.  3,  and  I  am  almost  sure  it  is  elongated  a  very  little." 
Pos  =  3°  30'  (by  a  single  measure  marked  +). 

"  January  14, 1837.  Being  a  most  glorious  night,  I  waited  till  lOh.  20m.  Sid.  T,  and  then  attacked  y  Yirginis. 
Capitally  defined,  though  catching.  Bore  No.  4  well.  In  some  moments  I  keep  suspecting  an  elongation  from 
/  to  p,  but  at  others  it  is  quite  round.  Put  on  aperture  2\  inches — a  beautiful  planetary  disc  without  rings.  If 
it  be  elongated  the  major  axis  is  not  more  than  ^  greater  than  the  minor.  In  short,  I  came  to  the  conclusion 
that  for  anything  I  could  see  to  the  contrary  the  star  is  single.  In  this  state,  turned  the  telescope  on  y  Centauri 
which  the  powers  No.  3  and  No.  4  distinctly  elongate,  consequently  I  conclude  that  the  distance  of  y  is  at  most  J, 
perhaps  |  that  of  y  Centauri,  which  is  certainly  under  1"." 

"  April  24,  1837.  The  best  sight  of  y  Virg.  I  have  ever  got  since  my  residence  at  the  Cape.  Quite  round 
with  No.  4,  nor  the  smallest  sign  of  elongation  that  I  can  perceive.  The  rings  brandish  a  little,  but  slowly,  and 
the  disc  moulds  a  little,  but  it  is  altogether  finely  defined,  and  examined  quite  at  ease.    2  west  of  merid." 

"May  18,  1837.  Scarcely  a  doubt  of  elongation.  Long  contemplated  with  No.  4.  It  is  surely  not  round, 
and  position,  by  3  measures,  =  202°  0'.  (Brandishing  but  a  disc.)  After  an  hour's  rest  of  the  instrument  much 
less  evidently  elongated.    Still  I  think  it  is  so,  but  am  by  no  means  so  certain  as  when  first  seen." 

"  June  27,  1837.  I  am  almost  certain  of  an  elongation  60°  ±  n  f  or  s  p  ;  but  the  star  will  not  bear  No.  4. 
No.  3  shows  it  round,  but  wants  power.  A  reading  (such  as  it  was)  of  the  micrometer  taken,  gave  Pos  =  211° 
407' 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


293 


"  July  19,  1837.  Certainly  elongated.  Of  this  I  have  no  douht.  The  star  is  better  defined  than  I  ever  saw 
it  at  the  Cape  under  No.  4.  Definition  excellent — for  this  star  unequalled.  Pos.  by  a  single  reading  210°  20'. 
—Further  examined.  When  best  in  focus,  i.  e.  when  disc  reduced  to  its  least  magnitude,  perfectly  round.  Turned 
the  telescope  on  f3  Corvi  and  d  Corvi.  In  similar  state  of  the  focus  I  see  the  same  elongation  in  the  same  direc- 
tion, but  when  perfectly  adjusted  the  discs  are  quite  round,  and  so  is  that  of  y  Virginis." 

(190)  Such  is  the  history  of  my  observations  of  this  star  during  its  perihelion  appulse. 
The  time  of  the  perihelion  passage  appears  to  have  been  retarded  nearly  two  years  beyond  that 
predicted  in  my  first  calculation  of  the  orbit,  the  elements  of  which,  however,  as  subsequent 
observation  has  shown  (with  the  exception  of  the  excentricity),  are  incapable  of  representing  the 
motion  of  the  stars  far  beyond  the  limits  for  which  they  were  calculated,  however  completely  the 
conditions  of  it  were  satisfied  by  them  within  those  limits.  The  reason  of  this  abandonment  of 
the  old  supposed  orbit,  and  the  substitution  for  it  of  one  differing  so  very  widely  from  it  in  all 
but  the  single  element  above  mentioned,  which  the  further  progress  of  observation  has 
necessitated  will  be  readily  understood  by  the  inspection  of  the  annexed  figure,  in  which 


m 


MDAB  represents  the  actual]  orbit  described  by  the  one  star  about  the  other  at  S,  and 
m  d  a  b  the  orbit  represented  by  my  first  elements.  It  will  be  seen  that  the  two  orbits  are 
almost  exactly  coincident  over  all  that  portion  of  each  which  corresponds  to  the  interval 

4  p 


294 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


embraced  by  the  observations  from  1781  to  1835,  within  which  alone,  micrometrical  measures 
had  been  at  that  time  obtained — the  actual  or  smaller  ellipse  being  curiously  packed  within 
the  other  in  the  manner  of  an  osculating  curve,  intersecting  it  in  four  points,  and  deviating  from 
it  in  the  intervals  between  them  by  a  quantity  much  too  small  to  excite  any  suspicion  of  error  at 
that  time. 

(191)  This  is  not  the  first  by  many  instances  in  the  history  of  scientific  progress  where,  of 
two  possible  courses,  each  at  the  moment  equally  plausible,  the  wrong  has  been  chosen.  But  in 
this  case,  the  adoption  of  the  larger  ellipse  seemed  to  be  necessitated  by  the  positions  concluded 
from  the  observations  of  Mayer  in  1756,  and  of  Bradley  in  1718,  which  it  appeared  desirable,  if 
possible,  to  conciliate.*  Now,  however  that  micrometric  measures  have  been  sufficiently  mul- 
tiplied, positions  obtained  like  that  of  Bradley  by  mere  allineations  with  distant  stars,  one  eye 
being  at  the  telescope,  the  other  directed  to  the  heavens  ;  or  like  that  of  Mayer,  by  a  still  more 
insecure  method,  viz.,  by  independent  differences  of  R  A  and  P  D  taken  from  a  catalogue,  can 
by  no  means  be  admitted  among  the  normal  data  to  be  used  in  the  determination  of 
elements. 

(192)  The  lapse  of  a  very  few  years  sufficed  to  show  that  the  movements  of  the  stars  are 
performed  with  much  greater  rapidity,  and  in  a  much  smaller  orbit  than  that  at  first  assigned  to 
them.  Elements  of  their  orbit  have  been  computed  from  time  to  time  by  Messrs.  Maedler, 
Encke,  Captain  Smyth,  the  late  lamented  Professor  Henderson,  and,  recently,  by  Mr.  Hind  ; 
also  by  myself,  in  1843  (to  which  reference  has  been  made  by  Captain  Smyth,  in  his  useful  and 
elaborate  work,  "A  Cycle  of  Celestial  Objects,"  ii.  p.  281).  It  is  not  a  little  remarkable  that  all 
these  calculations  agree  in  assigning  almost  precisely  the  same  value  to  the  excentricity  (physically 
speaking,  the  most  important  of  all  the  elements)  as  that  resulting  from  my  earlier  calculations, 
though  they  differ  materially  from  each  other  in  the  position  of  the  orbit  in  space,  and 
especially  in  the  period;  Captain  Smyth's  period  still  extending  to  196  years,  while,  with  a 
certain  combination  of  other  elements,  so  low  a  period  as  124  years  seemed  to  myself  not 
absolutely  excluded ;  at  least  if  all  the  micrometrical  observations  on  record  be  considered  as 
entitled  to  equal  credit. 

(193)  This,  however,  for  reasons  which  will  presently  appear,  I  consider  more  than 
questionable ;  and  as  the  complete  establishment  of  the  elliptic  motion  of  this  binary  star  is  a 
point  of  high  importance — one  of  the  great  facts  indeed  of  modern  astronomy — a  re-investigation 
of  its  orbit,  founded  on  careful  examination  of  all  the  recorded  measures  will  not  be  deemed 
irrelevant  in  this  place.    To  this  end  there  are  assembled  in  the  following  table  the  mean  results 


*  In  my  earlier  investigations  of  the  orbit  of  this  star,  a  mistake  of  10°  was  committed  in  reading  off  from  a 
celestial  chart  the  angle  of  position  of  the  two  stars  a  and  S  Virginis,  with  which  Bradley  compared  the  double 
star.  Mr.  Henderson  has  rectified  this  mistake.  In  consequence  of  it  the  agreement  of  my  first  orbit  with 
Bradley's  observations  is  only  apparent,  my  calculated  position  for  1718  being  159°  17',  and  the  position  actually 
resulting  from  Bradley's  comparison  (with  the  due  corrections  for  precession  and  ocular  equation)  being  150°  52', 
instead  of  1G0°  52',  as  set  down  in  my  paper  (Mem.  Art.  Soc.  1832).  It  is  remarkable,  however,  that  Mr. 
Henderson  deduces  from  his  own  elements,  a  position  of  161°  16'  for  the  epoch  in  question,  differing  by  less  than 
2°  from  my  computation,  though  starting  from  such  widely  different  elements.  Both  are  erroneous,  however, 
and  this  important  observation  of  Bradley's  will  be  found  very  satisfactorily  represented  by  the  elements  about  to 
be  given  further  on. 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


295 


of  all  the  recorded  observations  of  its  angles  of  position  (micrometrically  measured)  which  had 
come  to  my  knowledge  up  to  Sept.  1845. 


No. 

t 

9 

Obs. 

No. 

t 

9 

Obs. 

No. 

t 

9 

Obs. 

1781.89 

1 70°  ia! 

J  TP 

H 

20 

l8'J2.'JO 

6q°  CC' 

D 

1837.21 

265°  27' 

Sm 

2 

1803.20 

I20  15 

H 

21 

.40 

71  26 

Sm 

40 

.41 

257  55 

2 

3 

1820.29 

105  15 

2 

22 

.52 

73  3° 

2 

41 

.48 

256  24 

M 

4 

1822.25 

IO3  24 

Sh 

23 

1833.18 

61  46 

h 

42 

1838.08 

237  28 

h 

5 

•35 

I02  44 

2 

24 

.30 

61  9 

D 

43 

.28 

235  41 

Sm 

6 

1825.32 

96  53 

S 

25 

•33 

63  10 

Sm 

44 

.32 

233  26 

D 

7 

.32 

97  55 

2 

26 

•37 

65  32 

2 

45 

•43 

231  5 

O 

8 

1828.35 

90  30 

h 

27 

1834.30 

47  9 

Sm 

46 

•43 

229  12 

M 

9 

.38 

91  30 

2 

28 

■31 

46  48 

D 

47 

1839.32 

214  35 

D 

IO 

1829.22 

87  43 

h 

29 

•38 

51  40 

2 

48 

.40 

217  12 

Sm 

ii 

•39 

88  17 

2 

30 

.41 

39  0 

h 

49 

1840.38 

205  43 

D 

12 

1830.38 

82  5 

h 

31 

.84 

33  26 

2 

50 

•45 

205  42 

0 

13 

•39 

81  29 

D 

32 

1835. 11 

21  27 

h 

51 

1841.34 

200  3 

D 

H 

•59 

82  10 

B 

33 

•38 

15  29 

52 

•35 

200  1 1 

M 

15 

1831.33 

77  12 

h 

34 

.40 

14  59 

Sm 

53 

1842.34 

197  25 

A 

16 

•35 

78  12 

D 

35 

1836.28 

350  9 

D 

54 

.41 

194  59 

D 

17 

.36 

80  55 

2 

36 

•34 

349  48 

Sm 

55 

1843.33 

191  36 

Sm 

18 

.38 

77  54 

Sm 

37 

.41 

331  34 

s 

56 

1845.34 

185  24 

Sm 

J9 

1832.27 

70  20 

h 

38 

1837.20 

280  25 

E 

In  this  table,  the  positions  set  down  on  the  authority  of  each  observer  (with  exception  of 
those  of  M.  Struve  in  1834)  are  the  means  of  his  recorded  observations  for  each  year.    The  first 
column  contains  a  number  for  reference  ;  the  second,  headed  t,  the  mean  epoch  of  observation  ; 
the  third,  headed  0,  the  angle  of  position  corresponding,  and  the  fourth,  the  initial  of  the 
observer's  name.* 

(194)  If  these  positions  be  projected  on  a  chart  of  engraved  squares  for  the  purpose  of 
mutual  intercomparison,  in  order  to  the  construction  of  an  interpolating  curve  representing  the 
most  probable  course  of  the  variation  of  this  element  during  the  whole  interval  of  observation,  it 
will  at  once  be  apparent  that  the  observations  of  M.  Struve  from  1828.38  to  1834.38,  both 
inclusive,  cannot  possibly  be  used  in  conjunction  with  the  rest  of  the  series.  A  curve  drawn 
through  the  points  representing  these  observations,  separates  itself  gradually  and  systematically 
from  that  which  expresses  with  the  utmost  consistency  and  regularity  the  general  course  of  the 
movement  as  deduced  from  all  the  other  authorities,  the  amount  of  deviation  at  length  reaching 
no  less  than  9°,  after  which  it  ceases  abruptly,  the  subsequent  results  of  M.  Struve's  measure- 
ments, as  well  as  those  previous  to  1828,  being  in  good  accordance  with  the  rest,  on  their 
whole  evidence,  as  so  represented.  This  is  clearly  a  case  in  which  no  middle  course  can  be 
taken.  To  include  these  observations  with  the  rest  by  a  system  of  taking  means,  would 
be  to  sacrifice  the  validity  of  both  series,  and  to  mar  the  chain  of  data  at  a  most  important 

*  A.  Airy;  B.  Bessel;  D.  Dawes;  E.  Encke;  H.  Sir  William  Herschel ;  h.  Herschel,  junior :  M.  Maedler; 
0.  Otto  Struve;  S.  South;  Sm.  Smyth;  2.  Struve;  s.  Sabler. 


296 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


point  of  its  history.  I  shall,  therefore,  proceed  independently  of  them,  and  as  it  would  be 
manifestly  unfair  in  an  investigation  of  this  nature  arbitrarily  to  retain  some  and  reject  others, 
among  a  series  of  results  recorded  by  the  same  observer,  shall  leave,  in  what  follows,  M.  Struve's 
measures  out  of  consideration,  proposing  on  another  occasion  to  make  them  a  subject  of  especial 
inquiry  with  a  view  to  the  determination  of  an  orbit  resting  solely  on  their  evidence.*  The 
observation  No.  53  having  been  made  with  a  double  image  micrometer,  giving  confessedly  dis- 
torted images,  and  standing,  moreover,  in  irreconcilable  contradiction  to  the  general  evidence  of 
all  the  other  observations  from  1840  to  1845  inclusive,  is  also  rejected. 

(195)  The  following  tables  express,  the  first,  a  series  of  mean  epochs  and  positions  deduced 
by  taking  means  of  the  observations  of  each  year  (with  the  exceptions  specified);  and  the 
second,  the  course  of  the  interpolating  curve  which  on  a  general  and  perfectly  impartial  con- 
sideration of  all  their  evidence,  appears  to  me  to  exhibit  the  most  probable  course  of  the 
movement  throughout  (as  deduced  from  observation  without  the  aid  of  any  elliptic  hypothesis), 
and  more  especially  during  the  year  1836,  when,  owing  to  the  excessive  closeness  of  the  stars,  all 
micrometrical  measurement  was,  if  not  precluded,  at  least  rendered  liable  to  errors  of  unusual 
magnitude. 


TABLE  OF  MEAN  OBSERVED  EPOCHS  AND  ANGLES  OF  POSITION  OF  y  VIRGINIS. 


t 

9 

0  1 

Observ.  used. 

t 

9 

0  / 

Observ.  used. 

t 

9 

0  / 

Observ.  used. 

1781.89 

130  44 

I 

1832.32 

7°  34 

19,  20,  21 

1838.31 

233  22 

42,  43.  44 

1803.20 

120  15 

2 

J833.27 

62  2 

23,  24,  25 

45.46 

1822.25 

103  24 

4 

1834.34 

44  19 

27,  28,  30 

1839.36 

215  53 

47.  48 

1825.32 

96  53 

6 

1835.25 

18  13 

32>  34 

1840.41 

205  42 

49.  5° 

1828.35 

90  30 

8 

1836.31 

349  ss 

35.  36 

1841.34 

200  7 

5i.  52 

1829.22 

87  43 

10 

1836.41 

331  34 

37 

1842.41 

194  59 

54 

1830.44 

81  55 

12,  13,  14 

1837.30 

267  25 

3»»  39.4i 

1843.33 

191  36 

55 

1831.35 

77  46 

15,  l6,  18 

1845.34 

185  24 

56 

TABLE  OF  INTERPOLATED  EPOCHS  AND  ANGULAR  VELOCITIES  OF  y  VIRGINIS  FOR  ANGLES 

OF  POSITION  FROM  io°  TO  io°. 


9 

t 

AB 

9 

t 

dd 

9 

t 

&9 

9 

t 

d9 

dt 

dt 

dt 

dt 

0 

0 

O 

0 

O 

0 

0 

O 

130 

1783.41 

0.48 

5° 

1834.04 

18.2 

33° 

1836.37 

62.0 

250 

1837.72 

34-5 

120 

1803.61 

0.60 

40 

1834.51 

23.3 

320 

1836.53 

67.2 

240 

1838.04 

28.0 

1 10 

1816.60 

0.99 

30 

1834.90 

29.4 

310 

1836.67 

70.8 

230 

1838.46 

20.9 

100 

1824.20 

1.74 

20 

1835.23 

33-3 

300 

1836.81 

72.0 

220 

1839.06 

14.9 

90 

1828.47 

3-i 

10 

1835.52 

37.0 

290 

1836.95 

71.2 

210 

1839.94 

9.6 

80 

1830.90 

5-i 

0 

1835.78 

41.7 

280 

1837.09 

66.4 

200 

1841.34 

5.6 

70 

1832.43 

8.2 

35° 

1836.01 

47.6 

270 

1837.25 

55.6 

190 

1843.84 

3.2 

60 

1833.40 

12.7 

34o 

1836.20 

55.6 

260 

1837.46 

43-9 

185 

1845.50 

2.7 

*  This  only  applies  to  the  observations  marked  2.  Those  by  M.  Otto  Struve,  with  the  Pulkova  telescope 
are,  of  course,  retained ;  as  also  the  highly  important  joint  observation  No.  37,  which  cannot  be  dispensed  with. 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


297 


(196)  Setting  out  with  this  latter  table  as  a  basis  of  calculation,  I 
Excentricity,  .  .  .  . 

Inclination  to  the  plane  of  projection,  .... 
Position  of  ascending  node,  ..... 
Angular  distance  of  Perihelion  from  Node  on  the  plane  of  the  i 
orbit,  or  true  angle  between  the  lines  of  Nodes  and  Apsides,  3 
Epoch  of  Perihelion  Passage,  ..... 
Periodic  time,  ....... 

and  the  following  formulae  of  computation  thence  resulting : 

tan  0  —  46°  15')  =  [0-03791]  .  tan  (0  —  5°  33') 

tan  I  m  =  [9  40293] .  tan  i  v. 

1836-43— t  =  [9-70408] .  { u  —  [170237]  .  sin  u.  ] 

(197)  Comparison  of  these  Formula  and  Elements  with  the  Table  of  mean  observed  Epochs, 
Art.  (191). 


t 

0C 

0c- 

■00 

t 

0c 

0c- 

-00 

t 

0c 

0c- 

-00 

0  / 

O 

0  / 

0 

0  / 

O 

1781.89 

131  0 

+  ° 

16 

1832.32 

70  8 

—  0 

26 

1838.31 

234  12 

+  0 

5° 

1803.20 

121  2 

+  1 

47 

1833.27 

60  10 

—  1 

52 

1839.36 

216  24 

+  0 

31 

1822.25 

IO4  52 

+  1 

28 

1834.34 

44  24 

+  0 

5 

1840.41 

206  4 

+  0 

22 

1825.32 

99  6 

+  2 

13 

1835.25 

20  26 

+  2 

'3 

1841.34 

199  50 

—  0 

"7 

1828.35 

9°  57 

+  0 

27 

1836.31 

333  27 

-16 

3i 

1842.41 

!94  33 

—  0 

26 

1829.22 

87  55 

+  0 

12 

1836.41 

325  40 

—  7 

44 

1843.33 

190  55 

—  0 

42 

1830.44 

82  24 

+  0 

29 

1837.30 

269  6 

+  1 

4i 

1845.34 

185  24 

—  0 

8 

1831.35 

77  13 

—  0 

33 

(198)  Comparison  of  the  same  Elements  and  Formula  with  the  Table  of  interpolated  Epochs. 


0 

0c- 

-00 

0 

0c- 

-00 

0 

0c- 

-00 

0 

0c- 

-00 

0 

O 

/ 

0 

/ 

O 

O 

0 

0 

'3° 

+0 

34 

50 

— 0 

40 

330 

-4 

8 

250 

+  1 

7 

120 

+  1 

47 

40 

4-0 

29 

320 

-4 

9 

240 

+0 

55 

1 10 

+  1 

59 

30 

+  1 

7 

310 

-4 

7 

230 

■+o 

59 

100 

+  1 

18 

20 

+  1 

2 

300 

-3 

22 

220 

4-o 

29 

90 

+0 

38 

10 

+  0 

28 

290 

—2 

43 

210 

+0 

12 

80 

—0 

6 

0 

—0 

52 

280 

+0 

4 

200 

—0 

9 

70 

—0 

46 

350 

—  2 

24 

270 

+  1 

33 

190 

—0 

5° 

60 

—  1 

14 

340 

-3 

30 

260 

+  1 

35 

185 

— 0 

34 

(199)  It  will  not  be  found  easy  to  represent  either  the  interpolated  or  the  mean  observed 
epochs  throughout  much  more  closely  than  by  these  elements.  With  regard  to  the  deviation  of 
16°  31'  in  the  observed  epoch  of  1836.31,  neither  Captain  Smyth  nor  Mr.  Dawes  are,  I  believe, 
disposed  to  attribute  any  weight  to  their  observations  at  that  epoch  ;  the  stars  being  then  so 

4  G 


find  the  following  elements  : 

e  -  0.87952 

y  =  23°  35'  40" 
«  =    5°  33' 

X  =  313°  45' 

1  =  A.D.  183643 

P  =  18212  years. 


298 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


excessively  close  that  a  doubtful  elongation  was  all  the  indication  of  its  being  actually  double 
afforded  by  their  instruments.  The  Dorpat  angle  at  the  perihelion  epoch  though  stated  by  M. 
Struve  (MensurcB  Micrometricte,  &c.  p.  288)  to  be  the  result  of  three  days'  observations  by 
Messrs.  Otto  Struve  and  Sabler,  is  in  fact  the  mean  of  two  measures  of  the  latter,  which,  no 
doubt  for  valid  reasons,  he  has  considered  preferable  to  the  others,  and  indeed  the  great 
difference  among  the  individual  measures  on  these  three  days  (which,  allowing  for  the  motion  of 
the  stars  in  the  interval,  amounts  to  fully  12°)  clearly  shows  the  difficulty  of  the  observation  and 
the  necessity  of  exercising  some  judgment  in  giving  a  preference  to  some  one  result  over  the 
other.  Now  one  of  M.  Sabler's  observations  thus  preferred  gives  329°  42'  for  the  position  at  the 
epoch  1836.41,  differing  only  by  4°  2'  from  our  computation.  The  other  discordances  are  not 
greater  than  may  very  reasonably  be  looked  for  in  the  present  and  past  state  of  this  inquiry,  even 
when  dealing  with  the  mean  results  of  several  observers :  and  the  chief  among  them  (that  of 
1825.32)  would  be  reduced  to  little  more  than  half  its  amount,  had  M.  Struve's  observation  at 
that  identical  epoch  been  used  in  place  of  that  actually  employed.  On  the  whole  showing, 
therefore,  I  think  it  will  be  readily  admitted  that  the  elliptic  hypothesis  is  very  satisfactorily 
sustained.  The  apparently  systematic  alternation  of  positive  and  negative  errors,  each  prevailing 
over  considerable  arcs  of  the  orbit,  might  indeed  be  regarded,  in  a  more  advanced  state  of  the 
subject,  as  indicative  of  some  disturbing  cause  of  a  periodical  character,  but  at  present  such  a 
conclusion  would  be  quite  premature. 

(200)  The  allineation  of  Bradley  and  Pound  of  the  two  stars  of  y  with  the  line  joining  a  and 
b  Virginis  in  1718.10  has  not  been  included  among  the  data  of  our  interpolations,  which  extend 
only  from  1781  to  1845.  It  will  therefore  be  interesting  to  see  how  nearly  our  new  elements 
represent  this  remarkable  observation.  I  have  already  observed  (see  note  on  Art.  191)  that 
the  true  angle  of  position  resulting  from  this  allineation  at  the  epoch  in  question  is  150°  52' 
instead  of  160°  52',  as  by  a  mistake  of  10°  in  reading  off  the  angle  of  position  of  those  two  stars, 
I  originally  stated  it.  Now  if  we  calculate  the  position  for  that  epoch  from  the  elements  above 
given,  we  find  it  to  be  149°  16',  differing  by  only  1°  36'  from  Bradley's  comparison  duly 
corrected  for  the  ocular  equation.  This  is  certainly  very  satisfactory,  being  within  the  limits  of 
what  we  must  even  now  call  good  micrometrical  measurement.  The  error  of  the  position 
concluded  from  the  places  of  the  two  stars  in  Mayer's  Catalogue  for  1756  is  —  5°  26'. 

(201)  Hitherto  no  notice  has  been  taken  of  the  apparent  distances.  They  have  formed  no 
part  of  the  data  from  which  any  of  the  elements  above  stated  have  been  computed.  The 
following  comparison  of  the  measures  taken  at  different  epochs  and  by  different  observers  with 
those  calculated  by  the  aid  of  these  elements  for  the  respective  epochs  exhibits  a  correspondence 
which,  under  all  the  circumstances  of  the  measurements,  must  be  regarded  as  in  the  highest 
degree  satisfactory,  and  as  completing  beyond  all  reasonable  doubt  the  evidence  in  favour  of 
elliptic  movement. 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


299 


t 

po 

pc 

pc — po 

Authority. 

t 

po 

pc 

u 

pc — po 

// 

Authority. 

1781.9 

5.63 

5.60 

—0.03 

H.  (?) 

1833.4 

1. 1 8 

I. IO 

—0.08 

Sm.  2. 

1803.2 

5.91 

+•97 

-0.94 

H-  (?) 

1834.3 

1.07 

O.84 

—0.13 

Sm,  h,  D,  2. 

1819.4 

3.56 

3-54 

— 0.02 

2. 

1835.4 

0.51 

O.64 

+0.13 

2,  Sm. 

1822.2 

3.32 

3.19 

-0.13 

2,  Sh. 

1836.4 

0.26 

O.5O 

+0.24 

2.  (?) 

1823.2 

3.30 

3.04 

—0.26 

Amici. 

1837.4 

0.60 

O.57 

—0.03 

2,  E,  M. 

1825.3 

2.8 1 

2.74 

—0.07 

2,  S. 

1838.4 

0.83 

O.86 

+0.03 

Sm,  O,  M. 

1828.4 

2.07 

2.21 

+0.14 

2. 

1839.4 

1.00 

I.02 

+0.02 

Sm. 

1829.3 

1.79 

2.05 

+0.26 

2,  h. 

1 840.4 

j.28 

I.37 

+0.09 

O,  D. 

1830.4 

1.90 

1.82 

—0.08 

B,  h. 

1841.3 

1.65 

I.6l 

—0.04 

D,  M. 

1831.3 

1.77 

1.62 

-0.15 

D,  h,  2,  Sm. 

1842.4 

1.72 

1.86 

+0.14 

A,  D. 

1832.4 

1.23 

i-37 

+0.14 

D,  h,  2,  Sm. 

1843.3 

1.90 

2.06 

+0.16 

Sm. 

In  this  table  po  denotes  the  observed  and  pc  the  calculated  apparent  distance  or  radius  vestor 
of  the  ellipse.  The  observations  of  1781  and  1803,  as  well  as  that  of  1836,  at  the  epoch  of  the 
perihelion  passage,  are  founded  on  estimation  of  diameters,  and  are  therefore  necessarily  liable  to 
greater  error  than  the  others,  which  all  rely  on  micrometrical  measures.  In  particular,  the 
estimate  of  1803  is  certainly  much  too  large.  That  of  1836  is  doubtless  an  under  estimate, 
owing  to  the  peculiar  and  difficult  circumstances  of  the  observation  of  which  an  account  may  be 
seen  in  M.  Struve's  great  work  (Mensures  Micrometricce,  &c.)  The  other  errors  are  all  within 
the  limits  which  the  different  micrometers,  and,  above  all,  the  different  habits  of  observers  in 
clipping  the  stars  more  or  less  closely,  &c,  have  hitherto  (unfortunately)  been  found  to  admit  as 
easily  possible,  and  which  render  it,  in  my  opinion,  impossible  to  employ  the  measurements  of 
distance  hitherto  recorded,  as  safe  elements  of  calculation.  The  semi-axis  of  the  real  orbit  which 
these  comparisons  suppose  is  9".69.* 


*  Since  the  greater  part  of  these  calculations  were  made,  I  have  received,  through  the  kindness  of  M.  Maedler, 
the  following  series  of  observed  epochs:  1841-355,  Pos  200°  6';  1842-361,  196°  11';  1843349,  192°  9';  1844356, 
188°  55';  1845-367,  186°  57'.  These  epochs  have  not  been  included  in  our  interpolation,  and  cannot  therefore  be 
fairly  compared  with  its  results.  When  projected  separately,  they  exhibit  a  systematic  and  regularly-increasing 
deviation  from  the  projection  of  Mr.  Dawes'  and  Captain  Smyth's  observations,  of  the  very  same  nature  as  that 
which  compelled  me  to  abstain  from  including  among  our  normal  data  the  Dorpat  observations  from  1828  to 
1834.  Facts  of  this  kind  go  to  prove  that  full  confidence  cannot  yet  be  placed  in  any  micrometrical  measures, 
even  of  position  angles,  and  in  the  case  of  easy  stars  (as  this  is  once  more  become) ;  and  they  lead  us  to  insist  on 
the  necessity  of  an  immense  accumulation  of  measures  from  a  variety  of  observers,  and  unremittingly  continued 
for  a  long  series  of  years,  as  the  only  ground  of  hope  for  the  attainment  of  accurate  elements  of  this  or  any  other 
double  star.  This  communication  is  accompanied  by  a  set  of  elements—  (the  fourth  now  calculated  by  this  inde- 
fatigable astronomer) — placing  the  perihelion  epoch  at  1836-29,  and  assigning  a  period  of  14878  years.  Com- 
paring the  orbits  which  seem  entitled  to  most  reliance,  it  appears  certain  that  the  excentricity  lies  between  0-855 
and  0-880,  the  inclination  between  23°  and  27°,  the  perihelion  epoch  between  1836-20  and  1836-45,  and  the  period 
between  140  and  190  years.  The  best  defined  element  is  that  which  is  usually,  but  absurdly,  called  the  place  of 
the  perihelion  on  the  orbit  (or  ft  +  \  in  the  notation  of  Art.  192),  which  cannot  differ  above  a  degree  one  way  or 
the  other  from  319°  20'.  This  language  ought  to  be  reformed,  and  the  element  itself  disused,  by  general  consent 
among  astronomers,  as  a  source  of  endless  misapprehension  and  mistake. 


300 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


(202)  k  Centauri.  R  A.  13"  42m,  N  P  D.  122°  9'.  In  obs.  1729  (Equatorial  Measures)  this 
star  was  measured  at  the  moment  when  close  to  and  almost  in  contact  with  Halley's  comet.  On 
the  measured  distance  I  can  place  no  reliance,  but  the  position  is  good  and  agrees  within  0°  42' 
with  the  mean  result  of  all  the  equatorial  measures,  and  within  0°  29'  of  the  twenty-feet  position 
corrected  for  bias.  No  argument  in  favour  of  any  refraction  in  the  atmosphere  of  the  comet  can 
be  drawn  from  the  measures  in  question. 

(203)  a  Centauri.  This  superb  double  star,  beyond  all  comparison  the  most  striking  object  of 
the  kind  in  the  heavens,  and  to  which  the  discovery  of  its  parallax  by  the  late  Professor 
Henderson  has  given  a  degree  of  astronomical  importance  no  less  conspicuous — consists  of  two 
individuals,  both  of  a  high  ruddy  or  orange  colour,  though  that  of  the  smaller  is  of  a  somewhat 
more  sombre  and  brownish  cast.  They  constitute  together  a  star  which  to  the  naked  eye  is  equal 
or  somewhat  superior  to  Arcturus  in  lustre.  Individually  their  magnitudes  have  been  very 
differently  estimated  by  other  observers  from  what  I  consider  to  be  the  correct  values.  All  agree 
indeed  in  assigning  the  first  magnitude  to  the  principal  star,  or  that  which  follows  in  R  A,  but 
whereas  Lacaille,  and  after  him  Fallows,  Johnson,  Taylor,  and  Messrs.  Dunlop  and  Riimker, 
estimate  the  preceding  star  as  of  the  fourth  magnitude,  I  have  never  estimated  its  magnitude  as 
seen  with  the  equatorial  lower  than  2.3,  and  the  mean  of  all  the  magnitudes  assigned  to  it  with 
that  instrument  is  1.73  or  If  by  a  mean  of  eleven  observations.  With  the  twenty-feet  it  is 
stated  on  the  only  three  occasions  on  which  its  magnitudes  has  been  registered  as  2,  1|,  and  3, 
but  the  latter  is  decidedly  an  under-estimate,  as,  on  the  very  numerous  occasions  in  which  the 
star  has  been  viewed  in  that  instrument,  my  habitual  judgment  has  inclined  rather  to  the  first 
than  the  second  magnitude — and  on  the  whole  evidence  afforded  by  my  experience,  I  am  dis- 
posed to  assign  to  it  a  magnitude  which  may  be  deemed  indifferently  either  a  very  low  first  or  a 
very  high  second.  That  this  judgment  is  not  to  be  lightly  put  aside,  appears  from  the  following 
note  which  I  find  appended  to  the  20-feet  observation  of  sweep  578  (April  24,  1835),  after  its 
measurement  as  a  double  star.  "  A  truly  noble  object.  The  image  received  on  a  sheet  of  good 
thick  letter  paper"  [N.B.  It  was  good  royal  superfine  drawing  paper.  Note  added  April  25#] 
"  was  distinctly  seen  behind  it;  when  the  paper  was  tripled  it  required  some  attention,  but  when 
doubled  it  was  conspicuously  visible.  At  four  feet  from  the  eyepiece,  it  showed  on  the  paper,  seen 
in  front  (by  reflected,  not  transmitted  rays),  a  superb  double  star.  The  light  was  very  strong,  and 
the  distance  might  easily  have  been  measured  with  a  pair  of  compasses  could  the  tube  have  been 
kept  steady.  The  ratio  of  the  lights  of  the  two  images  appeared  much  more  unequal  than  when 
viewed  through  the  telescope." 

(204)  It  is  not  necessary  to  recur  to  the  hypothesis  of  variability  to  account  for  this  diffe- 
rence of  estimation.  To  any  one  accustomed  to  the  use  of  large  telescopes,  as  compared  with 
those  with  which  the  observations  of  the  astronomers  above  enumerated  were  made,  the  fact  must 
be  familiar,  that  the  apparent  inequality  of  two  stars  seen  at  once  in  the  same  field  of  view 
diminishes,  as  the  light  of  the  telescope  is  greater.  With  the  cause  of  this  phenomenon,  which 
is  to  be  sought,  no  doubt,  in  the  physiology  of  vision,  we  have  here  no  concern,  but  it  ought  to 
be  always  borne  in  mind  when  the  comparative  magnitudes  of  stars  is  under  discussion.  I  may 
take  this  opportunity  to  mention,  that  advantage  may  be  taken  of  it  in  photometric  comparisons 
of  bright  objects,  when  it  is  required  to  decide  which  of  two,  nearly  equal,  is  the  brighter.  The 


*  On  actual  inspection  of  the  paper  next  morning  by  daylight. 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


301 


light  of  both  being  weakened  by  reflexion,  more  or  less  oblique,  at  a  glass  or  metallic  surface, 
degrees  of  inequality  will  be  rendered  evident,  in  a  manner  to  leave  no  doubt,  which  would 
otherwise  escape  notice.  I  have  more  than  once  had  recourse  to  this  mode  of  observation  in  the 
photometric  comparison  of  nearly  equal  bright  stars,  where  some  degree  of  uncertainty  has 
remained  as  to  their  rank  in  magnitude.  Of  course  it  is  necessary  that  both  should  be  reflected 
at  the  same  angle — a  condition  easily  satisfied  by  holding  the  reflecting  surface  so  that  the  line 
joining  the  reflected  images  shall  be  parallel  to  that  joining  the  direct  ones. 

(205)  The  proper  motion  of  this  double  star  is  so  considerable  (amounting,  according  to 
Mr.  Henderson's  determination,  to  3". 58  per  annum*),  that,  unless  a  physical  connexion  between 
the  individuals  be  supposed,  such  that  the  movement  of  translation  through  space  be  common, 
the  one  star  would,  in  the  interval  since  Lacaille's  observations,  have  left  the  other  behind  nearly 
5'  in  arc.  This  consideration  alone  suffices  to  decide  us  in  admitting  a  binary  connexion  between 
them,  and  it  will  therefore  be  interesting  to  see  what  evidence  observation  furnishes  of  orbitual 
motion  round  their  centre  of  gravity.  For  this,  however,  the  data  are  somewhat  precarious,  as 
we  have,  until  recently,  only  catalogued  differences  of  Right  Ascensions  and  Polar  Distances,  from 
which  to  calculate  the  angle  of  position  and  distance  at  the  epochs  of  observation.  This  done, 
and  the  results  tabulated,  together  with  my  own  positions  and  distances,  obtained  by  direct 
measurement  with  the  equatorial,  and  Mr.  Dunlop's,  recorded  in  his  paper  on  the  Southern 
Double  Stars,  we  have  as  follows : — 


Authority. 


Lacaille, 
Fallows, 
Brisbane,  . . . . , 
Dunlop,t- 

Johnson,  

Taylor  

Herschel,  jun.. 

Do. 

Do. 

Do. 

Do. 


Epoch  of 
Observation. 


1750 
[822  : 
[824  : 
825 
830 
831 
834.68 
834.79 
835.86 

837-34 
837.44 


A  R  A. 


—  1.70 
— 1.90 
-1.74 
-1.783 

-i-53 

—  1.77 


ANPD. 


+  16.0 
+  25.0 
+  18.3 
+  18.788 
+  16.3 
+  18.29 


Pos. 


218  44 
209  36 
215  25 
213  11 
215  2 
215  58 

218  30 

219  30 

220  42 


Dist. 


20.51 
28.75 
22.45 
22.45 
19.95 
22.56 
1743 


16.12 


(206)  Mr.  Fallows's  determinations  in  this  series  are  open  to  objection  from  the  decidedly 
inadequate  instrumental  means  by  which  they  were  furnished  (a  small  altitude  and  azimuth 
circle).  Mr.  Taylor's  results  also  rest  on  so  few  observations,  as  to  entitle  them  to  little 
weight.  It  will  be  observed  that  neither  here  nor  in  the  sub-epochs  calculated  in  the  general 
synopsis  of  my  equatorial  measures,  is  there  any  distance  assigned  for  the  middle  epoch, 
including  the  observations  from  1835.271  to  1836.285  inclusive.  The  reason  is  that  all  the 
distances  in  that  interval  were  obtained  with  the  thick  wires,  and  with  absolute  zeros,  and  are  not 


*  There  is  a  misprint  in  Mr.  H.'s  list  of  proper  motions,  Mem.  R.  A.  S.  xv.  The  star  is  called  a  Centauri, 
but  it  cannot  be  doubted  that  a  is  intended.    See  Johnson  and  other  authorities. 

t  The  distance  in  this  case  is  computed  from  Mr.  Dunlop's  measured  Position  and  difference  of  declinations. 

■     4  H 


302 


SPECIAL  REMARKS  ON  THE  MEASURES  OF 


therefore  entitled  to  be  brought  into  comparison  with  the  others  procured  with  the  spider  lines 
and  with  cross  zeros.  Indeed,  it  is  obvious  from  the  results  of  those  measures  set  down  in  the 
general  register,  as  corrected  by  the  Table  in  p.  246  (like  all  the  rest  in  that  register  so 
measured),  that  the  empirical  correction  so  applied  is  clearly  too  great  for  this  star,  which  from 
the  extraordinary  brightness  of  its  individual  constituents  must  be  held  to  be  an  exceptional 
case.    Neither  are  these  measures  included  in  the  general  epoch. 

(207)  Though  it  is  obviously  impracticable  to  deduce  any  elliptic  elements  from  such  a 
series,  there  are  some  features  which  it  is  impossible  not  to  recognise.  There  can  be  no  doubt 
that  the  distance  has  gone  on  steadily  decreasing  since  1822  at  least ;  and  the  comparison  of  the 
measures  least  open  to  objection,  leads  us  to  conclude  that  for  the  thirteen  years  previous  to 
1838,  the  rate  of  decrease  was  -fa,  or  a  little  more  than  half  a  second  per  annum,  which,  if 
continued,  will  bring  on  an  occultation,  or  exceedingly  close  appulse  about  the  year  1867.  The 
small  amount  of  variation  in  the  angle  of  position,  shows  that  the  plane  of  orbitual  motion 
passes  nearly,  but  not  quite  through  our  system,  while  its  actual  tendency  to  increase  exemplifies 
the  general  law  of  increase  of  angular  velocity  with  diminution  of  distance.  Mr.  Fallows's 
distance  is  probably  too  great  by  '6"  or  4"  ;  but  in  the  long  interval  between  1750  and  1822  (at 
the  former  of  which  epochs  the  distance  must  have  been  on  the  increase),  there  is  room  for  a 
very  much  greater  excursion  of  the  small  star  towards  its  apparent  aphelion,  so  that,  although 
we  are  sure  that  the  major  axis  of  the  real  orbit  must  materially  exceed  24",  it  is  impossible  a 
present  to  say  how  much  it  ma}7  exceed  that  limit.  Taking,  therefore,  the  co-efficient  of  parallax 
for  a  Centauri,  as  determined  by  Professor  Henderson  at  1',  it  will  follow,  from  what  has  been 
said,  that  the  real  diameter  of  the  relative  orbit  of  one  star  about  the  other  cannot  be  so  small  as 
that  of  the  orbit  of  Saturn  about  the  sun,  and  exceeds,  in  all  probability,  that  of  the  orbit 
of  Uranus. 

(208)  The  plane  of  the  orbit  in  the  case  of  a  Centauri,  as  in  that  of  44  Bootis,  passing 
nearly  through  our  system,  my  method  of  approximating  to  the  elliptic  elements  (Mem. 
Art.  Soc.  Vol.  V.),  becomes  inapplicable,  and  for  their  determination,  measures  of  the  distance 
of  the  stars  from  each  other  can  alone  be  relied  on.  No  subject  more  worthy  of  diligent 
and  continued  inquiry  can  possibly  be  urged  on  the  attention  of  southern  astronomers.  I  am 
not  aware  of  any  micrometric  measures  taken  since  1838.* 

(209)  77  Lupi.  R  A  14"  54m  NPD  136°  23'.  The  sub-epochs  calculated  in  the  Synoptic 
Catalogue,  resting  as  they  do  on  a  sufficient  total  number  and  value  of  measurements,  must  be 
held  conclusive  as  to  the  fact  of  a  considerable  retrograde  angular  movement  of  this  star, 
amounting  to  about  2°  6'  per  annum.  There  is  but  one  20-feet  measure  of  this  star,  viz. 
in  sweep  695  (1836.263),  which  (corrected  for  bias)  gives  a  position  of  109°  12',  agreeing 
well  with  the  equatorial,  considering  the  difficulty  of  the  star. 

(210)  y  Lupi.  R  A  15h  24m  NPD  130°  35'.  On  account  of  the  closeness  and  difficulty 
of  this  beautiful  double  star,  I  have  divided  the  whole  series  of  measures  into  two  sub-epochs. 


*  It  is  impossible  not  to  be  struck  with  the  parallel  which  obtains,  in  a  great  many  physical  peculiarities, 
between  the  two  double  stars  a  Centauri  and  61  Cygni.  Both  consist  of  nearly  equal  stars,  which  in  both  are  of 
a  colour  strongly  verging  to  red.  Both  have  very  unusually  large  proper  motions.  Both  have  measurable 
amounts  of  parallax,  and  both  are  clearly  binary  systems,  of  unusually  large  apparent  angular  dimensions. 


PARTICULAR  DOUBLE  STARS  IN  THE  FOREGOING  CATALOGUES. 


303 


So  treated,  they  afford  no  evidence  of  angular  motion  at  all  to  be  relied  on.  There  is  but 
one  20-feet  measure  of  it,  which,  corrected  for  bias,  gives  95°  24',  agreeing  remarkably  with  the 
general  mean  94°  6'  of  the  whole  equatorial  series. 

(211)  R  A  ]7h34mNPD  145°  20'.  If  this  star  be  really  double  (for  I  cannot  help 
suspecting  an  illusion),  it  must  be  in  a  most  rapid  state  of  angular  change. 

(212)  £  51.  Libra.  R  A  15"  55m  N  P  D  100°  54'.  The  general  epoch  calculated  in  the 
Synoptic  Catalogue  for  1835-40,  compared  with  the  mean  result  of  my  measures  for  1830,  given 
in  my  first  series  of  micrometrical  measures  (Nos.  397,  398,  399,  400),  afford  an  angular 
velocity  of  this  close  and  difficult  double  star,  which  may  probably  be  relied  on  with  some 
confidence. 

Epoch.  —  1830-26  —  4  nights'  obs.  —  Pos  =   l°-4  value  (8) 
"        1835-40  —  8         "         "         10  -1     "  (22) 

+5-14  +8°-7 

corresponding  to  a  direct  motion  of  +  1°.69  per  annum. 

(213)  y  Corona:  Australis.  R  A  18h  55m  N  P  D  127°  18'.  The  epochs  calculated  in  the 
Synoptic  Catalogue  leave  no  shadow  of  doubt  as  to  the  reality  of  a  considerable  retrograde 
orbitual  movement  of  1°.47  per  annum  in  this  beautiful  double  star.  The  distance  2".66 
renders  it  easy  of  measurement,  and  the  individuals  being  exactly  equal,  one  of  the  greatest 
hinderances  to  precision  in  this  respect  is  absent.  The  20-feet  measures  afford  no  information, 
one  of  the  only  two  taken  being  obviously  affected  by  some  mistake,  either  in  reading,  or 
otherwise.    In  those  taken  with  the  equatorial  I  have  the  most  entire  confidence. 

(214)  C  Aquarii.  R  A  22h  20m  N  P  D  90°  53'.  Respecting  the  continual  retrograde 
movement  of  this  star,  no  possibility  of  doubt  is  now  left.  The  positions  reported  in  my  two 
former  series  of  a  micrometrical  measures,"  compared  with  those  here  delivered,  stand  as 
follows  :— 

h.  1st  series,  general  mean,  .  .  .  356°  23'  —  1829-11 
Dawes  (as  reported  in  2nd  series),  .  .  356  15  —  1831-54 
h.  2nd  series,     .....      356  12  —  1831-64 

Mean  of  all,         .         .         .         .356  17  —1830  76 
h.  Synoptic  Catal.  as  above,      .         .         .      352    0  —  1836-25 

-4°  17'—  +5-49 

being  at  the  rate  of  —  0°.783  per  annum. 


CHAPTER  III. 


OF  ASTROMETRY,  OR  THE  NUMERICAL  EXPRESSION  OF  THE  APPARENT 

MAGNITUDES  OF  THE  STARS. 

SECTION  I.— OF  THE  METHOD  OF  SEQUENCES. 

(215)  A  method  of  determining  with  precision  the  relative  magnitudes  of  the  fixed  stars, 
that  is  to  say,  of  assigning  to  each  at  a  given  epoch,  a  number  expressing  on  a  certain  scale  the 
intensity  of  its  light,  has  long  been,  and  still  remains  a  desideratum  in  Astronomy.  The  inquiry 
is,  in  fact,  beset  with  many  and  great  difficulties,  which  have  only  been  partially  met  by  any  of 
the  various  contrivances  which  have  been  devised  for  the  purpose,  into  any  account  or  criticism 
of  which,  however,  it  is  not  my  intention  to  enter.  Some  of  these  difficulties,  indeed,  seem  alto- 
gether insuperable — those,  namely,  which  arise  from  the  diversity  of  colour  in  the  light  of  the 
stars  themselves ;  since  it  seems  hardly  possible  to  assign  any  precise  meaning  to  the  equality  or 
other  proportion  of  total  brightness  of  two  stars  differing  sensibly  in  colour.  In  such  a  case 
the  total  impression  made  on  the  eye  is  a  complex  effect,  about  which,  probably,  no  two 
observers  would  ever  agree  if  numerical  precision  were  insisted  on  ;  though,  on  the  other  hand, 
all  will  admit  that  even  greater  differences  of  colour  than  the  light  of  any  two  stars  offers,  would 
not  prevent  a  certain  approach  to  agreement  of  judgment  as  to  the  general  impression  produced 
on  the  eye,  in  at  least  a  great  number  of  cases.  No  one,  for  example,  hesitates  in  placing 
a  Lyra  above  Aldebaran,  or  Arcturus  above  Spica,  though  between  Antares  and  a  Crucis,  or 
even  between  e  Ursae  and  a  Persei,  or  Pollux  and  Spica ;  there  would  be  room  for  difference  of 
judgment,  and  different  eyes  would,  probably,  always  come  to  opposite  conclusions  as  to  the 
order  of  precedence.  Nothing  short  of  a  separate  and  independent  estimation  of  the  total 
amount  of  the  red,  the  yellow,  and  the  blue  rays  in  the  spectrum  of  each  star  would  suffice  for 
the  resolution  of  the  problem  of  Astrometry  in  the  strictness  of  its  numerical  acceptation  ;  and 
this,  the  actual  state  of  optical  science  leaves  us  destitute  even  of  the  means  of  attempting,  with 
the  slightest  prospect  of  success.  For  the  present,  therefore,  and,  probably,  for  a  long  time  to 
come,  so  far  as  stars  differing  in  colour  are  concerned,  we  must  be  content  with  a  somewhat  rude 
and  coarse  approximation  to  precision  in  assigning  numerically  their  places  in  a  photometric 
scale ;  and  even  in  the  case  of  stars  offering  no  marked  peculiarity  of  colour,  there  are  so  many 
causes  which  practically  interfere  with  the  application  of  instrumental  methods,  such  as  have 
from  time  to  time  been  proposed,  and  the  results  afforded  by  those  methods  have  in  many 
instances  proved  so  strongly  at  variance  with  the  plain  judgment  of  the  unaided  eye,  that  I  feel 
little  disposed  to  make  an  exception  in  their  favour. 


OF  THE  METHOD  OF  SEQUENCES. 


305 


(216)  Meanwhile,  the  requirements  of  astronomy  are  urgent  and  pressing,  and  make  even 
such  an  approximation  very  desirable.  I  can  add  little  to  the  arguments  advanced  on  this 
subject  by  Sir  William  Herschel  in  his  papers  on  the  comparative  brightness  of  the  fixed  stars, 
published  in  the  Transactions  of  the  Royal  Society,  beyond  the  impression  produced  by  the 
extraordinary  phenomena  presented  by  the  southern  star  v  Argus  (which  have  been  described  in 
the  former  part  of  this  work),  and  those  of  variable  stars  generally,  that  no  time  ought  to  be 
lost  in  endeavouring  to  establish,  by  direct  and  extensive  observation,  a  scale  of  magnitudes 
which  shall  be  really  applicable,  with  some  reasonable  degree  of  exactness,  to  the  state  of  the 
heavens  as  we  find  it,  so  as  to  serve  as  a  record  to  future  ages — if  not  of  indefeasible  accuracy, 
at  least  sufficiently  correct  to  ensure  the  detection  of  changes  such  as  there  is  abundant  reason  to 
believe  a  great  number  of  stars  have  undergone  within  the  period  of  astronomical  history. 
Nothing,  indeed,  can  be  more  inconvenient  and  misleading  than  to  find  in  our  catalogues  mag- 
nitudes assigned  to  stars,  so  far  above  or  below  the  truth,  that  a  single  glance  at  the  heavens 
suffices  to  expose  the  error ;  as  where,  for  instance,  we  find  9  Scorpii  (a  star  of  the  second  mag- 
nitude, or  2.3  at  the  lowest)  rated  as  of  the  5th,  or  A.  of  the  same  constellation,  a  star  between 
the  1st  and  2nd  magnitudes,  set  down  as  of  the  3d ;  a  Columbae  and  8  Orionis  (the  former  a 
star  of  the  3d  magnitude,  the  latter  not  much  more),  as  of  the  2d,  &c. 

(217)  Without  dissuading  from  the  introduction  of  new,  and  the  improvement  of  old 
instrumental  contrivances  (or  astrometers)  for  this  purpose,  and  having  myself  attempted  it,  not 
as  I  think  without  some  degree  of  success,  as  will  hereafter  be  explained,  I  am  yet  disposed  to 
rely  mainly  for  the  formation  of  a  real  scale  of  magnitudes  on  comparisons  made  by  the  un- 
assisted judgment  of  the  naked  eye.  The  method  which  I  have  followed  for  this  purpose,  and 
which,  to  distinguish  it  from  others  which  have  been  or  may  hereafter  be  proposed,  I  shall 
term  the  method  of  Sequences,  is  in  some  sort  an  extension  and  carrying  out  of  Sir  William 
Herschel's  method  of  naked-eye-comparisons,  described  in  his  papers  above  mentioned,  so  mo- 
dified and  generalized  (possibly  with  some  sacrifice  of  its  rigorous  precision,  though  more  so  in 
appearance  than  in  reality)  as  to  afford  a  handle  for  educing  from  it  a  numerical  scale  of  values  of 
the  magnitudes  of  the  stars  compared,  which  it  was  not  capable  of  doing  in  its  original  form,  and 
as  practised  by  him.  In  this  method,  stars  visible  at  one  time,  and  favourably,  or  rather  not  un- 
favourably situated  for  comparison,  are  arranged  in  sequences  by  the  mere  judgment  of  the  unaided 
eye,  and  these  sequences  treated  according  to  a  certain  peculiar  and  regular  system  (to  be  explained 
presently),  are  employed  to  obtain  in  one  unbroken  series,  a  graduating  scale  of  steps,  from  the 
brightest  down  to  the  faintest  stars  visible  to  the  eye.  Numerical  values  are  then  subsequently 
assigned,  and,  as  the  scale  in  this  case  is  entirely  arbitrary,  and  no  photometric  relations 
but  those  of  more  and  less  bright  are  used,  these  numbers  may  be  so  assigned  as  to  conform  on  a 
general  average  to  any  usage  or  nomenclature  which  may  be  fixed  upon  or  taken  as  the  general 
average  of  astronomers.  Waving  all  discussion  of  the  greater  or  less  propriety  of  the  magnitudes 
assigned  by  this  or  that  observer,  I  have  thought  it  best,  on  the  whole,  to  adopt  as  my  standard 
of  astrometrical  nomenclature,  the  catalogue  of  the  Astronomical  Society  of  2881  stars  published 
in  1827,  being  well  aware  that  the  magnitudes  there  assigned  are  those  of  different  epochs  and 
of  different  observers  (but  all  of  eminence),  and  that  in  individual  cases  many  and  considerable 
errors  exist.  The  mode  in  which  I  have  eliminated  those  errors,  and  secured  a  true  coincidence 
between  the  results  of  my  observations  and  the  magnitudes  in  the  catalogue  in  question,  taken  as 

4  i 


306 


OF  THE  METHOD  OF  SEQUENCES. 


a  whole,  will  be  explained  in  due  course,  and  will,  I  believe,  be  found  quite  free  from 
objection. 

(218)  In  Sir  William  HerschePs  catalogues  of  comparative  brightness,  his  object  was 
sufficiently  attained  by  so  identifying,  as  it  may  be  termed,  the  lustre  of  each  star  as  to  enable  a 
future  observer  to  satisfy  himself  whether  or  no  a  change  had  taken  place,  and  to  this  end 
each  star  was  compared  with  one,  or  at  most,  two  others  judged  to  be  either  exactly  equal  to  it, 
or  as  little  as  possible  unequal,  so  as  to  establish  a  system  of  binary  or  ternary  sequences  or 
equalities.  And  it  is  clear  that  this  being  done  (as  it  was  done  by  him),  for  each  visible  star, 
no  change  of  magnitude  could  take  place  without  being  detected.  But  for  the  purpose  of 
establishing  an  unbroken  chain  of  gradation  from  the  brightest  to  the  faintest  visible  star,  it 
would  be  requisite  that  these  sequences  should  run  together,  by  the  last  in  one  always 
becoming  the  first  of  another ;  and  that  in  such  a  way  that  many  extensive  sequences  should 
have  several  stars  in  common  throughout  their  entire  scale — a  condition  neither  attained  nor 
attempted  to  be  attained  in  those  observations.  For  the  purpose  proposed  by  myself,  however, 
it  was  necessary  to  establish  much  more  extended  sequences,  in  each  of  which  at  least  a  con- 
siderable interval  of  the  scale  of  magnitude  should  be  embraced.  And  having  accumulated  by 
sufficiently  continued  and  extensive  observation  many  such  sequences,  it  was  further  neces- 
sary to  secure  means  of  combining  them  into  general  sequences,  including  all  the  stars 
observed. 

(219)  The  process  therefore  which  I  pursued  was,  in  general,  the  following.  Choosing 
perfectly  clear  nights  (which  for  this  purpose  are  quite  indispensable),  a  succession  of  stars  was 
picked  out  by  actual  inspection  of  the  heavens  from  the  largest  above  the  horizon  down  to 
some  of  considerably  inferior  magnitude,  and  noted  down  in  a  list,  in  a  vertical  column — 
leaving  blank  intervals  more  or  less  considerable,  according  as  the  steps  of  the  skeleton  scale  so 
picked  out  were  wider  or  closer — but  taking  care  that  between  the  skeleton  stars  arranged 
seriatim,  there  should  always  be  an  unequivocal  descending  step  of  apparent  lustre.  The  business 
of  the  night  then  was  to  fill  in  as  far  as  practicable  the  steps  of  this  scale  into  an  unbroken 
chain  of  downward  gradation,  placing  each  newly  added  star  by  actual  judgment  and  comparison 
with  its  immediate  neighbours,  in  its  proper  order,  until  the  scale  became  so  gradual  in  its 
declension  that  it  was  no  longer  possible  to  insert  fresh  stars  with  certainty  between  its  members, 
in  which  case  they  were  set  down  as  equal  to  some  of  those  already  noted  down. 

(220)  Sir  William  Herschel's  comparisons  were  instituted  between  stars  at  the  same,  or 
nearly  the  same  altitude,  and  in  each  other's  immediate  vicinity.  In  mine,  these  conditions 
could  not  be  complied  with.  Care,  however,  was  taken  to  avoid  low  altitudes,  and  the  exceeding 
purity  of  the  atmosphere  of  the  Cape  allowed  a  range  of  60  or  even  70  degrees  from  the  zenith 
in  all  directions,  with  little  or  no  fear  of  being  materially  misled.  The  neighbourhood  of  the 
moon  was  avoided,  but  every  night  in  the  absence  of  the  moon  being  precious  for  the  observation 
of  nebulas,  it  was  not  practicable  to  avoid  moonlight  nights  for  the  comparisons,  as  would, 
doubtless,  have  been  desirable.  It  was  my  earnest  wish  to  have  carried  on  these  comparisons 
during  the  whole  of  our  homeward  voyage  (the  observations  being  easily  made  on  ship-board),  so 
as  to  interweave  in  sequences  sufficiently  numerous  and  extensive,  at  least  all  the  most  con- 
spicuous stars  of  both  hemispheres :  but  in  this  I  was  disappointed,  at  least  to  that  extent ;  as  a 
totally  overcast  state  of  the  sky  prevailed  from  the  day  of  our  departure  from  Table  Bay  until 


OF  THE  METHOD  OF  SEQUENCES. 


307 


we  reached  nearly  the  latitude  of  St.  Helena,  with  the  exception  of  a  single  fine  night 
on  the  Equator,  on  the  28th  of  March,  1838,  advantage  of  which  was  taken  to  procure  a  short 
sequence,  and  several  valuable  comparisons  of  southern  stars  with  stars  of  equal  or  nearly  equal 
lustre  in  good  situations  for  European  observation.  But,  with  this  exception,  no  other  available 
opportunity  occurred  till  the  14th  and  15th  of  April,  when  two  sequences  were  observed 
in  lat.  17°  and  18°  north,  but  in  these  the  more  southern  stars  were  already  too  low  for 
fair  comparison. 

(221)  The  sequences  observed  at  the  Cape,  and  during  the  voyage  home,  are  given  at 
length.  For  their  better  understanding,  and  to  avoid  mistakes,  it  is  necessary  to  mention-  that 
the  charts  referred  to  during  the  observations,  were  either  those  of  Bode's  Atlas,  or  working 
copies  of  them  formed  by  pricking  off  the  stars,  carefully  lettering  them  to  correspond  with  the 
originals ;  outlining  the  constellations  precisely  as  in  Bode,  and  breaking  them  afterwards  up 
into  triangles,  by  drawing  lines  from  the  large  stars  (chosen  as  the  most  conspicuous,  not  by  the 
maps,  but  by  actual  inspection  of  the  heavens),  with  a  view  to  the  insertion  within  such  triangles 
of  every  star  visible  to  the  naked  eye,  and  of  those  only.  In  consequence,  the  nomenclature 
used  was  necessarily  Bode's,  with  all  its  faults  and  mistakes  (and  they  are  not  a  few*).  The 
latter  have  been  carefully  rectified :  the  former  I  was  compelled  to  tolerate  at  the  time,  and 
throughout  much  of  the  subsequent  discussion  of  the  observation  ;  no  systematic  reformation  of 
sidereal  nomenclature  having  then  been  attempted,  like  that  which  has  been  carried  out  by  Mr. 
Baily  in  the  catalogue  of  the  British  Association.  On  the  publication  of  that  catalogue,  however, 
it  became  a  serious  matter  of  consideration  whether  to  alter  the  names  by  which  the  stars  are 
called  in  the  observed  sequences  to  correspond  throughout  with  that  catalogue,  or  no.  To  have 
done  so  would  have  been  to  cut  off"  the  connexion  of  the  printed  sequences,  not  only  with  the 
original  observations,  but  with  a  great  mass  of  manuscript  work  intervening  between  them  and 
the  concluded  magnitudes,  in  all  which  the  nomenclature  of  Bode  had  been  used,  and  which  to 
have  altered  throughout  in  correspondence,  would  have  infallibly  entailed  a  multitude  of  errors, 
and  ultimately  involved  the  whole  in  confusion.  I  the  less  regret  having  been  obliged  to  come 
to  this  decision,  because  I  have  already  recorded  my  conviction  that  for  this  especial  purpose 
an  entire  remodelling  of  the  whole  system  of  constellations,  both  northern  and  southern,  is 
necessary.  And  I  take  this  opportunity  once  more  to  express  that  conviction,  and  the  hope 
that  another  decade  will  not  be  allowed  to  pass  over  without  the  accomplishment  of  so  useful  a 
work,  without  which  the  progress  of  this  department  of  astronomy  will,  of  necessity,  be  slow  and 
uncertain. 

(222)  There  is  one  constellation,  however,  in  which  it  was  found  imperatively  necessary 
to  revise  with  the  greatest  care  the  original  nomenclature, — viz.  Argo — the  distinction  into 
compartments  independently  lettered  being  indicated  by  no  clear  lines  of  demai'kation  in  Bode's 
chart,  and  it  having  therefore  been  necessary  in  observing  to  adopt  a  temporary  division  and 
nomenclature  for  the  purpose  of  avoiding  the  unutterable  confusion  of  Greek,  Roman,  and 


*  Still  I  must  render  grateful  tribute  to  the  valuable  aid  actually  afforded  me  by  these  charts,  which  are,  in 
fact,  the  only  ones  in  which  the  smaller  southern  circumpolar  stars  are  laid  down  (or  at  least  were  so  at  the  time 
I  used  them)  on  the  stereographic  projection,  which  is  indispensable  for  the  purpose  in  question. 


308 


OF  THE  METHOD  OF  SEQUENCES. 


Italic  alphabets  there  prevalent.  In  this  constellation,  then,  I  have  gladly  availed  myself  of  the 
fixation  of  the  lettering  of  the  several  subdivisions  Vela,  Carina,  Puppis,  and  Malus,  afforded  by 
the  labours  of  Mr.  Baily,  and  have  scrupulously  conformed  the  lettering  of  my  sequences  to  his 
nomenclature,  in  every  instance  identifying  the  stars  with  the  utmost  care.  In  so  doing, 
Bode's  constellation  Pyxis  has  been  abandoned.  So,  also,  in  his  interpolated  constellations  of 
Nubecula  Major,  and  Machina  Typographica,  in  each  of  which  only  one  star,  and  in  Hell's 
constellation  of  "  Harpa,"  in  which  only  two  are  included  in  the  sequences  (and  where,  therefore, 
it  could  be  safely  as  well  as  easily  done),  the  names  or  numbers  in  the  British  Association 
Catalogue  are  substituted  for  Bode's. 

(223)  In  the  names  of  Bode's  constellations,  for  brevity,  the  following  changes  or  con- 
tractions have  been  habitually  made  in  constructing  the  sequences  : — 

Tubus  is  used  for  Telescopium ;  Fornax,  for  Apparatus  Chemicus ;  Machina,  for  Machina 
Electrica  ;  Sculptor,  for  Apparatus  Sculptoris ;  Pictor,  for  Equuleus,  or  Pluteum  Pictoris  ; 
Volans,  for  Piscis  Volans ;  Mensa,  for  Mons  Mensa? ;  Musca,  for  Apis  (to  avoid  confusion 
with  Apus). 

(224)  To  obviate  the  possibility  of  mistake  or  doubt  in  particular  cases,  the  following  rules 
are  to  be  borne  in  mind  in  reading  the  sequences  here  recorded. 

1st.  The  constellations  and  letters  are  those  of  Bode's  maps,  except  where  the  contrary  is 
expressly  stated,  either  in  what  is  said  above,  or  in  the  appended  notes. 

2nd.  Whenever  on  reference  to  the  catalogue  of  the  British  Association  it  has  been 
ascertained  that  a  difference  in  either  of  those  respects  subsists  between  these  nomenclatures, 
the  star  is  identified  by  attaching  to  it  Flamsteed's  number  (if  any),  as  given  in  that  catalogue, 
or  by  stating  in  a  note  the  number  of  the  star  in  the  catalogue  itself.  As  such  reference  has 
been  actually  made  in  every  case  where  there  has  been  the  least  reason  to  suppose  a  discordance 
would  exist,  I  presume  that  among  the  lettered  stars  in  the  sequences,  hardly  one  will  be  found 
unidentified. 

3d.  A  great  number  of  stars  have  been  observed  and  included  in  the  sequences  which  occur 
in  Bode's  map,  without  letters.  There  is  scarcely  a  single  instance  in  which  such  stars  have 
failed  to  be  identified  with  stars  in  the  British  Association  Catalogue  (BAC),  in  Lacaille's 
Ccelum  Australe  Stelliferum  (L),  or  in  the  Histoire  Celeste  (H  C);  the  last  two  catalogues  as 
reduced  and  published  by  the  British  Association,  or  speedily  about  to  be  so  published.  In 
these  cases,  as  no  nomenclature  was  in  question,  since  the  stars  must  necessarily  be  cited  by 
number,  the  numbers  adopted  are  those  of  the  catalogues  above  mentioned,  with  their  initials 
annexed.    By  far  the  great  majority  carry  the  initials  BAC. 

4th.  Besides  these,  a  great  many  stars  have  been  observed  which  do  not  occur  in  any  maps 
or  catalogues.  These  have  been  at  the  time  inserted  in  the  skeleton  triangles  by  configurations 
with  neighbouring  stars,  and  they  are  designated  in  the  sequences  by  their  Right  Ascensions 
and  N.  P.  distances  for  1801  (the  epoch  of  Bode),  as  transferred  graphically  to  his  charts,  and 
therefore  as  affected  with  the  local  errors  of  the  charts  (which  in  some  parts  are  very  con- 
siderable). They  are,  however,  for  the  most  part  insignificant  stars,  not  exceeding  the  6th 
magnitude,  on  which  it  did  not  seem  worth  while  to  bestow  any  further  pains. 

(225)  The   following  marks  also  require  explanation  : — When  two  or  more   stars  are 


OF  THE  METHOD  OF  SEQUENCES. 


309 


bracketed  together  without  the  sign  =,  a  perceptible,  but  very  trifling  difference  of  brightness 
is  indicated,  the  upper  being  the  brighter.  But  when  the  sign  =  is  added,  a  perfect  equality  is 
meant,  and  it  is  indifferent  which  order  they  are  placed  in. 

The  sign  +  placed  after  the  number  of  a  catalogued  star  (thus  B  2686  +)  indicates  that  the 
star  in  question  with  either  the  next  to  it  in  the  catalogue  (B  2687),  or  some  one  very  nearly 
adjacent,  form  a  coarse  double  star,  seen  by  the  naked  eye  as  one  star,  or  at  least  not  dis- 
criminated as  two  at  the  moment  of  observation,  though,  perhaps,  longer  or  closer  inspection 
would  have  shown  them  separate. 

Numbers  are  annexed  after  the  names  of  the  stars  in  all  the  sequences,  which  occur  above 
the  double  dotted  lines.  For  the  meaning  of  these  numbers,  and  the  explanation  of  those  dotted 
lines,  see  Art.  252. 


310 


Sequences  and  Equalities  in  the  Apparent  Magnitudes  of  Stars,  observed  at  Feldhausen, 
from  July  16,  1835,  to  February  25,  1838,  and  on  board  the  H.  E.  I.  C.  S.  Windsor,  at  sea,  from 
March  28,  to  April  15,  1838,  inclusive. 


Sequence  i. 
July  16,  1835. 

1  Antares   1.27 

2  \  Scorpii   1.78 

3  0  Scorpii    2.28 

4  £  Scorpii    2.78 

5  S  Scorpii   >   2.86 

6  k  Scorpii   $  2.86 

7  /3  Scorpii   2.98 

8  v  Scorpii   1   3.37 

9  7r  Scorpii  $  3.37 

10  i  Scorpii   }  3.45 

11  a  Scorpii   3.45 

12  t  Scorpii   j  3.45 

13  y  Tubi   3.62 

14  ?/  Scorpii   3.80 

15  fi  1  Scorpii    3.98 

16  ft  2  Scorpii    4.16 

17  ?  2  Scorpii   4-34 

18  p  Scorpii   4.42 

19  to  1  Scorpii    4.50 

20  v  Scorpii   4.58 

21  a  Norms   4.67 

22  (3  Normse   4.68 

23  i  Scorpii. 

24  o)  (Clust).  Scorpii. 

25  at  2  Scorpii. 

26  g  Ophiuchi. 

27  (a  Ophiuchi. 

28  d  Scorpii. 

29  c  2  Scorpii. 

30  x  Scorpii. 
310  Ophiuchi. 

32  0  Ophiuchi. 

33  ^  Scorpii. 

Note. — The  order  of  the  chief  stars  in 
Scorpio  as  stated  in  my  paper  on  the 
revision  of  the  Southern  Constella- 
tions, Mem.  R.  Ast.  Soc.  xii.  p.  215, 
is,  by  an  unfortunate  misprint,  thus 
stated,  a,  S,  0,  t.    For  S  read  X. 


Sequence  2. 
July  17,  1835. 

1  t  Sagittarii   )   2.27 

2  6  Scorpii  J  2.27 

3  a  Sagittarii   „  }   2.58 

4  f  Scorpii   \  2.58 

5  £  Sagittarii   1   2.79 

6  k  Scorpii   \  2.79 

7  S  Sagittarii    2.99 

8  \  Sagittarii   3.13 

9  jt  Sagittarii    3.27 

10  a  Arse    3.40 


11  (3  Arse    3.50 

12  y  Sagittarii    3.61 

13  0  Sagittarii    3.71 

14  j3  Tubi  -j  3.82 

15  y  Tubi                             J-  =  3.82 

16  y  Arse  J  3.82 

17  r  Sagittarii. 

18  K2  Sagittarii. 

19  a  Tubi. 

20  0  Sagittarii. 

21  /3  1  Sagittarii. 

22  a  Sagittarii. 

23  /3  Coron.  Aus.  -\ 

24  a  Coron.  Aus.  V-  = 

25  y  Coron.  Aus.  J 

26  p  Sagittarii. 

27  E  Sagittarii. 

28  S  Coron.  Aust. 

29  £  Coron.  Aust. 

30  {3  2  Sagittarii. 

31  K  1  Sagittarii. 

32  v  Sagittarii.  "\ 

33  b  (terebelli)  f   

34  c  (terebelli)  f 

35  (1)  Sagittarii  J 

36  d  Sagittarii. 

37  G  Sagittarii. 

38  H  Sagittarii. 

39  £  Coron.  Aus. 

40  t  Coron.  Aus. 


Sequence  3. 
August  15,  1835. 


1  a  Eridani   0.93 

2  a  Gruis  ,   1-67 

3  (3  Gruis   2.36 

4  «  Phoenicis    2.64 

5  y  Gruis   2.92 

6  [3  Hydri    3.19 

7  a  Hydri    3.26 

8  £  Gruis   3.33 

9  a  Toucani   3.40 

0  *  Gruis   3.47 

1  (3  Phoenicis    3  54 

2  y  Phoenicis    3.61 

3  <p  Eridani   3.68 

4  y  Hydri    3.75 

5  j3  Toucani   3.81 

6  x  Eridani   3.86 

7  $  Phoenicis    3.92 

8  £  Phoenicis    3.97 

9  £  Phoenicis    4.03 

20  k  Phoenicis    4.08 

21  k  Eridani   4. 14 

22  £  Gruis   4.19 

23  0  Gruis   4-25 

24  1  1  Gruis   4-3° 

25  S  2  Gruis   4.36 


26  t  Hydri   4.42 

27  S  Hydri  4.48 

28  t)  Phoenicis    4.55 

29  ?  Toucani   4.62 

30  1  Pise.  Aust   4.69 

31  1  Phoenicis   4.75 

32  9  Phoenicis    4.82 

33  X  Gruis   4.89 

34  e  Toucani   4-96 

35  ?  Hydri    5.02 

36  0  Phoenicis    5.02 

37  H  Eridani   5  02 

38/1  Phoenicis    5.02 

39  X  Phoenicis    5.02 

40  1}  Toucani   5.02 

41/1  Gruis. 

42  >i  Gruis. 

43  p  Gruis. 

44  >)  Hydri. 

Note. — No.  9  is  a  Toucani,  observed  by 
mistake  for  y,  by  which  name  the  star 
is  erroneously  called  in  the  original 
sequence.  No.  5  is  called  y  Gruis, 
but  cannot  be  that  star. 


Sequence  4. 
February  11,  1836. 

1  Canopus    0.22 

2  a  Centauri    0.34 

3  Arcturus    0.45 

4  j3  Centauri    1.14 

5  a  Crucis   $  1.2 1 

6  Spica   J  1.27 

7  Antares   1.39 

8  i]  Argus    — 

9  j3  Crucis    L57 

10  y  Leonis    2.42 


Sequence  5. 
February  15,  1836. 

1  Sirius    o.id 

2  Canopus    0.22 

3  a  Centauri    0.34 

4  (3  Centauri    114 

5  Spica    1 .2 1 

6  a  Crucis    1.39 

7  j3  Crucis    1.57 

8  y  Crucis    1.72 

9  (3  Argus   1  __  2.06 

10  y  Argus   S  2-°6 

11  £  Argus    2.17 

12  a  Trianguli   2.23 

131?  Argus    2.44 


SEQUENCES  AND  EQUALITIES  IN  THE  APPARENT  MAGNITUDES  OF  STARS. 


311 


14  6  Centauri    2-55 

15  y  Centauri   i   2-72 

16  t  Argus  S  2.72 

17  £  Argus    2-74 

18  a  Lupi   )  _  2.80 

19  e  Centauri    >  2.83 

20  /3  Lupi   2.90 

21  £  Centauri   "\  2.96 

22  8  Centauri   /   2.96 

23  k  Argus   I  2-96 

24  n  Centauri   J  2.96 

25  k  Centauri    3.24 

26  y  Lupi   3.30 

27  1  Centauri   3. 40 

Notes. — On  this  night,  tj  Argus  was 
placed  above  but  nearly  equal  to 
/3  Crucis. — No.  12,  a  Trianguli,  too 
near  the  horizon  for  a  good  com- 
parison. 


Sequence  6. 
February  18 — March  6,  1836. 

1  Sirius    0.10 

2  Canopus    0.22 

3  a  Centauri    0.34 

4  a  Eridani   0.61 

5  Arcturus    0.88 

6  fi  Centauri    1.14 

7  a  Crucis    1.21 

8  Spica    1.27 

9  Antares    1.39 

10  Regulus   J   1.57 

lit]  Argus   J  .... 

12  /3  Crucis    1.62 

13  y  Crucis    1.72 

14  p  Argus    2.01 

15  y  Argus    2.1 1 

16  e  Argus   2.17 

17  \  Scorpii   2.20 

18  a  Trianguli   2.23 

19  y  Centauri    2.27 

20  \  Argus   I   2.32 

21  6  Scorpii  }  2.37 

22  8  Argus   >   2.44 

23  6  Centauri   j  2.55 

24  t  Argus  I  2.73 

25  £  Argus   S  2.74 

26  a  Lupi  1  2.80 

27  t  Centauri  \  2.83 

28  8  Centauri  -v  2.92 

29  rj  Centauri                           v  2.93 

30  £  Centauri   J  2.94 

31  «  Argus   1  3.04 

32  /3  Hydri   S  3.08 

33  fi  Argus   !  )  3.13 

34  j3  Lupi  S  3.21 

35  t  Centauri   3.22 

36  /3  Trianguli                           )  3.30 

37  a  Musca?  $  3.35 

38  y  Lupi   3.38 

39  9  Argus    3.42 

40  k  Centauri    3.47 

41  y  Trianguli   3.52 

42  r  Argus    3.55 

43  c  Crucis    3.58 

44  /3  Musca?  }  3.63 

45  v  Argus   S  3.66 

46  N  Velorum   )  3.70 

47  a  Circini   $  3.72 

48  y  Hydri    3.75 


49  a  Doradus    3-7^ 

50  to  Argus    3-8o 

51  a  Pictoris   3  82 

52  X  Centauri    3-84 

53  p  Carina?   3.85 

54  q  Carinas   3-86 

55  a  Reticuli   3-87 

56  Centauri    3.92 

57  v  Centauri    3.93 

58  x  Argus    4-03 

59  1  Carina?    4-13 

60  t  Lupi   4.23 

61  <p  Argus    4.32 

62  p"  Reticuli   4.39 

63  £  Lupi   4  44 

64  £  Crucis    4.60 

65  <p  Centauri    4.62 

66  a  Carina?. 

67  8  Muscse. 

68  3984  B  A  C. 

69  y  Volantis. 

Notes. — No  46  is  3269  B  A  C. — No. 
53  is  3619  B  A  C  erroneously  marked 
with  the  letter  e  in  Bode's  Atlas. — 
No.  54  is  3526  B  A  C. — No.  59  is 
3353  B  A  C. — No.  60  is  4734  B  A  C, 
erroneously  included  by  Bode  in  the 
constellation  of  the  Centaur. — No.  66 
is  3149  B  A  C. 

The  following  stars  are  classed  in  groups 
of  nearly  the  same  magnitudes  in  each 
group,  all  inferior  to  the  foregoing, 
and  each  group  (generally  speaking  1 
consisting  of  stars  larger  than  those  of 
the  groups  below  it. 


Sequence  6. 
1st  Group  of  Unarranged  Stars. 

1  (8  Chamseleontis. 

2  (3  Apodis. 

3  u  Carinas. 

4  £  Volantis. 

5  a  Volantis. 

6  j3  Volantis. 

7  o  Carinse. 

8  I  Carinas. 

9  v  2  Centauri. 
10  y  Muscae. 

n  {  Centauri. 

12  O  Crucis  (Bode). 

13  a  Centauri. 

14  y  Apodis. 

Notes. — No.  3  is  marked  k  by  mistake 
in  Bode's  map. — No.  12  seems  to  be 
the  pair  of  stars  or  coarse  double  star 
Nos.  4325  +  4327  B  A  C,  seen  as 
one  star. — No.  7,  o  Carina?,  Bode  = 
3441  B  AC  ? 


Sequence  6. 
2nd  Group  of  Unarranged  Stars. 

1  %  Centauri. 

2  8  Trianguli. 

3  £  Volantis. 

4  c  Carina?. 

5  i  Carina?. 

6  h  Carina?. 


7  v  1  Centauri. 

8  h  Centauri. 

9  i  Centauri. 
10  k  Centauri. 
us  Carina?. 
12  8  Volantis. 

13^  Chamael.  )  

14  y  Chamael.  $ 
155  Doradus. 

16  V  Centauri.  )  

17  7r  Centauri.  S 

18  a  Apodis. 

19  a  Velorum.  )  

20  b  Velorum.  $ 

21  c  Velorum. 

Notes. — s  Carina?  is  Bode's  S  Roboris. 
— V  is  Bode's  letter  in  Centaurus  for 
4735  BAG. — c  Velorum  is  equal  to 
c  Carina?,  and  greater  than  either 
a  or  b  Velorum. 


Sequence  6. 

3rd  Group  of  Unarranged  Stars. 

1  \  Crucis. 
1  k  Crucis  (clust). 
£  Crucis. 
ri  Crucis. 
8  Apodis. 
f  Trianguli. 
r  Centauri. 

8  (3  Circini. 

9  y  Circini. 

10  *  Volantis  =  B  A  C.  2835  +  2837. 

11  d  Carina?. 

12  B  A  C.  3986. 

13  X  Velorum. 

14  A  Centauri  (Bode). 

15  g  Carina?. 

16  f  Muscae. 

17  B  A  C.  4461. 

18  B  A  C.  4412. 

19  >(:  Musca?  =  B  A  C.  4469  4-  4475- 

20  B  A  C.  5566. 
ii  it  Lupi. 

22  d  Velorum. 

23  e  Velorum. 

24  P  Puppis. 

25  R  Puppis. 

26  B  A  C.  2670. 

27  BAG.  2642. 

28  L  2  Puppis. 

29  I  Puppis. 

30  B  A  C.  2375. 

Notes. — No.  10,  two  stars  seen  as  one. 
— 14,  called  A  by  Bode,  is  B  A  C. 
3935. — 18  is  the  second  of  the  stars 
marked  S  in  Bode's  Centaurus. — 19  is 
two  stars  seen  as  one. 


Sequence  6. 

^th  Group  of  Unarranged  Stars. 

6  1  Crucis. 
£  Chamasleontis. 
S     9h  3°' 
<  i5i°49 
f  Carina;. 
B  A  C.  4000 
y  Carina?. 


3  * 


I1 


1800). 


312 


SEQUENCES  AND  EQUALITIES  IN  THE 


7  m  Carinas. 

8  T  Velorum. 

9  B  A  C.  3636. 

10  K  Carinse. 

11  D  1  Carina;. 

12  B  A  C.  1926. 

1 3  M  Centauri  (Bode). 

14  i)  Muscae. 

15  hi  Puppis. 

16  h  2  Puppis. 

17  B  A  C.  2176. 

18  L  1  Puppis. 

19  H  Puppis. 

Notes. — No.  3  not  identifiable.  — No.  6 
misplaced  by  Bode  in  Centaurus,  is 
B  A  C.  3835.— No.  13,  called  M 
Centauri  by  Bode,  is  B  A  C.  4580. — 
No.  19  is  B  A  C.  2332. 


Sequence  6. 

5th  Group  of  Unarranged  Stars. 

r  i  Lupi. 
t  2  Lupi. 
t  Crucis. 
9  2  Crucis. 
6  Volantis. 
k  Carina;. 

B  A  C.  3923  +  3924. 


8  P  Velorum. 

9  V  Velorum. 

10  t  2  Carina;. 

11  F  Centauri  ? 

12  B  A  C.  3706  4-  3707. 

13  B  A  C.  4284? 

14  £  2  Muscae. 

15  e  Carina;. 

16  B  Carina; 

17  Y  Centauri  (Bo.) 

18  N  Centauri  (Bo.) 

19  R  Centauri  (Bo.) 

20  B  A  C.  4422. 

21  3  Circini. 

22  B  A  C.  4644  ? 

23  B  A  C.  401 1. 

24  0  Argus. 

25  A  Velorum. 

26  f  Velorum. 

27  g  Velorum. 

28  H  Velorum. 

29  K  Puppis. 

30  Q  Puppis. 

31  B  A  C.  2415. 

32  S  Carina;. 

33  Q  Carina;. 

34  R  Carina;. 

35  B  A  C.  2339. 

Notes. — No.  io,  t2  Carina;  is  B  A  C. 
3655.  —  No.  11,  F  Centauri,  is  L. 
5092. — No.  13,  B  A  C.  4284,  is  called 
45  m  by  Lacaille,  but  6  m  in  B  A  C. 
— No.  15,  query  whether  BAG.  2920 
or  2921,  or  both  seen  as  one  star. — 
No.  16,  both  Bode's  map  and  BAG. 
have  two  stars  marked  B  Carina;,  viz. 
B  A  C.  2259  and  2770.  The  identity 
therefore  doubtful,  I  suppose  my  star 
to  be  the  former. — Nos.  17,  18,  19, 
are  B  A  C.  4749,  4616,  4695,  but 
have  no  letters  attached. 


Sequence  6. 
6th  Group  of  Unarranged  Stars. 

1  b  1  Carina;. 

2  b  2  Carina;. 

3  L  Carina;. 

4  k  Chamaeleontis. 

5  C  Carina;. 

6  B  A  C.  4117  4-  4118. 

7  B  A  C.  3993. 

8  B  A  C.  3706  ? 

9  B  Velorum. 

10  B  A  C.  2955. 

11  BAG.  2963. 

12  C  Velorum. 

1 3  D  Velorum. 

14  E  Velorum. 

15  B.  3098. 

16  K  2  Puppis  (Bode). 

17  Y  1  Puppis. 

18  Y  2  Puppis. 

19  P  Carina;. 

Notes. — No.  8  may  possibly  be  B  A  C. 
3694. — No.  11  is  marked  "neb"  in 
B  A  C,  no  nebula  noticed  about  it 
with  the  naked  eye. — No.  16,  not 
lettered  in  B  AC,  but  the  letter  K 
is  attached  to  No.  2753  in  that  Cat., 
which  is  Bode's  K  1. 

Notes  on  Seciuence  6. — ?  1  Muscse 
=  B  A  C.  4161,  k  Muscse  =  B  A  C. 
4542,  M  Puppis  =  B  A  C.  2426,  and 
G  Velorum  =  B  A  C.  2873,  are  not 
visible  to  the  naked  eye.  G  could 
barely  be  seen  in  a  night-glass. 


Sequence  7. 
March  22,  1836. 

1  a  Centauri    0.34 

2  Rigel   0.76 

3  Procyon    0.85 

4  a  Crucis   ^   1.30 

5  Spica  S  1.30 

6  a  Orionis   1.41 

7  n  Argus    — 

8  Regulus    1.48 

9  Pollux    1.5 1 

10  (3  Crucis    1.57 

11  y  Crucis    1.72 

12  t  Canis   1.89 

13  /3  Leonis    1.9 1 

14  y  Leonis    1.95 

15  Castor    1.97 

16  £  Orionis   2.00 

17  /3  Argus    2.01 

18  y  Orionis   2.08 

19  Z  Orionis   2.09 

20  y  Argus    2.1 1 

21  e  Argus   2.17 

22  a  Trianguli   2.23 

23  (5  Orionis   2.30 

24  0  Canis   2.34 

25  y  Geminorum   2.40 

26  0  Centauri   2.45 

27  /3  Canis   2.48 

28  k  Orionis   2.52 


29  8  Argus   )   2.58 

30  a  Hydra;  5  2-58 

317  Corvi   2.70 

32  (3  Corvi   2.80 

33  y  Centauri    2.87 

34  0  Leonis    2.95 

35  y  Virginis   3.05 

36  c  Corvi   3.20 

Note. — The  stars  in  this  secpaence  were 
first  placed  together  in  classes,  and 
the  stars  in  each  class  then  arranged 
in  order  of  apparent  brightness.  The 
lines  drawn  between  the  stars  separate 
the  classes.  ^This  is  a  bad  mode  of 
procedure.) 


Sequence  8. 
March,  1836. 

1  y  Muscae. 

2  0  Muscse. 

3  I  Carina;. 

4  a  Chamaeleontis    4.79 

5  y  Apodis   4.82 

6  a  Apodis   4.85 

7  8  Chamaeleontis    4.88 

8  0  Chamaeleontis    4.91 

9  /3  Chamaeleontis. 
10  t  Chamaeleontis. 


Sequence  9. 
March,  1836. 

1  /3  Volantis    4.51 

2  £  Crucis    4.56 

3  n  Crucis    4.60 

4  a  Volantis                          \   4.65 

5  y  Chamaeleontis   J  4.65 


Sequence  10. 
April  25,  1836. 

1  6  Centauri    2.55 

2  y  Centauri    2.71 

3  a  Lupi   2.80 

4  £  Centauri    2.88 

5  7/  Centauri    2.88 

6  £  Centauri    2.91 

7  1  Centauri   3.21 

8  (3  Lupi   3.22 

9  y  Lupi   3-38 

10  k  Centauri    3-66 

11  ju  Centauri    3.92 

12  v  Centauri    3,93 

13  £  Lupi   3-95 

14  £  Lupi    4-oa 

15  £  Lupi   4-°7 

16  (p  1  Lupi   4'  '8 

17  t  Lupi  *   4-29 

18  k  Lupi   4-4° 

19  7r  Lupi   4-5 1 

20  tp  Centauri    4-62 

21  ti  1  Centauri. 


APPARENT  MAGNITUDES  OF  STARS. 


313 


Note.  —  No.  17  is  placed  in  Bode's 
map  in  Centaurus,  and  lettered  t ; 
but  there  is  another  1  Centauri 
(B  A  C.  4458).  It  is  entered  in 
BAC.  (No.  4734)  as  1  Lupi.  In 
that  Catalogue  (as  also  in  Bode's 
map)  there  is  another  t  Lupi,  viz., 
No.  5139.  I  use  1  Lupi  to  designate 
No.  4734,  as  being  the  more  conspi- 
cuous of  the  two  iotas,  and  on  account 
of  its  proximity  to  two  stars  r  1  and 
r  2,  which,  though  placed  by  Bode  in 
Centaurus,  undoubtedly  belong  to 
Lupus,  the  real  r  Centauri 
near  y. 


Sequence  ii. 
April  26,  1836. 

1  0  Centauri    2.55 

2  y  Centauri    2.71 

3  a  Lupi  }   2.81 

4  t  Centauri   J  2.81 

5  r)  Centauri   )  2.91 

6  /3  Lupi  5  3.00 

7  Z  Centauri   (   3.02 

8  t  Centauri  J  3.02 

9  y  Lupi   3-38 

10  ic  Centauri    3.66 

11  8  Lupi   -\  3.93 

12  ft  Centauri   V  =  3.93 

13  v  Centauri   J  3.93 

14  £  Lupi   4.00 

15  t  Lupi   4.05 

16  ^  1  Lupi  )   4.10 

17  t)  Lupi  \  4.10 

18  n  Lupi   4.27 

19  vi  Centauri   4-34 

20  (p  Centauri    4.62 

21  7r  Lupi   4.67 

22  d  Centauri    4.70 

23  b  Centauri    4.73 

24  c  Centauri    4.75 

25  X  Lupi   4.76 

26  g  Centauri    4.78 

27  k  Centauri    4.80 

28  i  Centauri   4.82 

29  if/  Centauri    4.84 

30  a  Centauri    4.86 

31  p  Lupi   4.88 

32  a  Lupi. 

33  0  Lupi. 

34  h  Centauri. 

35  v  2  Centauri. 

36  r  2  Lupi. 

37  0  2  Lupi. 

38  t  Centauri. 

39  o  Lupi. 

40  BAC.  5139- 

41  d  Lupi. 

42  BAC.  5165. 

43  z  Centauri. 

44  BAC.  4744. 

45  t  i  Lupi. 

46  8  Normae. 

47  r)  Normae. 

48  e  Lupi. 

49  y  Centauri. 


Notes. — No.  8.  This  is  the  true  1  Cen- 
tauri.— No.  30.  BAC.  4759. — No. 
36.  Misplaced  by  Bode  in  Centaurus. 
See  note  on  No.  17  of  Sequence  10. 
— No.  38.  The  true  t  Centauri. — 
No.  40.  Miscalled  1  Lupi  in  B  A  C. 


Sequence  12. 
April  27,  1836. 

1  y  Centauri    2.57 

2  0  Centauri    2.70 

3  a  Lupi  }   2.82 

4  t  Centauri  J  2.82 

5  ?;  Centauri    2.91 

6  /3  Lupi   3.02 

7  Z  Centauri    )   3.18 

8  1  Centauri  $  3.18 

9  y  Lupi   3.38 

10  k  Centauri   ,  .  .  . .  3.66 

11  J  Lupi   -j  3.93 

12  jti  Centauri   S-  =  3.93 

13  v  Centauri   J  3.93 

14  £  Lupi   4.01 

15  £  Lupi   4.05 

16  ?j  Lupi   4.10 

17  1  Lupi    4.17 

18  0i  Lupi   4.25 

19  k  Lupi   4-32 

20  ;r  Lupi   4.40 

21  n  Lupi   4.47 

22  v  1  Centauri  4.55 

23  <p  Centauri   4.62 

24  \  Lupi. 

25  c  Centauri. 

Note. — No.  25  is  B  A  C.  4852. 


Sequence  13. 

May  31,  1836. 

Moon  one  day  past  the  full. 
Altitude  io°.  .20°. 

1  Sirius    o.  10 

2  Canopus    0.22 

3  a  Centauri    °-34 

4  Arcturus    0.45 

5  Saturn     

6  (3  Centauri    1.14 

7  a  Crucis    1.21 

8  Spica    1.39 

9  jj  Argus    

10  (3  Crucis    1.57 

117  Crucis    1.72 

12  |3  Argus    2.01 

137  Argus    2. 1 1 

14  £  Argus    2.17 

15  a  Trianguli   )  2.23 

16  8  Argus   $  2.44 

17  \  Argus    2.48 

18  0  Centauri    2-55 

19  y  Centauri    2.71 

20  1  Argus   2.73 

21  £  Centauri    2.80 

22  a  Lupi   2.83 

4  L 


23  £  Centauri    a.88 

24  >)  Centauri   2.91 

25  0  Centauri?  ?  (clouded)   3.00 

Notes. — No.  9,  rj  Argus,  not  entitled 
to  a  place  in  the  first  class  of  stars. — 
|3  Crucis  is  less  than  rj  Argus. — 
a  Crucis  is  but  a  little  greater  than 
Spica.  —  6  Centauri  is  to-night  de- 
cidedly greater  than  y. 


Sequence  14. 
May  31,  1836. 

1  a  Pavonis  (low)   ji   2.55 

2  6  Centauri   S  2.55 

3  y  Centauri    2.71 

4  t  Argus   2.73 

5  £  Centauri    2.80 

6  a  Lupi   2.83 

7  fi  Argus  ?   2.86 

8  £  Centauri    2.88 

9  i]  Centauri    2.90 

10  y  Corvi   2.91 

1 1  j3  Corvi   2.93 

12  S  Centauri    3.00 

13  k  Argus    3.04 

14  1  Centauri  }   3.08 

15  y  Virginis                          5  3.08 

16  a  Librae    )   3.15 

17  (i  Librae   j  3.15 

18  £  Corvi   3.22 

19  S  Corvi   3.25 

20  y  Hydrae    3.28 

21  0  Crucis    3.31 

22  9  Argus   3.34 

23  a  Muscae   3.36 

24  (3  Lupi   3.39 

25  y  Lupi  ?  ?  ^{    3.45 

26  v  Argus   J   3.50 

27  y  Triang  S  3-5° 

28  Triang   3.55 

29  X  Centauri    3.59 

30  N  Velorum   3.62 

31  u  Argiis    3.66 

32  7r  Hydrae   3.70 

33  a  Circini   3.75 

34  k  Centauri                           (  3.79 

35  (3  Muscae                              f  3.82 

36  8  Lupi  J  3.85 

37  £  Lupi    3.89 

38  p  Carinae   3.94 

39  q  Carinae   3.99 

40  £  Lupi   4.05 

41  fx  Centauri    4.09 

42  v  Centauri    4.15 

43  £  Crucis    4.60 

44  8  Muscae    4.60 

45  /,-  Lupi   4.61 

46  B  A  C.  3984    4.61 

47  O  Crucis   4.61 

48  y  Muscae   4.62 

49  0  Centauri    4.62 

Notes. — No.  25,  the  moon  too  near. 


Sequence  15. 
June  7,  1836. 
1  a  Centauri    0.34 


314 


SEQUENCES  AND  EQUALITIES  IN  THE 


2  a  Lyne   0.66 

3  a  Eridani   0.93 

4  j3  Centauri    1.14 

5  a  Crucis    1.2 1 


6  Antares   1.27 

7  a  Aquilae   1.33 

8  Foiualhaut    1.45 

9  X  Scorpii  J   1.6 1 

10  a  Gruis                              J  1.6 1 

11  a  Cygni : ;  (low)   1.95 

12  t  Sagittarii    2.23 

13  a  Trianguli    2.26 

14  a  Pavonis   2.29 

156  Scorpii   2.32 

16  a  Sagittarii    2.36 

17  (3  Gruis   2.38 

18  8  Scorpii   2.86 


Sequence  16. 
July  14,  1836. 

1  Canopus  (low)   0.22 

2  a  Centauri    0.34 

3  a  Eridani   0.93 

4  j3  Centauri    1.14 

5  a  Aquilae   1.27 

6  Antares   1.33 

7  Fomalhaut    1.45 

8  a  Gruis   1.67 

9  X  Scorpii   1.95 

10  a  Trianguli    2.23 


1 1  /3  Ceti    2.24 


12  a  Andromedae  (low)    2.25 

13  e  Sagittarii   }   2.26 

14  a  Pavonis  j  2.26 

156  Scorpii    2.28 

16  /3  Gruis   2.36 

170-  Sagittarii    2.38 

18  t  Pegasi    2.51 

19  a  Pegasi    2.65 

20  (3  Pegasi    2.78 

21  a  Phoenicis    2.92 

22  y  Pegasi    3.05 

23  j3  Hydri    3.19 

24  a  Toucani   3.38 

25  a  Pictoris   3.56 

26  y  Gruis   3.65 

27  a  Indi    3.68 

28  y  Hydri    3.75 

29  a  Doradus    3.82 

30  a  Reticuli   3.87 


31/3  Doradus. 
Note. — No.  17  low. 


Sequence  17. 
July  16,  1836. 


1  /3  Hydri    3.19 

2  £  Sagittarii    3.24 

3  a  Toucani   3.30 

4  8  Sagittarii    3.35 

5  y  Aquilae   3.41 

6  a  Hydri    3.46 


7  7r  Sagittarii    3.52 

8  y  Gruis   3.57 

9  <p  Eridani   3.63 

10  y  Hydri    3.68 

11  a  Indi    3.75 


12  <p  Sagittarii    3.83 

13  /?  Pavonis   3.91 

14  e  Gruis   4.00 

15  8  Pavonis  4.00 

i6/3  Toucani   4.01 

17  r  Octantis    4. 11 

i8/3  Indi   4.22 

19  £  Pavonis  . ,   4.33 

20  y  Toucani   4-44 

21  (8  Octantis    4.50 

22  £  Pavonis   4.56 

23  y  Pavonis   )   4.62 

24  8  Toucani  $  4.62 


Sequence  18. 
August  7,  1836. 

1  a  Centauri    °-34- 

2  a  Lyra  (low)    0.66 

3  a  Eridani   0.93 

4  a  Aquilae   1.27 

5  Antares   1.33 


6  Fomalhaut    1.45 


7  /3  Crucis    1.57 

8  a  Gruis   1.67 

9  X  Scorpii   1.97 


10  0  Scorpii    2.26 

11  £  Sagittarii    2.28 

12  a  Pavonis   2.33 


130-  Sagittarii    2.38 


14  r)  Ophiuchi    2.89 

15  t  Ophiuchi    2.97 


16  <J  Sagittarii    2.99 


17  £  Sagittarii    3.01 

18  y  Aquilae   3.07 

19  X  Sagittarii    3.13 

20  v  Ophiuchi    3.26 


21  7r  Sagittarii    3.40 


22  £  Aquilae    3.45 


23  r]  Serpentis    3.51 


24  6  Aquilae   )   3.57 

25  X  Aquilae   )  3.57 


26  8  Aquilae   3.64 

27  7r  Ophiuchi   3.71 

28  <p  Sagittarii    3.73 

29  t  Sagittarii. 

30  £  2  Sagittarii. 

3 1  £  Ophiuchi. 


32  9  Serpentis. 

33  (3  Aquilae. 


34  Aquilae  (1  Fl.) 

35  7]  Aquilae. 

36  0  Sagittarii. 


37  p.  Sagittarii. 


38  Aquilae  (6  Fl.) 

39  i  Aquilae. 

40  p  Sagittarii. 

41  Aquilae  (9  Fl.) 


42  q  Scuti  (Bode). 


43  £  1  Sagittarii. 

Notes. — Nos.  34,  38,  41,  are  the  stars 
called  in  Bode's  maps,  m,  1,  and  k 
Scuti  respectively. — No.  42  (q  Scuti) 
is  B  A  C.  6324. 


Sequence  19. 
November  12,  1836. 


1  a  Orionis  ^   0.88 

2  Rigel                                S  ~  0.88 

3  Procyon    0.90 

4  a  Eridani  (low)    0.93 

5  a  Crucis    1.07 

6  Aldebaran   1.2 1 


7  T)  Argus    - 

8  Pollux  (low)   1.5 1 

9  £  Canis   1.89 

10  y  Orionis   1.92 

11  £  Orionis   1.97 

12  Castor  (lotc)   2.02 

13  a  Hydrae   2.08 

14  £  Orionis   2.16 

15  y  Argus    2.22 

16  0  Canis   2.35 

17  /3  Canis    2.41 

18  y  Geminor    2.52 


19  8  Orionis   2.55 

20  k  Orionis   2.66 

21  £  Argus    2.75 

22  a  Leporis   2.83 

23  t]  Canis   2.96 


24  a  Columbae   3-05 

25  /3  Eridani   3.20 

26  p  Argus    3.32 

27/3  Leporis   3.42 

28  1  Orionis   3-58 

29  £  Canis   3.65 

30  o  2  Canis   3.72 


31  7]  Orionis. 

32  y  Canis. 

Notes. — Before  the  commencement  of 
this  sequence,  Jupiter  and  Mars  were 
compared  as  follows  : — 

1  Jupiter. 

2  Sirius. 

3  Canopus. 

4  a  Orionis.  >  

5  Mars.       S  ~ 

— No.  26  is  miscalled  1  in  Bode's 
map.     It  is  15  Fl.  Argus,  and  is 


APPARENT  MAGNITUDES  OF  STARS 


315 


called  in  B  A  C  (No.  2728)  p  Argus. 
— y  C'anis  at  3h  zom  A  M.  was  of 
5th  magnitude.  Bode  sets  it  down  as 
variable. 


Sequence  20. 
Nov.  13,  1836. 


1  a  Orionis  1   0.88 

1  Rigel  \  ~  0.88 


3  y  Orionis   1.77 

4  t  Canis   1.77 

5  t  Orionis   1.89 

6  £  Orionis   2.13 

7  8  Canis   2.40 

8  /c  Orionis   2.59 

9  /3  Canis   2.64 

10  £  Argus   2.67 


11  8  Orionis   2.74 

12  r)  Canis   2.84 

13  a  Leporis   2.99 

14  7r  Argus    3.10 

15  /3  Canis  Minor   3.20 


16  1  Orionis    3.30 

17  /3  Leporis   3.41 

18  q  Orionis   3.51 

19  0  Columbae   3.62 

20  £  Canis   3.69 


21  £  Argus    3.72 

22  o  2  Canis   3.76 


23  <r  Argus    3.79 

24  v  Argus    3.82 

25  t  Leporis   3.85 

26  r  Orionis   3.89 

27  t]  Orionis   f   3.92 

28  fi  Leporis   $  3.92 

29  z  Orionis   3.95 

30  £  Leporis   3.99 

31  v  2  Eridani   4.02 

32  X  Orionis   4.05 

33  j]  Leporis   4.09 

34  y  Leporis  )  4.12 

35  c  Leporis  )  4.15 

36  fi  Eridani   4.19 

37  L  2  Puppis   4.2a 

38  r  Orionis   4.25 

39  k  Puppis    4.29 


40  9  Orionis. 

41  <y  Orionis. 

42  X  Eridani. 

43  Eridani. 

44  7r  1  Orionis. 


45  k  Leporis.  -j 

46  t  Leporis.    V  = 

47  X  Leporis.  J 

48  7r  2  Orionis. 


49  £  Eridani  ? 

50  c  Eridani  ? 

5 1  v  Leporis. 


Notes.  —  No.  18  is  Flamsteed's  1 
Orionis,  B  A  C  i486,  there  called 
tt  i. — No.  26  is  FI.  3  Orionis,  B  A  C 
1495,  there  called  tt  3. — No.  29  is 
FI.  8  Orionis  =  B  A  C.  1514,  there 
called  jr  5. — No.  44  is  FI.  2  Orionis 
=  B  A  C.  149 1,  called  tt  2  ;  and  No. 
48  is  BAG.  1516,  the  ir  4  of  that 
Catalogue.  To  prevent  confusion,  I 
have  adhered  to  the  old  lettering. 
The  five  7r's  of  the  B.  A.  Catalogue 
are  spread  over  a  space  nearly  50  in 
extent. — Nos.  34,  35.  Very  nearly 
ecpaal,  but  y  a  trifle  larger.  In  Bode, 
8  is  a  whole  magnitude  above  y. — 
No.  37  is  B  A  C.  2392. — No.  39  is 
erroneously  marked  k  in  Bode's  map, 
where  it  is  called  Markeb.  It  is 
double,  the  two  being  seen  as  one 
to  the  naked  eye. — No.  40.  The  tra- 
pezium in  the  nebula  seen  as  one  star. 
Nos.  49,  50.  Hazy. 


Sequence  21. 
November  26,  1836. 


1  Sirius    0.10 

2  Canopus    0.22 

3  Rigel   0.76 

4  a  Orionis   0.93 

5  a  Eridani   1.10 

6  Fomalhaut    1.45 

7  t]  Argus    — 

8  a  Gruis   1.67 


9  e  Canis   1.77 

10  t  Orionis   1.89 


11  £  Orionis  }  1.97 

12  a  Pavonis  )  1.99 

13  /3  Argus    2.01 

14  y  Argus   ^   2.13 

155  Canis  $  2.13 

16  /3  Gruis   2.21 

17  £  Argus   \   2.3 1 

18  y  Orionis                          J  2.31 

19  a  Arietis    2.40 

20  8  Argus    2.44 


2i/3  Ceti    2.51 

22  k  Orionis   2.59 


23  a  Phoenicis    2.62 

24  8  Orionis   2.65 


25  a  Leporis   -\  3.05 

26  a  Toucani   V  3.09 

27  ,8  Hydri  J  3.17 


28  a  Hydri    3.26 

29  a  Columboe   3.36 

30  t  Argus    3.50 

31  a  Indi    3.55 

32  y  Hydri    3.60 

33  a  Pictoris   3.64 

34  £  Canis   3.66 


35  v  Argus    3.68 

36  y  Gruis   3.70 

37  p  Leporis   3.72 


38  9  Eridani   3.72 


39  ji  Columbae   3.73 

40  a  Doradus    3.78 

41  ji  Phoenicis    3.84 


42  y  Phoenicis    3  90 


43  0  Eridani   3.94 

44  £  Gruis   3.98 

45  /3  Toucani    4-°4 

46  a  Reticuli  )   4.09 

47  x  Eridani  J  4.09 


48  8  Phoenicis    4.18 

49  y  Volantis    4.28 

50  k  Eridani   4.33 


51  £  Phoenicis    4.36 

52  k  Phoenicis    4-4° 

53  y  Toucani   4.44 


54  1  Gruis   4.48 

55/3  Volantis    4.51 

56  )3  Reticuli   4.52 


57  8  Volantis   4.54 

58  £  Hydri   4.58 


59  8  Hydri    4.60 

60  £  Toucani   4.62 

61  a  Volantis    4.65 

62  |8  Doradus    4.67 

63  £  Toucani   4.70 

64  £  Volantis   4.73 

65  a  Chamsel  4.79 

66  £  Volantis   4.84 

67  y  Doradus    4.87 

68  c  Doradus    4.90 

69  9  Chamsel   4.91 

70  £  Hydri   4.92 


7 1  £  Doradus    4.93 

72  £  Reticuli   4.95 

73  £  Doradus   4.96 


74  B  A  C.  1 103    5.00 

75  £  Horologii   5.01 

76  B  A  C.  956   5.03 


Sequence  22. 
March  10,  1837. 

1  Canopus    0.22 

2  a  Centauri    0.33 

3  Arcturus    0.45 

4  An  tares  }  0.60 

5  Saturn   £  — 


6  a  Ci'ucis    1. 10 

7  (3  Centauri    1.24 


8  Spica    1.39 

9  Argus   — 


10  f3  Crucis    1.57 


11  y  Argus   ^   1.92 

12  j3  Argus   S  1.92 


13  y  Crucis    2.30 


316 


SEQUENCES  AND  EQUALITIES  IN  THE 


14  6  Centauri    2.55 

157  Centauri    2.71 

16  y  Corvi  )  __  2.86 

17  t  Centauri                  . .  . .  $  2.86 

18  y  Virginis   ~\  2.95 

19  ft  Corvi                             >  =  2.95 

20  S  Centauri                       J  2.95 

21  £  Centauri    3.04 

22  8  Corvi   3.15 

23  t  Corvi  )   3.31 

24  v  Hydra?   5  3.31 

25  1  Centauri   3.45 

26  $  Crucis    3.60 

27  t  Crucis   >  4.60 

28  a  Corvi  S  4-60 

29  jj  Corvi  

30  £  Corvi  


SEQUENCE  23. 

April  9,  1837. 

1  y  Crucis    1.72 

2  y  Argus    2.01 

3  j3  Argus    2. 1 1 

4  a  Trianguli    2.23 

5  y  Centauri    2.71 

6  y  Corvi   2.90 

7  ft  Corvi   2.93 

8  y  Virginis  }   3. 11 

9  0  Corvi  S  3. 1 1 

10  t  Corvi   3.31 

11  it  Scorpii   3.38 

12  r  Scorpii   3.45 

13  ft  Trianguli   3.50 

14  y  Trianguli   3.52 

150  Crucis    3.60 

16  £  Virginis   3.70 

17  a  Circini    3.80 

18  c  Virginis  ,   3.90 

19  t)  Virginis   4.00 

20  7]  Lupi   4.10 

21  ?  Hydra;   4.15 

22  £  Crucis    4.60 

23  a  Corvi   4.61 

24  O  Crucis   4.61 

25  p  Centauri    4.63 

26  0  Centauri    4,66 

27  a  Normae   4.67 

28  ft  Normae   4.68 

29  ft  Crateris   4.68 

30  jj  Corvi. 

31  o  Crateris  (Bode). 

32  £  Crateris. 


33  a  Hydrae 


34  BAG  4284? 

35  H  Centauri. 

36  r  Centauri. 

Notes. — No.  21  is  called  in  A  S  C  S 
Hydr.  et  Crat. — No.  29  is  B  A  C. 
3826. — No.  31  is  22339  Hist.  Cel. — 
No.  32  =  B  A  C.  3978. — No.  33  is 
the  well-known  double  Star  17  Hydrae 
Fl.— No.  35  is  B  A  C.  4344.— No.  36 
=  B  A  C.  4437. — No.  34  identity 
doubtful.  My  star  is  noted  in  the 
working  chart  as  about  2"'  following 
and  15'  north  of  the  star  B  A  C.  4284, 
which  is  correctly  placed  by  Bode. 


sequence  24. 
April  9,  1837. 

1  y  Argus    2.01 

2  ft  Argus    2. 1 1 

3  X  Argus    2.48 

4  X,  Argus    2.74 

5  it  Argus    2.96 

6  v  Argus  -\  3.26 

7  r  Argus                             L  3.55 

8  (7  Argus                              J  3.79 


sequence  25. 
April  10,  1837. 

1  »;  Argus    — 

2  £  Canis   1.89 

3  y  Argus    2.01 

4  ft  Argus    2. 1 1 

5  S  Canis   2.34 

6  £  Argus    2.74 

7  it  Argus    2.90 

8  ft  Corvi   }  3.00 

9  fi  Argus   S  3- 10 

10  £  Corvi   3.31 

1 1  £  Canis  ?    3.40 

12  a  Muscae  }   3.45 

13  y  Virginis  J  —  3.45 

14  p  Argus    3.52 

15/3  Muscae   3.60 

16  r  Argus    3.66 

1702  Canis   3.70 

18  v  Argus    3.73 

19  £  Argus    3.77 

20  tj  Canis  >   3.79 

21  a  Argus   \  3.79 

22  c  Puppis    3.91 

23  /c  Canis   4-°4 

24  X  Canis   4.16 

25  k  Puppis    4.29 

26  o  1  Canis   4-3° 

27  a  Puppis    4.31 

28  v  Pictoris  (Bode)  4.32 

29  jfc  B  A  C.  2562    4.32 

30  a  Mali    4-33 

31  0  Argus    4.34 

32  *■  Argus    4.35 


33  p  Velorum    4.50 

34  q  Velorum    4.65 

35  b  Mali   }  _  4.81 

36  c  Mali   S  ~  4.81 

37  y  Columbae   )   4.91 

38  k  Columbae   $  4.91 

39  to  Canis   4-93 

40  p  Puppis    4.96 

41  6  Columbae   4.98 

42  0  Puppis. 

43  f  Puppis. 

44  D  1  Canis  (Bode). 

45  M  Velorum. 

46  B  AC.  3382. 

47  m  Puppis. 

48  BAG.  2560. 

49  B  A  C.  3276. 

50  t  Velorum. 

51  u  Velorum. 

52  Q  Velorum. 

5  3  R  Velorum. 

54  BAC.  3348. 

55  BAC.  3501. 

56  B  A  C.  2214. 

57  BAC.  2219. 

58  BAC.  3379. 

59  h  Canis  (Bode). 

60  B  A  C.  2565. 

61  BAC.  3512. 

62  BAC.  3461. 

63  y  Velorum. 

64  t  Puppis.  ) 

65  g  Puppis  (Bode).  > 

66  C  Canis  (Bode). 

67  s|t  not  identified. 

68  BAC.  2557. 

69  BAC.  3396. 

Notes. — Nos.  5  and  11  set  down  in  the 
original  as  y  and  but  this  is  clearly 
by  mistake  for  S  and  £. — No.  14,  mis- 
lettered  1  by  Bode. — No.  22  =  B  A C. 
2580. — No.  23  is  Bodes  k  2  =  B  A  C. 
2246;  27  is  B  A  C.  2634;  28  is 
BAG.  1933,  placed  in  that  Cat.  in 
Puppis;  30,  35,  36,  are  respectively 
B  A  C.  2964,  2935,  and  3010;  42  is 
BAC.  2594;  43  is  2523;  44  == 
2109;  45  =  3300  B  A  C;  47  = 
BAC.  2525;  51  =  337°;  52  = 
3472;  S3  =  3499;  59  =  2251;  65 
=  2252;  66  =  2127  of  the  same 
Catalogue. 


Sequence  26. 
April  10,  1837. 

1  Arcturus    0.45 

2  Saturn   — 

3  Antares   1-27 

4  Spiea    i-39 

5  6  Scorpii   2.28 

6  6  Centauri   }  2.55 

7  a  Ophiuchi   S  2.67 

8  £  Centauri    2.80 

9  a  Lupi  I   2.84 

10  £  Scorpii  )  2.84 


APPARENT  MAGNITUDES  OF  STARS 


31 


10  S  Scorpii   )  2-86 

11  /3  Scorpii                            S  2-88 

12  r\  Ophiuchi    2-89 

13  r)  Centauri    2.91 

14  k  Scorpii   2.93 

15  a  Serpentis   2.95 

16  Z  Ophiuchi    2.97 

17  fi  Ophiuchi    3.00 

18  j3  Herculis    3.02 

19  7)  Bootis  (low)   3.04 

20  /3  Librae    3.06 

21  a  Libra   \   3.16 

22  (3  Lupi  $  3.16 

23  y  Lupi   3.38 

24  a  Herculis    3.38 

25  (T  Scorpii   ~i  3.38 

26  r  Scorpii  }  =  3.38 

27  7r  Scorpii  3  3.38 

28  S  Lupi   3.95 

29  k  Lupi   3.96 

30  k  Ophiuchi    3.97 

317  Scorpii   3.98 

32  fi  Serpentis   3.99 

33/3  Serpentis    4.00 

34  t  Ophiuchi    4.01 

35  f  Lupi    4.02 

36  £  Virginis   4.06 

37  d  Scorpii    4.10 

38  fi  Serpentis    4^4 

39  o  Scorpii  ( 19  PL)    4.19 

40  z  Virginis  (109  Fl  )   4.23 

41  £  Serpentis    4.27 

42  X  Ophiuchi    4.32 

43  y  Serpentis    4.36 

44  fi  Virginis   4.40 

45  y  Libra    4.44 

46  1  Virginis   4.48 

47  p  Scorpii    4.52 

48  k  Virginis   4.56 

49  X  Lupi   4.59 

50  X  Virginis  >   4.63 

516  Librae   S  4.63 

516  Libra  )   4.63 

52  Z  Scorpii  (Bo.)  )  4.63 

53  a  Normse   4.67 

54  /3  Normse  >  4.68 

55  1  1  Libra   S 

56  0  Lupi. 

57  1  Ophiuchi. 

58  v  Ophiuchi. 

59  X  Serpentis. 

60  c  Libra  (16  Fl.)   )  _ 

61  e  Libra  (48  Fl.)    )  — 

62  a  Serpentis. 


63  0  Libra. 

Notes. — No.  31  is  20  Libra  Fl.  = 
B  A  C.  4950.  — o  Scorpii,  No.  39,  is 
B  A  C.  5455- — No.  40,  z  Virginis  = 
BAG.  4878. — No.  52  is  51  Libras 
Fl.  =  B  A  C.  5324,  a  well  known 
double  star. — Nos.  60  and  61  are  Nos. 
4927  and  5290  B  A  C.  None  of  these 
stars  have  letters  in  the  B  A  Catal. — 
No.  63,  0  Libra,  is  only  of  the  6  or 


5"  magnitude,  though  marked  4  m  in 
Bode  and  4^  in  B  A  C. 


Sequence  27. 
August  4,  1837. 

1  a  Aquilse   1.33 

2  Fomalhaut    1.45 

3  a  Gruis   1.67 

4  (3  Gruis  )  2.36 

5  <t  Sagittarii   $  2.38 

6  a  Pavonis   2.50 

7  t  Pegasi    2.62 

8  y  Aquilse   2.73 

9  |3  Aquarii   2.85 

10  a  Aquarii   2.97 

11  if  Toucani   3.08 

12  fi  Capricorni   3.20 

13/3  Capricorni    3.32 

14  y  Gruis   3.44 

15  y  Pavonis   3.56 

16  a  Indi    3.68 

175  Aquarii   3.79 

18  t  Gruis   3.88 

19  a  2  Capricorni   3.94 

20  y  Capricorni   3.98 

2i/3  Pavonis   4.0 1 

22  £  Aquarii. 

23  y  Aquarii. 

24  X  Aquarii. 

25  r\  Aquarii. 

26  c  2  Aquarii  (88  Fl.) 

27  (3  Aquilse. 

28  T  Aquarii. 

29  9  Aquarii. 

30  tj  Gruis. 

31  b  1  Aquarii  (98  Fl.) 

32  a  1  Capricorni. 

33  t  Aquarii. 

34  £  Pise.  Aust. 
35/3  Pise.  Aust. 

36  b  2  Aquarii  (99  Fl.) 

37  7r  Aquarii. 

38  b  4  Aquarii  (101  Fl.) 

39  y  Pise.  Aust.  (22  Fl.) 

40  fi  Pise.  Aust.  (23  Fl.) 

41  /'  Pise.  Aust. 

42  c  3  Aquarii  (89  Fl.) 

43  c  1  Aquarii  (86  Fl.) 

44  o  Aquarii  (31  Fl.) 

45  7r  Pise.  Aust.  (75  Fl.) 

46  L  Aquarii  (61  Fl.) 

47  c  Aquarii. 

48  p  Aquarii. 

49  v  Pise.  Aust.  (Bode). 

Notes. — No.  39  is  mis-lettered  £  in 
Bode's  map  ;  and  No.  40  is  there 
lettered  o. — Nos.  45  and  46  have  no 
letters  in  B  A  C.  Those  used  here 
are  Bode's. — No.  49  is  B  A  C.  7702. 
4  M 


N.B.  a  1  and  a  2  Capricorni  dis- 
tinctly seen  as  two  stars  with  the 
naked  eye. 


Sequence  28. 
September  24,  1837. 

1  (3  Gruis   2.36 

2  a  Arietis    2.40 

3  j3  Ceti    2.66 

4  a  Phcenicis    2.92 

5  /3  Hydri    3.19 

6  a  Ceti    3.46 

7  9  Eridani   3.73 

8  a  Hydri    3.33 

9  y  Eridani   3.93 

10  r\  Ceti    4.03 

11  a  Piscium  )  4. 1 3 

12  y  Ceti                                   5  4-24 

13  t  Ceti    4.28 

14  0  Ceti    4.33 

15  <J  Eridani   4.37 

16  v  Ceti  +  t  Ceti    4.42 

17  £  Eridani  ^\  4.46 

18  k  Eridani                              t  4.51 

19  a  Fornacis  (Bode)                 f  4.55 

20  s  Eridani  (Fl.  16)   J  4.59 

21  i]  Eridani   4.63 

22  7r  Ceti    4.67 

23  fi  Ceti    4.7 1 

24  t  Eridani  (19  Fl.)   \  4.74 

25  E  Eridani  (11  Fl.)  $  4.78 

26  g  Eridani   4.81 

27  f  2  Eridani    4.85 

28  m  1  Eridani  (27  Fl.)    4.S5 

29  Z,  Ceti    4.86 

30  r  i  Eridani  (1  Fl.)    4.86 

31  £  Ceti    4.86 

32  p  Ceti   ,   4.87 

33  1  1  Eridani  (33  Fl.)    4.88 

34  1  2  Eridani  (36  Fl.)   4.89 

35  h  Eridani   4.89 

36  Eridani  (15  Fl.) 

37  <r  Ceti. 

38  £  Eridani. 

39  X  2  Ceti  ( Bode). 

40  m  2  Eridani  (28  Fl.) 

41  c  Ceti  (46  Fl.) 

42  F  Eridani  ( 20  Fl. ) 

43  b  Ceti  (37  Fl.) 

44  t  2  Eridani  (2  Fl.) 

45  v  1  Ceti  (56  Fl.) 

46  u  Ceti  (75  Fl.)  I 

47  o  Ceti  ?   "  S 

Notes.— In  this  Sequence  the  lettering 
is  that  of  Bode's  Atlas,  Plate  XVII. 
But  the  stars  have  been  all  carefully 
identified  by  the  aid  of  the  B  A  C.  with 
Flamsteed  s,  wherever  a  difference  of 
lettering  arising  from  the  carrying  out 
of  Bayer's  system  in  that  Catalogue 
renders  a  doubt  possible.  To  have 
changed  all  the  letters  would  have 
inevitably  induced  complete  confusion. 
— No.  14  is  9  1  Ceti  Bode,  but  9  2 
being  a  distant  and  inconspicuous 
star  (7  m),  the  1  is  dropped. — No.  16 


318 


SEQUENCES  AND  EQUALITIES  IN  THE 


is 

25  =  r  3, 
33  =  r  8, 

44  =  T  2, 


near  v  is  t,  but  both  arc  here  seen  as 
one  star. — No.  19.  The  a  of  Fornax 
is  retained  in  B  A  C.  No.  997  with 
the  constellation  Eridanus,  so  that  in 
that  Catalogue  the  star  stands  as 
«  Eridani.  It  is  12  Fl.  Eridani. — 
No.  20  is  r  4,  No.  24  is  r  5,  No. 

No.  28  =  r  6,  30  =  r  1, 
34  =  t  9,  40  =  r  7,  and 
of  the  B  A  C— No.  26  is 
B  A  C.  1201,  there  called  v  2  ;  No.  27 
=  B  A  C.  1 199  ;  35  =  B  A  C.  11 51, 
there  called  v  I ■;  36  =  B  A  C.  1031  ; 
39  is  simply  lettered  x  Ceti  in  B  A  C. ; 
41  is  B  A  C.  429  ;  42  =  B  A  C.  1 1 1 5  ; 
43  =  B  A  C.  372  ;  45  =  594  ;  and 
46  =  778,  of  that  Catalogue. — In  this 
Sequence,  strong  suspicions  of  tem- 
porary dimness  from  flitting  haze, 
and  certainly  north  of  the  equator 
there  was  no  deciding  with  certainty 
on  the  magnitudes.  Even  a,  y,  and  S 
Ceti  were  occasionally  touched.  Bode's 
6  2  Ceti  and  his  \  1  Ceti  not  seen ; 
X  2  conspicuous,  5  m. 


Sequence  29. 
September  25,  1837. 

1  /3  Ceti    2.46 

2  a  Ceti    3.14 

3  1;  Ceti    4.00 

4  t  Ceti    4.28 

5  9  Ceti    4.30 

6  S  Eridani   4.33 

7  t  Eridani   4.40 


33  y  2  Eridani. 

34  H  C.  6161. 


8  a  Sculptoris. 

9  v  2  Ceti. 


10  i  Sculptoris. 

11  v  2  Machinse. 


12  £  Sculptoris. 

13  <d  Fornacis. 

14  0  1  Ceti  (17  Fl.) 

15  %  2  Ceti. 

16  /3  Machinse. 

17  vi  Machinal. 

18  7r  Eridani  (26  F.) 

19  *  Ceti  (48  Fl.) 

20  %  Ceti  4396  H  C. 


21  vi  Ceti  (56  F.) 

22  a  Machinse. 

23  t  Machinse. 

24  F  Ceti  (67  F.) 

25  F  Eridani  (20  F.) 


26  \p  Ceti. 

27  t  Ceti  (57  F.) 

28  \p  2  Machinse. 

29  c  Ceti  (46  F.) 

30  0  2  Ceti  (19  F.) 

31  p  3  Erid.  (10  F.) 

32  *  Ceti  C 18  F. ) 


35  B  A  C.  203. 

36  H  C.  7422.  jf  

37  c  Eridani.  j 

38  H  C.  4466. 

39  p  2  Eridani  (9  F.) 

40  H  C.  1245. 

41  Ceti  (27  F.) 

42  H  C.  3479. 

43  B  A  C.  776. 

44  D  Eridani. 

45  k  1  Sculptoris.  )  

46  k  2  Sculptoris.  $ 

47  $  Sculptoris. 

48  t  Sculptoris. 

49  11  Ceti  (75  F.) 

50  B  A  C.  1 1 52. 

51  B  Eridani. 


52  1^  1  Machinse. 

53  0  3  Ceti  (22  F.) 

54  0  4  Ceti  (23  F.) 

55  Ceti  (28  F.) 

56  Ceti  (30  F.) 

57  p  1  Eridani  (8F.) 

58  q  Ceti. 

59  6  2  Ceti. 

60  x  1  Ceti. 

Notes. — The  nomenclature  is  that  of 
Bode's  Chart,  PI.  17  for  lettered  stars. 
The  identifications  with  B  A  C.  and 
the  Histoire  Celeste  are  as  follows : — 


No.=BAC. 

11  643 

12  8352 
790 


!3 

*5 
16 

17 
22 
23 
26 


103 1 
688 
627 

54-1 
489 

"5 


No.=BAC. 
28  460 


45  10 

46  23 

47  135 

48  72 
50  1152 


52 
58 


458 
230 


No.=HC. 

33  7600 

34  6161 

36  I  74" 
3   <  7423 

37  7273 
of  4466 

38  *  4467 


No.=HC. 

S  I245 
4°  \  1246 
44  6535 
51  6661 

59  2848 

60  3137 


The  bracketed  numbers  are  probably 
only  duplicates.  Bode's  tt  and  6  For- 
nacis are  invisible  to  the  naked  eye. 


Sequence  30. 
Oct.  24,  1837. 

1  Canopus    0.22 

2  a  Orionis  (high)   0.50 

3  a  Eridani   0.80 

4  a  Orionis  (low)    1.07 

5  Rigel     1.27 

6  Fomalhaut    1.45 

7  Aldebaran    1.54 

8  a  Gruis   1.67 


9  a  Arietis   )   2.40 

10  a  Pavonis  $  2.40 

1 1  f3  Ceti    2.43 

12/3  Gruis   2.46 

13  k  Orionis   2.58 

14  a  Phoenicis   2.70 

15  a  Ceti    2.82 

16  a  Leporis   2.94 

17/8  Eridani   3.06 

18  a  Columbae   3.18 

19  /3  Hydri    3.27 

20  a  Hydri    3.37 

2i/3  Arietis    3.49 

22  a  Toucani   3.61 

23  6  Eridani   3.73 

24  y  Hydri    3.77 

25  a  Doradus   1   3.80 

26  a  Pictoris  $  3.80 

27  a  Reticuli  (   3.87 

28  y  Gruis  j  3.94 

29  [5  Phoenicis    4.01 

30  f  Gruis   4.05 

31  y  Phoenicis    4.10 

32  &  Toucani    4. 1 5 

33  0  Eridani   4.20 

34  y  Ceti    4-24 

35  S  Hydri   >_  4.29 

36  f  Hydri   J  4.29 

37  x  Eridani   4.33 

38  y  Volantis   4.37 

39  (3  Doradus    4.40 

40  y  Toucani  4.43 

41  Z,  Phoenicis    4.47 

42  f  Phoenicis    4.50 

43  a  Volantis   4.53 

44  8  Volantis   -\  4.56 

45  j3  Reticuli    V  4.58 

46  1  Eridani  J  4.60 

47  £  Toucani   4.62 

48  r  Eridani   4.65 

49  /3  Volantis    4.68 

50  e  Ceti    4.71 

51  £  Volantis  4.73 

52  S  Phoenicis   )  4.75 

53  i)  Phoenicis    \  4.78 

54  K  Phoenicis    4.81 

55  y  Doradus    4.83 

56  tVolantis   4.85 

57  a  Chamseleontis    4.88 

58  Z  Toucani   4.90 

59  £  Doradus   4.92 

60  0  Toucani   4.94 

61  c  Doradus   4.96 

62  t  Toucani   4.97 

63  y  Reticuli   4.98 

64  B  A  C.  1 103    4.99 

65  X  Phoenicis   4.99 

66  /}  Toucani   5.00 

67  5  Horologii  (Bo.)    5.01 

68  f  1  Eridani    5.02 

69  X,  Hydri    5.02 

70  B  A  C.  582. 

71  B  A  C.  604. 

72  S  Reticuli. 

73  G  Carina?. 

74  t)  Hydri. 

75  fi  Phoenicis. 

76  k  Toucani. 


APPARENT  MAGNITUDES  OF  STARS. 


319 


77  £  Reticuli. 

78  p  Phoenicis. 

79  1  Reticuli. 

80  v  Hydri. 

81  p  Toucani. 

82  B  A  C.  958. 

83  (3  Horologii  ?  ? 

84  B  A  C.  2835  + 

85  r)  Yolantis. 

86  v  Toucani. 

Notes. — No.  60  is  the  great  cluster 
B  A  C.  85,  seen  as  a  star;  67  = 
B  A  C.  1048  +  1051  ;  68  is  B  A  C. 
828  :  83  not  identified;  84  is  B  A  C. 
2835  +  2837,  seen  as  one  star  = 
Bode  16  +  17. 


Sequence  31. 
Nov.  16,  1837. 
1  Fomalhaut    1.47 


Notes.  —  Seven  of  the  Pleiades  seen 
with  the  naked  eye  and  equalized  as 
follows  : — 


2  (3  Gruis  }   2.36 

3  a  Arietis   J  2.40 


4  /3  Ceti    2.4 


5  a  Ceti    3.14 

6  y  Gruis   3.66 

7  £  Aquarii   3.80 


y  1  Eridani   3.95 


9  i)  Ceti    4-°9 

10  y  Ceti    4-24 

n  j  Eridani   4.26 

12  s  Eridani  (16  F.)   4.28 

13  c  2  Aquarii  (low)   4.30 


14  o  Tauri   4.32 

15  £  Eridani   )   4.34 

16  a  Piscium  $  4.34 

17  £  Tauri   4.36 


18  t]  Eridani   4.38 

19  v  Tauri   4-4° 

20  <r  Eridani   4.42 

21  Tauri  (10  F.)    4.43 

22  7r  Ceti    4-45 

23  E  Eridani   4.47 

24  £  2  Ceti    4.49 

25  m  1  Eridani   4.51 

26  t  Eridani    4.53 


27  d  Eridani   4.55 

28  t  1  Eridani    4.57 

29  fi  Ceti  ~   4-59 

30  1  2  Eridani    4.61 

31-  p  Sceptri  (Bo.)    4.62 

32  t  2  Eridani. 

33  £  Eridani. 

34  1  1  Eridani. 

35  Eridani  (17  F.) 

36  x  2  Ceti. 

37  Pise.  Aust.  (19  F.) 


1  /;  Tauri 

d  Eridani 

2  f  Pleiadum 
r]  Eridani 

3  b  Pleiadum 
7r  Eridanf 

4  c  Pleiadum 

5  d  Pleiadum 

6  e  Pleiadum. 

7  h  Pleiadum. 


)- 
s~ 
X- 
s~ 
f_ 
s~ 


They  glimmer,  however,  fully  a  magni- 
tude +  and  —  c  and  d  are  rather  less 
than  7r  Eridani ;  e  rather  less  than  c  or 
d;  h  barely  discernible. — No.  31  is  53 
Fl.  Eridani  =  B  A  C.  1441. 


Sequence  32. 
December  16,  1837. 

1  Sirius    o.  10 

2  Canopus    0.22 

3  i)  Argus  (low)  )  — 

4  Rigel  J  0.76 

5  a  Eridani   °-93 

6  a  Orionis   1.00 

7  Aldebaran   1.07 

8  t  Orionis   1.77 

9  £  Canis   1.89 

10  fi  Argus    1.95 

1 1  £  Orionis   2.04 

12  y  Argus    2.1 1 

13^  Canis   z-34 

14  y  Orionis   2.42 

15  k  Orionis  }  2.59 

16  fi  Canis                                $  2.64 

17  £  Argus    2.74 

18  3  Orionis   2.79 

19  i]  Canis   2.84 

20  7r  Argus    2.96 

21  a  Leporis   3.05 

22  a  Columba?   3.09 

23/3  Leporis   3.20 

24  1  Orionis    3.30 

25  /3  Columbse   3.37 

26  /3  Eridani   3.44 

27  r  Argus    3.55 

28  ff  Argus    3.79 

29  £  Leporis   3.85 

30  y  Leporis  }  3.87 

31  fi  Leporis  >  3.90 

32  £  Leporis  )  3.99 

33  r)  Leporis   4.09 

34  8  Leporis   4.15 

Notes. — On  this  occasion  the  great  and 
sudden  increase  of  brightness  in  t) 
Argus  was  first  noticed.  Bode  has 
two  £  Normal's,  one  near  e  and  6,  and 


a  pair,  £  1  and  £  2,  near  k,  none  of 
them  exceed  7  m,  being  barely  percep- 
tible in  an  opera-glass. 


Sesuence  33. 
December  28,  1837. 

1  Jupiter   — 

2  Sirius    0.10 

3  Canopus    0.22 

4  ?)  Argus  (high)  J  _  — 

5  a  Centauri  (low)  $  0.34 

6  Rigel   0.76 

7  a  Eridani  ^  0.85 

8  Procyon   J  0.93 

9  fi  Centauri  (low)  /  1.14 

10  a  Crucis   $  1.21 

11  £  Orionis   1.40 

12/3  Crucis    1.60 

13  £  Canis   1.74 

14  7  Crucis    1.86 

15  £  Orionis   1.95 

16  (3  Argus    2.01 

17  y  Argus    2.10 

18  S  Canis   2.16 

19  t  Argus   2.27 

20  y  Orionis   2.42 

21  k  Orionis   2.59 

22  (3  Canis   2.64 

23  £  Argus    2.74 

Note. — When  a  Centauri  was  higher, 
t]  Argus  was  a  little  inferior. 


Sequence  34. 
December  29,  1837. 

1  Jupiter   — 

2  Sirius    0.10 

3  Canopus    0.22 

4  a  Centauri  (io°)  1  0.34 

5  17  Argus  (400)   5  — 

6  Rigel   0.76 

7  a  Eridani   0.85 

8  Procyon    0.93 

9  a  Orionis   1.00 

10  Aldebaran    1.07 

11  fi  Centauri    }  1.14 

12  a  Crucis   }  1.2 1 

13  Spica   1. jo 

14  Pollux    1.5 1 

15/3  Crucis    1.57 

16  Regulus    1.62 

17  y  Crucis    1.72 


320 


SEQUENCES  AND  EQUALITIES  IN  THE 


t  Orionis   }  

£  Orionis  S 

£  Orionis   )  

f  Canis  S 

y  Orionis 


•97 


y  Argus    2.04 

23  ;3  Argus    2.10 

24  f  Argus   2.17 

25  S  Canis   2.26 

26  S  Argus    2.35 

27  a  Hydrae   2.41 

28  X  Argiis    2.48 

29  /3  Hydri    3.19 

30  S  Crucis    3.60 

31  v  Centauri   )   3.92 

32  /3  Doradus   J  3.92 

33  p,  Centauri    3.93 

34  0  Centauri    4.30 

35  f  Volantis    4-5° 


36  £  Volantis   4.60 

37  8  Volantis   4.69 

38  p  Lupi   4.72 

39  £  2  Centauri   4.77 

40  f  Centauri   4.81 

41  8  Doradus  )  4.85 

42  t  Volantis   S  4-9° 

43  V  Centauri    4.90 

44  v  1  Centauri    4.91 

45  a)  Centauri  (J)    4.9 1 

46  x  Centauri    4.92 

47  d  Centauri    4.92 

48  ?  ?   4.92 

49  n  Centauri    4.93 

50  BAG.  2835  4-    4.93 

51  v  Doradus    4-94 

52  9  Doradus    4.94 

53  y  Pictoris   4.95 

54  B  Carinas  J   4.95 

55  C  Carina;  \  4.95 

56  p  Pictoris   4.96 

57  {  Doradus   4.96 

58  B  A  C.  1502. 

59  B  A  C.  1926. 

60  a  Centauri. 

61  v  2  Centauri. 

62  1  Pictoris  ? 

63  £  1  Centauri. 

64  e  Centauri. 

65/3  Mensae. 

67  X  Centauri.  )  

68  Y  Centauri.  ]  ~ 

69  a  Mensse. 

70  y  Mensee. 

7 1  tt  i  Doradus.  )  

72  7r  2  Doradus.  S 

73  B  AC.  2333. 

74  B  A  C.  2032. 

75  t]  1  Doradus. 

76  t]  2  Doradus. 

77  v  Pictoris. 


78  M  Centauri. 

79  m  Centauri. 

80  K  Centauri. 


81  B  AC.  2146. 
p  Pictoris. 
B  AC.  2108. 
B  AC.  2686  + 
N  Centauri. 


83 


85 
86 

87 


B  AC.  4625  >_ 
B  AC.  4635  S~ 


B  AC.  4693. 

89  *  not  identified. 

90  z  Centauri. 

91  w  Centauri. 

92  s|«  not  identified. 

93  B  A  C.  4482. 

94  Not  identified. 

95  Not  identified. 

96  Not  identified. 

97  Cent.  1 54  Bode. 

98  BAC.  2124?  ' 

99  B  A  C.  2108. 

100  B  A  C.  2408. 

101  B  A  C.  341 1  ? 

102  BAC.  3435  ? 

103  Not  identified. 

104  B  A  C.  4704. 

Notes. — No.  40  is  BAC.  4377. — The 
stars  after  No.  64  are  merely  grouped, 
but  under  each  group  unarranged  in 
any  order  of  brightness.  —  No.  14. 
15  Pollux  and  f3  Crucis  were  not  com- 
pared together.  Both  were  greater 
than  Regulus  and  less  than  Spica. — 
Nos.  48,  101,  102.  These  three  stars 
are  called  </>  1,  <p  2,  and  0  3,  Carina;. 
I  find  no  such  marks  in  any  of  my 
working  charts.  I  suppose  0  1  must 
be  <p  Argus,  and  that  0  2  is  BAC. 
341 1,  and  0  3  =  B  A  C.  3435,  near  f. 

No.  is  BAC. 


No.  is  BAC. 
S  2835 
*  2837 
2770 


5° 


54 
55 
56 
63 
64 
65 
67 
68 
69 
75 


2796 
1993 
+368 
4316 
1606 
4709 

4749 
2053 
2003 


76 

77 
78 

79 
80 
82 


85 
90 

9i 


203 1 
2093 
4580 
4417 
4495 
2167 
S  2686 
( 2687 

4616 

4586 
4409 


Of  the  stars  not  identified,  the  places  for 
1800,  taken  from  Bode's  map,  are  as 
follows  : — 


R 

A 

N  PD. 

No. 

h. 

ni. 

0  / 

89 

13 

49 

140  45 

92 

13 

37 

138  55 

94 

12 

56 

131  40 

95 

12 

59 

133  20 

96 

«3 

2 

133  20 

103 

7 

5* 

153  0 

i  Pictoris  (No.  62)  is  called  t  Doradus 
in  MS. ;  but  as  there  is  no  such  star 
in  Bode's  chart,  this  must  have  been 
a  mistake  for  the  star  here  set  down 
=  B  AC.  1 52 1. 


Sequence  35. 

January  2,  1838. 

Not  a  good  night. 

1  Rigel   0.76 

a  Procyon    0.85 

3  a  Eridani   0.93 

4  a  Orionis   1.00 

5  /?  Centauri    1.14 

6  Pollux   i.ig 

7  a  Crucis   /  i.xi 

8  f3  Centauri   \  1.30 

9  (3  Crucis    1.57 

10  Castor    1.67 

11  ci  Hydrae   1.73 

12  t  Orionis   1.77 

13  £  Canis   ^  1.99 

14  y  Orionis    I    1.99 

15  £  Orionis    f  1.99 

16  j8  Argus  J  1.99 

17  y  Argus    2.14 

18  S  Argus    2.29 

19  e  Canis   2.4c 

20  k  Orionis   2.59 

2 1  j3  Canis   2.64 

22  a  Leporis   2.80 

23  a  Museae  )  2.90 

24  y  Corvi  )  — 

24  y  Corvi  )   2.97 

25  j8  Leporis                         )  2.97 

26  /3  Eridani  )  3.06 

27  a  Columbse  $  3.13 

28  fi  Corvi   3.19 

29  n  Argus    3.23 

30  8  Corvi   3.27 

31  t  Argus   ^  3.36 

32  £  Hydrae                            f  3.44 

33  £  Corvi                               r  3.48 

34  ^3  Muscae  J  3.52 

35  £  Crucis    3.62 

36  j3  Canis  Minor   3.65 

37  v  Hydrae   3.69 

38  f  Hydrae  -v  3.72 

39  a  Doradus   (.  3.7J 

40  v  Hydri  J  3.77 

41  0  Crateris   "\  3.80 

42  p.  Centauri   /  3.88 

43  v  Centauri   C  3.97 

44  a  Reticuli   J  4.02 

45  a  Pictoris   4.09 

46  X  2  Hydrae    4.18 

47  /3  Cancri    4.27 

48  y  Volantis    4,37 

49  /3  Hydrae   4.46 

50  (3  Reticuli   4.58 

51  £  Crucis    4.60 

52  p.  Hydrae   4.61 

537  Crateris     4.62 

54  t  Hydrae    4.63 

55  v  1  Hydrae    4.64 

56  a  Crateris   4.65 

57  15  Hydrae    4.66 


APPARENT  MAGNITUDES  OF  STARS 


321 


58  n  Hydras  . . 
59/3  Crateris. . 

60  a  Corvi. 

61  r  2  Hydrae. 

62  <r  Hydras. 

63  1;  2  Hydras. 

64  r  1  Hydras. 


4.67 
4.68 


65  B  A  C.  4265.  }  _ 

66  BAG.  4221.  S~ 

67  Not  identified.  }  

68  Not  identified.  S 

Notes. — Nos.  5  and  8,  sic  in  MS. — 
No.  18  called  £;  no  doubt  S.— The 
places  of  the  unidentified  stars  on 
Bode's  chart  for  1800  are  respectively  : 

R.  A.  12*  24"      NPD.  1500  45' 
12    19  150  20 

I  cannot  be  quite  sure  of  the  entire 
absence  of  cloud  in  the  early  part  of 
the  night,  though  I  think  the  sky  was 
good. 


Sequence  36. 
January  6,  1838. 

1  Sirius    0.10 

2  Canopus    0.22 

3  a  Centauri      0.34 

4  n  Argus    

5  Rigel   0.76 

6  Procyon    0.85 

7  a  Eridani   0.93 

8  a  Orionis   1.00 

9  Aldebaran  2    1.07 

10  a  Crucis    1.2 1 

11  Pollux   1.5 1 

12  ft  Crucis    1.57 

137  Crucis    1.72 

14  e  Cards   1.77 

15  f  Orionis  1  1.89 

16  £  Orionis                             \  1.97 

17  ft  Argus    2.01 

18  y  Argus                             1   2.09 

19  y  Orionis  J>  2>  \  2.09 

20  4  Argus   2.17 

21  a  Hydrae  >   2.32 

22  d  Canis  J  2.32 

23  0  Argus    2.44 

24  X  Argus    2.48 

25  y  Geminorum   2.50 

26  ft  Canis   2.56 

27  k  Orionis   2.60 

28  £  Argus    2.69 

29  j]  Canis   2.80 

30  <c  Argus   2.85 

31  7r  Argus    2.93 

32  1  Argus   3.00 

33  P  Argus   >  3-08 

34  a  Leporis  )  3.08 

35  v  Argus    3.16 

36  a)  Argus    3.25 

37  r  Argus    1  3.36 

38  ft  Leporis  J  3.36 

39  ft  Canis  Min   3.49 


40  ft  Eridani   3.55 

41  a  Hydri   ^   3.62 

42  ft  Hydri   J  —  3.62 

43  a  Pictoris   3.68 

44  y  Hydri    3.70 

45  v  Argus    3.73 

46  v  Hydras   )  3.76 

47  *  Argus   \  3.79 

48  a  Doradus    3.82 

49  a  Reticuli   3.87 

50  X  Argus    3.93 

510  Argus    3.99 

52  a  Carinas    4.05 

53  a  Mali   )  4.11 

54  t  Hydras   \  4.17 

55/3  Pictoris   4.23 

56  y  Volantis    4.28 

57/3  Volantis    4.51 

58  £  Volantis   4.73 

59  b  Mali    4.81 

60  t  Volantis   4.82 

61  a  Volantis    4.83 

62  a  Velorurn    4.86 

63  b  Velorum    4.89 

64  q  Velorum    4.92 

65  B  Carinas   4.95 

66  P  Puppis   4.95 

67  c  Velorum    4.95 

68  R  Puppis  4.95 

69  N  Carinas   4.95 

70  y  Pictoris   4.95 

71  £  Doradus. 

72  L  2  Puppis. 

73  I  Puppis. 

74  B  A  C.  2642.  ) 

75  BAG.  2670.  j 

76  B  A  C.  2955. 

77  d  Velorum. 

78  e  Velorum. 

79  h  1  Puppis  i  

80  h  2  Puppis  S 

8 1  B  Carina;  )  

82  C  Carinas  $ 

83  1  Pictoris. 

84  8h  38'",  1420  30'. 

85  g  Carinas  }  

86  f  Carinas  5 

87  e  1  Carinas  ) 

88  e  2  Carinas  S 

89  H  Velorum. 

90  p  Pictoris. 

91  X  Doradus. 

92  L  1  Puppis. 

93  BAG.  2332. 

94  B  A  C.  2404. 

95  D  Velorum. 

96  b  1  Carinas  ^ 

97  b  2  Carinas  $ 

Note. — No.  65  is  B  A  C.  2259  ;  No. 
81  is  B  A  C.  2770 ;  both  are  called 
B  Carinas  in  B  A  C,  but  the  latter, 
being  not  far  from  C,  is  preferably  to 
be  so  called. 

4  N 


Groups  observed  in  Sequence  36,  of 
magnitudes  inferior  to  the  foregoing 
— the  Stars  in  each  Group  being 
unarranged. 

Group  1st,  6th  Mag. 


I 

S  Carinas. 

2 

Q  Carinas. 

3 

6  Pictoris. 

4 

V  Puppis. 

5 

Z  Puppis. 

6 

£  Pictoris. 

7 

X  Pictoris. 

8 

f  Velorum. 

9 

g  Velorum. 

10 

B  Velorum. 

11 

BAG.  2336. 

12 

BAG.  2474 

J3 

BAG.  1890 

J4 

B  A  C.  1917 

s~ 

IS 

BAG.  2289 

l- 

16 

BAG.  2328 

s 

17 

BAG.  2375 

18 

BAG.  2963 

BAG.  3045 

i_ 

20 

BAG.  3077 

<>- 

21 

BAG.  2847 

22 

B  A  C.  2733 

s= 

23 

BAG.  3081 

24 

7h  16'",  1410 

40'. 

25 

8     2  133 

5° 

Group  2.    6.7  Mag. 

p  Pictoris. 

n  1  Pictoris.   

//  2  Pictoris. 
G  Puppis. 


Y  1  Puppis.  )  

Y  2  Puppis.  S 
A  Velorum. 
C  Velorum. 

9  h  Velorum. 

10  F  Velorum. 

11  B  A  C.  2325. 

12  B  A  C.  2598  >  _ 

13  BAG.  2645  $ 

14  B  A  C.  2956. 

15  BAG.  3098. 

16  8h  56"',  1310  20'. 


Group  3.     7  Mag.  and  Under. 

1  E  Velorum. 

2  K  2  Puppis. 

3  <j>  Pictoris  (Bode). 

Notes. — The  right  ascensions  and  polar 
distances  of  the  unidentified  stars  are 
for  1800,  as  read  off  from  their  places 
projected  on  Bode's  Chart,  No.  XX. 
— K  2  Puppis,  the  2nd  of  Group  3, 
is  B  A  C.  2767. — <p  Pictoris,  the  3rd 
of  that  Group,  is  Lac.  1751. 


Seciienxe  37. 
January  7,  1838. 

1  a  Centauri    0.34 

2  n  Argus    


322 


SEQUENCES  AND  EQUALITIES  IN  THE 


3  Arcturus    °-45 

4.  Procyon    0.85 

5  a  Eridani   0.93 

6  a  Crucis    1-14 

7  ;3  Centauri   

8  Spica    139 

9  fS  Crucis   .'   1. 57 

10  c  Canis   1.89 

11  8  Canis   2.30 

12  a  Hydrae   2.34 

13  c  Argus    2-44 

14  \  Argus    2.48 

15  I  Argus   2.74 

16  n  Leporis  

17  a  Columbse  


2 1  /3  Columbse  

22  £  Hydra?   

23  a  Hydri    3.72 

24  /3  Hydri    3.72 

2c  9  Eridani   3.73 

26  y  Hydri    3.75 

27  a  Argus    3.79 

28  a  Doradus   }   3.81 

29  a  Pictoris  J  3.81 

30  e  Leporis   3.84 

31a  Reticuli  )   3.87 

32  n  Leporis  )  3.87 


No.  is 

B  AC. 

No.  is  B  AC. 

3.05 

41 

1429 

55  "59 

3.09 

42 

1201 

56  1125 

3-39 

44 

1441 

62    145 1 

46 

1 1 19 

69  1906 

3-69 

47 

H33 

72  $  I04? 

'  t  i°5« 

3.70 

48 

1372 

3.71 

49 

'933 

80  1422 

3-7i 

54 

1044 

38 

39 


33/3  Doradus   

34  ip  Eridani  

35  a  Horologii  

36  >p  Argus   

37  y  Volantis   

Columbse   

Hydri   

40  e  Hydri  

41  v  2  Eridani  

42  g  Eridani  

43  (5  Reticuli  

44  p  Sceptri  

45  11  Eridani  

46  f  2  Eridani   

47  v  2  Eridani  (52  F.). .  . 

48  Y  Eridani  (43  F.)  ... 

49  v  Pictoris  (Bode)    . . . 

50  k  Eridani  

51  y  Doradus   

52  1  Leporis  

53c  Leporis  

54  e  Eridani   

55  h  Eridani   

56  y  Eridani   

57  X  Leporis  

58  y  Reticuli  

59  y  Columbse  

60  a  Coeli  

61  y  1  Coeli   

62  r  Sceptri  

63  oj  Eridani  

64  X  Columbse  

65  8  Horologii  ^ 

66  t  Reticuli  J 


] 


3-  97 
4.07 
4.17 
4.28 

4-  35 
4-39 
443 
4.48 
4.50 

4-53 
4.58 
4.62 
4.65 
4.69 
4.72 
4-75 
4-79 
4.83 
4.87 
4.88 
4.88 
4.89 
4.89 
4.89 
4.90 
4.91 
4.91 
4.92 
4.92 

4-93 
4.94 
4.94 

4-95 
4-95 


67  8  Reticuli   4.96 

68  X  Eridani   4.97 

69  £  2  Columbse   4.97 

70  9  Columbse   4.98 

7 1  i£  Eridani   4.99 

72  5  —  Horologii  }   5.00 

73  B  A  C.  1 103  S  5-°° 

74  r  Hydri    5.01 

75  /(  Columbse   5.01 

76  t  Reticuli   5.01 

77  Z  Hydri    5.02 

78  H  C.  19034.  )  _ 

79  H  C.  19035.  S 

80  v  1  Eridani. 

81  x  Leporis. 

Notes. — Identifications  with  B  A  C.  of 
stars  disagreeing  in  their  letters,  &c. 


No.  81  is  Hist.  Cel.  9354. 

Unarranyed  Groups. 
1st  Group  6  Mag. 


1  /3  Horologii.  ) 

i.  J 


2  y  Horologii. 

3  p  1  Coeli. 

4  ?  Leporis  (8  F.) 

5  v  Columbse. 

6  a  Columbse. 

7  B  A  C.  1773. 

8  B  A  C.  1634. 

9  B  A  C.  1803. 

10  5h  nm,  m°  40'. 

Notes. — No.  1  is  B  A  C.  931. — No.  3 
is  B  A  C.  1559.— No.  5  =  B  A  C. 
1947. 


2nd  Group  6.7  m 

1  (3  Cceu. 

2  jj  1  Coeli. 

3  B  Fornacis. 

4  P  Eridani. 

5  c  Eridani  (51  F.) 

6  v  1  Eridani. 

7  9  Sceptri. 

8  v  Leporis. 

9  z  Sceptri. 

10  s  Sceptri. 

11  H  C.  8951. 

No.=B  AC. 

2  15 1 1 

3  1273 

4  145° 
No.  6  is  H  C 


4  Columbse. 

5  H  C.  10254. 


No.  =B  A  C. 
7  1443 
9  *4*4 
10  1498 

8589. 


Group  3  below  6.7  m. 
A  Fornacis. 


2  q  Sceptri. 
302  Coeli. 


No.  is  B  AC. 
1 
3 
4 


1250 

1559 
166  c 


No.  is  H  C. 
2  8996 


Note  on  Sequence  37  in  general.  A 
very  fine  night,  but  a  great  deal  of 
moonlight.  The  following  stars  of 
Bode's  Chart  xviii.  were  not  seen,  but 
are  not  certainly  above  7  m. 

1  k  Horologii. 

2  M  Eridani. 

3  o  Coeli. 

4  k  Coeli. 

5  v  Horologii. 

6  S  Coeli. 

7  £  Coeli. 
8^2  Coeli. 
9  1  Coeli. 

10  9  Coeli  ? 

11  p  1  Columbse. 

12  p  2  Columbse. 

13  7r  Columbse. 


Sequence  38. 
January  10,  1838. 

1  a  Crucis    i.zi 

2  /3  Crucis    1.57 

3  y  Crucis    1.72 

4  £  Canis   1.75 

5  Regulus    1.80 

6  £  Orionis   1.85 

7  y  Argils    1.9 1 

8  £  Orionis   1.98 

9  /3  Argus   2.02 

10  £  Argus   2.10 

11  y  Orionis   2.23 

12  8  Canis   2.27 

13  8  Argus    2.34 

14  a  Hydrae   2.41 

15  X  Argus    24.8 

16  j3  Canis  )   2.53 

17  y  Leonis   )  2.53 

18  Z  Argus   )_  2.66 

19  /3  Leonis   S  2.66 

20  y  Centauri   )   2.82 

21  k  Argus   >  2.82 

22  n  Canis   2.88 

23  8  Centauri    2.92 

24  1  Argus    2.95 

25  y  Virginis  )   3.00 

26  £  Corvi  5  3.00 

26  £  Corvi  ?  3.00 

27  p.  Argus   J  3.08 

27  fi  Argus   ^   3.08 

28  ir  Argus   5  3-°8 


APPARENT  MAGNITUDES  OF  STARS. 


323 


29  a  Leporis   3.15 

30  9  Argiis    3.22 

31a  Columbae   3.28 

32  a  Muscae   3.40 

33  8  Leporis   3.51 

34.  N  Velorum   3.60 

35  v  Argus   i   3.61 

36  3  Columbae  \~  3.61 

37  d  Crucis    3.67 

38  y  Hydri    3.70 

39  q  Carina   3.73 

40  a  Pictoris  ~l  3.79 

41  0  2  Canis  >=  3.79 

43  o  Doradus   . . .  )  3.79 

44  \  Centauri    3.80 

45  8  Muscae   3.81 

46  m  Argus    3.83 

47  X  Argus    4.05 

48  y  Volantis    4.28 

49  Argus    4.35 

50  B  A  C.  3984    4.43 

51  u  Carinas   4.51 

52  t  Crucis    4.60 

53  p  Carinas   4.61 

54  1  Carinse    4.63 

55  a  Mali    4.64 

56  rr  Centauri    4.66 

57  S  Muscae    4.67 

58  I  Carinae   4.69 

59  y  Muscae  . ,   4.70 

60  O  Crucis  (Bo.)    4.72 

61  y  Chamael   4.73 

62  3  Chamael   4.75 

63  £  Chamael   4.76 

64  8  Chamael    4.73 

65  a  Chamael   4.79 

66  x  Carinae   4.83 

67  £  Crucis    4.87 

Notes.— Moon  full.— No.  60  is  called 
in  the  original  o  Centauri,  but  this  is 
an  evident  mistake  for  O  Crucis. 


Hie  following  Groups  of  unarranged 
Stars  were  also  noted  in  this  Se- 
quence. 

1st  Group  of  Unarranged  Stars. 

1  e  Muscae. 

2  9  Chamaeleontis. 

3  rj  Crucis. 

4  B  A  C.  4189. 

5  B  A  C.  3986. 

6  B  A  C.  4000. 


z?id  Group  of  Unarranged  Stars. 


1  9  1  Crucis. 

2  E  Carinae. 

3  G  Carinae. 
4/12  Chamael. 


5  h  Carinae. 

6  G  Carinae  (neb.) 

7  B  A  C.  3923  + 

Notes. — 9  1  Crucis  is  called  in  the 
MS.  9  2,  from  Bode's  map,  in  which 
the  stars  are  misplaced.  It  is  the 
southern  star.  —  No.  6  is  B  A  C. 
3802. 

3  rd  Group  of  Unarranged  Stars. 

1  9  2  Crucis. 

2  z  1  Carinae. 

3  K  Carinae. 

4  L  Carinae. 

5  fi  1  Chamael. 

6  1  Chamael. 

7  £  2  Muscae. 

8  B  A  C.  401 1. 

9  B  A  C.  3976. 

10  B  A  C.  3958. 

11  B  A  C.  3939. 

12  I2h  14"',  143°  l6'. 

13  II    24,     149  50. 

14  II    23,     I49  15. 

q.th  Group  of  Unarranged  Stars. 

1  z  2  Carinae. 

2  M  Carinae. 

3  £  Chamael. 

4  B  A  C.  3960. 

5  B  A  C.  3806. 

6  B  A  C.  3839. 

7  B  A  C.  4001. 

8  B  A  C.  3624. 

9  B  A  C.  3215  4- 

10  B  A  C.  3264  + 

11  nh  40™,  1550  45'. 


Sequence  39. 
January  13,  1838. 

1  a  Centauri    0.34 

2  t]  Argus    — 

3  Rigel   0.76 

4  Procyon    0.85 

5  a  Eridani   0.93 

6  a  Orionis  ,   1.00 

7  Aldebaran   1.07 

8  (3  Centauri  (low)   1.14 

9  a  Crucis    1.2 1 

10  Pollux   1.5 1 

1 1  (3  Crucis    1.57 

12  y  Crucis    1.72 

13  t  Orionis   1.77 

14  £  Canis   1.89 

15  ?  Orionis  }   1.99 

16  (3  Argus   ]  —  i.99 

17  e  Argiis   2.08 

18  y  Argus    2.16 

19  (3  Tauri  (low)    2.20 

20  0  Canis   2.26 

21  Castor  (low)   2.32 

22  3  Argus   )   2.40 

23  a  Hydrae  $  ~  2.40 

24  y  Geruinorum   2.50 

25  (3  Canis   2.58 


26  'C  Argus    2.66 

27  k  Argus    2.75 

28  n  Canis   2.82 

29  «  Argus   2.90 

30  a  Leporis   3.02 

31a  Columbae   3.09 

32  8  Leporis  )  3.14 

33/3  Hydri  (low)  \  3.19 

34  t  Orionis    3.32 

35  a  Hydri    3.45 

36  v  Argus    3.58 

37  £  Canis   3.69 

38  y  Hydri    3.75 

39  q  Carinae   3.76 

40  o  2  Canis  1   3.77 

41  a  Pictoris  J  3.77 

42  a  Doradus    3.82 

43  a  Reticuli   3.85 

44  w  Argus    3.85 

45  X  Argr's    }—  4  06 

46  cr  Canis   }  4.06 

47  k  2  Canis   ^   4.28 

48  y  Volantis   S  4.28 

49  0  1  Canis   4.43 

50  6  Doradus    4.58 

51  Z  Volantis   4.73 

52  v  2  Canis   4.75 

53  b  Mali   -j  4.81 

54  y  Canis  )  4.81 

55  v  3  Canis. 


56  vi  Canis. 

Note. — Moon  three  days  past  the  full 
superb  sky. 


Sequence  40. 
January  21,  1838. 

1  Sirius    0.10 

2  Canopus    0.22 

3  Arcturus  (low)    0.45 

4  7)  Argus   — 

5  f3  Centauri   )  r.14 

6  a  Crucis   )  1.21 

7  Spica   1.30 

8  3  Crucis   )   1.60 

9  Regulus   5  1.60 

10  y  Argus   }  2.01 

11  3  Argus   )  2. 1 1 

12  £  Argus    2.17 

13  y  Leonis   1  2.36 

14  a  Hydrae  $  2.42 

14  a  Hydrae   }   2.42 

15  9  Centauri   )  2.42 

16  S  Canis   2.50 

17/3  Leonis    2.63 

Note. — Moon  rising  and  flying  clouds 
about. 


324 


SEQUENCES  AND  EQUALITIES  IN  THE 


Sequence  41. 
February  24,  1838. 

1  Jupiter   — 

2  Sirius    0.10 

3  Canopus    0.22 

4  «  Centauri    0.34 

5  i}  Argus    — 

6  Rigel   0.76 

7  a  Cruris    1.14 

8  /3  Centauri    1.2 1 

9  Spica   1.39 

10  j3  Cruris    1.57 

11  y  Crucis    1.72 

12  t  Canis   1.89 

13  y  Argus    2. 1 1 

14  t  Argus   )   2.23 

15  a  Hydrae  )  2.23 

16  S  Canis   2.34 

17  J  Argus    2.44 

18  X  Argus    2.48 

19/3  Canis   2.64 

20  y  Centauri    2.71 

21  X  Argus    2.74 

22  n  Canis   2.84 

23  7r  Argus    2.96 

24  a  Columbae  }   3.06 

25  (i  Argus    S  3-°6 

26  c  Centauri    3.10 

27  (i  Argus  (Sic)   3.10 

28  p  Argus    3.34 

19  v  Argus   )    3.58 

30  v  Hydrae  )  3.58 

30  v  Hydrae  ^  3.58 

3 1  8  Crucis   )  3.60 

32  ?  Argus    3.74 

3302  Canis   3.76 

34  q  Carinas   3.76 

35  u>  Argus   )  3.83 

36  8  Crateris  )  3.86 

37  %  Hydrae    3.95 

38  x  Argus    4  05 

39  (3  Virginis   4.14 

40  X  2  Hydrae  (41  F.)   4-24 

41  7  Volantis    4.28 

42  k  Puppis    4.29 

43  Tp  Argus   I  _  4.35 

44  P  Hydrae  J  4.35 

45  a  Mali   }   4.38 

46  (  Hydras   f  4.38 

47  q  Monocerotis   4.41 

48  Argus  (Fl.)   4.44 

49  q  Velorum    448 

50  v  1  Hydrae    4.52 

516  Canis   4.55 


52  y  Canis  ^  4.58 

53  c  Mali  $  4.62 

54  f  Sextantis  ( 1 5  F.)   )  4.66 

55/3  Crateris  J  4.66 

56  <p  Leonis    4.72 

57  a  Antliae    4.75 

58  xi  Centauri   4.78 

59  b  Mali   4.81 

60  n  Monocerotis  (26  F.) 

61  y  Monocerotis. 

62  9  Crateris. 

63  d  Mali. 

64  H  C.  19034  }  

65  H  C.  19035  J 

66  *  Puppis  (19  Fl.) 

67  t]  Antliae. 

Notes. — Nos.  25  and  27,  sic  in  MS. — 


No.  is  B  A  C. 
40  3473 

47  2825 

48  2562 
54  3458 


No.  is  B  A  C. 
58  4174 

60  2542 

61  2975 
66  2750 


48  has  the  letter  r  attached  by  mistake 
in  Bode. — No.  58  is  called  in  the  MS. 
z  1  Centauri,  but  this  is  an  obvious 
mistake  for  x  1.  The  B  A  C.  calls 
this  star  and  its  near  companion  k  i 
and  k  2  ;  but  this  is  also  a  mistake  for 
x  1  and  x  2.  The  real  k  Argils  is 
B  A  C.  4928,  and  is  there  so  correctly 
lettered  ;  60  is  called  y  Monocerotis 
in  B  A  C. ;  61  is  Flamsteed's  12 
Hydrae.  ;  66  is  Bode's  star  B  in 
Machina  Typographies. 


Sequence  42. 
February  24,  1838. 

1  a  Centauri    0.34 

2  Arcturus   0.45 

3  n  Argus    

4  Saturn  }   

5  Antares  5  *-27 

6  /3  Centauri   J  1.14 

7  a  Crucis   $   1.2 1 

8  Spica   1.39 

9  (3  Crucis    1.57 

10  y  Crucis    1.72 

11  X  Scorpii   1.86 

12  (3  Argus    2.01 

13  y  Argus    2.1 1 

14  a  Trianguli   2.23 

15  6  Scorpii   2.28 

16  a  Hydrae  )  2.29 

17  £  Argus   $  2.30 

18  8  Argus    2.44 

19  X  Argus    2.48 

20  6  Centauri    2.55 

21  y  Centauri   )   2.72 

22  t  Argus  j  2.72 

23  £  Scorpii    2.78 


24  £  Centauri   2.8o 

25  a  Lupi  }  2.83 

26  8  Scorpii  5  2.86 

27  £  Centauri    2.88 

28  y  Corvi  }  2.90 

29  n  Centauri   5  2.91 

30  y  Virginis   2.93 

31  (3  Corvi   2.95 

32  k  Argils    2.98 

336  Argus    3.00 

34  j3  Scorpii  \  3.02 

35  fi  Argus   V  3.04 

36  k  Scorpii   )  3.07 

37  8  Centauri    3.10 

38  /3  Arae    3.12 

39  1  Centauri  1   3.16 

40  £  Corvi  j  3.16 

41  j3  Lupi   3.22 

42  tt  Scorpii   3.30 

43  a  Muscae  "\  3.35 

44  7  Lupi   f  3.36 

45  11  1  Scorpii  f  3.37 

46  c  Corvi   J  3.40 

47  a  Arae    3-4° 

48  v  Scorpii   3.42 

49  8  Crucis    )   3.4.6 

50  r  Scorpii  5  3.46 

51  y  Trianguli   3.48 

52  N  Velorum   3.50 

53  y  Hydrae   3.52 

54  j3  Trianguli   3.55 

55  i)  Argus    3.58 

56  t  Scorpii   1  3.61 

57  X  Centauri   5  3  64 

57  X  Centauri   j  3.64 

58  (3  Muscae  5  >-66 

58  j3  Muscae  )  3.66 

59  k  Centauri    J  3.67 

60  y  Tubi   3.70 

61  a  Circini   3.73 

62  q  Carinae   3.76 

63  a  Scorpii   3.77 

64  5T  Hydrae   3.79 

65  n  Scorpii   3.80 

66  y  Arae    3.82 

67  <i)  Argus    3.83 

68  8  Crateris   3.85 

69  v  Centauri  "j  3.88 

70  fi  Centauri   f  3.91 

71  1  Lupi  J  3.95 

72  £  Lupi   3.99 

72  8  Lupi   4.03 

73  Z  Lupi   4.07 

74  £  2  Scorpii    4.34 

75  <p  Centauri    4.62 

76  n  Virginis. 

Note. — No.  60  is  B  A  C.  6018,  marked 
as  4  m,  but  having  no  letter  attached. 


Sequence  43. 
February  25,  1838. 

1  Sirius    0.10 

2  Canopus    0.22 

3  a  Centauri    0.34 


APPARENT  MAGNITUDES  OF  STARS 


4  r)  Argu3    - 

5  Rigel   0  76 

6  Procyon    0.85 

7  a  Orionis   0.10 

8  a  Crucis    1.14 

9  /3  Centauri  (low)   1-45 

10  Pollux   1.5 1 

11  fi  Crucis   )  i-S7 

12  Regulus   S  '-62 

13  y  Crucis    1.72 

14  y  Orionis  ^   1.90 

15  £  Orionis  j  1.90 

16  t  Canis   1.94 

17  £  Orionis   1.97 

18  y  Argus   )  2.01 

19  /3  Argus   $  2. 1 1 

20  £  Argus   2.17 

21  a  Trianguli   2.23 

22  a  Hydrae    }  2.30 

23  0  Canis  J  2.34 

24  y  Leonis    2.42 

25  c  Argus   2.44 

26  \  Argus    2.48 

27  6  Orionis   "\  2.62 

28  y  Centauri   >  =  2.62 

29  y  Geminorum  )  2.62 

30  1  Argus   2.73 

31  £  Centauri  (sic)    2.73 

32  £  Argus    2.74 

33  1}  Canis   2.83 

34  £  Centauri  (sic)    2.84 

35  7r  Argus    2.89 

36  /3  Corvi   2.93 

37  y  Corvi   2.96 

38  c  Centauri    3.00 

39  k  Argus    3.04 

40  fi  Argus   >       3. 11 

41  p  Argus  S  3-n 

42  S  Corvi  2       3.1 1 

43  £  Centauri   J       3.1 1 

44  £  Hydrse    3.21 

45  9  Argus   3.31 

46  f3  Trianguli  >   3.40 

47  £  Corvi  J  3.40 

48  y  Trianguli   3.52 

49  r  Argus    3.55 

50  y  Hydrse   3.57 

51  v  Argus    3.58 

52  (3  Muscae   3.60 

53  c  Crucis  )   3.67 

54  v  Hydrse  \  3.67 

55  v  Argus    3.72 

56  a  Pictoris   3.78 

57  cr  Argus    3.79 

58  a  Circini   3.92 

59  x  Argus    4.05 

60  Argus   )   4.18 

61  \  2  Hydrae   J[  4.18 

62  y  Volantis    4.28 

63  t"  Muscae    4.40 

64  a  Chamaeleontis    4.50 


65  S  Chamaeleontis    4.55 

66  a  Mali   4.60 

67  S  Volantis   4  64 

68  e  Crucis   -\  4.64 

69  y  Muscae    y  =  4.64 

70  0  2  Apodis  J  4.64 

7i/3  Chamael  4.72 

72  b  Mali   4.81 

73  9  Chamael   4.91 

74  c  Mali. 

75  y  Chamael. 

76  £  Trianguli. 

77  £  Chamael. 

Note.  —  Nos.   31  and  34  £  Centauri, 
twice  entered  in  the  original  MS. 


Sequence  44. 
March  28,  1838. 
At  Sea.    Crossing  the  Line. 

1  Sirius    o.  10 

2  Canopus    0.22 

3  a  Centauri    0.34 

4  Arcturus    0.45 

5  t)  Argus    — 

6  Rigel   0.76 

7  Procyon    0.85 

8  a  Orionis   1.00 

9  Aldebaran    1.07 

10  a  Crucis    1.2 1 

11  Spica   1. 41 

12  (3  Crucis   \  1.57 

13  Regulus   $  1.62 

14  y  Crucis   )  1.72 

15  £  Canis   S  189 

16  a  Ursse  )  1.93 

17  £  Ursse  )  1.97 

i8/3  Argiis   )  2.01 

19  a  Hydrse  )  2.17 

19  a  Hydrae  }   2.17 

20  £  Argiis  $  2.17 

20  £  Argus  >  2.17 

21  y  Argiis   J  2.17 

22  y  Leonis. 

23  i)  Ursse. 

Notes. — Nos.  12,  13  /3  low,  Regulus 
very  high;  14,  15  y  low,  £  high ;  18, 
19  /3  20°  high,  a  in  zenith. 


The  following  short  sequences  and  equal- 
izations were  also  made  for  the  express 
purpose  of  connecting  the  scales  of 
northern  and  southern  magnitudes. 


I. 


a  Hydrae. 

<5  Canis.  >  

Z  Ursse.  S  ~ 


II.  £  Argus. 
f3  Leonis. 
S  Argiis. 


III.  j3  Leonis.    )  . 
y  Centauri.  J  ' 


325 

IV.   t  Argus.  I 
y  Ursse.  S 


V.     y  Ursae  7  7  2  Argus. 


VI.  n  Argus. 

e  Bootis.  } 
c  Centauri.  S 


VII.  Cor  Caroli.  i 
9  Argus.  J 


Sequence  45. 
April  14,  1838. 
At  Sea.    Lat.  170  N. 


1  Jupiter   — 

2  Sirius    0.10 

3  Canopus    c.22 

4  Arcturus   0.45 

5  Capella   0.56 

6  Procyon   )  0.76 

7  Rigel  )  0.85 

8  a  Orionis   i-oo 

9  7)  Argus    — 

10  Aldebaran   1-07 

11  Pollux    1.51 

12  Regulus   1-57 

13/3  Crucis    1.62 

14  £  Ursae   i-79 

15  a  Ursse   1.96 

16  r)  Ursse   2.13 

17  a  Hydrae   2.30 

18  y  Leonis    2.42 

19  £  Ursae   2.45 

20  /3  Tauri   2.48 

21  j3  Aurigae   2.52 

22  (3  Leonis   ^   2.55 

23  9  Centauri   )  2.55 

24  y  Ursse   2.62 


25  £  Bootis    2-7° 

26  /3  Ursae   2  78 

27  a  Coronae   2.85 

28  (3  Corvi   2.93 

29  6  Leonis    2.96 

30  (3  Librae    2.99 

31  y  Corvi   3.02 

32  a  Librae    3.05 

33  1}  Bootis    3  08 

34  e  Virginis   3. 11 

35  a  Serpentis    3- 14 

36  y  Virginis   3.17 

37  Cor  Caroli    3  20 

38  t  Centauri   3.22 

39  S  Corvi   3.25 

40  e  Corvi   3.31 


41  i|/  Ursse   3.33 

42  fx.  Ursae   3.35 


43  r  Lyncis    3.38 

44  y  Bootis    3.40 

45  £  Leonis    3.43 

46  v  Hydrae  ™  3.46 

47  y  Hydrae   3-5° 


326 


SEQUENCES  AND  EQUALITIES  IN  THE  APPARENT  MAGNITUDE  OF  STARS. 


48  £  Hydrae   3.55 

49  8  Ursae   3.61 

50  ?  Virginis  }   3.70 

51  8  Bootis   $  3.70 

52  ft  Bootis    3.80 

53  8  Virginis   3.90 

54  ft  Virginis   4. 14 

55  K  Ursae   4.20 

56  \  Bootis    4.26 

57  t)  Virginis   4.31 


Notes. — 6,  7  Procyon  at  750  altitude, 
Rigel  at  300;  13,  /}  Crucis  only  120 
high  when  observed ;  22,  23  ft  in 
Zenith,  6  at  350  alt.;  44,  called  X 
Bootis  in  the  MS.,  but  y  was  no  doubt 
the  star  observed. 


The  following  triad  is  also  recorded  on 
this  evening. 

1  ft  Ursae  Minoris. 

2  y  Crucis. 

3  a  Polaris. 

ft  Urs.  Min.  at  300  alt.,  the  others  at 
1 50  each. 


Sequence  46. 
April  15,  1838. 
At  Sea.    Lat.  180  N. 
1  1  Ursa?. 


2  Castor. 

3  a  Ursae. 

4  t)  Ursae. 


5  y  Leonis    2.42 

6  ft  Ursae  Min  )  _  2.46 

7  a  Hydrse  J  2.46 

8  y  Geminorum   2.50 

9  £  Ursae   2.54 

10  a  Polaris   2.59 

1 1  a  Coronas   2.63 

12  ft  Leonis    2.68 

13  t  Bootis    2.72 

14  ft  Ursae  )  2.76 

15  y  Ursae                                j  2.80 

16  S  Leonis    2.85 


17  y  Corvi  )  2.90 

18  ft  Corvi  )  2.93 


19  y  Virginis  1  2.97 

20  Cor  Caroli   5  3.25 

20  Cor  Caroli   }   3.25 

21  8  Corvi   5  3.25 

22  e  Corvi   3.31 


23  y  Bootis    3.36 

24  ^  Ursae   3.40 

25  y  Hydrae  )  _  3.45 

26  £  Hydrae   J  3.45 

27  S  Ursae   3.58 


28  £  Virginis   3.70 


29  6  Leonis    3.80 

30  8  Virginis   3.90 

31  ft  Virginis   4.14 

32  t  Leonis    4.22 

33  ri  Virginis   4.3 1 


34  a  Crateris. 

35  v  Leonis. 

Notes.— 6,  7,  ft  230  high  and  6o°;  10, 
Polaris  180;  25,  26,  y  300,  I  6o° 
high. 


327 


Step  I. —  Of  the  formation  of  corrected  Sequences  by  the  collation  of  several  observed  Sequences,  and 
of  the  elimination  of  discordant  and  contradictory  observations. 

(226)  If  observations  of  this  nature  could  be  made  with  perfect  exactness,  all  sequences  in 
which  the  same  stars  occur  should  present  them  in  the  same  order  of  succession,  in  so  far 
as  it  may  not  have  been  disturbed  by  a  real  variability  in  the  stars  observed.  But  as  this  is  very 
far  indeed  from  being  the  case,  owing  to  the  many  disturbing  influences,  and  the  slight 
differences  of  magnitude  between  particular  stars  which  have  to  be  discriminated,  it  is  necessary 
to  fix  upon  some  criterion  by  which  the  most  probable  order  of  arrangement  can  be  discovered 
among  a  number  of  discordant  ones.  Such  a  criterion  is  supplied  by  an  enumeration  of  cases, 
in  which  either  of  two  stars  (A  and  B),  whose  order  is  to  be  settled,  has  been  declared  brighter, 
and  in  which  less  bright  than  the  other — allowing  the  greater  number  to  preponderate.  In 
case  of  equality  of  numbers,  the  equality  of  the  stars  must  be  admitted  at  least  provisionally, 
and  so  far  as  direct  comparisons  are  concerned.  But  it  is  a  case  of  very  common  occurrence, 
that  in  arranging  the  order  of  three  stars,  A,  B,  C,  although  the  direct  comparisons  between 
B  and  C  leave  it  doubtful  which  of  these  two  is  the  brighter,  yet  A  may  be  found  on  a  revision 
of  all  the  sequences  to  be  decidedly  superior  to  C  and  not  to  B,  having  been  compared  on 
different  occasions  with  both  these  stars,  but  not  both  on  the  same  night.  In  such  a  case  we 
have  ground  for  placing  B  above  C,  while  otherwise  it  would  have  been  left  undecided  which 
should  be  considered  the  brig-liter. 

(227)  To  determine  therefore  the  order  in  which  any  two  stars  should  be  placed  in  a 
general  sequence  (could  such  be  obtained)  of  all  the  visible  stars,  or  their  order  of  precedence 
with  respect  to  each  other,  all  that  is  necessary  is  to  count  the  number  of  times  that  one  of 
them  (A)  has  been  estimated  as  superior,  and  as  inferior  to  the  other  (B).  In  such  enumerations, 
an  observed  equality  must  be  considered  as  counting  both  ways.  If  the  superiorities  on  the  whole 
preponderate,  A  must  rank  in  precedence  of  B ;  if  the  contrary,  B  must  take  the  higher  rank  : 
if  neither,  they  must  be  set  down  temporarily  as  equal,  or  rather  as  doubtful,  leaving  the 
decision  to  implications  arising  from  the  comparisons  of  both  with  other  stars.  If  there  be  no 
direct  comparison  recorded  between  A  and  B,  their  order  will,  of  course,  come  to  be  deter- 
mined solely  by  such  implications.  If,  indeed,  they  have  often  been  compared,  an  equality 
in  the  numbers  of  superiorities  and  inferiorities  (especially  if  occasionally  declared  equal),  will 
afford  a  presumption  of  actual  equality  not  to  be  disturbed  by  such  implications.  And  on  the 
other  hand,  if  seldom  directly  compared  (once  or  twice  for  instance)  strong  implications 
arising  from  much  more  frequent  comparisons  with  other  stars,  may  suffice  to  reverse  our 
conclusion  respecting  their  order,  drawn  from  such  direct  comparison. 

(228)  It  might  appear  then  that  so  much  is  left  to  judgment  in  such  cases,  as  to  induce 
uncertainty  in  the  final  result.  But,  in  fact,  it  is  only  in  the  case  of  stars  which  really  are 
nearly  equal  that  doubts  on  such  points  ever  arise.  Push  observation  and  reasoning  to  what 
extent  we  will,  there  will  always  be  shades  of  difference  too  slight  for  certain  discrimination ; 
and  practically  speaking,  I  am  disposed  (from  my  experience  in  these  reductions)  to  consider 
a  misarrangement  to  the  extent  of  a  tenth  of  a  magnitude  in  one  of  our  corrected  sequences, 
arising  from  such  causes  of  uncertainty,  as  a  very  unlikely  occurrence. 

(229)  It  will  occasionally  happen,  however,  that  real  contradictions,  arising  from 
undoubted  error  of  observation,  will  occur  —  and  it  is  the  spirit  of  this  method  to  bring 


328 


OF  THE  FORMATION 


clearly  into  evidence  such  irreconcilable  discordances,  while  minor  errors  eliminate  and 
destroy  each  other  by  a  system  of  impartial  combination.  Thus,  for  instance,  it  will  sometimes 
happen  that  a  star  D  is  placed,  in  consequence  of  direct  comparisons,  after  several  others  as 
ABC,  making  the  order  A  B  C  D,  while  in  consequence  of  indirect  implications  of  the  nature 
above  alluded  to,  the  order  D  A  B  C  would  arise.  In  this  case  there  is  a  contradiction ;  and  if 
on  examination  of  the  sequences  the  faulty  observation  cannot  be  detected  (which  it  very  often 
may),  the  star  D  must  be  rejected  from  our  corrected  sequence ;  or  it  may  happen  that  by  the 
sacrifice  of  this  single  observation  all  discordances  are  reconciled.  Thus,  in  sequences  14  and 
42,  the  star  k  Centauri  is  placed  below  v  Argus  and  N  Velorum,  while  in  sequence  6  it  is  placed 
above  them.  The  preponderance  of  direct  comparisons  gives  v  N  k  for  the  order  of  pre- 
cedence. But,  on  the  other  hand,  in  sequence  6,  k  is  placed  also  above  t  Argus,  which  star, 
from  the  accumulated  evidence  of  sequences  6,  14,  35,  38  and  43,  is  superior  in  brightness  to 
both  the  other  stars  v  and  N,  whence  the  order  ktdN  would  result.  Referring,  however,  to 
the  original  sequences,  we  find  that  the  order  k  t  is  the  result  of  the  single  comparison  in 
sequence  6,  and  are  therefore  left  at  no  loss  to  conclude  that  in  that  sequence  k  has  been 
misplaced — and  this  observation  being  given  up,  the  order  v  N  k  remains  unimpeached.  It 
may  serve  to  show  how  small  are  the  shades  of  difference  which  are  thus  brought  into  conflict 
if  we  refer  to  the  numerical  evaluation  of  the  magnitudes  of  the  stars  in  question  in  the 
subjoined  catalogue  of  stars  C,  arranged  in  alphabetical  order,  where  it  will  be  seen  that  the 
actual  magnitudes  are  as  follows, — viz.  :  r  Argus  3.50;  v  Argus  3.53;  N  Velorum  3.60; 
k  Centauri  3.60, — the  extreme  range  of  discordance  being  no  more  than  one-tenth  of  a 
magnitude. 

(230)  The  process  practically  adopted  for  the  application  of  this  principle  to  the  con- 
struction of  corrected  sequences,  (by  which  I  mean  sequences  cleared  of  conflicting  errors),  and 
adopted  for  amalgamation  into  normal  sequences,  may  be  thus  explained.  Let  any  extensive 
observed  sequence  be  fixed  upon  embracing  a  considerable  amplitude  in  Right  Ascension, 
and  of  which  a  great  many  stars  occur  frequently  in  other  sequences, — as  for  example, 
sequence  6.  Now,  in  the  first  place,  it  is  clear  that,  although  there  may  be  room  for  doubt 
whether  particular  stars  really  stand  in  that  sequence  in  the  exact  order  in  which  they  ought 
to  have  been  placed,  there  can  be  no  doubt  whatever  that  if  10  or  12  stars  of  the  sequence, 
following  in  succession,  be  taken,  the  first  in  order  of  occurrence  among  them  is  really  superior 
in  brightness  to  the  last;  and  that  among  all  the  12  taken  en  masse,  a  general  downward 
tendency  subsists,  though,  possibly,  here  and  there  interrupted  by  error  of  observation  in 
particular  instances.  Take,  therefore,  a  certain  moderate  and  easily  manageable  number 
(say  12#)  of  stars,  the  first  in  order  on  the  sequence,  and  for  convenience  of  inspection  and 
brevity  of  writing,  denote  them  by  letters  of  the  Roman  alphabet,  thusf 

A  =  Sirius.  E  =  Arcturus.  I  =  Antares. 

B  =  Canopus.  F  =  (3  Centauri.  K  =  Regulus. 

C  =  a  Centauri.  G  =  a  Crucis.  L  =  (3  Cruris. 

D  =  a  Eridani.  H  =  Spica.  M  =  y  Crucis. 

*  I  find  that  the  use  of  a  full  alphabet,  or  twenty-six  at  a  time,  is  more  than  can  be  easily  managed  without 
incurring  risk  of  error:  as  the  names  of  so  many  stars  cannot  be  carried  in  the  memory  securely  while  looking 
down  the  observed  sequences. 

t  »;  Argus  is  omitted,  being  known  to  be  variable. 


OF  CORRECTED  SEQUENCES. 


329 


Each  observed  sequence  is  then  to  be  consulted,  and  in  every  one  in  which  two  or  more 
individuals  of  this  list  occur,  they  are  to  be  extracted  and  set  down  (designated  by  their 
assumed  letters)  in  order,  omitting  all  the  rest,  in  manner  following  : — 


Seq. 

Order. 

Seq. 

•  Order. 

Seq. 

Order. 

4 

B  C  E  F  G  H  I  L 

21 

A  B  D 

37 

C  E  D  G  F  H  L 

5 

ABCFHGLM 

22 

BCEIGFHLM 

38 

G  L  M  K 

6 

ABCDEFGHIKLM 

26 

E  I  H 

39 

C  D  F  G  L  M 

7 

F  G  H  K  L  M 

30 

B  D 

40 

ABEFGHLK 

13 

ABCEFGHLM 

32 

A  B  D 

41 

ABCGFHLM 

15 

C  D  F  D  I 

33 

ABCDFGLM 

42 

C  E  I  F  G 

16 

A  B  C  D  F  I 

34 

ABCDFGHLKM 

43 

ABCGFLKM 

18 

C  D  I  L 

35 

D  (F  =  G)  L 

44 

ABCEGHLKM 

19 

D  G 

36 

A  B  C  D  G  L  M 

45 

A  B  E  K  L 

(231)  The  enumeration  of  relative  superiorities  and  inferiorities  is  most  compendiously 
and  correctly  executed  by  constructing  a  diagram  in  manner  here  represented : 

MLKI         H  GFEDCB 


330 


OF  THE  FORMATION 


To  fill  in  this  diagram,  we  begin  with  the  first  sequence  set  down,  viz.,  seq.  4 ;  and  since 
B  is  there  declared  to  be  superior  to  C,  E,  F,  G,  H,  I  and  L,  we  place  a  dot  above  the  hori- 
zontal line  marked  B  in  each  of  the  vertical  columns  of  cells  headed  with  the  other  letters 
C,  E,  &c.  in  question.  Again,  in  the  same  sequence,  C  being  declared  superior  to  EFG  H  I  L> 
a  dot  is  placed  over  the  horizontal  C  in  the  respective  columns  so  indicated,  and  so  on 
throughout  the  whole  sequence.  And  the  same  process  is  to  be  carried  out  through  all  the 
other  sequences.  If  in  any  case  (as  in  seq.  22,  in  the  case  of  F  and  I),  a  letter  (I)  is  declared 
superior  to  another,  F,  which  precedes  it  in  the  alphabet,  the  dot,  instead  of  being  placed  above 
the  horizontal  line  I,  in  the  vertical  column  F  (for  which  there  is  no  cell),  must  be  placed 
below  the  horizontal  line  F,  in  the  vertical  column  I.  And  to  avoid  mistakes  in  this  (which 
otherwise  are  exceedingly  apt  to  arise),  the  better  way  is  to  pursue  the  horizontal  line  I,  from 
left  to  right,  as  if  in  search  of  the  column  F,  and  on  arriving  at  the  letter  I  at  its  right  hand 
extremity,  thence  to  direct  the  eye  upwards  along  the  column  I  till  it  encounters  the  horizontal 
line  F,  under  which  the  dot  is  to  be  deposited.  These  directions  may  appear  trivial  and 
mechanical,  but  nothing  is  really  trivial  by  which  in  long  and  tedious  processes  attention  is 
relieved,  and  mistakes  avoided. 

(232)  When  all  the  sequences  are  so  gone  through,  the  next  step  is  to  determine  from  the 
comparative  numbers  of  dots  above  and  below  each  line,  the  order  of  succession  of  the 
letters :  which  is  best  done,  systematically,  by  the  con- 
struction of  another  diagram,  as  here  shown.  A  vertical 
column  and  horizontal  lines  across  it  being  ruled,  all  the 
letters  in  their  order,  down  to  the  last  but  one,  are  to  be 
placed  in  the  cells  of  the  column,  and  each  subsequent 
letter,  as  compared  with  any  one  preceding  it  in  the 
alphabet,  is  to  be  placed  on  the  right  hand  in  the  appro- 
priate horizontal  line  if  the  preceding  letter  be  found  to 
have  more  dots  indicating  superiority  than  the  con- 
trary :  if  fewer,  on  the  left  (as  in  the  case  of  the  letters 
L  K  M  in  our  example).  If  the  numbers  be  equal,  the 
precedence  must  be  left  in  doubt  (as  in  the  case  D  —  E, 
indicated  by  the  sign  — )  if  there  be  only  one  dot  on  each 
part.  But  if  two  or  more  (as  is  the  case  with  H  as  com- 
pared with  I),  the  stars  may  be  declared  equal  (H  =  I), 
provided  no  implications  of  the  nature  already  explained 

arise  to  indicate  a  superiority  in  either. 

(233)  This  done,  the  order  of  precedence  results,  as  a  matter  of  course,  with  more  or 
less  consideration,  as  the  case  may  require.    In  the  example  before  us,  it  is 

ABCD-EFGH=ILKM 
or,  restoring  the  Names  of  the  Stars — Sirius,  Canopus,  a  Centauri,  {Arcturus  —  a  Eridani},  /3  Centauri,  a  Cruets, 
{Spica     Antares}  (3  Cruris,  Regulus,  y  Cruris. 

(234)  If  contradictory  arrangements  result  by  implication,  as  above  explained,  a  minute 
examination  of  the  numbers  and  of  the  evidence  generally  must  be  gone  into,  which  will 
almost  invariably  lead  either  to  the  detection  of  some  evidently  faulty  comparison,  or  to  the 


A 

BCDEFGHIKLM 

B 

CDEFGHIKLM 

C 

DEFGHIKLM 

D 

FGHIKLM  (D-E) 

E 

F  G  H  I  K  L  M 

F 

G  H I K  LM 

G 

HIKLM 

H 

KLM                       11  =  1 

I 

KLM 

L 

K 

M 

L 

M 

OF  CORRECTED  SEQUENCES. 


331 


conclusion  that  the  stars  concerned  are  really  so  nearly  equal,  that  it  is  of  little  consequence 
which  is  placed  first.  Not  unfrequently,  however,  it  will  happen  that  a  star  must  he  thrown 
out  of -the  sequence  altogether,  as  not  determinahle  from  the  observations  with  that  degree  of 
precision  which  is  required  for  the  object  in  view.  Still,  in  such  a  case,  the  limits  between 
which  its  place  falls  should  be  noted  as  affording  an  approximate  value  of  its  magnitude  when 
numerical  values  come  to  be  assigned.  Or  it  may  find  a  definite  place  in  some  other  corrected 
sequence. 

(235)  We  now  proceed  to  the  next  stars  in  succession  of  our  original  sequence  (No.  6). 
And  as  in  this  case  the  lower  star  (y  Crucis)  has  preserved  its  place  at  the  bottom  of  the  first 
sub-sequence  (so  we  may  term  these  temporary  groups),  and  as  there  can  be  no  doubt  of  the 
superiority  of  Regulus  to  j3  and  y  Argus,  it  will  suffice  to  provide  for  the  possibility  of  a 
change  of  order  at  the  junction  of  the  sub-sequence,  if  we  make  the  last  star  of  the  first 
sub-sequence  the  first  of  the  second.  Denoting,  then,  the  stars  of  this  sub-sequence  by 
letters,  thus : — 

A  =  y  Crucis.  E  =  X  Scorpii.  1  =  6  Scorpii. 

B  =  /3  Argus.  F  =  a  Trianguli.  K  =  5  Argus. 

C  =  y  Argus.  G  =  y  Centauri.  L  =  0  Centauri. 

D  =  e  Argus.  H  =  \  Argus.  M  =  t  Argus. 

collecting,  as  before,  the  sequences  in  which  these  stars  occur  into  one  abbreviated  synoptic 
view,  by  leaving  out  all  intermediate  stars,  and  following  out,  mutatis  mutandis,  the  subsequent 
steps  of  our  process,  we  arrive  at  the  following  order. 

ABCDFIKHLGM 

that  is  to  say,  y  Crucis,  (3  Argus,  y  Argus,  t  Argus,  a  Trianguli,  9  Scorpii,  6  Argils,  A  Argus,  6  Centauri,  y  Cen- 
tauri, i  Argus. 

The  star  E  or  A  Scorpii  is  rejected  from  this,  and  left  to  find  its  definite  place  in  another 
corrected  sequence  (its  place  being,  however,  certainly  between  y  Crucis  and  a  Trianguli), 
by  reason  of  the  doubtful  comparisons  B  —  E,  C  —  E,  and  D  — •  E.  Between  D  and  I  also  the 
direct  comparisons  leave  a  doubt;  but  as  there  is  no  such  doubt  with  respect  to  the  pre- 
cedences DF,  FI,  and  I  K,  the  place  of  I  is  sufficiently  ascertained. 

(236)  The  star  A  (y  Crucis),  the  last  star  of  the  first  sub-sequence  being  left  by  this 
process  at  the  head  of  the  second,  it  is  not  necessary  to  re-examine  (by  a  similar  process 
instituted  with  four  or  five  letters)  the  order  of  the  stars  Regulus,  y  Crucis,  /3  Argus,  and 
y  Argus,  which  in  the  contrary  event  would  have  been  requisite  before  the  two  sub-sequences 
could  be  connected  into  one.  We  may,  therefore,  proceed  to  form  a  third  sub-sequence 
headed  by  t  Argus,  the  last  star  of  the  second.  This  treated  in  the  same  systematic  manner, 
affords  for  the  order  of  the  third  sub-sequence,  as  follows  : — 

i  Argus,  Z  Argus,  {a  Lupi  =  e  Centauri},  £  Centauri,  n  Centauri,  3  Centauri,  k  Argus,  /3  Hydri,  fi  Argus,  j3  Lupi, 
i  Centauri. 

Proceeding  exactly  in  the  same  manner,  we  arrive  at  a  fourth  sub-sequence  (from  which 
k  Centauri,  which  occurs  in  the  original  sequence  is  rejected,  its  place,  however,  being  certainly 
between  y  Trianguli  and  /3  Muscce)  viz., — i  Centauri,  6  Argus,  a  Muscce,  y  Lupi,  /3  Trianguli, 


332 


OF  THE  FORMATION 


y  Trianguli,  r  Ar(/us,  v  Argus,  8  Crucis,  N  Velorum,  (3  Muscat.  A  fifth  sub-sequence  requires  the 
rejection  of  A  Centauri,  and  q  Carinse,  and  a  sixth,  of  (  Lupi  and  y  Volantis,  and  in  all,  the 
overlapping  of  the  sub-sequences  remains  undisturbed.  Assembling  then  the  whole,  our  final  or 
corrected  sequence  results  as  follows  : — 


Sirius. 

9  Scorpii. 

(  Centauri. 

p  Carina?. 

Canopus. 

8  Argus. 

9  Argus. 

a  Reticuli  ^ 
H  Centauri  J 

a  Centauri. 

X  Argiis. 

a  Musca?. 

Arcturus  i 

9  Centauri. 

y  Lupi. 

v  Centauri. 

a  Eridani.  ) 

y  Centauri. 

(3  Trianguli. 

X  Argus. 

{3  Centauri. 

i  Argus. 

y  Trianguli. 

1  Carina?. 

a  Crucis. 

£  Argus. 

t  Argus. 

i  Lupi. 

Antares.  £ 

a  Lupi.  l 

v  Argus. 

<j>  Argus. 

Spica.  S 

£  Centauri.  > 

8  Crucis. 

(3  Reticuli. 

j3  Crucis. 

?  Centauri. 

N  Velorum. 

e  Crucis. 

Regulus. 

i]  Centauri. 

S3  Muscae. 

<p  Centauri. 

y  Crucis. 

8  Centauri. 

a  Circini. 

a  Carina?. 

13  Argus. 

k  Argus. 

y  Hydri. 

8  Musca?. 

y  Argus. 

(3  Hydri. 

a  Doradus. 

B  A  C.  3984. 

{  Argils. 

fi  Argus. 

a  Pictoris. 

a  Trianguli. 

f3  Lupi. 

to  Argus. 

(237)  In  general,  however,  as  we  get  lower  down  in  a  sequence,  it  becomes  necessary  to 
pay  continually  greater  attention  to  the  overlapping  of  our  several  consecutive  groups  ;  and  in 
order  to  be  quite  secure,  it  is  advisable  to  repeat  the  whole  process  with  new  groups,  each 
consisting  of  the  lower  half  of  one  of  the  old  ones,  and  the  upper  half  of  that  following  it. 
Moreover,  when  we  come  down  to  stars  of  the  4th  and  lower  magnitudes,  it  becomes  necessary 
to  embrace  a  greater  number  of  individuals  16  or  even  20  in  a  group,  to  give  any  misplaced 
star  a  full  and  fair  opportunity  of  settling  ultimately  at  its  proper  level  in  the  corrected 
series. 

(238)  Such  is  the  treatment  which  each  observed  sequence  has  to  undergo  to  convert  it 
into  a  corrected  sequence,  capable  of  being  employed  in  the  subsequent  part  of  our  process. 
Each  of  the  46  observed  sequences  has  been  so  treated.  The  process,  though  no  doubt  tedious 
and  laborious,  is  one  of  no  difficulty ;  and  once  gone  through,  facilitates,  in  a  remarkable 
degree,  every  succeeding  step  of  the  work. 


Step  II. —  Of  the  Consilience  of  Sequences,  or  the  Formation  of  Normal  Sequences,  by  the  partial  or 
entire  combination  of  several  corrected  ones ;  and  of  the  Assignment  of  a  Series  of  Provisional 
Magnitudes,  to  serve  as  a  basis  for  those  to  be  finally  adopted. 

(239)  Suppose  that  in  any  one  sequence  the  stars  A,  B,  C,  D  were  found,  arranged  in  that 
order — that  in  another  were  found  D,  E,  F,  G,  so  arranged — in  a  third,  an  arrangement  such 
as  B  D  G  H,  and  so  on.  Then  it  is  evident  that,  if  no  contradictory  arrangements  be  found 
to  occur  in  any  of  the  other  sequences,  ABCDEFGH  will  be  the  true  order  to  be  finally 
adopted. 


OF  NORMAL  SEQUENCES. 


333 


(240)  From  the  mode  in  which  the  normal  sequences  are  deduced,  as  above  explained,  it 
is  only  in  comparatively  rare  cases  that  contradictory  arrangements  can  occur,  since  each  is 
formed  on  the  total  evidence  of  all  the  observed  sequences,  synoptically  brought  under  review. 
Whenever  they  do  so,  it  can  only  arise  from  different  implications,  causing  diversity  of  judg- 
ment in  the  several  cases,  or  from  a  conflict  of  the  result  of  implications  in  one  case  with  that 
of  direct  comparison  in  another.  In  such  cases,  the  evidence  on  both  sides  must  be  revised, 
and  if  found  to  be  irreconcilable,  or  to  give  no  assured  ground  of  preference,  the  star 
which  causes  the  difficulty  must  be  rejected  from  the  normal  sequence  we  are  constructing. 

(241)  As  an  example,  let  us  take  the  stars  usually  considered  as  of  the  first  magnitude, 
which  occur  in  our  46  sequences,  assigning  to  each  of  them  a  temporary  letter,  as  follows :  — 


A.  Sirius. 

B.  Canopus. 

C.  a  Centauri. 

D.  Arcturus. 

E.  Capella. 

F.  Lyra. 


G.  Rigel. 

H.  Procyon. 

I.  a  Eridani. 
K.  a  Orionis. 
L.  Aldebaran. 
M.  /3  Centauri. 


N.  a  Crucis. 
O.  Antares. 
P.  a  Aquilae. 
Q.  Spica. 
R.  Fomalhaut. 
S.  Pollux. 


T.  (3  Crucis. 
U.  Regulus. 
V.  a  Gruis. 
W.  a  Cygni. 


The  corrected  sequences  in  which  any  two  or  more  of  these  stars  occur,  and  their  arrange- 
ments in  those  sequences  respectively  are  as  below. 


Seq. 

Order. 

Seq. 

Order. 

Seq. 

Order. 

3 

I  V 

20 

G  K 

36 

ABCGHIKLNST 

4 

BCDMNOQT 

21 

A  B  G  I  K  R  V 

37 

ADHIMNQT 

5 

ABCMNT 

22 

BCDMNOQT 

38 

N  T 

6 

ABCDIMNOQTU 

26 

D  O  Q 

39 

CGHIKLMNST 

7 

GHKMNQSTU 

27 

P  R  V 

40 

ABDMNQTU 

13 

ABCDMNQT 

30 

B  G  I  K  R  L  V 

41 

ABCGMNQT 

15 

C  F  I  M  N  0  P  R  V  W 

32 

AB  G I K  L 

42 

C  D  M  N  O  Q  T 

16 

BCIMOPRV 

33 

ABCGHIMNT 

43 

ABCGHKMNSTU 

18 

CFIOPRTV 

34 

ABCGHIKLMN 

44 

ABCDGHKLNQTU 

19 

G  H  I  K  L  N  S 

35 

G  H  I  K  L  N  S  T 

45 

ABDEGHKLSTU 

Examining  these,  we  find  that  F  (a  Lyrae)  cannot  be  exactly  placed,  but  that  the  alpha- 
betical arrangement  is  everywhere  followed,  with  the  single  exception  of  the  order  R  L  instead 
of  L  R  in  sequence  30.  Now,  there  is  no  other  sequence  in  which  R  and  L  occur  together, 
and  this  single  direct  comparison  which  might  have  been  influenced  by  some  accidental 
circumstance  (as  altitude  or  moonlight),  cannot  be  allowed  to  stand  against  the  strong  impli- 
cation of  sequences  15,  16,  and  18,  in  which  R  is  declared  inferior  to  M,  N,  O,  and  P, — all  of 
them  inferior  to  L.  Granting,  then,  that  Lyra  is  rightly  placed  (as,  indeed,  I  find  it  to  be  by 
subsequent  observation  made  under  more  advantageous  circumstances — it  being  a  low  star  at 
the  Cape),  the  final  arrangement  of  the  stars  in  question  will  be  in  the  order  in  which  they  are 
above  set  down. 

(242)  The  object  of  the  formation  of  a  normal  sequence  being  to  obtain  if  possible,  or  as 
far  as  possible,  an  extensive  and  equal  hold  upon  all  the  observed  and  corrected  ones,  the 
successive  groups  of  stars  to  be  brought  into  comparison  with  each  other  must  be  composed  of 

4  Q 


334 


OF  THE  FORMATION 


stars  differing  only  by  moderate  intervals  in  respect  of  brightness,  chosen  from  among  all  the 
sequences.  The  groups,  therefore,  must  for  this  purpose  be  as  large  as  can  be  securely 
managed;  and  in  treating  them  according  to  the  method  described  in  Art.  (230,  231),  {using, 
however,  now  the  corrected  instead  of  the  observed  sequences),  it  will  be  found  that  by  far  the  greater 
number  will  drop  out  for  want  of  mutual  direct  comparisons.  Nevertheless,  it  will  be  found 
possible  to  preserve  an  unbroken  chain  or  scale  of  magnitudes  down  to  any  grade  at  which  we 
may  think  fit  to  stop.  I  have  purposely  limited  myself  to  the  fifth  full  magnitude,  and  shall 
here  present  the  resulting  secpience  ;  suppressing,  however,  all  the  work  (which  is  exceedingly 
voluminous,  and  which  it  would  answer  no  good  purpose  to  publish),  as  well  as  the  corrected 
sequences  themselves ;  which,  however  useful,  and,  indeed,  indispensable,  as  steps  in  the 
process,  offer  no  other  point  of  interest  sufficient  to  compensate  for  the  space  they  would 
occupy.  Nor  is  it  necessary  to  refer  to  them  as  a  test  of  the  correctness  of  the  work,  since  the 
normal  sequence  resulting  from  them,  once  obtained,  may  be  tested  by  comparing  it  (in  the 
mode  already  dwelt  upon),  with  the  whole  mass  of  the  original  sequences ;  and  has,  in  fact, 
been  twice  subjected  to  this  ordeal,  by  breaking  it  up  into  two  distinct  systems  of  mutually 
overlapping  groups,  and  found  to  be  sufficiently  coherent  and  consistent  with  the  totality  of  the 
evidence  to  answer  every  purpose  for  which  it  is  intended. 

Normal  Sequence  (A)  resulting  from  the  Consilience  of  corrected  Sequences,  and  subsequently  verified 
by  direct  comparison  tvith  the  observed  Sequences.  First  step  to  the  assignment  of  numerical 
values  as  provisional  magnitudes  of  the  Stars  it  comprises. 


Star's  Name, 
Constellation,  and 
Letter. 


&  -5 
-  -—5 


P. 


Star's  Name, 
Constellation,  and 
Letter. 


o 


Star's  Name, 
Constellation,  and 
Letter. 


fl 
Ss 


Sirius 
Canopus 
a  Centauri 
Arcturus 
Capella  . . 
Lyra  .... 

Rigel  

Procyon. . , 
a  Eridani 
a  Orionis 
Aldebaran 
/3  Centauri 
a  Crucis 
Antares  . . 
a  Aquilae 
Spica  .... 
FomaLhaut 
Pollux    . . 
(3  Crucis 
Regulus. . 
a  Gruis  . . 
y  Crucis 
t  Orionis 
t  Canis  . . 
£  Orionis 
(3  Argils .  . 
y  Orionis 
y  Argils. . 
£  Argus  . . 


1.2 

1.2 

2 

I.4 

I 

i-7 

2 

2.0 

2.3 

2. 1 

2.3 

*-S 

*-3 

2-5 

3 

2.4 

2 

2.3 

2 

2.2 

2 

2.0 

2 

2.2 

o.  10 
0.22 

0.34 
0.45 

0.56 

0.66 

0.76 

0.85 

°-93 
1. 00 
1.07 
1. 14 
1.21 
1.28 

i-35 
1. 41 
1.47 

i-53 
1.59 
1.64 
1.69 
1.74 
1.80 
1.86 
1.91 
1.96 
2.01 
2.09 
2.14 


a  Trianguli  . 
£  Sagittarii . .  . 
9  Scoqni  . .  . 
a  Hydrse    . .  . 

3  Canis  

j3  Gruis  

a  Sagittarii  . 
a  Arietis  . .  . 
y  Leonis   . . . 

3  Argus  

X  Argils  

y  Geininorum 
9  Centauri . .  . 
;c  Orionis  . .  . 

(3  Canis  

3  Orionis  . . . 
y  Centauri . .  . 

1  Argus  

£  Argus  

£  Scorpii    . .  . 

«  Lupi   

£  Centauri . . . 

r\  Canis  

3  Scorpii  . . . 
£  Centauri . . . 

y  Corvi  

i)  Centauri . . . 

(3  Corvi  

tt  Argus  


3 
5 
2 

3-4 
3 
3 
3 

2 

3 

34 
3 
2 

3 

2.3 


3 
3 
3 
3 
3 
3 
3 
3 
3 
2.3 

3-4 


2.8 
2.8 
31 
3-5 
3-5 
2.7 
2.7 
2.8 
2.9 
2.9 
2.7 
2.9 
2.8 
2.5 
2.5 
2.5 

2-5 
2.6 


3.0 
3.0 
3.0 
3.0 
3.0 
2.9 
3.0 
3.0 
3.0 


2.18 
2.22 
2.27 
2.31 
2.36 
2.40 
2.44 
2.48 
2.52 

*-55 
2.58 
2.61 
2.64 
2.68 
2.71 
2.74 
2.77 
2.80 
2.82 
2.85 
2.88 
2.90 
2.92 
2.95 
2.97 
2.99 
3.01 

3-°3 
3.06 


y  Virginis  . 
3  Centauri . 
k  Argus  . . . 
a  Leporis  . 
a  Columbae 
ft  Argus . . . 
/3  Eridani  . 
)3  Hydri... 
f3  Lupi  . . . 
1  Centauri  . 
3  Corvi  . . . 
£  Corvi  . .  . 
tt  Scorpii  . 
a  Muscse  . 
y  Lupi  .  .  . 
a  Aree  . .  . 
v  Scorpii  . 
t  Scorpii  . 
(3  Trianguli 
y  Trianguli 
t  Argus . . . 
v  Argus  . . . 
3  Crucis . . . 
N  Velorum 
\  Centauri. 
k  Centauri . 
(3  Muscee  . 
a  Indi  ..  • 
£  Canis  . . . 


3 
3 
3 

3-4 
2 

3 
3 
3 

3-4 
3 
3 
4 

3-4 
4 
4 

3 

3-4 
3-4 
3 
3 
4 

3-4 
3 
5 
4 
3 
4 
3 
3 


3-° 
3.2 
2.9 
2.9 
2.9 
2.9 
2.9 
3-i 
3-i 
3-3 
3-4 
3-5 
3-7 
3-7 
3.6 
3.6 

34 
3.2 

34 
34 
3-3 
3-7 
3-7 
3.8 
3.8 
3.8 

34 
3.2 

3-5 


3.08 
3.10 
3-i3 
3-i5 
3.17 
3.19 
3.21 

3-23 
3.25 
3.27 
3.29 
3-31 
3-33 
3-35 
3.38 
3.40 
3.42 
3-44 
347 
349 
3-52 
3-54 
3-S6 
359 
3.61 
3.64 
3.66 
3.69 
3.71 


OF  NORMAL  SEQUENCES. 


335 


Star's  Name, 
Constellation,  and 
Letter. 


/8  Columbae  . 
6  Eridani  . .  . 

£  Argus  

y  Hydri  

q  Carinse  .  .  . 
o  2  Canis  . .  . 
a  Pictoris  . .  . 

a  Argus  

a  Doradus. . . 

u>  Argus  

p  Carinse  . . . 
S  Crateris  . .  . 
a  Reticuli  . . . 
y  Phcenicis  . 
H  Centauri. . . 
v  Centauri . .  . 
S  Lupi   


si 

•a  u  o 

bo  a.  w 

a  8 


3 

4-5 
4 
3 
5 
4 
4 
4 
3 

4-5 
4 
3-4 
3-4 
3 
4 
4 
S 


•3  a 


3-5 
3-5 

3-  9 

4-  i 
4.0 
4.0 
4.0 
3-9 
3-9 
3.8 
3-7 
3-7 
3.6 
3.6 

3-  9 
4.1 

4-  3 


o  si 
&a 

a>  in 


3-73 
3-75 
3-77 
3.80 
3.82 
3.84 
3.87 
3.89 
3.92 
3-94 
3-97 
3-99 
4.02 

4.05 
4.08 
4.11 
4.14 


Star's  Name, 
Constellation,  and 
Letter. 


t  Lupi  . .  . 
£  Lupi  . .  . 
ij  Lupi  . .  . 
5  Hydras  . 
/3  Virginis  . 
\  2  Hydrae 
y  Volantis  . 
k  Puppis  . 
a  Puppis  . 
ip  Argus . . . 
t  Columbae 
S  Hydri . . . 
e  Hydri  . . . 
/3  Volantis  . 
j3  Reticuli 
£  Crucis . .  . 
0  Centauri. 


=  bo 
to  a. 
£  « 


4-5 
4 

5 
4 

3-  4 

4-  5 

5 

4-5 

5 

4-5 
4 
4 
5 
5 
4 
4 
5 


4-5 
4-5 
4.2 
4.2 
4.4 
4-3 
4-5 
4-7 
4.8 
4.6 
4-5 
4-5 
4.4 
4.4 
4.6 
4.6 
4.6 


a)  to 
a"  -5 


4.16 
4.19 
4.22 
4.25 
4.28 
4.31 

4-34 
4-37 
4.40 

4-43 
4.46 
4.49 
4.52 

4-55 
4.58 
4.61 
4.64 


Star's  Name, 
Constellation,  and 
Letter. 


5  Volantis  . 
a  Volantis  . 

d  Ceti  

£  Volantis  . 
v  2  Canis  . 
a  Chamael  . 
b  Mali  . . . 
£  Volantis  . 
y  Doradus. 

0  Doradus  . 

6  Chainsel  . 
£  Doradus  . 
£  Doradfls  . 
£  Horologii 

1  Hydri . .  . 
B  A  C.  956 


t3 

;ude 
rue. 

t% 

Si  * 

11 

3  to 

—'a 

0  bo 

i  3 

Wg 

5 

4.6 

4.67 

5 

4.8 

4.70 

4 

4.8 

4-73 

5 

4.8 

4.76 

5 

4.8 

4-79 

5 

5.0 

4.82 

5 

5.0 

4.86 

5 

5.0 

4.89 

5 

5.0 

4.92 

5 

5.0 

4-95 

5 

5.0 

4.98 

5 

5.0 

5.01 

5 

S-° 

5.03 

4-5 

5.0 

5.06 

5 

5.09 

5 

5.12 

(243)  The  first  step  which  is  here  made  to  the  assignment  of  numerical  values  to  the  mag- 
nitudes, is  based  on  the  following  principle.  The  first  column  of  numbers  contains  (so  to  speak) 
the  rough  magnitudes  as  set  down  in  the  catalogue  of  the  Astronomical  Society ;  that  being  the 
system  of  magnitudes  to  which,  on  a  general  average,  it  has  been  resolved  to  conform,  agreeably 
to  what  is  stated  in  Art.  (217).  These,  it  will  be  observed,  run  very  unecpially  ;  and  it  is 
sufficient  to  cast  an  eye  down  this  column  to  be  fully  satisfied  of  the  necessity  of  a  reformation 
in  the  practice  of  astronomers  in  this  department  of  their  science.  In  order,  in  some  degree, 
to  smooth  down  their  grosser  irregularities,  and  prepare  them  for  graphical  interpolation  by 
means  of  a  curve,  the  second  column  of  numbers  exhibits  for  each  star  the  mean  of  its  own 
magnitude  as  stated  in  the  former  column,  and  those  of  the  two  stars  immediately  preceding, 
and  the  two  immediately  following  it  in  order.  Thus,  2.1,  the  number  in  this  column  opposite 
to  y  Crucis,  is  the  mean  of  1,2,  2\,  2|,  2$,  the  rough  magnitudes  of  the  five  stars,  among 
which  y  Crucis  occupies  the  middle  place.  Taking  now  the  numerical  order  of  each  star  from 
the  beginning  of  the  sequence  for  an  abscissa,  and  erecting,  on  a  chart  of  engraved  scpjares,  an 
ordinate  equal  to  the  mean  so  derived  for  that  star,  a  series  of  points  is  obtained,  still  very 
irregularly  disposed,  but  in  which  it  is  easy  to  recognise  the  prevalence  of  a  tendency  towards 
the  formation  of  a  curve  of  magnitudes,  which  is  accordingly  drawn,  on  a  general  impression 
of  its  whole  aspect  as  agreeing  best  with  the  distribution  of  the  points  laid  down,  entirely 
regardless  of  the  abrupt  and  irregular  undulations  they  would  appear  to  indicate,  which  are 
manifestly  caused  by  enormous  errors  in  the  original  magnitudes  from  which  we  set  out ;  as, 
for  instance,  that  of  5  assigned  as  the  magnitude  of  6  Scorpii,  2  to  a  Columbae,  5  to  q  Carinae, 
&c.  This  curve  is  then  read  off,  and  the  readings  set  down  in  the  last  column,  which 
therefore  exhibits  a  series  of  magnitudes  which,  while  they  tend  always  in  the  right  direction, 
conform  to  the  system  of  our  adopted  catalogue  as  nearly  as  the  errors  and  contradictions 
of  that  system  will  allow ;  and  are  therefore  fitted  to  afford  a  consistent  basis  to  our  further 
operations. 

(244)  The  earlier  part  of  the  scale  is  arbitrary,  and  is  founded  on  a  purely  imaginary — 
perhaps  a  fanciful  idea  of  the  rounding  off  of  the  curve  at  its  origin.  It  suffices,  however  (which 


336 


OF  THE  FORMATION  OF  NORMAL  SEQUENCES. 


is  all  that  is  at  present  needed),  to  keep  the  order  of  the  larger  stars  distinct.  Theoretically, 
correct  numbers  can  only  be  assigned  by  photometric  measurements,  with  which,  in  this  stage 
of  the  inquiry,  we  have  no  concern. 

(245)  This  first  approximation  being  made  to  numerical  values  of  the  magnitudes  of  all 
the  stars  in  our  normal  sequence,  places  it  in  our  power  greatly  to  extend  that  sequence,  and 
to  take  in  a  multitude  of  stars  whose  magnitudes  are  on  the  whole  quite  satisfactorily  defined 
by  the  corrected  sequences  in  which  they  occur,  but  which  were  rejected,  or  which  dropped 
out  for  want  of  connecting  links  referring  them  strictly  to  their  immediate  predecessors  and 
successors  in  the  scale.  Take,  for  example,  0  Ceti.  This  star  in  the  corrected  sequence  No.  21, 
is  found  between  8  Argus  (2.55)  and  k  Orionis  (2.68),  being  the  only  star  in  that  sequence 
intermediate  between  them.  The  arithmetical  mean  between  these  values  is  2.61.  Again,  in 
the  corrected  sequence  No.  28,  I  find  interposed  between  a  Arietis  (2.48),  and  /3  Hydri  (3.23), 
three  stars,  /3  Ceti,  and  a  Phcenicis,  and  a  Ceti,  from  which,  supposing  these  arithmetical 
means  equidistant  from  each  other  and  the  two  extremes,  we  find  the  value  2.67.  And,  again, 
in  the  corrected  sequence  No.  30,  I  find  /3  Ceti  singly  interposed  between  (3  Arietis  (2.48)  and 
k  Orionis  (2.68),  which  affords  a  third  value  2.58  for  the  numerical  expression  of  its  magnitude 
on  this  scale.  The  mean  of  these  three  determinations  2.62,  which  may  be  regarded  as  the 
magnitude  (on  this  scale)  within  very  moderate  probable  limits  of  error. 

(246)  So,  again,  to  take  another  instance,  in  the  case  of  a  Circini.  In  corrected  sequence  6, 
it  is  found  to  occur  singly  interposed  between  N  Velorum,  3.63,  and  y  Hydri,  3.80,  which 
gives  as  a  medium  value  for  the  star  in  question,  3.71.  In  corr.  seq.  14,  it  occurs  in  like 
manner  singly  interposed  between  /3  Muscae,  3.63,  and  w  Argus,  3.94,  whence  arises  3.78  as 
another  interpolated  value.  Again,  in  cor.  seq.  23,  it  stands  as  the  second  of  four  stars 
interposed  between  8  Crucis  3.55  and  77  Lupi  4.21,  whence  we  get  3.81  for  a  third  value.  In 
cor.  seq.  42,  it  is  singly  interposed  between  (3  Muscae,  3.63,  and  q  Carinae,  3.82,  giving  3.72 ; 
and,  lastly,  in  cor.  seq.  43,  it  is  the  first  of  two  interposed  between  (3  Muscee  3.63  and  a  Pictoris, 
3.87,  whence  we  get  3.71  for  an  interpolated  magnitude.  Assembling  these  five  results,  and 
taking  their  mean,  we  finally  arrive  at  3.75  for  the  provisional  magnitude  of  a  Circini. 

(247)  In  this  manner  provisional  values  of  all  the  stars  which  occur  in  the  corrected 
sequences  interposed  between  the  stars  of  our  normal  list  have  been  obtained,  and  a  new  and 
much  more  extensive  normal  sequence  constructed  by  inserting  them  in  their  proper  places 
among  the  stars  of  that  list.  This  sequence  has  then  been  treated  exactly  as  the  original  normal 
sequence  of  which  it  is  an  extension,  and  is  presented  below.  Col.  1,  contains  the  names  of 
the  stars  ;  col.  2,  their  rough  magnitudes  from  the  catalogue  ;  col.  3,  their  equalized  magnitudes, 
and  col.  4,  their  interpolated  magnitudes  read  off  from  a  curve  constructed  as  already  ex- 
plained. The  stars  of  the  first  magnitude,  as  low  as  /3  Crucis  inclusive,  remaining  unchanged 
in  this  process,  are  omitted. 


PROVISIONAL  MAGNITUDES.  337 


Provisional  Magnitudes.    Sequence  (B)  resulting  from  the  extension  of  Sequence  {A)  by  the  Interpola- 
tion of  Stars  from  the  corrected  Sequences.    {Italics  indicate  Stars  which  occur  in  Sequence  A.) 


Star's  Name, 
Constellation,  and 
Letter. 


Regulus 
a  Gruis  ... . 
y  Cruris    . . 
e  Orionis  . . 
f  Ursae 
\  Scorpii  . . 
i  Canis  ... . 
a  Ursae  ... . 
£  Orionis  .. 
(3  Argus. .  .  . 
n  Ursae 
y  Orionis  . . 
y  Argus    . . 
a  Pavcmis  . . 
£  Argus  ... . 

/3  Tauri  

a  Trianguli 
£  Sagittar. 
6  Scorpii  .. 
a  Hydras  . . 
(3  Ursae  Min 
3  Canis  . .  . . 
/3  Gruis 
a  Sagittarii 
a  Arietis   . . 
y  Leonis   . . 
3  Argus..  . . 
t  Pegasi . . .  • 
X  Argus. . . . 
y  Geminor 
£  Ursae 
(3  Ceti  .... 
6  Centauri 
f3  Aurigae  . . 
k  Orionis  . . 
a  Polaris  . . 
a  Pegasi . . . . 
(3  Canis 
3  Orionis  . . 
(3  Leonis   . . 
a  Cor.  Bor. 
a  Ophiuchi 
y  Centauri 
i  Argus  . . . . 
£  Argus. . . . 
(3  Pegasi 
£  Bootis 
a  Phoenicis 
e  Scorpii  . . 
y  Ursae 
a  Lupi 
(3  Ursae 
£  Centauri. . 
rj  Canis 
3  Scorpii  . . 
3  Leonis    . . 
£  Centauri. . 
y  Corvi 
t)  Centauri 
a  Ceti    . . . . 
/3  Corvi 


i 

2 

*-3 
*-3 

3 

3 

2.3 

1.2 

3 

2 
2.3 
2 
2 
2 
2 
2 
2 
3 

5 

2 

3 

34 
3 
3 
3 
2 

3 

2.3 
34 

3 

3 

2.3 
2 
2 
3 

2.3 

2 
2.3 

2 
2.3 

2 

2 

3 

2 

3 
2 

3 

3 
2 


3 
3 
3 
3 
3 
3 
3 

2.3 
2.3 


W2 


2.2 
2.6 
2.7 
2.5 
2.6 

2.4 
2.3 

2.2 
2.3 
2.1 
2.1 
2.0 
2.0 
2.2 
2.8 
2.8 

3.0 

3-3 
3-3 
2.9 

3-i 

2.9 
2.8 
2.7 
2.8 
2.8 
3.0 
2.9 
2.8 
2.5 
24 
2.4 
2.3 
2.4 
2.4 
2.3 

2.2 
2.1 
2.3 
2.3 
2.4 
2.4 
2.6 
2.6 
2.6 

2.6 
2.6 
2.6 
2.6 
2.8 
2.8 

3.0 
3.0 
3.0 
2.9 

2.8 

2.7 

2.8 


ft  3 


1.62 
1.67 
1.72 

1.77 
1.81 

1.8s 

1.89 
1.93 
1.97 

2.01 
2.04 
2.08 

2.1  I 

2.14 

2.17 

2.20 
2.23 
2.26 

2.28 

2.30 
2.32 

2.34 

2.36 

2.38 

2.40 
2.42 

2.44 

2.46 

2.48 

2.50 

2.51 
2.53 
2.55 
2.57 

2.59 
2.60 
2.62 
2.64 
2.65 
2.67 
2.68 
2.70 
2.71 

2.73 
2.74 

2-75 
2.77 

2.78 
2.79 
2.80 
2.81 
2.83 
2.84 
2.86 
2.87 
2.88 
2.90 
2.91 
2.92 
2.93 


Star's  Name, 
Constellation,  and 
Letter. 


n  Ophiuclii  . 
7T  Argus  . . . 
y  Virginis. . . 
£  Ophiuchi  . 
13  Scorpii  . . . 
y  Pegasi. . . . . 
3  Centauri . . . 
3  Ophiuclii 
£  Sagittarii  .  . 
k  Scorpii  . . . 

k  Argus  

(3  Herculis . . . 
a  Leporis  . . . 

(3  Librae  

tj  Bootis  

a  Columbte  • 

fi  Argus  

£  Virginis  . . . 

a  Librae  

a  Cor.  Carol. 
(3  Eridani  . . . 
a  Serpentis  . 
X  Sagittarii  . 
(3  Hydri    . . . 

(3  Lupi  

1  Centauri . . . 
S  Sagittar. . . . 

S  Corvi   

9  Argus  

(3  Arae   

j3  Leporis  . . . 

£  Corvi   

7r  Scorpii  . . . 
a  Toucani  . .  . 
a  Muscae   . . . 

p  Argus  

y  Lupi  

o-  Scorpii  . . . 

a  Aral   

Ii  1  Scorpii  . 
v  Scorpii  . . . 
1  Scorpii  . . . 
t  Scorpii  . . . 
7r  Sagittarii  . . 
y  Aquilae  . . . 
y  Hydrse  . . . 
(3  Triang.  . . . 
j3  Arietis  . . . 
y  Triang.  . . . 

a  Hydri  

t  Argils  

£  Hydras  . . . 
t  Orionis   . . . 

v  Argils  

v  Hydras   . . . 

S  Cruris  

j3  Can.  Min.  . 
N  Velorum  . 
q  Orionis  . .  . 
\  Centauri  . 
y  Gruis  


2.3 
34 
3 

2 
2.3 
3 
3 

34 


34 
2.3 

3 

2 

3 

34 
3 
2.3 

3 

2.3 
4 
3 

34 
3 

34 
3 
2 

3 
4 
4 

34 
3 
4 

34 
4 
4 
3 

34 
34 
4-5 
34 
4-5 
3 

4-5 
3 
3 
3 
3 
4 
4 

34 
34 

4 

3 

3 

5 

4 

4 

4 


£33 


2.8 

2.7 

2.8 

2.7 
2.8 
3.0 
3-2 

3-i 

3-1 
2.8 
2.8 


2.9 
2.8 
3.0 
2.9 
3.0 
3.0 
3.2 
3.2 
34 
3^ 
3.0 
2.9 

3-i 

3.2 

3-3 
3-5 
3-7 
3.6 
3-6 
3-7 
3-7 
3.6 
3.6 

3-7 
3.6 

3-9 
3.8 
4.0 

3-7 
3.6 

3-3 
3-3 
3.2 

34 
3-5 
3-6 
3.8 
3.6 
3-4 
3-7 
3.8 
3.8 
4.0 
4.0 
3.6 


2.94 
2.96 
2.97 

2.98 
2.99 
3.00 
3.02 
3-°3 

3.04 

3-°5 
3.06 
3.08 

3-°9 
3.10 
3. 11 
3.12 
3.14 

3-i5 
3.16 
3.18 
3.19 
3.21 
3.22 
3.24 

3-25 
3.26 

3.28 
3.29 
3.31 
3-3* 
3-33 
3-35 
3.36 

3-38 

3-39 
3.40 

342 
343 
3-44 
345 
3.46 
3.48 

349 
3.50 

3-5i 
3-52 
3-54 
3-55 
3.56 

3-57 
3-58 

3-59 
3.60 
3.61 
3.62 

3-63 
3.64 
3.65 


Star's  Name, 
Constellation,  and 
Letter. 


k  Centauri 
(3  Muscm  . 
£  Virginis .  ■ 
a  Indi    . . . . 
£  Canis  ... , 
(3  Phoenicis 
(3  Columbai 
£  Hydrae    . . 
a  Circini  . 
0  Eridani  . 
£  Argus. . .  ■ 
y  Hydri  . 
q  Carina  . . 
o  2  Canis  . . 
7r  Hydrae  . 
v  Argus. . . . 
a  Pictoris. . 
n  Scorpii  . , 
(T  Argils. . . , 
£  Gruis  ...  , 
y  Arae   ... . 
a  Doradus 
S  Virginis  . . 
w  Argus    . . 
£  Leporis  . , 
p  Carina  . . 
3  Crateris . . 
c  Puppis    . , 
a  Reticuli  . . 
H  Leporis  . . 
<r  Canis 
y  Phoenicis 
n  Virginis  . , 
fi  Centauri 
v  Centauri 
<p  Eridani  . . 
k  Ophiuchi 
3  Lupi 
fi  Serpentis 
y  Scorpii  . . 
(3  Serpentis 
£  Ophiuchi 

X  Argus  

£  Lupi 
o  Argus ... . 
(3  Toucani . . 
£  Lupi  . . . . 
k  2  Canis  . . 
tj  Lupi 
y  Ceti    ... . 
a  Horologii 
£  Hydra   . . 
X  Canis 
a  Carinae  . . 
X  Eridani  . . 

0  1  Lupi  . . 
(3  Virginis . . 

1  Lupi  .... 
X  2  Hydra 
k  Lupi  ... . 
(3  Cancri   , . 


3 
3 
4 
3 
3 

34 
3 
5 
4 

4-5 
4 
3 
5 
4 

4-5 
S 
4 
4 
4 
4 
3 
3 

34 
4-5 
4 
4 

34 
4 

34 
S 

34 
3 

34 
4 
4 

4 
5 

3 

34 
34 

3 

3 

4-5 
4 

34 

4 

4 

5 

3 

5 

4 

4 

5 

4 

5 
34 
4-5 
45 

5 

4 


3  be 


3.6 

34 
3.2 

3-3 
3-3 
3-5 

3-  7 
4.0 
4.1 
4.1 
4.1 
4.1 
4.1 

4-  3 
45 
4-3 
43 
4.2 
3.8 
3.6 

3-5 
3.6 
3.6 
3-8 
3-9 
4.0 
3.8 
4.0 

3-9 
3.8 

3-7 
3-8 
3.6 

3-7 
4.1 

4.0 

3-9 
3-8 
3.6 
3.2 
3-5 
3-6 
3-6 
3.8 
4.0 
4.1 

3-  9 
4.2 
4.2 
4.2 
4.2 
44 
44 

4-  3 
44 
43 
45 
4-3 
4.6 
4.6 


O  = 


£  2 


3.66 
3.67 
3.68 
3.68 
3.69 
3.70 

3-7i 
3-72 
3.72 

3-73 
3-74 
3-75 
3-76 
3.76 
3-77 
3.78 
3.78 
3-79 
3-79 
3.80 

3.81 
3.82 
3.83 

3-83 
3.84 

3-85 
3.86 

3.87 
3.87 
3.88 
3.89 
3.90 
3.91 
3.92 
3-93 

3-94 
3-95 
3.96 

3-97 
3.98 

3-99 
4.00 
4.02 
4.04 
4.05 
4.07 
4.09 
4.10 
4.12 
4.13 
4.15 
4.16 
4.17 
4.19 
4.20 
4.22 
4.23 
4.24 
4.26 
4.27 


4  R 


338 


OF  THE  COMPLETE  INTERPOLATION 


Star's  Name, 
Constellation,  and 
Letter. 


y  Volantis 

k  Puppis   

1  Carina;   

a  Puppis   

£  2  Scorpii  

y  Toucani  

4/  Argus   

fi  Hydra;   

0  i  Cards   

1  Hydra;   

7T  Lupi  

t  Columbm  

*  Phoenicis  

£  Phoenicis    . . . 

5  Hydri  

v  Pictoris  

ft  Lupi   

(3  Pictoris  

/3  Doradfls  

6  Hydri  

<p  Argils  

u  Carina;   

a  Mali   

Volantis  

B  A  C.  2562 . . . 
v  2  Eridani  . . . 


5 

4-5 

5 

s 

3 
4 
4-5 
4 
4 
5 
5 
4 
4 
5 
4 
5 
5 

4-5 
4 
5 
4 
5 

4-5 

5 

5 

4 


!& 


4-7 
4-7 
4-5 
4-3 
4-3 
4.1 

3-  9 

4-  3 
4-5 
4.4 
4.4 
4.6 
4.4 
4.4 
4.6 
4-7 
4-5 
4-7 
4-5 
4-5 
4-5 
4-7 
4-7 
4-7 
4-7 
4.6 


O  3 


4.28 
4.29 
4.3O 
4.32 

4-33 
4-34 
4-35 
4.36 

4-37 
4.38 

4-39 
4.40 
4.41 
4.42 

4-43 
4.44 

4-45 
4.46 

4-47 
4.48 
4.49 
4.50 
4.51 
4.51 
4.52 
4-53 


Star's  Name, 
Constellation,  and 
Letter. 


g  Eridani  . . 
/3  Hydra;  .. 
v  1  Centauri 
8  Phoenicis 
(3  Reticuli  . . 
£  Crucis. . . . 
f  Crucis. . .  • 
k  Phoenicis 
<j>  Centauri 
rj  Crucis  . . 
S  Volantis. . 
g  Centauri. . 
a  Volantis.  ■ 
I  Carina;  . . 
1  Eridani  . . 
k  Eridani  .. 
8  Toucani  . . 

8  Ceti  

p  Velorum . . 
8  Muscse  . . 
£  Volantis. . 
y  Musca;  . . 
O  Crucis  . . 
v  2  Canis  . . 
n  Phoenicis 
q  Velorum . . 


5 
4 
5 
4 
4 
5 
4 
5 
5 
4-5 
5 
5 
5 
5 
4-5 
4-5 
5 
4 
S 
4 
5 
4 
S 
5 
5 
4 


4.6 
4.4 
4.4 
4.4 

4-4 
4.4 
4.6 
4-7 
4-7 
4.9 
4.9 
4.9 

4-9 
4.8 
4.8 
4.6 
4.6 

4-5 
4.6 
4.4 
4.6 
4.6 
4.8 
4.6 
4.8 
4.8 


4-54 
4-55 
4.56 

4-57 
4.58 

4-59 
4.60 
4.61 
4.62 
4.63 
4.64 
4.65 
4.65 
4.66 
4.67 
4.68 
4.69 
4.70 
4.71 
4.72 
4-73 
4-73 
4-74 
4-75 
4.76 

4-77 


Star's  Name, 
Constellation,  and 
Letter. 


p  Lupi   

a  Chamaleontis 
%  2  Centauri  . .  . 

bMali   

y  Apodis   

f  Centauri  

£  Toucani  

£  Volantis  

a  Apodis   

7  DoradHs  

0  Chamseleontis 
£  Toucani  

8  Doradus  

6  Chamaieontis 
(3  Chama;leontis 

?  Doradus  

X  Phoenicis    . .  . 

e  Reticuli   

£  Doradfis  

y  Reticuli  

n  Toucani  .... 
B  A  C.  1 103..  . 
£  Horoloyii  . .  . 
f  1  Eridani  . .  . 

£  Hydri   

B  A  C.  956 


5 
5 
5 
5 
5 

5.6 
5 
5 

4-5 
5 
S 
S 

s 

5 
S 

s 

5 
S 
5 
5 
S 
6 

4-5 
S 
5 
5 


(248)  Five  stars,  viz.,  a  Phoenicis,  (  Ophiuchi,  k  Scorpii,  /3  Herculis,  and  Eridani,  which 
occur  in  the  corrected  sequences  having  heen  accidentally  omitted  in  the  process  by  which  the 
provisional  magnitudes  in  this  list  were  obtained,  are  here  inserted  in  their  places,  but  without 
annexed  numbers.  As  their  omission  from  among  the  data  cannot  have  the  smallest  per- 
ceptible effect  on  the  final  result,  it  has  not  been  thought  necessary  to  go  over  again  the  whole 
of  the  subsequent  work  on  that  account. 


Step  III.  Of  the  Complete  Interpolation  of  the  observed  Sequences,  the  conclusion  of  an  Independent 
Numerical  Result  from  each  Observation  of  each  Star,  and  the  assemblage  of  their  results  for  the 
final  Determination  of  its-  Magnitude. 

(249)  The  whole  of  the  work,  up  to  the  actual  point  at  which  we  are  arrived,  is  merely 
preliminary,  and  has  for  its  object  to  enable  us  to  assign  to  each  star,  in  each  observed  sequence, 
a  numerical  magnitude  which  shall  be  at  the  same  time  individual  as  regards  that  particular 
sequence  (i.  e.,  affected  with  the  peculiar  errors  of  observation  which  prevail  in  that  sequence), 
and  yet  comparable  with  the  general  scale  of  magnitudes  which  prevails  through  all  the 
sequences  collectively. 

(250)  To  this  end,  in  every  observed  sequence,  opposite  to  each  star  therein  which  occurs 
in  the  extended  normal  sequence  B,  is  to  be  written  the  provisional  numerical  magnitude 
assigned  to  it  in  the  last  column  of  that  sequence,  leaving  the  intermediate  stars  without 


OF  THE  OBSERVED  SEQUENCES. 


339 


numbers.  If  the  sequence,  then,  were  corrected  ones,  or  if  they  were  free  from  error  of 
observation,  the  numbers  so  written  in  each  would  form  an  uninterruptedly  increasing  series, 
each  being  greater,  or,  at  all  events,  not  less  than  all  which  follow  it.  In  many  they  do  so ; 
and  in  such  cases  all  that  remains  to  do,  is  to  interpolate 
values  to  fill  up  the  blanks  on  the  principle  already 
explained  in  Art.  (245).  But  in  other  instances  such  is 
not  the  case,  owing  to  accidental  error  in  the  observations 
themselves,  and  to  possible  remaining  error  in  the  pro- 
visional magnitudes  used,  which,  though  not  considerable, 
certainly  must,  in  some  cases,  affect  the  order  of  the  stars,  as 
arranged  by  them  alone.  Thus,  to  take  an  example :  in 
sequence  20,  the  stars  succeed  each  other  in  the  order  here 
set  down,  and  the  arithmetical  order  of  precedence  is  in- 
terrupted in  the  cases  of  a  Leporis  and  ( Canis,  in  the  2d 
column  annexed.  Taking,  then,  a  chart  of  engraved 
squares,  laying  down  points  corresponding  to  the  abscissas  1,  2,  3,  8,  9,  10,  11,  and  the 
respective  ordinates  2.84,  3.05,  2.96,  3.71,  3.69,  3.74,  3.76,  and  passing  an  interpolating  curve 
among  them,  we  find,  by  reading  off  its  ordinates  for  all  the  abscissas  from  1  to  11,  the  values 
set  down  in  the  last  column,  not  only  for  the  seven  stars  which  furnished  the  original  (but  now 
abandoned)  points,  but  also  for  the  four  intermediate  ones.  And  thus  we  proceed  in  all  similar 
cases  ;  only,  in  constructing  these  curves,  we  must  be  careful  to  keep  as  near  to  all  the  points  as 
the  condition  of  a  continual  increase  of  the  ordinate  will  allow. 

(251)  In  cases  where  the  intervals  are  large,  as  they  sometimes  are,  a  good  deal  of 
discretion  and  latitude  must  exist,  especially  where  the  intervals  are  irregular,  and  the  number 
of  intermediate  stars  considerable.  Error  is  thus,  of  necessity,  induced.  And  it  would  seem, 
moreover,  that  by  adopting  the  newly  interpolated  magnitudes  for  the  normal  stars  as  well  as 
for  the  intermediate  ones,  to  the  exclusion  of  their  provisional  magnitudes,  we  are  undoing 
what  we  have  taken  considerable  pains  to  do,  and  in  effect  reviving  and  bringing  again  into 
view  errors  of  observation  which  the  object  of  all  the  former  part  of  the  process  was  to  smooth 
down  and  obliterate.  An  attentive  consideration  of  the  several  steps  will  show  that  this  is 
unavoidable,  and  that  in  no  other  way  can  the  sequences  be  impartially  treated  so  as  to  preserve 
a  due  relation  between  the  interpolated  and  the  normal  stars.  And  when  the  individual  results 
for  stars  which  occur  in  several  sequences  are  assembled,  and  means  taken,  the  normal 
magnitudes  are  found  to  be,  in  effect,  very  nearly  indeed  re-produced,  as  will  presently 
appear. 

(252)  The  process  above  indicated  having  been  carried  out  in  each  observed  sequence,  so 

far  downwards  as  the  normal  list  B  extends,  and  a  dotted  line  drawn  in  each 

sequence  below  the  last  normal  star  which  occurs  in  it  (as  in  sequence  1,  below  r  Scorpii — in 
seq.  2,  below  a  Arse,  &c.)  each  star  above  such  dotted  line  will  have  assigned  to  it  a  numerical 
magnitude  comparable  with  all  the  rest.  And  these  are  the  values  which,  so  obtained,  are  set 
down  opposite  to  the  names  of  the  stars  in  all  the  observed  sequences  above  recorded.  A 
general  index  then  being  made  of  the  stars  which  occur  in  all  the  sequences,  all  the  individual 
values  so  found  assigned  to  each  star  are  assembled  together.    Of  these  a  final  mean  is  taken 


t)  Canis   

a  Leporis   

7r  Argus   

(3  Can.  Min  

t  Ononis  

(3  Leporis  

q  Orionis  

j3  Columbae  

£  Canis  

£  Argus   

o  2  Canis  


2.84 

2.84 

3.05 

2.99 

2.96 

3.10 

3.20 

3.30 

3.41 

3-5i 

3-71 

3.62 

3.69 

3.69 

3-74 

3.72 

3.76 

3.76 

340 


OF  THE  COMPLETE  INTERPOLATION  OF  THE  OBSERVED  SEQUENCES. 


in  those  cases  where  the  star  only  occurs  above  the  dotted  lines,  reserving  the  cases  of  stars  which 
occur  in  some  sequences  above,  and  in  some  below  them,  and  in  which,  therefore,  all  the 
values  cannot  yet  be  assigned  numerically  for  subsequent  determination. 

(253)  Table  (C)  annexed  below,  exhibits  this  assemblage  of  individual  results,  according  to 
an  alphabetic  arrangement,  which  makes  it  easy  to  refer  to  it  for  any  particular  star  whose 
magnitude  may  be  wanted.  The  mean  results  which  have  no  asterisk  (*)  annexed  to  them  are 
those  obtained  in  conformity  with  the  conditions  of  the  last  article,  and  which  depend  directly 
on  the  normal  stars  alone,  or  which  are  themselves  normal. 

(254)  These  values,  when  obtained,  are  used  to  continue  the  interpolation  downwards  below 
the  limit  where  the  normal  stars  cease  to  afford  us  their  aid.  They  are  treated  for  this  purpose 
exactly  as  described  in  Art.  (250,  Sec),  and  the  interpolating  curves  being  constructed  and  read 
oft",  the  resulting  magnitudes  are  attached  to  their  respective  stars  below  the  dotted  line,  which 
done,  another  double  dotted  line  is  drawn  (when  necessary)  marking  the  lower  limit  of  this 
second  or  supplementary  interpolation  in  each  sequence ;  as,  for  instance,  in  sequence  1  below 
r]  Scorpii,  in  2  below  y  Arte,  &c.  And  proceeding  with  these  values,  as  with  those  of  the  first 
interpolation,  the  results  are  obtained  which  in  Table  C  are  marked  with  a  single  asterisk  (*). 
These,  again,  are  employed  to  continue  the  interpolation  yet  one  stage  lower,  below  the  doubly 
dotted  line,  by  which  a  few  more  (confessedly  very  precarious)  results  marked  with  two  asterisks 
(*  *)  are  obtained. 

(255)  There  still  remain  outstanding  some  portions  of  the  sequences  which,  for  want  of 
data  in  accordance  with  the  normal  data  of  sequence  B,  cannot  be  interpolated.  These  we  must 
leave  till  further  observation  shall  enable  some  future  inquirer  who  may  be  disposed  to  follow 
up  this  subject  on  the  plan  here  sketched  out,  to  interlink  them  with  the  general  mass.  Nearly 
the  whole  of  sequence  29  is  in  this  predicament,  and  the  greater  portion  of  sequel  27.  Mean- 
while the  number  of  stars  (452)  to  which,  now  for  the  first  time,  magnitudes  upon  a  systematic 
plan  have  been  assigned,  is  considerable  enough  to  serve  as  a  fair  specimen  of  the  practical 
application  of  our  method.  I  may  add,  too,  that  since  my  return  to  England  I  have  been,  and 
am  still,  engaged  in  extending  its  application  to  the  northern  stars,  with  some  perseverance, 
and  I  venture  to  hope  not  without  some  corresponding  degree  of  success.  Sixty-one  sequences, 
in  addition  to  those  above  recorded,  have  been  observed  and  partially  reduced,  and  where  com- 
pletely so,  and  brought  into  comparability  with  the  southern  sequences  by  means  of  the  inter- 
tropical stars  common  to  both  series,  will  afford  a  uniform  system  of  astrometrical  nomenclature 
on  which  I  have  every  reason  to  believe  considerable  reliance  may  be  placed.  This  work, 
however,  besides  that  it  is  as  yet  incomplete,  cannot  properly  find  its  place  in  a  volume  of 
Southern  Observations. 


RESULTING  MAGNITUDES. 


341 


(C)  Assemblage  of  individual  Results  from  the  Interpolation  of  the  observed  Sequences,  and  final  Deter- 
mination of  the  Magnitudes  to  be  adopted.  [For  Stars  brighter  than  Regulus,  see  the  Magni- 
tudes assigned  in  the  Normal  Sequence,  A]. 


N.B.  The  first  numbers  in  each  line  refer  to  the  observed  Sequences,  from  which  the  others,  expressing  the  Magnitudes  whose 

mean  is  taken,  are  derived. 


a 

Androm. 

16 

2.25 

a 

Antliae. 

4' 

4-7  S 

a 

Aquarii. 

27 

2.97 

a  Arse. 

2 

3.40 

42 

3.40 

3.40 

a 

Arietis. 

21 

2.40 

28 

2.40 

30 

2.40 

31 

2.40 

2.40 

a 

Apodis. 

8 

4.85 

a 

Can.  ven. 

Cor  Caroli. 

45 

3.20 

46 

3-25 

3.22 

a 

2  Capric. 

27 

3-94 

a  Ceti. 

28 

3.46 

3° 

2.82 

3.14 

Somewhat  doubt- 
ful. 


ct 

Chamael. 

8 

4-79 

21 

4-79 

30 

4.88 

38 

4-79 

43 

4.50 

4-75 

0 

Circini. 

6 

3-74 

3-75 

23 

3.80 

42 

3-73 

43 

3.92 

i  78 

a  Caeli. 

37 

4.92 

a 

Columbae. 

*9 

3.05 

21 

3.36 

30 

3.18 

32 

3.09 

35 

3-13 

37 

3.09 

38 

3.28 

39 

3.09 

41 

3.06 

3-i5 

a 

Cor.  Bor. 

46 

2.63 

a  Corvi. 

22 

4.61 

23 

4.61 

3  5 


4.68  + 
*  *  4  63 


a  Cygni. 
16  1.95 
Very  doubtful. 


a 

Doradus. 

6 

3.78 

16 

3.82 

21 

3.78 

30 

3.80 

35 

3-75 

36 

3.82 

37 

3.81 

38 

3-79 

39 

3.82 

3.80 

a 

Fornacis. 

28 

*  4-55 

a  Geminor.  Castor. 

7 

1.97 

19 

2.02 

35 

1.67 

39 

2.32 

1.99 

a  Gruis. 

3 

1.67 

15 

1.61 

16 

1.67 

18 

1.67 

21 

1.67 

27 

1.67 

30 

1.67 

1.66 

a 

Herculis. 

26 

3.28 

Variable. 

a 

Horolog. 

37 

4.17 

a 

Hydra?. 

1 

2.58 

!9 

2.08 

34 

2.41 

35 

'•75 

36 

2.32 

37 

2.34 

38 

2.41 

39 

2.40 

40 

41 
42 
43 
44 
45 
46 


2.42 
2.30 
2.29 
2.30 
2.17 
2.30 
2.46 

2.30 
Variable  ? 

a  Hydri. 


3 

3.26 

17 

3-46 

21 

3.26 

28 

3.83 

30 

3-37 

36 

3.62 

37 

3.72 

39 

3-45 

*  3-44 

Variable  ? 


16 

17 
21 

27 


Indi. 
3.68 
3-75 
3-55 
3.68 

3.67 


a  Leonis  Regulus. 

6  1.62 

7  i-4« 
34  1.62 
38  1.80 
40  1.62 
43  1.62 

1.6! 


a  Leporis. 

2.83 
2.99 

3-°5 
2.94 

3-°5 
2.80 
3.0S 
3-°5 
315 
3.02 

3.00 


a  Librae. 


14 

3-15 

26 

3.16 

45 

3.05 

3.12 

a  Lupi. 

5 

2.80 

6 

2.80 

10 

2.80 

2.81 

12 

2.81 

r3 

2.83 

14 

2.83 

26 

2.84 

42 

2.83 

2.82 

a 

Muscse. 

6 

3-35 

'4 

3.36 

25 

3.66 

35 

3-45 

38 

3.40 

42 

3-35 

3-43 

a 

Normae. 

23 

*  4-67 

a 

Ophiuchi. 

26 

2.67 

a 

Pavonis. 

'4 

2.55 

'5 

2.29 

16 

2.26 

18 

2.33 

21 

1.99 

27 

2.50 

30 

2.40 

2.33 

Variable  ? 

a 

Pegasi. 

16 

2.65 

a 

Phoenicis. 

3 

2.64 

16 

2.92 

2 1 

2.62 

28 

2.92 

30 

2.70 

2.78 

a 

Pictoris. 

6 

3.82 

10 

3-5° 

21 

3.64 

7.0 
j 

1.80 

35 

4.09 

36 

3.68 

37 

3.81 

38 

3-77 

1  78 

43 

3.78 

3-77 

a 

Piscium, 

28 

4.13 

31 

4-34 


^  4-  J9 

a 

Reticuli. 

6 

3.87 

16 

3.87 

21 

4.09 

30 

3.87 

35 

4.02 

36 

3.87 

37 

3-87 

39 

3.85 

3.91 

a 

Serpentis. 

45 

3.14 

a 

Toucani. 

3 

3.40 

16 

3.38 

17 

3.30 

21 

3.09 

27 

3.08 

30 

3.61 

3.32 

342 


FINAL  CONCLUSION  OF 


a 

Trianguli. 

c 

j 

2.23 

6 

2.23 

2.23 

'3 

2.23 

»5 

2.26 

16 

2.23 

2.21 

42 

2.23 

43 

2.23 

2.23 

a  Ursse. 

44 

1.93 

45 

1.96 

1.94 

a 

Ursse  Min. 

Polaris. 

46 

2.59 

a 

Volantis. 

30 

36 


4.65 
4.65 

4-53 
4.83 

4.66 


(3  Arae. 


42 


3.50 
3.12 

*  3-31 


22 
23 
24 
z5 
3- 
33 
34 
35 
36 
38 
39 
40 
42 
43 


2.01 
2.02 
1.99 
2. 1 1 
2.01 
2.11 

2.03 


/3  Aquarii. 
27  2.85 


/3  Argus. 

2.06 
i  2.01 
2.01 
;  2.01 
2.01 
1.92 
2.1 1 
2. 1 1 
z.i  1 
1.95 
2.01 
2. 11 
1.99 


(3  Arietis. 
30  3.49 


(3  Corvi. 


{3  Aurigae. 
45  2-5i 


j3  Bootis. 
45      *  3-8° 


/3  Cancri. 
35  4-^7 


/3  Canis. 

2.48 
2.41 
2.64 
2.64 
2.64 
2.64 
2.56 
2.53 
2.58 
2.64 

2.58 


(3  Can.  Min. 


20 

35 
36 

37 


3.20 
3-65 
3-49 
3-32 

3.41 


(3  Capricor. 
27  3.32 


(3  Ceti. 


16 
21 
28 
30 


2.24 
2.51 
2.66 
2.43 

2.46 


(3  Chamsel. 


38 
43 


4.91  + 

4.78 

4.72 

*  4-80+ 


(3  Columbae. 

10  3.62 

11  3-73 

12  3-37 
37  3-71 
58  3.61 


7 

2.80 

14 

a-93 

22 

2.93 

23 

2.93 

25 

3.00 

35 

3.19 

42 

2.95 

43 

2.93 

45 

2.93 

46 

2.93 

2.95 

f3  Crateris. 


41 

4.66 

Doradus. 

21 

4.67 

30 

4.40 

34 

3.92 

37 

3-97 

39 

4.58 

4.31 

(3  Eridani. 


19 

3.20 

30 

3.06 

32 

3-44 

35 

3.06 

36 

3-55 

3.26 

(3  Gruis. 


3 

2.36 

'5 

2.38 

16 

2.36 

21 

2.21 

27 

2.36 

28 

2.36 

30 

2.46 

3> 

2.36 

2.36 

(3  Hydri. 


3.61 


3 
6 
16 

17 
21 
28 


(3  Herculis. 
26  3.02 


(3  Hydra. 
35  445 


3.19 
3.08 
3.19 
3.19 
3.17 
3.19 


30 

34 
36 

37 
39 


3.27 
3.19 
3.62 
3.72 
3.19 

3.27 
Variable  ? 


(3  Indi. 

17         5)4  4.22 

(3  Leonis. 


7 
38 
40 

45 
46 


1.91 

2.66 

2.50+ 

2.55 

2.68 


2.63 

Rejecting  1.9 1  and 
2.50  + 


(3  Leporis. 


19 

3.42 

20 

3.41 

21 

3.72 

32 

3.20 

35 

2.97 

36 

3-36 

37 

3-39 

38 

3-51 

39 

3'4 

3-35 

Probably 

variable. 

f3  Librae. 

14 

315 

26 

3.06 

45 

2.99 

3.07 

/3  Lupi. 

5 

2.90 

6 

3.21 

10 

3.22 

1 1 

3.00 

12 

3.02 

14 

3-39 

26 

3.16 

42 

3.22 

3.14 

f3  Muscae. 

6 

3.63 

14 

3.82 

25 

3.60 

35 

3-5* 

38 

3.81 

42 

3.66 

43 

3.60 

3.67 

(3  Normae. 
23  4.68 

(3  Octantis. 
17  4.50 

(3  Triang. 

6  3.30 

14  3-55 
23  3.50 

4*  3-55 
43  3-4° 

3.46 

(3  Pavonis. 

17  3.91 
27  4.01 

*  3-96 

(3  Pegasi. 
16  2.78 

i3  Tubi. 
2      s|t  3.76 

(3  Ursae. 

45  2-78 

46  2.76 

2.77 

(3  Phoenicis. 

3  3-54 
21  3.84 
30  4.01 

3.80 

/3  Ursse  Min. 
46  2.46 
Variable. 

/3  Virginis. 
41  4.14 

f3  Pictoris. 
36  4.23 

(3  Volantis. 

9  4-5> 
21  4.51 
30  4.68 
36  4.51 

4-57 

(3  Reticuli. 

6  4.39 
21  4.52 
30  4.58 
35  4-56 
37  4-58 

4-53 

y  Apodis. 
8  4.82 

(3  Scorpii. 

1  2.9X 
26  2.88 
42  3.02 

2.96 

y  Aquilae. 

17  3.41 
27  2.73 

3.07 

Very  doubtful. 

26  4.OO 

y  Arse. 
42  3.82 

(3  Tauri. 
39  2.20 
45  2-48 

2.34 

y  Argus. 

5  2.06 

6  2.11 

7  2.11 
13          2. 11 
19  2.22 

21  2.13 

22  1.92 

23  2.01 

24  2.01 

25  2.01 

32  2. ii 

33  2.10 

(3  Toucani. 

3  3-8' 
2 1  4-°4 
30  4.15 

4.00 

NUMERICAL  MAGNITUDES. 


343 


34 

2.04 

35 

2.25 

36 

2.09 

38 

1.9 1 

39 

2.16 

40 

2.01 

41 

2. 1 1 

42 

2. 1 1 

43 

2.01 

44 

2.17 

2.08 

7 

Bootis. 

45 

3.40 

46 

3.36 

*  3-38 

y  Canis. 


'9 
39 
4i 


3-72  + 
4.81  + 
4.58 


*  4-7° 
Rejecting  3.72+ 


y  Capricorni. 
27      *  3.98 


7 

Centauri. 

5 

2.72 

6 

2.27  :: 

7 

2.87 

10 

2.71 

1 1 

2.71 

12 

2.57 

13 

2.71 

14 

2.71 

22 

2.71 

23 

2.71 

33 

1.82 

4i 

2.72 

42 

2.71 

43 

2.62 

2.68 

y  Ceti. 
30  4.24 


r 

9 
38 
43 


Chamael. 

4.65 

4-73 
4.91  + 

*  4.76  + 


7  Coeli. 
37  4-92 


y  Columbae. 
37  4-91 


y 

Corvi. 

7 

2.70 

14 

2.91 

22 

2.86 

23 

2.90 

35 

2.97 

42 

2.90 

43 

2.96 

45 

3.02 

46 

2.90 


2.90 

r 

Crateris. 

35 

$  4.62 

r 

Crucis. 

5 

1.72 

6 

1.72 

7 

1.72 

13 

1.72 

22 

2.30 

33 

1.86 

34 

1.72 

36 

1.72 

38 

1.72 

39 

1.72 

41 

1.72 

42 

1.72 

43 

1.72 

i-73 

Rejecting  2.30. 

7 

Doradus. 

21 

4.87 

30 

4.83 

37 

4.87 

4.86 

r 

Eridani. 

28 

3-93 

31 

3-95 

*  3-94 

7 

Geminor. 

7 

2.40 

J9 

2.52 

36 

2.50 

39 

2.50 

43 

2.62 

46 

2.50 

2.51 

y  Gruis. 

16 

3.65 

17 

3-57 

21 

3.70 

27 

3.44: 

30 

3.94: 

3.66 

7 

Hydra;. 

3.28 

42 

3.52 

43 

3-57 

3.46 

7 

Hydri. 

3 

3.75 

6 

3-75 

16 

3-75 

17 

3.68 

21 

3.60 

30 

3-77 

35 

3-77 

36 

3.70 

37 

3-75 

38 

3.70 

39 

3-75 

3.72 

7 

Leonis. 

4 

2.42 

7 

1.95 

38 

2.53 

40 

2.36 

43 

2.42 

45 

2.42 

46 

2.29 

2.34 

Rejecting  1.95. 


7 

Leporis. 

20 

4.12 

32 

3.87 

j|e  4.00 

y 

Librce. 

26 

*  *  4-44 

t  Lupi. 

5 

3.20 

6 

3.38 

10 

3.38 

1 1 

3.38 

12 

3-38 

14 

3-45 

26 

3.38 

42 

3-36 

3.36 

7 

Muscae. 

'4 

4.66 

38 

4.70 

43 

4.64 

4.67 

7 
'9 

20 
21 
32 
33 
34 
35 
36 
38 
43 


Orionis. 

2.08 
1.92 

i-77 
2.3 1 
2.42 
2.42 
1.97 
1.99 
2.09 
2.23 
1.90 

2.10 
Variable  ? 


y  Pavonis. 

4.62 
3.56 


17 

27 


*  4.09 

Very  doubtful  or 
variable. 


y 

Pegasi. 

16 

3.05 

7 

Phcenicis. 

3 

3.6 1 

21 

3.90 

3° 

4.10 

3.87 

7 

Pictoris. 

34 

4'95 

r 

Reticuli. 

30 

4.98 

37 

4.91 

4-95 

7 

Sagittar. 

2 

*  3.58 

7 

Scorpii. 

26 

3.98 

7 

Serpentis. 

26 

*  *  4-36 

7 

Toucani. 

21 

4.44 

30 

4-43 

4.44 

42 


Trianguli. 

3.52 
3.50 
3.52 
3-48 
3.52 

3-5i 


Tubi. 
3.62 
3.82 

3.70 

*  3-7i 


Ursse. 


45 
46 


2.62 
2.80 

2.71 


y  Virginis. 


7 

3.05 

14 

3.08 

22 

2.95 

23 

3. 11 

25 

3-45 

38 

3.00 

42 

2.93 

45 

3.17 

46 

2.97 

3.08 

y 

Volantis. 

6 

4.62+ 

21 

4.28 

30 

4-37 

34 

4.50 

35 

4-37 

36 

4.28 

37 

4-35 

38 

4.28 

39 

4.28 

41 

4.28 

43 

4.28 

4-35 

8 

2  Apodis. 

0  Argus. 


43 


4.64 


8  Aquarii. 

3-79 
3.80 


27 
31 


3.80 


8  Aquilse. 
18  3.64 


5 

2.44 

6 

2.44 

7 

2.58 

'3 

2.44 

21 

2.44 

34 

2.35 

35 

2.29 

36 

2.44 

37 

2.44 

38 

2.34 

39 

2.40 

41 

2.44 

42 

2.44 

43 

2.44 

2.42 

8  Bootis. 
45  3-70 


8  Canis. 


7 

2.34 

19 

2.35 

20 

2.40 

21 

2.13 

32 

2.34 

33 

2.16 

34 

'  2.26 

35 

2.45 

36 

2.32 

37 

2.30 

38 

2.27 

39 

2.26 

40 

2.50 

41 

2.34 

43 

2.34 

2.32 

8  Capricorni. 


27 

3.20 

s 

Centauri. 

5 

2.96 

6 

2.92 

13 

3.00 

14 

3.00 

22 

2.95 

38 

2.92 

41 

3.10 

42 

3.10 

43 

3.00 

2.99 

8  Ceti. 

30 

4.71 

8  Chamsel. 
4.88 


38 
43 


4-75 
4-55 

4-73 


344 


FINAL  CONCLUSION  OF 


8  2  Columbae. 
37  4-97 

8  Corvi. 


7 
i4 
22 
23 

35 
42 

43 
45 
46 


3.20 
3-a5 
3-!5 
3. 11 
3.25 
3.40 
3. 11 
3.25 
3.25 

3.22 


8  Crucis. 


6 

22 
23 
34 
35 
38 
41 
42 

43 


21 

3° 
34 


8  Crateris. 

5  3-8o 

1  3-86 

1  3-85 


3.58 
3.31 
3.60 
3.60 
3.60 
3.62 
3.67 
3.60 
3.46 
3.67 

3-57 


5  Doradus. 


4.90 
4.92 
4-85 

4.89 


8  Eridani. 

28  4.37 
29 
3' 


4-33 
4.26 


*  *  4-32 


8  1  Gruis. 

3  4-3° 

8  2  Gruis. 
3  4-36 

8  Horolog. 
37  4-95 


0  Hydrae. 
35    *  4-66 


3 
21 

30 
37 


Hydri. 

4.48 
4.60 
4.29 
4-43 

4-45 


5  Leonis. 


7 
45 
46 


2.95 
2.96 
2.85 

2.92 


8  Leporis. 
20  4-15 


8  Lupi. 


10 

3-95 

1 1 

3-93 

12 

3-93 

14 

3.85 

26 

3-95 

42 

4.03 

3-94 

8  Muscse. 


6 

4.62  + 

8 

4-79- 

Mean 

4.71 

14 

4.60 

38 

4.67 

43 

4.40 

* 

4.60 

8  Ophiuchi. 


26 


3.00 


8  Orionis. 


7 
'9 
20 
21 
32 
43 


2.30 
2.55 
2.74 
2.65 
2.79 
2.62 

2.61 


8  Pavonis. 
17  4.00 


8  Phoenicis 

3 


30 


3.92 
4.18 
4-75 

4.28 
Doubtful. 


S  Reticuli. 
30  5-02+ 


37 


4.96 
4-99  + 


8  Sagittar. 
2.99 

3-35 
2.99 

*  3-u 


2 

17 
18 


15 
26 
42 


8  Scorpii. 
1  2.86 
2.86 
2.84 
2.86 


8  Serpentis. 
26  *  *  4.14 


8  Toucani. 
30  4-62 


8  Virginis. 
23  3-9° 


8  Volantis. 


21 

30 
34 
43 


4-54 
4.56 
4.69 
4.64 

4-59 


5 
6 

7 
13 
21 

33 
34 
36 

38 
39 
40 

41 
42 

43 
44 


s  Bootis. 


45 
46 


Canis. 


t  Argus. 

2.17 
2.17 
2.17 
2.17 
2.21 
2.27 
2.17 
2.17 
2.10 
2.08 
2.17 
2.23 
2.30 
2.17 
2.17 

2.18 


2.70 
2.72 

2.71 


7 

1.89 

'9 

1.89 

20 

1.77 

2 1 

1.77 

*5 

1.89 

32 

1.89 

33 

1.74 

34 

1.88 

35 

1.99 

36 

1.77 

37 

1.89 

38 

i-75 

39 

1.89 

41 

1.89 

43 

1.94 

44 

1.89 

1.86 

£  Centauri. 

5  *-83 

6  2.83 

0  2.83 

1  2.81 
2.82 
2.80 
2.80 
2.86 
2.80 
2.84 


2.82 


t  Ceti. 
28    *  4-87 


*  4.86+ 


Columbse. 


37 

4-39 

c 

Corvi. 

14 

3.22 

22 

3-31 

23 

3-31 

25 

3-31 

35 

3.48 

38 

3.00 

42 

3.16 

43 

340 

45 

3.31 

46 

3-3' 

3.28 

t  Crucis. 

6  4.60 

14  4.60 

22  4-60 

23  4.60 


35 
38 
43 


4.60 
4.60 
4.64 

4.61 


21 

30 
34 


Doradus. 

4.96 
4.96 
4.96 


4.96 


£  Eridani. 
28  4.46 
3 1  4-34 

*  4-4° 


t  Gruis. 


27 
30 


3-33  ? 
3.98 
3.88 
4.05 


3-97 

Rejecting  3.33 


£  Hydrae. 
35  3-72 


£ 

Chamsel. 

3 

8 

4.91  + 

21 

38 

4.76 

30 

43 

4.914- 

37 

Hydri. 


4.44 


£  Leonis. 
45     *  343 


£  Leporis. 


20 
37 


3.85 
3.84 

3.84 


£  Lupi. 


10 
1 1 
12 

26 


4.02 
4.05 
4.05 
3.89 
4.02 

3-99 
4.00 


l 

Orionis. 

7 

2.00 

'9 

1.97 

20 

1.89 

21 

1.89 

32 

1.77 

33 

1.40 

34 

1.88 

35 

i-77 

36 

1.89 

38 

1.85 

39 

1.77 

43 

1.84 

£ 

Pavonis. 

17 

*  4-33 

1 

Pegasi. 

l6 

2.51 

27 

2.62 

2.56 

£ 

Phoenicis. 

3 

3-97 

21 

4.36 

30 

4.50 

4.28 

i 

Reticuli. 

» 

4-95 

30 

5.02+ 

37 

4-95 

£  Ophiuchi. 
26  4-oc 


*    4-97  + 


4.42 
4.58 
4.29 
4.48 

  £  Sagittarn. 


15 
16 
18 


2.27 
2.23 
2.26 
2.28 

2.26 


f  Scorpii. 

1  2.78 
2.58 

42  2.78 
2.71 


£  Serpentis. 
26  *  *  4.27 

£  Toucani. 

3  4-96 
21 

3° 


4.70 
4-97 

4.88 


NUMERICAL  MAGNITUDES. 


345 


e  Ursae. 


44 

45 


i-97 
1.79 


t  Virginis. 
45  3-" 

s  Volantis. 


4.84 
4.85 
4.90 
4.82 

4.85 


30 

34 
36 


Z  Aquilse. 
18  *  #  3.45 


Z  Argus. 


5 
6 

*9 

20 

24 
*5 
32 
33 
36 

37 
38 
39 
41 
43 


2.74 
2.74 
2.75 
2.67 
2.74 
2.74 
2.74 
2.74 
2.69 
2.74 
2.66 
2.66 
2.74 
2.74 

2.72 


Z  Canis. 


J9 

3-65 

20 

3.69 

21 

3.66 

27 

3.40 

37 

3.69 

39 

3.69 

3-63 

2.91 

3.02 


Z  Ceti. 
28    *  4.: 


Z  Crucis. 
9  4-56 


38 


4.87 
4.71 


Z  Doradiis. 
21  4.93 
36  4-95+ 

*  4.94+ 


Z  Gruis. 
3  4-!9 


Z  Hydra?. 

35  3-44 
37  3-71 
43  3-*1 

3-45 


Z  Hydri. 

3  5-°2 

21  4.92 

30  5.02 

37  5-°2 

5.00 


Z  Leporis. 
20  3.99 


Z  Lupi. 


6 

4.44 

10 

4.07 

1 1 

4.00 

12 

4.01 

14 

4.05 

42 

4.07 

4.1 1 

Z  Centauri. 

5  2.96 
5  2.94 


12 

3.18 

7 

2.09 

13 

2.88 

J9 

2.16 

14 

2.88 

20 

2.13 

22 

3.04 

21 

1.97 

26 

2.80 

3* 

2.04 

42 

2.88 

33 

1.95 

43 

3. 11 

34 

1.88 

35 

1.99 

2.96 

36 

1.97 

Z  Ophiuchi. 
26  2.97 


Z  Orionis. 


38 
39 
43 


1.99 
1.97 


Z  Pavonis. 
17  4.56 


Z  Phoenicis. 

3  4-°3 
30  4.47 


4.25 


Z  Sagittar. 
2 
17 


2.79 
3.24 

3.01 


Z  2  Scorpii. 
42  4-34 


Z  Toucani. 

3  4.62 
21  4.62 
30  4.90 

4.71 


Z  Ursae. 


45 


2.45 
2.54 

2.50 


Z  Virginis. 

3.70 
4.06 


23 
26 


jj  Canis. 


19 

2.96 

20 

2.84 

32 

2.84 

36 

2.80 

38 

2.88 

J7 

2.82 

41 

2.84 

43 

2.83 

2.85 

n 

Centauri. 

5 

2.96 

6 

2.93 

10 

2.88 

1 1 

2.91 

12 

2.91 

13 

2.91 

14 

2.90 

26 

2.91 

42 

2.91 

2.91 

jj  Ceti. 

28  4.03 
31  4.09 

tfc  4.06 


jy  Crucis. 
9  4.60 


jj  Eridani. 
28  4.63 
31  4.38 

*  4-5° 


i)  Hydra;. 
35     *  4-67 


jj  Leporis. 
20  4-°9 


Z  Volantis. 
21  4.73 

3°  4-73 
34  4.60 

36  4-73 
39  4-73 

4.71 

j]  Lupi. 

11  4.10 

12  4.10 
23  4.10 

4.10 

jj  Ophiuchi. 

t]  Bootis. 

26  2.89 

26  3-°4 
45  3-°8 

jj  Orionis. 

3.06 

20  3.92 

jj  Phoenicis. 

4-55 
4.78 


3 
30 


4.66 


jj  Scorpii. 
42  3.80 

tj  Serpentis. 
18  *  *  3-51 


tj  Toucani. 

3  5-oa 
30  5.00 

5.01 


jj  Ursae. 
45  2-'3 


jj  Virginis. 


23 
42 


4.00 
4.62+ 

4-3  !  + 


0  Aquilse. 
18  *  *  3-57 


9  Argus. 


6 

14 

38 
42 

43 


3.42 

3-34 
3.22 
3.00 
3.31 

3.26 


9  Canis. 
39  4.81  + 

41  4-55 

*    4.68  + 


9  Centauri. 


1 1 
12 
r3 
14 

22 
26 
40 
42 
45 


2.55 
2.55 
2.45 
2.55 

2-55 
2.70 
2.55 
2.55 
2.55 
2.55 
2.42 
2.55 
2.55 

2.54 
4 


9  1  Ceti. 
28      *  4-33 


9  Chamael. 

8  4.91 
4.91 
4.91 
4.91 


38 
43 


4.91 


9  Columbas. 
37  4-98 


9  Doradus. 
34  4-94 

9  Eridani. 


28 
30 
37 


3-73 
3-73 
3-73 
3-73 

3-73 


9  Gruis. 


3 

4.25 

6 

Librae. 

26 

*  *  4-63 

9 

Phoenicis. 

3 

4.82 

6 

Scorpii. 

1 

2.28 

2 

2.27 

6 

2.37 

r5 

2.32 

16 

2.28 

18 

2.26 

26 

2.28 

42 

2.28 

2.29 

t 

Argus. 

5 

2.72 

6 

a-73 

!3 

2.73 

14 

2-73 

36 

3.00 

38 

2.95 

39 

2.90 

42 

2.72 

43 

2.73 

2.80 


346 


FINAL  CONCLUSION  OF 


Centauri. 


s 

3-23 

6 

3.23 

IO 

3.21 

3.02 

12 

3.18 

1  + 

3.08 

22 

3-45 

42 

3.16 

45 

3.22 

3.20 

t 

Eridani. 

3° 

4.60 

Gruis. 

3 

3-47  ? 

21 

4.48 

3-97 

Very  doubtful. 


1  Hydra;. 

35  4-63 

36  4-J7 
41  4.38 

4-39 


1  Leonis. 
46  4.22 

t  Leporis. 
37  4-88 


Lupi. 


6 
10 
12 
42 


4.23 
4.29 
4.17 
3-95 

4.16 


1  Orionis. 


"9 

20 
32 
39 


3.58 
3.30 
3-3° 
3-32 

3-37 


i  Phoenicis. 
3  4-75 


t  Pise.  Aust. 
3  4-69 


t 

Scorpii. 

I 

3-45 

42 

3.61 

3-53 

( 

Reticuli. 

30 

5.02  + 

37 

5.01 

*  5-0I  + 

t 

Virginis. 

26 

*  *  4.48 

k  Argus. 

5 

0 

3.04 

J4 

3.04 

36 

2.85 

38 

2.82 

39 

2.75 

42 

2.98 

43 

3.04 

2.94 

K 

2  Canis. 

25 

4.04 

39 

4.28 

4.16 

K 

Centauri. 

5 

3.24 

6 

3-47 

10 

3.66 

1 1 

3.66 

12 

3.66 

14 

3-79 

42 

3.67 

3.60 

K 

Columbse. 

25 

*  4-9 1 

K 

Eridani. 

3 

4.14 

21 

4-33 

30 

4.65 

37 

4.83 

4.51 

K 

Leporis. 

37 

4.88 

k  Phoenicis. 

3  4.08 
i  1  4.40 
4.81 


30 


4-43 
Doubtful. 


k  Scorpii. 
1  2.86 
2.79 
2.93 
3.07 


26 
42 


2.91 


k  Virginis. 
26   $  sj<  4  56 


X  Aquilse. 
18   **  3-57 

X  Argus. 


6 

2.32 

'3 

2.48 

24 

2.48 

34 

2.48 

36 

2.48 

37 

2.48 

38 

2.48 

41 

2.48 

42 

2.48 

43 

2.48 

2.46 

f.'  Lupi. 

X  Canis. 

10 

4.40 

25  4.16 

12 

4.32 

14 

26 

4.61 
3.96 

X  Centauri. 

6  3.84 

4.32 

14.  \.CQ 

K 

Ophiuchi. 

42  3.64 

26 

3-97 

3.70 

K 

Orionis. 

X  Eridani. 

7 

!9 

2.52 
2.66 

37  4-97 

20 

21 

2.59 
2.59 

X  Gruis. 

30 
32 

2.58 
2.59 

3  489 

33 

2.59 

35 
36 

2.59 
2.60 

X  2  Hydra;. 
35  4-i8 

2.59 

41  4.24 

43  4-i8 

X  Bootis. 
45  4»6 


4.20 


X  Leporis. 
37  4-9° 


X  Lupi. 
4.76 
4-59 

4.67 


X  Ophiuchi. 
26   *  *  4.32 

X  Orionis. 
201  4.05 


X  Phcenicis. 


3 
30 


5.02  + 
4.99 

*  5.00  + 


X  Sagittar. 
2  3.13 

X  Scorpii. 

1.78 


6 

15 
16 
18 
42 


2.20 
1.61 
1.95 
1.97 
1.86 

1.87 


X  Virginis. 
26   sjj  %  4.63 

ft  Argus. 


6 

3-!3 

H 

2.86 

25 

3.10 

35 

3.23 

36 

3.08 

38 

3.08 

41 

3.06 

42 

3.04 

43 

3.11 

3.08 

Centauri, 

6 

3.92 

10 

3.92 

11 

3-93 

1 2 

3-93 

14. 

34 

3-93 

35 

3.88 

42 

3.91 

3-93 

ju  Ceti. 

31 

*  4-59 

/* 

Columbae. 

37 

5.01 

P- 

Eridani. 

20 

4.19 

37 

4.6; 

4.42 

Hydrae. 

35 

4.61 

41 

4-35 

*  4-48 

Leporis. 

20 

3.92 

37 

3.87 

3.90 

u  Lupi. 

1 1 

4.27 

12 

4-47 

4-37 

Phcenicis. 

3 

>):  5.02 

H 

1  Scorpii. 

I 

3.98 

42 

3-37 

**  3.67 

2  Scorpii. 

1 

%  s(c  4.16 

Serpentis. 

26 

3-99 

H  Ursa;. 

45 

*  3-35 

Virginis. 

26 

*  *  4-4° 

1 

'  Argus. 

20 

3.82 

21 

3.68 

24 

3.26 

25 

3-73 

36 

3-73 

43 

3-72 

3-74 

Rejecting  3.26 

V 

2  Canis. 

39 

4-75 

V 

Centauri. 

6 

3-93 

10 

3-93 

1 1 

3-93 

12 

3-93 

*4 

4.15 

34 

3.92 

35 

3-97 

42 

3.88 

3-95 

V 

Doradiis. 

34 

4-94 

V 

2  Eridani. 

20 

4.02 

37 

4-5° 

4.26 

V 

Hydra;. 

22 

3-3' 

35 

3.69 

36 

3.76 

41 

3-58 

43 

3.67 

3.60 

NUMERICAL  MAGNITUDES. 


347 


v  Octantis. 


17 

*  4. 1 1 

V 

Scorpii. 

I 

4.58? 

42 

3.42 

%  H«  4-oo 

Very  doubtful. 

1 

Tauri. 

31 

*  4-4° 

<r 

Argus. 

20 

3.72 

25 

3-77 

4-1 

3-74 

3-74 

?  2 

Centauri. 

34 

4-77 

K 

2  Ceti. 

31 

*  4.49 

5  Hydrae. 


23 
41 


4.15 
3-95 

4.05 


§  Horolog. 


21 

30 


5.00 
5.00 

5.00 


§  Scorpii. 
26  4.63 

5  Tauri. 
31      *  4.36 


?  Ursa;. 
45      *  4-2° 

o  Argus. 
36  3.99 

0  1  Canis 


0  2  Canis. 


x9 

20 
25 
38 
39 
41 


3.72 
3.76 
3.70 
3-79 
3-77 
3.76 

3-75 


o  Tauri. 
31      #  4.52 


20 
24 
25 
32 
36 
38 
41 
43 


it  Argus. 

3.10 
2.96 
2.90 
2.96 
2.93 
3.18 
2.96 
2.89 


7r  Ceti. 
28  4.67 
31  4-45 


*  4-56 


Hydra;. 


42 


3.70 
3-79 

3-75 


10 
1 1 


tt  Lupi. 

4.51 
4.67 
4.40 

*  *  4-53 


tt  Ophiuchi. 
18    tfc  >jc  3.05 


7r  Sagittarii. 


'7 


3.27 
3.52 


3.40 


7r  Scorpii. 


1 

3-37 

25 

4.30 

26 

3-38 

39 

4-43 

42 

3-3° 

4.36 

3-35 

p  Argus. 


!9 

25 
41 

43 


3.32 
3.52 

3-34 
3.11 

3.32 


p  Centauri. 
23      *  4-63 

p  Ceti. 
28      *  4.87 

p  Lupi. 


1 1 

34 


4.88 
4.72 


**  4-S 


p  Scorpii. 

i  4.42 
26  4.52 

*  *  4-47 


<r  Argus. 


20 

3-79 

24 

3-79 

25 

3-79 

32 

3-79 

36 

3-79 

37 

3-79 

43 

3-79 

3-79 

a 

Canis. 

25 

3-79 

39 

4.06 

3.92 

a  Centauri. 


34 
38 


4.96  + 
4.66 

*  4.81  + 


<r  Eridani. 
3 1  442 


rs  Sagittarii. 

2  2.58 

ts  2.36 

[6  2.38 

[8  2.38 

•.7  2.38 

2.41 


Scorpii. 

I 

3-45 

23 

3.38 

26 

3.38 

42 

3-77 

3-5° 

r 

Argus. 

6 

3-55 

2  I 

3.50 

24 

3-55 

25 

3.66 

32 

3-55 

35 

3.36 

36 

3-36 

3-5° 

t  Ceti. 

28 

H«  4.28 

T  I 

Eridani. 

28 

4.86 

31 

4-57 

*  4.71 


t  Hydri. 
37    *  5-01 


t  Orionis. 
20  4.25 

r  Scorpii. 

1  3-45 
3-45 
3-38 
3.46 

3-44 


23 
26 
42 


v  Argus. 

3.66 

3-5° 
3.16 
3.61 

3-58 
3.58 
3.58 
3-58 

3-53 


34 


1  Centauri. 

4-34 
4-55 
4.91 


4.60 


v  1  Hydra;. 

35  4-64 
41  4.52 

4.58 


v  Pictoris. 


25 
37 


4.32 
4-79 

4-54 


v  Scorpii. 
1  3.37 


<p  Argus. 


6 
25 


4-32 
4-34 

4-33 


<p  Centauri. 

6  4.62 
12  4.62 

34  4-3° 
42  4.62 

4-54 

Sequences  10,  11, 
1 4  are  allowed  no 
influence. 


<p  Eridani. 

!  3-68 
3-94 


4.20 
4.07 


4.00 


<p  Leonis. 
41  4-72 


<p  1  Lupi. 

0  4.18 

1  4.10 
a  4.25 

4.18 


f  Phcenicis. 
3     *  5.02 


0  Sagittarii. 


3.71 
3.83 


2 
17 


*  3-77 


ip  Argus. 


25 

37 
38 
41 
43 


4-35 
4.28 

4-35 
4-35 
4.18 

4.30 


\p  Centauri. 

I  I     >)S    5fc  4.84 


i/<  Eridani. 
37  4-99 


4>  Ursse. 


45 
46 


3-33 
3.40 

3.36 


X  Argus. 


6 

4-°3 

36 

3-93 

38 

4.05 

39 

4.06 

41 

4.05 

43 

4.05 

4-°3 

X 

Eridani. 

3 

3.86 

21 

4.09 

3° 

4-33 

4.09 

Argus. 


6 

3.80 

14 

3.66 

36 

3.25 

38 

3.83 

39 

3.85 

41 

3.83 

42 

3-83 

3.72 

tii  Canis. 

25 

*  4-93 

hi 

1  Scorpii. 

I 

*  *  4-5° 

a 

Carinse. 

6 

4.62+ 

36 

4.05 

*    4-33  + 


348 


FINAL  CONCLUSION  OF 


a 

Centauri. 

1 1 

*  *  4.86 

a  Mali. 

4-33 

36 

4.1 1 

38 

4.64 

41 

4.38 

43 

4.60 

4.41 

a  Puppis. 

6 

4.31 

25 

4-31 

4.31 

a 

Velorum. 

36 

4.86 

b  Centauri. 

1 1 

*  *  4-73 

b  Mali. 

25 

4.81 

36 

4.81 

39 

4.81 

41 

4.81 

43 

4.81 

4.81 

b  Velorum. 

36 

4.89 

c 

3  Aquarii. 

31 

*  4-3° 

c  ) 

Centauri. 

1 1 

4-75 

c  Mali. 

25 

4.81 

41 

4.62 

43 

4.91  + 

*  4-78+ 


c  Puppis. 
25  3.91 


(1  Centauri. 


1 1 

34 


4.70 
4.92 

*  *  4-8 1 


d  Eridani. 
31     *  4.55 


d  Scorpii. 
26  4.10 


e  Eridani. 
37  4-8' 


f  Centauri. 
34  4-8i 


f  Eridani. 


30 
37 


5-01 
4.69 

4.85 


f  Sextantis. 
41  4.66 


g  Centauri. 
1 1       s(c  4.78 


g  Eridani. 
28  4.81 
37  4-53 

*  4.67 


h  Eridani. 
37  4-8 


i  Centauri. 
11  *  *  4-82 


k  Centauri. 
11  sfc  H<  4-8o 


k  Puppis. 

20  4.29 
41  4.29 

4.29 


1  Carina?. 


6 
38 


4.13 
4.63 

4.38 


1  1  Eridani. 
28    *  4.88 


1  2  Eridani. 
28    *  4-89 


m  1  Eridani. 

28  4.85 
31  4.51 

*  4.68 


n  Centauri. 
34  4-93 


o  Scorpii. 
26  4.19 


p  Carina?. 

6  3.85 
14  3.96 
38  4.61 

3-9° 

Rejecting  4.61. 
(Full  moon.) 


p  Puppis. 
15    *  4-96 


p  Sceptri. 
37  4-62 


p 

Velorum. 

2  S 

J 

A.  CO 

q 

Carina?. 

6 

3.86 

I4 

3-99 

38 

3-73 

39 

3-76 

41 

3.76 

42 

3-76 

3.81 

q 

Monocer. 

41 

4.41 

q 

Orionis. 

20 

3-51 

q 

Velorum. 

25 

4.65 

36 

4.92 

41 

4.48 

*  4.68 

r  Lyncis. 

45 

*  3-38 

r 

Orionis. 

20 

3.89 

r 

Sceptri. 

37 

4-93 

s  2  Eridani. 

(16  Fl.) 

4-59 
4.28 


3i 


*  4-43 


t  Eridani. 


28 
3i 


4-74 
4-53 

*  4-63 


u  Carina?. 
38  4.51 

x  Carina?. 
38  4-83 


y  Eridani. 
37  4-8; 


z  1  Centauri. 
41  4.78 


z  Orionis. 


34  4-95 

C  Carina?. 
34  4-95 

E  Eridani. 
28  4.78 
3 1  4-47 

*  4.62 


I  Carina?. 
38  4.69 


L  Puppis. 
20  4.22 


N  Velorum. 


14 

38 
42 


3.70 
3.62 
3.60 
3.50 

3.60 


O  Cruris. 
14  4.61 

V  Centauri. 
34  4-9° 

Y  Eridani. 
37  4-75 


3  Fl.  Argus. 
41  4.44 


20  3.95 

10 

Fl.  Tauri. 

z  Virginis. 

31 

*  4-43 

26  *  *  4-23 

B 

A  C.  956. 

21 

5-°3 

B  Carina?. 

B  A  C.  1 103. 
21  5.00 
30  4.99 


5.00 


B  A  C.  2562. 
25  4-32 


B  A  C.  3984. 
6  4.62  4- 

38  4.43 

*    4-52  + 


NUMERICAL  MAGNITUDES. 


349 


(256)  It  will  not  be  uninteresting  if  we  now  compare  the  values  thus  directly  deduced  from 
the  observed  sequences,  with  the  provisional  magnitudes  assigned  in  our  normal  sequence  B  from 
which  they  have  originated.  For  this  purpose,  confining  ourselves  in  the  first  instance  to  the 
stars  of  that  sequence  which  are  printed  in  italics,  and  which  occur  in  the  original  normal 
sequence  A,  118  in  number,  and  comparing  their  magnitudes  in  B  and  C  seriatim,  we  find  the 
following  distribution  of  the  amounts  of  discordance  between  the  two  series  exclusive  of  stars  of 
the  first  magnitude  brighter  than  Regulus : — 


Cases  of  exact  agreement,        ........  22 

Cases  of  disagreement  under  one-twentieth  of  a  magnitude,  .  .  .  .64 

Disagreements  of  one-twentieth,  but  under  one-tenth  of  do.  .  .  .  .26 

Do.  one-tenth,  but  under  one-eighth  of  do.  .  .  .6 


118 

In  no  instance  then,  among  these  stars,  does  the  magnitude  finally  resulting  differ  from  that 
provisionally  adopted  to  the  extent  of  one-eighth  of  a  magnitude. 

(257)  If  we  next  compare,  in  the  same  manner,  the  remaining  stars  of  the  list  B,  142  in 
number,  we  find  as  follows : — 


Cases  of  exact  agreement,        ........  9 

Disagreements  under  one-twentieth  of  a  magnitude,   .  .  .  .  .53 

Do.         of  one-twentieth,  but  under  one-tenth  of  do.   .  .  .  .  31 

Do.         of  one-tenth,  but  under  one-fifth  of  do.  .  .  .          .  37 

Do.         of  one-fifth,  but  under  one-third  of  do.  .  .  .  .10 

Do.         of  one-third,  but  under  one-half  do.  .  .  .  .2 


142 

Thus  we  see  that  there  are  only  12  cases  of  discordance,  to  the  extent  of  one-fifth  of  a  magnitude, 
between  the  provisional  and  adopted  magnitudes  out  of  the  whole  number  of  260  stars  compared, 
— and  these  are  no  more  than  might  reasonably  be  expected, — when  it  is  recollected  that  the 
list  B  contains  numerous  stars  which  had  been  struck  out  of  A  not  merely  for  want  of  connexion, 
but  on  account  of  actual  discordances  between  the  corrected  sequences,  of  the  kind  alluded  to  in 
Art.  (234).  The  two  worst  cases,  in  which  the  discordance  amounts  to  0.40  and  0.41  respec- 
tively, are  those  of  rj  Virginis  and  y  Aquilae.  In  both  cases  the  discordance  arises  from  widely 
deviating  observations  being  included  in  the  final  mean,  which  had  no  share  in  determining  the 
provisional  value. 

(258)  Several  of  the  stars  in  Table  C  are  marked  as  variable,  or  possibly  so.  Two  of  the 
most  remarkable  are  a  Hydras  and  /3  Ursse  Minoris.  As  regards  a  Hydrae,  in  December  1837, 
and  January,  February,  and  March  1838,  it  was  made  the  subject  of  frequent  comparisons  with 
e  Argus,  5  Canis,  and  b  Argus,  the  first  of  which  stars  (Mag.  2.18)  it  equalled  at  its  maximum, 
the  second  (2.32)  in  its  medium  state,  and  the  last  (2.42)  at  its  minimum,  with  a  period  of  about 
twenty-nine  or  thirty  days.  At  the  time  I  regarded  the  observations  as  satisfactory,  and  the 
result  as  sufficiently  established :  but  the  occurrence  of  a  similar  phenomenon,  with  a  period 
nearly  identical  in  the  case  of  a  Cassiopeia?,  the  period  in  both  cases  being  nearly  a  lunation, 
inclines  me  to  distrust  both  conclusions,  and  to  believe  that  the  colour  of  the  stars  (in  both  cases 

4  u 


350 


FINAL  CONCLUSION  OF 


verging  to  redness)  has  affected  the  judgment  in  the  presence  of  moonlight  differently  from  that 
of  the  stars  of  comparison.  Such  at  least  is  undoubtedly  the  case  with  a  as  compared  with 
y  Cassiopeia?,  a  white  star,  e  and  b  Argus  are  both  red,  however,  but  even  in  their  cases  a 
difference  in  their  proximity  to  the  moon  might  influence  the  observation. 

(259)  The  case  of  j3  Ursae  Minoris,  however,  admits  of  no  doubt  being  raised  on  this  score. 
It  is  now,  while  I  write  (May  14,  1846),  so  far  inferior  to  Polaris  in  the  absence  of  the  moon, 
and  at  a  higher  altitude,  that  no  observer,  however  unpractised,  could  hesitate  as  to  their 
relative  rank.  The  reverse  was  the  case  in  1840  and  1841,  in  the  former  of  which  years  I  find 
/3  placed  uniformly  above  a  (Polaris)  in  ten  sequences  observed  on  Jan.  2,  5  ;  April  30;  May  1, 
3 ;  Aug.  3,  4,  5,  23 ;  and  Nov.  27,  while  in  the  latter  of  these  years,  the  same  order  of  pre- 
cedence obtained,  and  was  so  recorded  on  the  19th  and  20th  of  August,  and  in  one  undated 
sequence  between  July  16  and  Aug.  18.  The  difference  of  brightness  on  May  3,  1841,  is  called 
"  one  step,"  and  on  Aug.  23  "  at  least  a  grade,"  intending  by  these  expressions  a  difference 
sufficiently  palpable  to  admit  of  no  hesitation. 

(260)  In  1838  and  1839,  the  difference  seems  to  have  been  somewhat  less  striking.  On 
Jan.  16,  1839,  I  find  it  recorded  that  /3  surpassed  a  by  a  "  small  grade."  In  the  sequence  (No. 
46,  of  April  15,  1838),  the  difference  as  concluded  from  the  interpolated  magnitudes  was  only 
0.13  mag.  In  that  observation,  Polaris  was  only  18°  high,  and  j3  considerably  more  elevated, 
and  it  may  therefore  be  presumed  that  the  stars  were  then  not  far  from  equality.  In  corro- 
boration of  this,  I  shall  take  the  liberty  of  translating  a  passage  from  a  letter  addressed  to  me  by 
M.  Struve  on  the  5th  Dec.  1838,  in  effect  as  follows:  "  I  would  call  your  attention  to  two  stars. 
Has  not  Capella  been  during  several  years  in  a  state  of  increase?*  and,  again,  a  Ursa?  Minoris 
(Polaris)  is  ordinarily  decidedly  brighter  (and,  indeed,  not  inconsiderably  so)  than  /3  Urs.  Min.  ; 
but  at  present  the  difference  is  scarcely  perceptible,  and  I  have  more  than  once  seen  /3  almost 
brighter  than  a."  That  the  change  has  taken  place  in  (3  and  not  in  a,  is,  I  think,  certain,  having 
no  reason  either  from  general  impression,  or  from  comparison  with  other  stars,  to  suspect  a  change 
to  any  sensible  extent  in  the  latter.f 

(261)  Future  observation  will  decide  whether  the  change  which  is  thus  proved  to  have  taken 
place  be  of  periodical  recurrence.  The  complete  period,  if  such  be  the  case,  and  supposing  the 
star  to  be  now  at  its  minimum  of  lustre,  can  hardly  be  shorter  than  ten  years,  which  is  still 
inferior  to  that  of  some  stars  supposed  to  be  regularly  variable.  Ignorant  as  we  are,  however, 
both  of  the  cause  of  solar  and  stellar  light,  and  of  the  conditions  which  may  influence  its  amount 
at  different  times,  the  law  of  regular  periodicity  is  one  which  ought  not  to  be  too  hastily 
generalized,  and  at  all  events  there  is  evidence  enough  of  slow  and  gradual  change  of  lustre  in 
many  stars,  since  the  earlier  ages  of  astronomy,  to  refute  all  a  priori  assumption  as  to  the  possible 
length  of  the  cycle  of  variation  of  any  particular  star.    The  subject  is  one  of  the  utmost  physical 


*  I  entirely  agree  with  M.  Struve  in  this  surmise.  Within  my  own  distinct  recollection,  I  always  considered 
Capella  inferior  to  Lyra,  whereas  it  is  now  certainly  superior. 

t  Since  this  was  written,  the  inequality  hetween  a  and  /3  Ursse  Minoris  has  greatly  diminished.  Already, 
on  the  15th  June,  (3  had  so  far  recovered  as  to  be  declared  nearly  equal  to  a,  and  on  several  occasions  since  (July 
1846),  though  still  somewhat  less,  it  has  been  found  not  easy  at  once  to  say  which  is  the  brighter.  >>  Ursse 
Majoris  is  now  certainly  by  far  the  brightest  of  the  seven  bright  stars  in  that  constellation,  whereas  in  1838  £  held 
that  rank  quite  as  indisputably. 


NUMERICAL  MAGNITUDES. 


351 


interest.  The  grand  phenomena  of  geology  afford,  as  it  appears  to  me,  the  highest  presumptive 
evidence  of  changes  in  the  general  climate  of  our  globe.  I  cannot  otherwise  understand  alter- 
nations of  heat  and  cold,  so  extensive  as  at  one  epoch  to  have  clothed  high  northern  latitudes 
with  a  more  than  tropical  luxuriance  of  vegetation ;  at  another,  to  have  buried  vast  tracts  of 
middle  Europe,  now  enjoying  a  genial  climate,  and  smiling  with  fertility,  under  a  glacier  crust  of 
enormous  thickness.  Such  changes  seem  to  point  to  some  cause  more  powerful  than  the  mere 
local  distribution  of  land  and  water  (according  to  Mr.  Lyell's  views),  can  well  be  supposed  to  have 
been.*  In  the  slow  secular  variations  of  our  supply  of  light  and  heat  from  the  sun,  which  in  the 
immensity  of  time  past  may  have  gone  to  any  extent,  and  succeeded  each  other  in  any  order, 
without  violating  the  analogy  of  sidereal  phenomena  which  we  know  to  have  taken  place,  we 
have  a  cause,  not  indeed  established  as  a  fact,  but  readily  admissible  as  something  beyond  a 
bare  possibility,  fully  adequate  to  the  utmost  requirements  of  geology. f  A  change  of  half  a 
magnitude  in  the  lustre  of  the  sun,  regarded  as  a  fixed  star,  spread  over  successive  geological 
epochs, — now  progressive,  now  receding,  now  stationary,  according  to  the  evidence  of  warmer  or 
colder  general  temperature  which  geological  research  has  disclosed,  or  may  hereafter  reveal, — is 
what  no  astronomer  would  now  hesitate  to  admit  as  in  itself  a  perfectly  reasonable  and  not 
improbable  supposition.  Such  a  supposition  has,  assuredly,  far  less  of  extravagance  about  it 
than  the  idea  that  the  sun,  by  its  own  proper  motion,  may,  in  indefinite  ages  past,  have  traversed 
regions  so  crowded  with  stars  as  to  affect  the  climate  of  our  planet  by  the  influence  of  their 
radiation.  Nor  can  it  be  objected  that  the  character  of  a  vera  causa  is  wanting  in  such  an 
hypothesis.  Of  the  exciting  cause  of  the  radiant  emanations  from  the  sun  and  stars,  we  know 
nothing.  It  may  consist,  for  aught  we  can  tell,  in  vast  currents  of  electricity  traversing  space 
(according  to  cosmical  laws),  and  which,  meeting  in  the  higher  regions  of  their  atmospheres  with 
matter  properly  attenuated,  and  otherwise  disposed  to  electric  phosphorescence,  may  render 
such  matter  radiant,  after  the  manner  of  our  own  aurora  borealis,  under  the  influence  of 
terrestrial  electric  streams.}  Or  it  may  result  from  actual  combustion  going  on  in  the  higher 
regions  of  their  atmospheres,  the  elements  of  which,  so  united,  may  be  in  a  constant  course  of 
separation  and  restoration  to  their  active  state  of  mutual  combustibility,  by  vital  processes  of 

*  A  considerably  greater  elevation  of  those  tracts  of  Europe  which  bear  the  marks  of  glacier  action  in  former 
ages  than  at  present,  might  suffice  (especially  if  aided  by  a  favouring  distribution  of  land  and  sea  generally)  to 
account  for  a  local  prevalence  of  cold  to  any  required  extent.  It  is  the  demand  for  not  merely  a  mild  but  a  hot 
climate,  and  the  absence  of  winter  in  high  latitudes,  which  causes  the  misgiving  I  have  ventured  to  express  in 
the  text  as  to  the  sufficiency  of  this  most  ingenious  theory,  rejecting  all  aid  from  external  causes,  to  account  for 
the  whole  phenomenon. 

f  "  Many  phenomena  in  natural  history  seem  to  point  out  some  past  changes  in  our  climates.  Perhaps  the 
easiest  way  of  accounting  for  them  may  be  to  surmise  that  our  sun  has  formerly  been  sometimes  more  and  some- 
times less  bright  than  it  is  at  present." — W.  Herschel  on  the  Changes  that  happen  to  the  Fixed  Stars.  Phil. 
Trans.  1796,  p.  186. 

\  This  is  not  the  first  time  that  a  possible  analogy  between  the  light  of  the  Sun  and  that  of  our  Aurora 
Borealis  has  been  suggested.  "  In  our  atmosphere,  the  extent  of  the  clouds  is  limited  to  a  very  narrow  compass  ; 
but  we  ought  rather  to  compare  the  solar  ones  to  the  luminous  decompositions  which  take  place  in  our  Aurora 
Borealis,  or  luminous  arches  which  extend  much  further  than  the  cloudy  regions.    The  density  of  the  luminous 

solar  clouds  may  not  be  exceedingly  more  so  than  that  of  our  Aurora  Borealis;  for  if  we  consider  what 

would  be  the  brilliancy  of  a  space  two  or  three  thousand  miles  deep  filled  with  such  coruscations  as  we  now  and 
then  see  in  our  atmosphere,  their  apparent  intensity,  when  viewed  at  the  distance  of  the  sun,  might  not  be 


352 


FINAL  CONCLUSION  OF  NUMERICAL  MAGNITUDES. 


extreme  activity  going  on  at  their  habitable  surfaces,  analogous  to  that  by  which  vegetation  on 
our  earth  separates  carbonic  acid  (a  product  of  combustion)  into  its  elements,  and  so  restores 
their  combustibility.  With  specific  hypotheses  as  to  the  cause  of  solar  and  sidereal  light  and 
heat,  we  have,  however,  no  concern.  It  suffices  that  they  must  have  a  cause,  and  that  this  cause, 
inscrutable  as  it  may  be,  does  in  several  cases,  and  therefore  may,  in  one  more,  determine  the 
production  of  phenomena  of  the  kind  in  question. 

(262)  To  return,  however,  to  our  numerical  magnitudes.  Having  obtained  by  the  processes 
above  explained,  a  series  of  values,  which,  while  agreeing  in  general  with  the  scale  adopted  in 
the  fundamental  catalogue,  are  yet,  in  each  particular  instance,  assuredly  far  more  correct  than 
in  that  catalogue,  there  is  no  reason  why  we  should  not  return  upon  our  steps,  by  employing 
these  more  correct  values  instead  of  the  catalogued  values  in  column  2  of  our  normal  sequence  A, 
and  proceeding  in  precisely  the  same  way  as  before,  deduce  from  them  a  new  progression  of 
equalized  values  (as  in  col.  3),  and  a  new  series  of  interpolated  magnitudes,  as  in  col.  4.  Then, 
in  like  manner,  step  by  step,  carrying  out  all  the  subsequent  work,  a  final  series  of  magnitudes 
would  emerge,  altogether  freed  from  the  influence  of  the  accidental  errors  of  the  original  catalogue. 
There  is  every  reason  to  believe,  however,  that  the  corrections  so  induced  upon  our  series  of 
magnitudes  as  stated  in  Table  C,  would  be  quite  immaterial,  for  which  reason  I  have  not  thought 
it  necessary  to  go  through  the  laborious  process  of  this  second  approximation.  In  case,  how- 
ever, of  the  subject  being  taken  up  de  novo,  by  the  observation  of  fresh  sequences  on  a  more 
regular  and  methodical  system,  for  which  the  way  is  now  clearly  chalked  out  (as  I  hope 
earnestly  will  be  the  case),  it  is  almost  needless  to  recommend  the  pursuance  of  this  course  in 
preference  to  recurring  again  to  the  rude  and  inaccurate  magnitudes  of  catalogues  actually  in 
use,  as  by  so  doing  we  start  from  a  more  advanced  point. 

(263)  Lastly,  it  is  right  to  mention,  that,  so  long  ago  as  the  year  1841,  pursuing  a  course 
based  upon  the  same  general  principles,  but  less  elaborate  and  less  systematic  in  its  details,  I 
had  derived  from  the  same  observed  sequences  which  are  here  discussed,  a  series  of  magnitudes 
comprising  the  great  majority  of  those  in  Table  C.  Comparing  these  with  the  magnitudes  now 
deduced  by  an  independent  and  more  regular  process,  I  find  the  results  to  agree  within  limits,  as 


follows  (stars  brighter  than  Regulus  being  excluded)  : — 

Discordances  not  exceeding  one-twentieth  of  a  magnitude,    .  .  .  .131 

Do.        above  one-twentieth,  but  not  exceeding  one-tenth,      .  .  .85 

Do.        above  one-tenth,  but  not  exceeding  one-fifth,    .  .  .  .58 

Do.        above  one-fifth,  but  not  exceeding  one-third,    .  .         .  .29 

Exceeding  one-third  of  a  magnitude  (=  0'35),  .....  1 


304 

By  far  the  larger  number  of  these  discordances  are  systematic,  and  depend  on  a  different 
course  assigned  in  the  earlier  process  to  the  interpolating  curve  for  the  provisional  magnitudes, 
and  which  further  inquiry  has  convinced  me  to  have  been  erroneous. 

inferior  to  that  of  the  lucid  solar  fluid." — W.  Herschel  on  the  Nature  of  the  Sun  and  Fixed  Stars.  Phil.  Trans. 
1/94,  p.  62.  It  is  rather  to  the  quiet  reposing  masses  or  clouds  of  auroral  light  than  to  its  more  vivid  coruscations, 
however,  that  the  analogy  seems  applicable. 


353 


SECTION  II.  — ACCOUNT  OF  SOME  ATTEMPTS  TO  COMPARE  THE  INTENSITIES  OF  LIGHT  OF  THE 
STARS  ONE  WITH  ANOTHER  BY  THE  INTERVENTION  OF  THE  MOON,  BY  THE  AID  OF  AN 
ASTROMETER  ADAPTED  TO  THAT  PURPOSE. 

(264)  The  process  by  which  these  comparisons  were  made,  consists  in  deflecting  the  light  of 
the  moon  by  total  internal  reflection  at  the  base  of  a  prism,  so  as  to  emerge  in  a  direction  nearly 
coincident  with  that  of  the  undeflected  light  of  one  of  the  stars  to  be  compared.  It  is  then 
received  upon  a  lens  of  short  focus,  by  which  an  image  of  the  moon  is  formed,  which,  viewed  at  a 
considerable  distance  by  an  observer  placed  in  or  near  the  axis  of  the  lens,  will  appear  to  him  as 
a  star.  This  artificial  star  is  then  to  be  approached  to  or  removed  from  the  eye,  until  its  light  is 
judged  to  be  exactly  equal  to  the  light  of  the  real  star,  which,  lying  in  nearly  the  same  direction 
from  the  observer,  will  be  seen  side  by  side  with  the  artificial  one  with  the  same  eye,  or  with  both 
eyes  at  once,  without  the  aid  of  a  telescope*  in  the  ordinary  mode  of  natural  vision.  The 
distance  from  the  eye  to  the  focus  of  the  lens  being  then  measured,  the  prism  and  lens  are  to  be 
so  placed  as  to  form  another  similar  artificial  star,  in  a  direction  nearly  coincident  with  that  of 
the  other  star  under  comparison  ;  and  another  equalization  being  made,  and  distance  measured,  it  is 
obvious  that  the  intensities  of  the  lights  of  the  two  stars,  or  at  least  their  effects  on  the  retina,  under 
the  circumstances  of  comparison,  will  be  to  each  other  in  the  inverse  ratio  of  the  squares  of  the 
distances  so  measured  respectively.  For  no  light  being  lost  by  total  internal  reflection  at  the 
base  of  a  prism,  and  the  light  lost  at  the  ingress  and  egress  of  the  moon's  rays  into  and  out  of  the 
prism,  being  at  such  moderate  angles  of  incidence  as  it  is  ever  necessary  to  employ  in  such 
comparisons,  very  nearly,  indeed,  in  an  invariable  ratio  to  the  total  incident  light,  the  artificial 
star,  or  lunar  image,  will  be  equally  luminous  in  both  cases,  and  its  effect  on  the  eye  will, 
therefore,  be  in  the  ratio  of  the  square  of  its  apparent  angular  diameter,  or  inversely  as  the 
square  of  its  distance. 

(265)  The  astrometer,  or  instrument  employed  for  this  purpose  in  the  observations  about  to 
be  recorded,  is  of  an  extremely  simple  construction.  It  consists  of  three  principal  parts, — an 
upright  pole  firmly  fixed  in  the  ground,  about  20  feet  high,  which  I  shall  call  the  standard;  a 
cylindrical  deal  rod  about  2|  inches  in  diameter,  and  12  feet  long,  which  may  be  termed  the  staff, 
furnished  with  pulleys  at  either  end  let  into  its  thickness,  and  with  two  iron  pivots  prolonging  its 
axis  both  ways,  as  presently  to  be  described  ;  and,  lastly,  a  slider,  consisting  of  a  rectangular  piece 
of  deal  15  inches  long,  2|  inches  broad,  and  two  inches  thick,  hollowed  out  at  its  under  surface 
along  its  whole  length  to  fit  and  slide  to  and  fro  upon  the  cylindrical  staff  being  retained  in 
contact  with  it  by  an  iron  strap  in  the  middle  of  its  length  passing  round  the  staff,  but  sufficiently 
loose  to  admit  between  them  a  steel  spring  fastened  to  the  strap,  and  keeping  up  a  constant 
pressure  on  the  surface  of  the  staff  most  remote  from  the  slider ;  being  so  formed  as  to  oppose 
no  impediment  to  the  free  motion  of  the  latter  either  way  on  the  staff,  while  yet  retaining  the 
concave  and  convex  surfaces  of  the  slider  and  staff  in  steady  contact  over  the  whole  extent  applied 
to  each  other. 


*  An  opera-glass  may  occasionally  be  used  with  advantage,  but  was  not  employed  in  any  of  the  comparisons 
here  recorded. 

4  x 


354 


INTENSITIES  OF  LIGHT  OF  STARS 


(266)  The  slider  carries  the  prism  and  lens  in  the  manner  represented  in  the  annexed 
woodcut,  where  A  B  is  the  main  body  of  the  slider,  drawn  to  and  fro  along  the  staff  by  a  cord 
attached  at  its  ends  to  the  hooks  at  A  B,  and  which  for  that  purpose  is  conducted  through  the 
two  pulleys  let  into  the  two  ends  of  the  staff,  and  also  through  a  small  loop,  H,  at  the  side  of  the 
slider,  to  prevent  its  sagging  down  unnecessarily,  being  purposely  made  so  long  as  to  be  slack 
when  not  strained  in  the  act  of  dragging  the  slider. 


c 


(267)  C  D  is  a  piece  of  board  resting  on  the  upper  or  fiat  surface  of  the  slider,  and  fastened 
to  it  by  a  pin  at  E,  on  which  it  can  turn,  as  on  a  pivot,  on  its  own  plane  :  motion  being  com- 
municated to  it  for  that  purpose  at  pleasure  by  two  strings  or  reins  attached  at  C  and  D,  and 
led  through  loops  I  K,  on  either  side  of  the  slider  to  the  hand  of  the  observer,  wherever  he  may 
be  stationed,  at  or  near  the  end  of  the  staff  towards  B.  The  pin  E  is  tightened  so  as  to  hold  the 
board  firmly  down  on  the  slider  in  any  position  without  the  possibility  of  shifting,  unless  by  the 
action  of  the  reins,  which,  acting  at  an  advantageous  leverage,  give  it  an  easy  and  perfectly 
regulated  motion. 

(268)  The  prism  P  is  of  crown  glass,  isoceles  and  right-angled.  That  used  was  a  beautiful 
specimen  of  Fraunhofer's  glass  and  workmanship.  It  is  mounted  by  a  brass  framing  upon  the 
board  C  D,  in  the  position  represented  in  the  figure — its  refracting  and  reflecting  surfaces  being 
at  right  angles  to  the  plane  of  the  board,  and  the  middle  of  that  side  of  it  through  which  the  rays 
are  transmitted  out  of  it  to  the  lens  being  precisely  over  the  centre  of  the  pivot  E,  on  which  the 
board  revolves.  Its  refractive  power  is  such,  that  a  ray  may  be  diverted  as  far  as  102°  43^'  from 
its  original  course  by  reflection  at  its  base  (inclusive  of  the  effect  of  transmission  through  both 
surfaces),  without  surpassing  the  limits  of  total  reflection  by  actual  measure.  This  gives 
p.  =  1.571  for  the  refractive  index. 


BY  THE  INTERVENTION  OF  THE  MOON. 


355 


(269)  F  G  is  a  diaphragm  sufficiently  large  entirely  to  intercept  all  light  from  the  prism  in 
every  position  except  such  as  traverses  the  aperture  L  of  0.12  inch  in  diameter,  occupied  by  a 
lens  0.2253  inch  in  focal  length.  By  the  action  of  this  lens,  rays  proceeding  from  the  moon  at 
M,  reflected  internally  at  the  base  of  the  prism,  and  proceeding  out  of  it  towards  L,  are  brought 
to  a  focus  N,  forming  there  the  image  of  the  moon,  our  artificial  star  above  mentioned.  This 
image  is  visible  to  an  eye  situate  anywhere  within  the  diverging  cone  of  rays  beyond  the  focus, 
and  of  equal  apparent  brightness  (at  equal  distances)  throughout,  except  just  at  the  edges  of  the 
cone,  allowing  the  observer  a  very  great  latitude  of  motion,  and  free  choice  of  position  in  making 
his  comparisons — a  matter  of  great  consequence  to  the  success  of  the  observation, — as  it  permits 
him,  without  shifting  the  apparatus,  and  by  merely  varying  his  own  position,  to  bring  the  real 
star  nearer  to  or  farther  from  the  artificial  one,  to  the  right  or  to  the  left  of  it,  above  or  below  it, — 
without  which  it  is  impracticable  to  judge  correctly  of  their  exact  equality,  by  reason  of  the 
impurities  floating  in  the  aqueous  humour  of  the  eyes,  and  innumerable  other  causes  which 
influence,  in  an  extraordinary  degree  (hardly  credible  without  trial),  our  judgment  in  such 
comparisons. 

(270)  Attached  to  the  iron  strap  R,  which  holds  the  slider  by  its  spring  on  the  staff,  and 
projecting  out  from  it  at  right  angles  to  the  length  of  the  slider  on  the  side  opposite  to  the  slider 
itself,  is  a  short  iron  rod  O,  carrying  an  adjustable  counter-weight  Q,  such  as  to  keep  the  weight 
of  the  slider  in  equilibrium  upon  the  staff  as  an  axis,  and  allow  the  whole  slider,  with  the  prism, 
&c,  and  the  staff  together,  to  rest  indifferently  in  any  position  with  respect  to  the  horizon  of  the 
flat  face  A  B,  so  that  when  the  whole  combination  is  rested  on  the  two  iron  pivots  in  the  pro- 
longation of  the  axis  of  the  staff,  it  shall  have  no  tendency  to  tilt  round,  whether  the  slider  be 
above,  below,  or  lateral,  with  respect  to  the  staff. 

(271)  The  standard  has  at  the  top  a  pivot  on  which  revolves  a  short  iron  arm  carrying  a 
pulley.  Through  this  pulley  passes  a  cord,  one  end  of  which  carries  a  small  ring,  the  other  hangs 
down  the  standard,  and  is  clewed  on  belaying  pegs  at  a  convenient  height  on  it.  Through  the 
ring  is  passed  the  iron  pivot  at  the  end  of  the  staff,  remote  from  the  observer  (its  upper  end), 
which  is  there  secured  from  slipping  out  by  an  iron  knot  screwed  on.  The  cord  serves  by  means 
of  this  ring  to  raise  the  upper  end  of  the  staff  to  any  required  altitude,  allowing  it  at  the  same 
time  to  turn  freely  on  its  axis,  so  as  to  admit  of  the  plane  C  D  (which  is  the  plane  of  reflection 
of  the  light  within  the  prism),  to  be  placed  at  any  angle  with  the  horizon. 

(272)  The  lower  pivot  of  the  staff  rests  on  and  turns  freely  in  an  iron  socket  carried  on  a 
portable  tripod  stand,  of  the  height  of  the  eye,  so  that  when  the  staff  is  directed  to  a  star,  such 
star  may  be  viewed  conveniently,  without  either  stooping  or  straining,  by  an  observer  standing 
at  the  tripod  and  looking  along  the  staff.  To  resist  the  pressure  of  the  staff  on  the  tripod,  which 
might  upset  it,  it  is  convenient  to  have  a  weight  ready  to  hang  on  below  its  centre  of  gravity. 

(273)  To  use  this  astrometer,  a  star  must  be  chosen  not  more  than  102°  43',  nor  less  than 
60°  or  70°  from  the  moon  (which  ought  not  to  be  too  near  the  full,  as  its  light  in  that  case 
interferes  most  materially  with  the  comparisons,  by  enfeebling  the  impression  of  the  stars).  To 
this  star,  the  staff  must  be  directed,  by  elevating  its  upper  end  by  means  of  the  cord  and  rini>-, 
and  by  moving  into  a  proper  situation  the  tripod-stand  carrying  its  lower  pivot.  This  done,  the 
staff  is  turned  round  on  its  axis  till  the  plane  of  the  board  C  D  passes  through  the  moon  and 
star,  and  the  face  P  of  the  prism  is  towards  the  moon.     Looking,  then,  along  the  staff",  the  reins 


356 


INTENSITIES  OF  LIGHT  OF  STARS 


attached  to  C  D  are  worked  until  the  proper  angle  of  reflection  is  attained,  and  the  artificial  star 
is  seen,  as  it  will  be,  side  by  side  with  the  real  one  under  comparison.  The  proper  adjustment 
is  attained  when  a  good  many  degrees  motion  one  way  or  the  other  of  the  prism  on  its  pivot  E, 
and  of  the  staff  on  its  own  axis,  produce  no  sensible  effect  in  causing  any  increase  or  diminution 
of  the  artificial  star.  The  slider  is  then  to  be  approached  to  or  removed  from  the  eye  along  the 
staff,  by  pulling  the  line  attached  to  the  hooks  A  B,  until  a  perfect  equality  between  the  real  and 
artificial  stars  is  procured. 

(274)  It  only  remains  to  measure  the  distance  of  the  latter  from  the  eye,  which  is  done  by  a 
measuring  tape  divided  into  inches,  the  zero  end  being  attached  to  a  pin  in  the  slider  at  F,  and 
the  inch  read  off  being  that  which  can  be  brought  to  contact  with  the  eyelid  at  a  moderate 
tension  of  the  tape.  A  sufficient  number  of  such  equalizations  ought  to  be  made  to  give  con- 
fidence in  a  mean  of  the  readings,  and  to  fix  the  limits  of  possible  error  both  in  excess  and  defect, 
as  well  as  to  destroy,  by  variety  of  position  of  the  observer's  head,  and  by  the  alternate  judgment 
of  the  right,  the  left,  and  both  eyes  (all  which  are  strangely  influential),  the  numerous  sources  of 
illusion  to  which  the  judgment  of  equality  is  subject.  This  done,  the  other  star  must  be 
similarly  treated. 

(275)  The  actual  comparisons  made  with  this  instrument  were  neither  very  numerous  nor 
performed  under  the  most  favourable  circumstances.  In  several  of  them  the  moon  was  nearly 
full,  and  though  I  had  expected  this  to  influence  the  results  when  compared  with  those  made  at 
earlier  or  later  periods  of  the  lunation,  I  was  by  no  means  prepared  for  the  enormous  extent  of 
that  influence.  In  fact,  in  the  original  conception  of  the  process,  I  had  hoped  that  the  image  of 
the  moon  so  formed,  as  above  described,  when  reduced  to  that  of  a  mean  full  moon,  by  allowing 
for  the  phase  and  apparent  diameter,  &c,  at  the  time  and  place  of  observation,  according  to  an 
appropriate  formula,*  would  afford  a  definite  standard  of  light  with  which  any  star  might  be 
directly  and  absolutely  compared.  It  is  true  that,  owing  to  the  inequality  of  illumination  of 
different  parts  of  the  moon's  disc,  the  phase  would  not,  strictly  speaking,  be  a  numerical  measure 
of  the  light,  but  at  least  in  the  same  phase  it  would  be  reducible  to  a  constant  standard.  But 
the  effect  of  the  illumination  of  the  sky,  as  will  presently  be  seen,  destroys  all  possibility  of 
obtaining  absolute  results  in  this  manner,  and  renders  it  necessary  to  regard  them  as  comparable 
only  with  those  taken  on  the  same  night  and  under  the  same  circumstances.  All  these  difficulties 
and  objections  would  be  got  over  by  using  Jupiter  instead  of  the  moon,  and  in  her  absence,  as  a 
standard  luminary,  and  properly  modifying  the  apparatus,  which,  for  this  purpose,  might  be  rendered 

*  The  formula  is  as  follows : — Let  A  represent  the  moon's  augmented  semidiameter,  in  seconds,  at  the  place 
and  moment  of  observation,  as  given  by  the  Nautical  Almanac  and  a  table  of  augmentations;  e  her  elongation 
from  the  sun  ;  R  the  earth's  radius  vector,  the  mean  value  of  R  being  =  1 ;  933'-5  the  moon's  mean  apparent  dia- 
meter. Take 

M=imiR^h^siniy 

then  will  M  express  the  absolute  quantity  of  light  in  the  moon's  image  (supposing  all  her  illuminated  surface 
M 

equally  bright),  and  ^  the  apparent  intensity  of  our  artificial  star  at  the  distance  d  from  the  eye.  If  great  exact- 
ness be  not  required,  the  correction  for  augmentation  may  be  neglected  (which  cannot  exceed  in  its  effect  fa  of 
the  whole),  and  instead  of  e  may  be  taken  the  difference  of  longitudes  of  the  sun  and  moon,  at  the  middle  time 
of  the  night's  comparison. 


BY  THE  INTERVENTION  OF  THE  MOON. 


357 


very  convenient  and  portable,  and  I  regret  that  this  idea  did  not  occur  to  me  when  it  might  have 
been  serviceable.  Whenever  a  definite  standard  of  light  is  required  for  photometrical  purposes, 
however,  in  which  the  light  to  be  measured  can  be  seen  on  a  perfectly  dark  ground,  the  lunar 
image  formed  as  above  described  affords  one  easily  available  in  practice.* 


Observations  made  with  the  Astrometer  above  described. 

(276)  In  the  following  statement  of  the  observations,  the  first  column  contains  the  mean 
time  at  Feldhausen.  The  second,  the  star  compared ;  the  third,  the  distances  at  which,  in  the 
several  comparisons  made,  the  star  was  declared  equal  to  the  lunar  image,  as  also  any  remarks 
made  at  the  time.  The  several  series  are  marked  with  letters  (A,  B,  C,  &c.)  for  convenience  of 
further  reference. 


e 

A  =  91 


A.    March  28,  1836. 

Being  the  first  trial  of  the  method. 

=  1290  29'  the  moon's  approximate  elongation. 
5"  her  apparent  semi-diam.    Log  R  =  9.9996  the 
Earth's  Rad.  Vect.    Log  M  =  2.8962. 


h. 

m. 

7 

30 

43-7 

7 

35 

49.8 

7 

40 

Rigel   

43.1 

7 

49 

106.2 

7 

55 

92.3 

7 

58 

99.9 

8 

2 

Rigel   

40.0 

8 

7 

100.8 

8 

5° 

127. 1 

Bad  obs.  Reject. 
Better.    Colour  trouble- 
some. 
White. 


Altitude  a  little  greater 
than  3 's. 


h. 

m. 

8 

58 

95.6. 

9 

2 

100.5. 

Better. 

9 

5 

108.6. 

9 

14 

105.8. 

Rejected. 

9 

17 

97-7- 

Rejected. 

9 

25 

85-3- 

Rejected. 

The  star  is  getting  too  low,  and  the  scintillation  makes  the 
comparison  difficult.  On  examination  I  find  the  prism 
covered  with  dew.  It  is  clear  that  the  last  observations  are 
all  vitiated,  and  probably  more.  Dismounted  the  prism, 
wiped  it  carefully,  and  warmed  it.  After  this  no  more  dew. 
Resumed. 


9  5° 

9  55 

10  2 

10  7 


Sirius  . 
(3  Canis 
e  Canis. 
d  Canis 


16.7. 

97-3- 
74.9. 
89.7. 


Uncertain,  too  near. 


*  The  use  of  a  prism  to  deflect  the  light  of  a  standard  luminary  by  total  reflexion  at  its  base,  is  common 
to  the  astrometer  described  in  the  text,  and  that  of  M.  Steinheil ;  but  the  idea  of  so  employing  it  was  not 
borrowed  from  that  ingenious  artist.  Deflexion  through  an  arbitrary  angle,  without  loss  or  with  trifling  and 
negligible  loss  of  light  variable  in  amount,  is  a  necessary  condition  of  the  problem  of  astrometry,  and  optical 
science  affords  no  other  means  of  operating  such  deflexion.  My  observations  were  commenced  in  March  1836. 
M.  Steinheil's  Memoir  was  read,  it  is  true,  before  the  Gottingen  Academy  in  1835,  and  printed  in  1836,  but  I  had 
no  knowledge  of  its  existence  until  my  return  to  Europe,  when  a  copy  of  it  was  placed  in  my  hands  by  the  kind- 
ness of  M.  Schumacher.  The  prism  used  in  my  observations  was  one  which  had  been  constructed  for  me  bv 
Fraunhofer  several  years  before,  with  circular  faces  for  the  transmission  of  the  incident  and  reflected  rays  ex- 
pressly as  a  substitute  for  the  oblique  metallic  mirror  in  a  proposed  Newtonian  adaptation  of  the  20-feet  reflec- 
tor ;  an  adaptation  defeated  in  practice  by  the  annoyance  of  dew,  though  it  gave  beautiful  images. 

I  may  here  mention  that  a  long  equilateral  prism  held  in  the  hands  across  the  eyes  is  a  most  convenient  aid 
to  naked  eye  comparisons  of  stars  not  very  remote  from  one  another ;  as  by  looking  downwards  into  its  base 
through  the  side  resting  on  the  nose  and  forehead,  and  turning  round  the  upper  part  of  the  person  in  azimuth, 
the  line  joining  the  reflected  images  may  be  brought  parallel  to  the  horizon  and  the  stars  contemplated  (with 
both  eyes)  in  a  position  of  great  comfort  and  advantage.  Occasionally,  too,  it  may  be  used  to  enfeeble  the  light 
of  nearly  equal  bright  stars,  by  external  reflexion,  in  an  equal  ratio  (by  bringing  the  line  joining  their  reflected 
images  parallel  to  that  joining  their  direct).  In  this  enfeebled  state,  shades  of  inequality  become  apparent  which 
would  otherwise  escape  detection.  By  increasing  or  diminishing  (equally)  the  angles  of  incidence,  the  reflected 
images  may  be  more  or  less  enfeebled.    A  plain  metallic  mirror  may  be  used  for  the  same  purpose. 

4  Y 


« 


358 


COMPARISONS  OF  LIGHT  OF  STARS 


h.  m. 
10  15 
10  25 


45 
o 


h. 
9 
9 

9 
9 

9 
9 


10 
1 1 


13 

20 


1  + 


i)  Canis  . 
7r  Argus 

£  Argus 
y  Argus 
y  Argus 

X  Argus 
?  Argus 

8  Argus 
Arcturus 


U9-7- 

125.5.  Went  in.  When  the  ob- 
servations were  resumed,  the 
moon  was  about  200  high. 

93-6.  97-5-  ]  Rejected. 

96.7,  92.3.  S 

82.1.  Satisfactory.  The  last 
observations  rejected  by  reason 
of  flying  clouds  near  the  moon. 

95.0. 

108.7.     Better.  Re-examined 

93.6  ;  far  too  bright. 
90.4. 

29.8.  Moon  too  low  to  give  pro- 
bably good  results. 


B.    March  30,  1846. 

34' ;  A  =  940" ;  Log  R  =  9.9998. 
Log  M  =  2.9  ~ 


*5 
34 

45 
52 
12 
20 
32 

53 
o 
12 
26 
48 
>3 


13  35 


Procyon 
Jupiter . . 


Procyon 
Sirius  . . 


£  Canis  

d  Canis  

Spica   

Saturn  

a  Centauri  .... 
j3  Centauri  .... 

Saturn  

a  Trianguli  .... 
y  Trianguli  .... 
(3  Trianguli  .... 
y  Trianguli  .... 


tj  Argus 
(3  Argus 
t  Argus 
t  Argus 
S  Argus 
k  Argus 
X  Argus 


£  Argus 

v  Argus 
fi  Argus 


6  Argus 


60.8. 

19.3.     Nearly    setting  behind 

Table  Mountain,  at  150  ± 
61.4. 

28.8,26.0.   Sky  perfectly  serene, 

most  superb. 
100.5. 
115.4. 

81.5. 

56.9. 

44.6,  49.2  better. 

59-5- 
54.8. 

96.0  :  :,  101.6. 

185.6,  188.0.    Both  rejected. 
181. 1. 

179.3.  —  N.B.  |8  to  the  eye  is 
a  little  greater  than  y,  but 
the  difference  is  so  slight  a 
shade  as  to  be  hardly  appre- 
tiable. 
89.1. 

112. 5. 

146.3. 

124.5. 

132.2. 

177-5- 
122.5. 


Rejected.    (See  below.) 


A  very  good  match  in 
respect  of  colour. 

1 16.3.  Re-examined,  124.5; 
found  too  faint. 

214.0. 

150.2.  Too  bright.  Rejected. 
155.5.  Better.  Re-examined. — 
The  moon  is  beginning  to  get 
low.  Capital  observations.  Not 
a  cloud,  haze,  or  vapour,  down 
to  the  very  horizon. 

173.4.  This  result  is  evidently 
vitiated  by  the  moon's  altitude  being  too  low  ;  and  repeating 
it,  it  came  out  still  too  faint,  so  that  it  is  time  to  desist. 
Sky  most  superb.  The  moon  wants  about  two  days  of  the 
full. — N.B.  About  full  moon  there  is  sure  to  be  a  cloudless 
night. 


C.    March  31,  1836. 

e  =  1670  o' :  A  =  952"  ;  Log  R  =  9.9999. 
Log  M  =  3.01 16. 

63.8,  61.5. 

100.0,  103.3,  99-5-  Affected  with 
a  cloud-drift,  which  came  on  at 
9h  ioD',  and  lasted  till  9*  25"', 
forming,  drifting,  and  dissolving 
about  the  region  of  the  moon. 

117.3,  120.4,  135.0. 
95.0,  94.0.    Both  rejected. 

1 10.4.  Satisfactory. — The  sky  is 
rapidly  purifying  itself,  but 
all  the  foregoing  results  are 
vitiated. 

62.4. 

96.4,  100.0,  104.6. 
110.0,  1 12.0  better. 
118,  120,  133,  127. 
64.7. 

Pestered  with  dew,  and  the  back  of  the  prism  often  dimmed. 
No  value  in  the  results  of  to-night. 


h. 

m. 

9 

9 

a  Centauri  .... 

9 

18 

/3  Centauri 

9 

5° 

a  Crucis  

9 

55 

10 

7 

a  Centauri  .... 

10 

10 

[3  Centauri  .... 

10 

20 

10 

23 

/3  Crucis  

11 

3 

a  Centauri  .... 

D.    April  1,  1836. 
e  =  1790  20'  ;    A  =  959";  Log  R  =  0.0001 . 
Log  M  =  3.0232. 

81.2,  82.0. 

122.2,  119. o,  123.5,  123.0,  113. 7 
was  also  obtained,  but  rejected 
on  re-examination  as  too  bright. 

82.0.     Clouded  from   S.E.,  and 

cleared  again. 
127.0,  127.4. 
150,  152,  150. 

83.0.     Rejected  75.0,  the  cloud 
now  drifting  up  fast,  and  the 
moon  becoming  veiled,  having 
a  double  halo. 
81,  85,  80,  83.  Clear. 
124.0,  126.5. 

134.3,  130.4,  130.5.    Very  clear. 
156,  153,  147. 
166,  160,  163,  162,  163. 

Clouded  thickly  over  from  S.S.E.  as  last  night,  but  the  cloud 
is  much  higher,  and  there  is  no  moisture.  The  prism  per- 
fectly free  from  dew. 


h. 

m. 

9 

22 

a  Centauri  .... 

9 

25 

[3  Centauri  .... 

9 

34 

a  Centauri  .... 

9 

42 

9 

5* 

(3  Crucis  

10 

3 

a  Centauri  .... 

10 

7 

a  Centauri  .... 

10 

33 

(3  Centauri  .... 

10 

45 

10 

48 

10 

52 

E.    April  3.  1836. 

e  =  200°  57' ;  A  =  976"  ;  Log  R  =  0.0003. 
Log  M  =  3.0234. 

Perfectly  clear.    Strong  south  wind.    Dry  thermometer  5  8°  ; 
wet  50°.    Very  arid  cold  wind.    No  dew. 

h.  m. 
11  16 


11  25 


a  Centauri 
(3  Centauri 

a  Centauri 
(3  Centauri 


61.5,  59,  61. 
94.0,  96. — These  measures  were 
taken  alternately  to  insure  a 
more  effectual  comparison. 
60,  57.5,  62,  60. 

84,  87,  91,  91-5. — Alternate  mea- 
sures taken  for  a  second  imme- 
diate comparison. 


BY  THE  INTERVENTION  OF  THE  MOON. 


359 


/3  Centauri 
a  Centauri 
a  Crucis 


13  Centauri 
a  Centauri 
a  Crucis  . 


/3  Crucis 
a  Crucis 

y  Crucis 
/3  Crucis 


ti  Argus  . . 
a  Crucis  . . 

a  Centauri 
a  Trianguli 


a  Trianguli 


a  Trianguli  . . 


a  Muscse 


15  10 
Left  off, 
strong 
night, 


84,  93,  87,  87,  86,  89. 
61.0. 

88,  95,  90,  91. — These  measures 
of  a  Crucis  and  /3  Centauri 
taken  alternately,  interposing 
one  measure  of  a  Centauri  as  a 
fiducial  star. 
90,  87,  84,  91. 
60.6. 

94>  97>  97- — The  foregoing  pro- 
cess repeated,  again  interposing 
a  fiducial  reference  to  a  Cen- 
tauri. 

120,  115,  123,  117,  122. 
97,  92,  95,  98. — Taken  alternately 
from  i2h  25"  to  I2h  33"'. 

130,  130,  128. 

118,  117,  117,  122. — Taken  alter- 
nately, throwing  the  eye  about 
and  never  letting  it  rest  on  either 
object,  or  directing  it  to  a  point 
intermediate  between  the  real 
and  artificial  stars.  It  is  the 
black  specks  floating  in  the 
aqueous  humour  of  the  eye, 
which  produce  all  this  con- 
fusion. 
107,  114,  108,  109,  113. 
95,  97,  99. — Taken  alternately,  as 

above  described. 
60,  61,  62. 

133.  !38>  J36>  I29,  '38.  134  — 
The  measure  129  was  got  by 
getting  the  real  star  between  the 
two  images  of  the  artificial  one 
formed  by  the  right  and  left 
eyes.  134  was  got  by  a  mean 
of  two  trials,  placing  the  false 
star  first  to  the  right  of  the  true 
one,  which  always  yives  it  too 
faint,  then  to  the  left,  which 
always  yives  it  too  briyht.  This 
is  perhaps  the  best  way  of  any. 
124,  136,  126,  133.  These  were 
obtained  with  the  right  eye, 
placing  the  false  star  first  to  the 
right  then  to  the  left  of  the  true 
alternately. 

131,  133,  135,  133.  These  were 
taken  in  the  same  manner  in  all 
respects,  only  using  the  left  eye 
instead  of  the  right. 

196.  Right  eye.  ^With  the  right 
198,  204.  Left.  \  eye  178  was 
first  obtained,  but  proved  quite 
unbearable  with  the  left ;  and 
being  re-examined  with  the  right 
was  rejected  as  certainly  mis- 
taken. 

Crucis   95.  93.  91,  95.  93.  98- 

\  Scorpii   127,  129,  131. 

a  Crucis   98,  95,  94.    Rejected  100. 

\  Scorpii   131,  133,  132,  135. 

6  Scorpii   150,  153,  153,  156,  150. 

t  Sagittarii  ....     153,  153,  155. 

a  Sagittarii  ....     168,  168,  173,  175,  177,  173,  167. 

t  Sagittarii  ....     152,  155. 

a  Crucis  ......    92,  92,  96,  97,  90,  96. 

£  Centauri    ....     179,  180,  174,  186. 

y  Centauri  ....     178,  180,  183,  176. 

some  cloud  flakes  beginning  to  drift  up.  Wind 
from  south,  and  very  cold.  Not  a  trace  of  dew  all 
and  everything  perfectly  dry. 


F.    April  4,  1836. 
e  =  221°  24' ;  A  =  278";  Log  R  =  0.0005. 


42,  45,  45,  43,  46.    Set  to  61. 

Quite  out  of  the  question. 
78,  76,  82,  75. 
44.  43- 

70,  74,  72. 
107,  105,  112,  109. 
98. 

Rejected  115. 


h. 

m. 

12 

'5 

a  Centauri 

12 

28 

(3  Centauri 

12 

42 

a  Centauri  .... 

12 

45 

12 

52 

!3 

2 

J3 

14 

a  Trianguli  .... 

13 

17 

J3 

40 

13 

5* 

y  Virginis  .... 

14 

2 

14 

22 

14 

42 

<r  Sagittarii  .... 

'5 

7 

<r  Sagittarii  .... 

!5 

9 

£  Sagittarii  .... 

15 

17 

f3  Centauri  .... 

15 

zo 

a  Centauri  .... 

74.  70,  71. 
in,  109, 

92>  93.  91.  92> 
130,  131,  128. 
94,  94,  98,  94,  96. 
54.  53.  56.  57- 

173,  170,  180,  187,  190.  Rejected 

'93.  J97>  on  re-examination. 
178,  179,  170,  172,  175. 
193,  195. 

142.    Rejected  154. — So  annoyed 
by  wind,  and  altogether  such  an 
unpleasant  night,  that  no  good 
results  can  be  got. 
136,  142,  130,    143.  Rejected 

151  on  re-examination. 
123,  120,  132,  133. 
82,  80,  84. 
42,  42. 

Obliged  to  desist  owing  to  wind  and  other  circumstances  un- 
favourable to  good  observing.  There  seem  to  have  been 
some  misreadings  as  in  the  case  of  y  Virginis,  and  alto- 
gether I  have  little  confidence  in  this  series. 


G.    April  7,  1836. 
e  =  2610  53'  ;  A  =  968"  ;  Log  R  =  0.0009. 


h. 

14 


Log  M  =  2.7861. 


14  36 


Arcturus  . . . 

Spica   

Saturn  

/3  Centauri  '. 
a  Centauri  . 
a  Crucis  . . . 


34,  34-,  35- 

44,  5°,  43,  48,  48 

42,  43,  43- 

43,  45,  44- 
27+  Uncertain. 

43,  44- 


H.    April  26,  1836. 

e  =  1200  54' ;  A  =  928"  ;  Log  R  =  0.003 1 
Log  M  =  2.8676. 

The  night  beautifully  clear  and  calm. 


m. 
2 1 

34 


36 
46 


8  32 


8  48 


Procyon 
Sirius  . . 


Procyon 
j3  Canis 
£  Canis . . 
8  Canis 
Spica  . . 
(3  Corvi 
S  Crucis 


y  Crucis  . . 
y  Centauri 


£  Centauri 
£  Centauri 
(3  Crucis  . . 


56,  54,  56.  Rejected  58  on  re- 
examination. 

18.5,  17.0,  18.0.  Too  near  to 
get  a  sharp  image  of  both  ob- 
jects. 

54,  53-  5*>  56- 

94,  98>  97,  98- 

86,  84,  89,  88. 

94,  94- 

68>  73-  74,  72- 
135,  138,  136. 

144,  150  at  =  altitude  with  the 

moon. 
88,  93,  91,  90. 

112,  112.  Very  satisfactory,  the 
real  and  artificial  star  being 
exactly  alike  and  not  distin- 
guishable from  each  other. 

113,  113,  116,  118,  114. 
129,  129. 

75.  75- 


360 


COMPARISONS  OF  LIGHT  OF  STARS 


h. 


L    April  27,  1836. 

e  —  1340  14';  A  =  944";  Log  R  =  0.0033 
Log  M  =  2.9320. 

A  calm  and  superb  night. 


a  Centauri 
/3  Centauri 
a  Crucis  .  . 
/3  Crucis  . . 


Crucis 
Crucis 


y  Crucis 
rj  Argus 


t)  Argus 
(3  Crucis 
y  Crucis 
;3  Argus 
1  Argus 
1  Argus 
ff  Argus 
\  Argus 
k  Argus 
§  Crucis 


a  Circini  ... . 
y  Trianguli  . . 
Antares  . .  . . 
o"  Scorpii  . .  . . 


\  Scorpii 
6  Scorpii 

€  Scorpii  , 


45.  43-5-  45-5- 
71,  68,  69,  72,  70. 

71.  73'  68>  7°- 

83,  82.5,  81,  79.  All  circum- 
stances favourable.  s(c  at  = 
altitude  with  3  . 

104,  103,  106,  no,  108. 

161,  165,  164.  A  perfect  re- 
semblance amounting  to  undis- 
tinguishable  identity  of  colour, 
light,  &c.  The  moon's  image 
is  too  yellow  for  a  or  (5  Crucis 
or  (3  Centauri. 

90.5,  92,  96,  93.  Good,  y  is 
too  red  for  the  moon. 

79,  81,  82,  82.  Good.  Exa- 
mined the  prism  and  found  it 
much  dewed.  In  consequence 
all  the  measures  of  this  star  as 
well  as  those  preceding  it,  both 
of  y  and  d  Crucis,  must  be  re- 
jected. Carefully  dried  and 
warmed  the  prism,  and  re- 
sumed. 


87,  93,  91. 
98,  104,  9S 
113,  114. 
133. 

"5.  "3- 
120,  120. 
124. 
152. 

180,  184. 

amined. 
194. 
169. 

70,  66,  69. 
136,  145 


,  100. 
No  dew. 


Prism  carefully  ex- 
No  dew. 


143,  140.  No  dew. 
The  preceding  of  the  two  eyes 
of  Scorpio  (<5  and  f3).  This  is, 
if  any  difference,  the  brighter  of 
the  two. 


101,  102. 
108,  no,  114 
altitude  as  }. 
136,  138.  Good. 


No  dew  ;  same 


J.    June  29,  1836. 

e  =  1930  o' ;  A  =  999"  ;   Log  R  =  0.0072 
Log  M  =  3.0389. 

a  Centauri  ....  66,  68,  69,  69.  At  exactly  equal 
altitude  with  the  moon.  All  cir- 
cumstances favourable.  Moon 
one  day  past  the  full.  Superb 
sky.  Calm. 
97.  99'  98. 

no,  108,  107,  in.  Low. 
172,  174;  very  satisfactory.  3> 
about  io°  higher,  but  6  also 
high. 

a  Lupi   204,  198,  205. 

No  dew  on  glasses.  Good  observations.  The  comparisons 
are  quite  satisfactory  as  to  the  undistinguishable  lustre  of 
the  real  and  false  stars. 


(3  Centauri 
a  Crucis  . . 
0  Centauri 


K.    July  22,  1836. 

e  =  1050  12'  ;  A  =  963" ;   Log  R  =  0.0068 
Log  M  =  2.8136. 

The  moon  hardly  more  than  dichotomized. 


a  Centauri 
(3  Centauri 
y  Centauri 
(3  Corvi  . . 
Arcturus  . . 


Arcturus  . 

a  Pavonis 
a  Triang. . 


a  Aquilae. 
Lyrae  . . . 


32,  35,  31,  34,  35,  32. 

S3.  56>  57.  56.  53- 
103,  in,  108. 
132,  130  :  : 

37.3.  Mean  of  four  measures,  to 
be  rejected,  the  glass  being 
found  dewed.    Carefully  dried. 

38,  41,  37,  49.    Went  in. 

Resumed,  carefully  first  drying 
the  prism. 

94,  94,  94.    Equal  alt. 

82,  78,  84,  79.  Nearer  to  the 
moon  than  a  Pav. 

62,  61.    Equal  alt. 

51,  53,  51.    Rejected  59. 


Sky  superb,  but  the  moon  ill  situated. 


L.    July  24,  1836. 

e  =  1330  12' ;  A  =  987  ;  Log  R  =  0.0067 
Log  M  =  2.9604. 


h.  m. 
10  19 


10  59 

11  29 
11  36 
11  44 
11  49 


,3  Centauri  . 
a  Centauri  . 
a  Pavonis  . 


a  Gruis  . .  . 
FomaLhaut  . 
a  Aquilse  . .  . 
$  Capricorni 
y  Aquilae  . . . 
a  Aquilse . .  . 


76,  76,  81,  81. 

50,  45,  48,  53,  48  ;  alt.  400. 

143,  137,  141.     These  two  stars 

nearly  equidistant  from  2) 
125,  128. 
97,  94,  98,  100. 
79.  79- 

169,  170,  168. 
164,  167. 

78.     Moon  and  star  at  nearly 
equal  altitudes. 


M.    July  26,  1836. 

e  =  1600  39' ;   A  =  995"  ;  Log  R  =  0.0066 
Log  M  =  3.0298. 

Moon  nearly  full.    Not  a  trace  of  cloud  in  the  sky.    A  dead 


h. 
9 


35 


a  Gruis  . 

f3  Gruis  . . 
(3  Centauri 
a  Centauri 

a  Triang. . . 

a  Lupi. .  .  . 
a  Centauri 


Antares 


a  Pavonis 


calm. 

158,    160,    160.    Rejected  169 

being  probably  misread. 
186,  189,  187. 
105,  101,  104. 

62,  63.  Rejected  59.  Prism  ex- 
amined.   No  dew  found  on  it. 

151,  152,  150.  Rejected  147  on 
re-examination.  Very  satisfac- 
tory, only  N.B.,  a  Trianguli  is 
considerably  higher  and  nearer 
to  the  moon  than  a  Centauri. 

199,  200. 

63,  66,  64.  Tried  a  Centauri 
with  59.  Much  too  bright  but, 
N.  B.,  a  is  now  somewhat 
lower.  Yet  the  sky  is  so  pure 
that  this  cannot  be  the  reason. 
Reject  59.  No  dew.  3  near 
zenith,  a  Lupi  and  a  Centauri 
at  equal  altitudes,  4C°-K 

100,  100,  101.    Excellent.  An- 
tares is  yellower  than  3  . 
161,  166,  160. 


BY  THE  INTERVENTION  OF  THE  MOON. 


361 


h.  m. 
10  53 


[  i  26 


12  26 


a  Gruis 
/3  Gruis 


a  Gruis  . . 
a  Aquilae . . 

a  Aquilae . . 
Fomalhaut 

j8  Ceti  .... 
a  Eridani . . 

a  Phoenicis 


148,  152,  146,  143,  147. 

168,  170,  170.  Rejected  160  on 
re-examination.  No  dew  on 
either  prism  or  lens.  N.B. 
This  is  an  extraordinary  discre- 
pancy. 180  is  bearable  with  (3 
Gruis,  though  it  is  too  feeble, 
190  cannot  be  borne. 

148,  151,  152. 

107,  102,  106.  Equidistant  from 
the  moon,  but  a  Gruis  is  the 
highest  in  altitude. 

109,  106,  107. 

119,  118,  118.  Nearly  at  equal 
altitudes.  Fomalhaut  is  rather 
farther  from  the  moon  which  is 
near  the  zenith. 

187,  187,  187. 

95,  91,  94,  95,  95.  Twinkling. 

Maximum  taken. 
196,  204,  199. 


N.    August  22,  1836. 

e  =  1300  o';  A  =  982"  ;  Log  R  =  0.0046 
Log  M  =  2.9493. 


h.  m. 
11  17 


11  47 


a  Eridani    ....  I  76,  74,  75,  75. 

(3  Ceti   117,  122,  120,  123,  118,  121. 

a  Phoenicis          I  146,  142,  145. 


O.    August  23,  1836. 

e  =  1430  1' ;  A  =  984" ;  Log  R  =  0.0046 
Log  M  =  2.9906. 


h.   in . 

9  56 


10  43 


Fomalhaut 


a  Aquilae 
Fomalhaut  . . 
a  Aquilae 
a  Pavonis    . . 
a  Gruis 
9  Scorpii 


110,  109,  117.    Rejected  102  on 
re-examination. 

9°.  93-  93.  94- 
112,  106,  105. 
96,  94,  90,  97. 

143.  134.  H°- 
122,  124,  124. 
136,  130,  130,  133. 


h.  m. 
10  14 


P.    November  19,  1836. 

e  =  1420  9' ;  A  =  922° ;   Log  R  =  9 
Log  M  =  2.95 19. 

Fomalhaut  ....  I  95,  92,  92,  94,  95. 
/3  Gruis   I  127,  127,  129. 


h.  m. 
10  34 


11  34 


a  Gruis  . 
a  Eridani 

Canopus 

£  Canis 

8  Canis 
j;  Canis 
0  2  Canis 
/3  Canis 
Sirius  . . 
Rigel   . . 


122,  120.    Rather  low. 

68,  67,  68.  Rejected  70  on  re- 
examination, a  Eridani  and 
the  2  have  equal  altitudes 
within  50,  a  being  the  higher 
and  the  whiter. 

35>  33>  3 5 j  32-  Canopus  is  too 
far  from  the  2)  (900).  Com- 
parison difficult.  Its  colour  is 
a  tolerable  match  with  that  of 
the  lunar  image.  Altitudes 
nearly  equal. 

109,  109,  110,  112.  Rejected 
100,  101,  on  re-examination. 

128,  124,  127. 

148,  148.  Good. 

202.    Good  measure. 

J34>  i33>  J34- 
24,  22. 

60,  60.  Good. 


Q.    November  25,  1836. 
e  =  211°  23';  A  =  886" ;  Log  R  =  9.9941 . 


36 


o  Orionis    ....  I  57,  56,  56. 

y  Orionis  |  87. 

The  position  being  too  inconvenient,  left  off. 


e  =  122 

h. 
10 


R.    December  17,  1836. 
59';  A  =  914";  R  =  9.9929  ;  Log  M  =  2.8836. 


m. 

58 


a  Orionis    ....  52,49,45,51. 

£  Orionis ......    95,  96. 

£  Orionis   88,  87. 

Sirius    18+ ;  imperfect  measure.  Posi- 

tion excessively  awkward,  and  eye  out  of  practice  ;  £  greater 
than  £,  these  two  stars  taken  alternately. 


S.    December  26,  1836. 

e  =  2230  35' ;  A  =  886"  ;   Log  R  =  9.9927 
Log  M  =  2.9048. 


h.  m. 
13  44 


a  Cruris 

t)  Argus 
/3  Cruris 


74.  74.  75.  75.  73-    Rejected  79 

on  re -examination. 
88,  86,  91,  88.5. 
86,  93,  87. 


(277)  In  order  to  prepare  these  observations  for  reduction,  it  is  first  necessary  to  collect 
together  the  measures  of  each  star  taken  on  the  same  night,  rejecting  such  as  are  in  any  decisive 
way  indicated  on  the  face  of  the  record  as  unworthy  of  reliance,  and  taking  a  mean  of  the  rest. 
It  is  not  necessar}'  to  go  into  further  minutiae  in  the  actual  state  of  the  subject.  And  it  will  be 
seen  that  by  so  dealing  with  the  observations  en  masse,  the  results  obtained  have,  upon  the 
whole,  such  a  degree  of  consistency  as  to  relieve  us  from  any  misgivings  on  the  score  of  exactness 
in  this  mode  of  procedure.  The  following,  then,  are  the  data  so  prepared  and  arranged  for  each 
night,  according  to  the  order  of  precedence  of  the  stars  observed,  as  collected  from  the  obser- 

4  z 


362 


COMPARISONS  OF  LIGHT  OF  STARS 


vations  themselves.  In  each  night's  results,  the  first  column  contains  the  name  of  the  star;  the 
second,  the  whole  number  of  individual  equalizations  made  of  it  with  the  lunar  image;  the  third, 
the  mean  of  this  number  of  individual  distances  as  read  off  (rejectis  regiciendis) ;  and  the  last,  the 
double  logarithms  of  those  means. 


Star. 


Sirius  

Arcturus  . 

Rigel  

a  Orionis  . 
f  Canis  . . . 
y  Argus . . . 
8  Canis  . . . 
c  Argus  . . . 
£  Orionis  . 
X  Argus  . . . 
ft  Canis  . . . 
k  Orionis  . 
t  Orionis  . 
S  Orionis  . 
a  Leporis  . 
£  Argus . .  . 
?)  Canis  . .  . 
7t  Argus  . 
t  Orionis  . 


(C) 
a  Centauri . . 
ft  Centauri . . 
a  Crucis    . . 
ft  Crucis    . . 


No. 


Jupiter  . . . 

Sirius  

a  Centauri. 
Saturn  . . . 
ft  Centauri . 
Procyon . . . 

Spica  

t)  Argus. . . 
a  Trianguli 
f  Canis  . . . 
ft  Argus.. . 
I  Canis  . . . 
e  Argus  . .  . 
\  Argus . . . 
c  Argus  . .  • 
t  Argus  . . . 
\i  Argus . .  . 
k  Argus . . . 
y  Trianguli 
ft  Trianguli 
v  Argus . . . 


(D) 
a  Centauri, 
ft  Centauri, 
a  Crucis  , 
ft  Crucis  . 
y  Crucis  . 


(E) 
a  Centauri. 


16.7 
29.8 
41.5 
49.8 

74-9 
82.1 
89.7 
90.4 
92.3 
95.0 
97.1 
99.0 
99.9 
106.2 
108.6 
108.7 
119.7 
125.5 
127. 1 


19.3 
27.4 
46.9 
55.8 

59-5 
6 1. 1 
81.5 
89.1 
98.8 
ico.5 
112. 5 

U5-4 
1 16.3 
122.5 
132.2 
146.3 
r55-5 
I77-S 
179.3 
1 8 1. 1 
214.0 


63.0 
100.6 
1 10.8 
124.4 


82.1 
123.0 
129.9 

162.8 


60.5 


Star. 


2.4454 
2.9484 
3.2371 

3-3945 
3.7490 
3.8287 
3.9056 
3.9123 
3-93°4 
3-9554 

3-  9744 
3.9910 
3.9991 
4.0522 
4.0717 
4.0743 
4.1562 

4-  1973 
4.2083 


2.5711 
2.8755 
3.3386 
3.4940 
3.5490 
3.5721 
3.8223 
3.8998 

3-  9^95 
4.0043 
4.1023 
4.1244 
4.1312 
4.1763 
4.2425 

4-  33°5 
4-3^35 
4.4984 
4.5072 
4.5158 
4.6608 


3-59g7 
4.0055 
4.0891 
4.1896 


3.8292 
4.1800 
4.2274 
4-3599 
4.42  33 


ft  Centauri. 
a  Crucis  . 
i;  Argus. . . 
ft  Crucis  . 
y  Crucis  . 
X  Scorpii  . 
a  Trianguli 
0  Scorpii  . 
t  Sagittarii. 
0-  Sagittarii 
y  Centauri. 
£  Centauri  . 
a  Muscse  . 


(F) 
a  Centauri. 
Arcturus  . 
a  Crucis  . 
ft  Centauri. 
t)  Argus . . . 
ft  Crucis  . 
y  Crucis  . 
£  Sagittarii. 
a  Trianguli 
a  Sagittarii 
y  Corvi  . .  . 
y  Virginis  . 
S  Corvi  . . . 


(G) 
a  Centauri. 
Arcturus 
Saturn  .  .  . 
a  Crucis  . 
ft  Centauri. 
Spica  


.5631 


(H) 

Sirius 

Procyon. . . 
Spica 
ft  Crucis 
£  Canis  . .  , 
y  Crucis  , 
S  Canis  . . . 
ft  Canis  . . , 
y  Centauri 
£  Centauri 
£  Centauri . 
ft  Corvi  . . . 
S  Crucis 


(I) 

a  Centauri . 
Antares  . . . 
ft  Centauri. 
a  Crucis 
ft  Crucis  . 
7]  Argus . .  . 


94.4 
1 10.2 
1 19.0 
129.3 
131. 1 
132.8 
152.4 
153.6 
171.6 
179.2 
179.7 
199.3 


43.6 
55.0 
71.8 
79.6 
93.2 
95.2 
108.8 
127.0 
129.7 
138.6 
174.8 
180.0 
194.0 


27.0 

34-3 
42.7 

43-5 
44.0 
46.6 


17.8 

54-4 
71.7 
75.0 
86.7 
90.5 
94.0 
96.7 
1 12.0 
1 14.8 
129.0 
136.3 
147.0 


44-7 
68.3 
70.0 
70.5 
85.2 
88.3 


2 logd. 


3.8972 
3.9496 
4.0844 
4.1511 
4.2234 
4.2354 
4.2463 
4.3654 
4.3728 
4.4689 
4.5069 
4.5093 
4.5992 


3.2782 
3.4807 
3.7126 
3.8015 
3.9388 

3-  9573 
4.0734 
4.2076 
4.2257 
4.2835 
4.4851 
4.5 106 

4-  5756 


2.8627 
3.0713 
3.2602 
3.2770 
3.2869 
3.3368 


2.5023 

3-4717 
3.71 16 
3.7501 
3-8765 
3-9J33 
3-9463 

3-  97I3 
4.0984 

4-  II99 
4.2219 
4.2692 
4.3346 


3.3000 
3.6692 
3.6902 
3.6964 
3.8610 
3.8922 


X  Scorpii 
y  Crucis 
B  Scorpii 
ft  Argus . . 
£  Argus  . . 
S  Argus  . . 
X  Argus., 
t  Argus  . . 
£  Scorpii 
S  Scorpii 
k  Argus  . . 
y  Trianguli 
c  Crucis. 
a  Circini 


(J), 
a  Centauri 
ft  Centauri 
a  Crucis 
6  Centauri 
a  Lupi  . . 


(K) 
a  Centauri . 
Arcturus  . 
a  Lyrae  . .  . 
ft  Centauri. 
a  Aquite  . 
a  Trianguli 
a  Pavonis  .  - 
y  Centauri. 
ft  Corvi  . .  . 


(L) 
a  Centauri 
ft  Centauri 
a  Aquilae 
Fomalhaut 
a  Gruis  . . 
a  Pavonis 
y  Aquilre 
8  Capricorni 


(M) 
a  Centauri  • 
a  Eridani  • 
Antares  . .  . 
ft  Centauri. 
a  Aquilse  . 
Fomalhaut . 
a  Gruis  . . . 
a  Trianguli 
a  Pavonis  - 
ft  Gruis  . . . 
ft  Ceti  . . . 
a  Lupi  . .  . 
a  Phcenicis 


101.5 
103.4 
108.0 
113. 5 
1 14.0 
120.0 
124.0 
133.0 
137.0 
141. o 
152.0 
169.0 
182.0 
194.0 


68.0 
98.0 
109.0 
173.0 
202.3 


33.2 
38.7 
51-7 
55-° 
61.5 
80.7 
94.0 
107.3 
131.0 


78.5 
78.7 

97-5 
126.5 
140.3 
165.5 
169.0 


63.4 
94.0 
100.3 
100.3 
106.2 
118. 3 
148.4 
1 51.0 
162.3 
169.3 
187.0 
199.5 
199.7 


BY  THE  INTERVENTION  OF  THE  MOON. 


363 


Star.  No. 

d. 

2  logd. 

Star. 

No. 

d. 

2  logd. 

Star. 

No. 

d. 

2  logd. 

(N) 
a  Eridani  .... 

4 
6 

3 

75-°. 

120.2 
I44.3 

3.7501 
4.1596 
4.3187 

(P) 

Canopus  .... 
Ri^el  

2 

4 

2 

3 
5 
4 
2 

3 
3 
3 
2 
1 

2I.O 

33-7 
60.0 
67.7 
93.6 
110. 0 
121.0 
126.3 
127.7 
133.7 
148.0 
202.0 

2.6444 
3-0565 
3-5563 
3.6608 
3.9426 
4.0828 
4.1656 
4.2030 
4.2121 
4.2518 
4.3405 
4.6107 

(Q) 

a  Ononis  .... 
y  Orionis  .... 

3 
1 

56.3 
87.0 

3-5OI5 
3.8790 

a  Phoenicis    . . 

a  Eridani  .... 
Fonialhaut .... 
c  Canis  

(R) 

1 

4 
2 
2 

18.0 
49.2 
87.5 
95-5 

2.5105 
3.3848 
3.8840 
3.9600 

(0) 

a  Aquilre  .... 
Fonialhaut .... 

a  Gruis  

6  Scorpii  .... 
a  Pavonis  .... 

8 
6 
3 
♦ 

3 

93-4 
108.2 
123.3 
132.2 
139.0 

3.9404 
4.0682 
4.1822 
4.2428 
4.2860 

a  Orionis  .... 
t  Orionis  .... 
£  Orionis  .... 

0  2  Canis  .... 

(S) 

a  Crucis  .... 
/8  Crucis  .... 

4 
4 

3 

74.0 
88.4 
88.7 

3-73^5 
3.8926 
3.8956 

(278)  The  influence  exercised  upon  these  comparisons  by  the  illumination  of  the  general 
surface  of  the  sky  on  which  the  stars  are  seen  projected  will  at  once  be  apparent,  if,  using  the 

formula       we  compute  from  it  the  results  in  the  case  of  any  one  star,  observed  on  several 

nights.  Taking  a  Centauri,  for  instance,  which  occurs  on  the  series  marked  B,  C,  D,  E,  F,  G,  I, 
J,  K,  L,  M,  we  find  the  several  results  come  out  as  follows,  viz. : — B,  0.443  ;  C,  0.259 ;  D,  0.156  ; 
E,  0.289;  F,  0.505;  G,  0.838  ;  I,  0.429;  J,  0.236 ;  K,  0.592 ;  L,  0.384;  M,  0.266.  Such 
enormous  differences  show  clearly,  that,  as  a  formula  of  reduction,  the  above  is  utterly 
inapplicable.  Indeed,  at  first  sight,  it  would  almost  appear  from  this  that  absolutely  no  con- 
clusion can  be  drawn  from  the  observations  or  the  method  in  question.  This,  however,  is  very 
far  from  being  a  correct  view  of  the  subject,  since,  if,  instead  of  comparing  the  results  in  this 
manner  for  a  single  star,  we  take  any  two  stars  which  occur  together  in  more  than  one  series, 
and  compare,  not  the  absolute  numbers  resulting  from  the  formula  in  question,  but  the  ratios  of 
those  numbers,  we  shall  find,  not,  indeed,  a  precise,  but,  with  a  few  exceptions  (such  as  might  be 
expected  in  the  first  trials  of  a  new  method),  a  reasonably  good  accordance.  Thus,  if  we  take  a 
and  /3  Centauri  for  our  stars  of  comparison,  and  fixing  upon  a  for  a  standard,  denote  its  light  by 
1.000,  we  shall  find  by  this  method,  for  /3  the  numbers  following,  viz. : — 


In  series  C  0.3919 
D  0.4459 
E  0.4633 


In  series  G  0.3766 
I  0.4072 
J  0.4815 


In  series  K  0.3635 
L  0.3865 
M  0.3764 


It  is  true  that  the  results  in  series  B  and  F  (the  only  others  in  which  both  these  stars  were 
observed),  diverge  greatly  from  the  above,  being  respectively  0.6160  and  0.2997.  But  in  the 
former  of  these  only  a  single  equalization  was  made  of  (3,  and  two  of  a,  and  that  while  yet 
unaware  from  experience  of  the  precautions  necessary  for  ensuring  correctness,  and  before  any 
habit  of  observing  had  become  established.  As  regards  the  series  F,  it  is  expressly  stated  to  have 
been  made  under  such  unfavourable  circumstances  as  to  destroy  all  confidence  in  its  results. 
Allowing  both  these  series,  however,  their  due  weights  {represented  by  the  sum  of  the  numbers  of 
equalizations  of  the  two  stars  in  each),  and  following  the  same  rule  with  the  others,  we  arrive  at  a 
mean  value  (3  =  0.4137  for  the  light  of  /3  Centauri  as  compared  with  a  =  1.000,  which,  as  a  first 
approximation  certainly  seems  entitled  on  the  mere  showing  of  the  numbers,  to  some  con- 
siderable degree  of  confidence. 


364 


COMPARISONS  OF  LIGHT  OF  STARS 


(279)  Let  us  now  take  a  third  star,  a  Crucis,  which  occurs  both  with  a  and  with  /3  Centauri 
in  the  series  C  D  E  F  G  I  J,  and  with  neither  of  them  in  any  other.  And  first,  comparing  it 
in  the  mode  above  indicated  with  the  former,  we  find  for  the  individual  resulting  values  (still 
on  the  scale  on  which  a  Centauri  is  1.000)  as  follows : — 


a  Crucis  by  C  =  0.3233 
D  0.3998 
E  0.4107 


a  Crucis  by  F  =  0.3678 
G  0.3852 


a  Crucis  by  I  =  0.4015 
J  0.3892 


which  treated  by  the  same  rule*  as  to  the  weight  of  the  several  results,  gives  0.3936.  The  same 
process  carried  out  between  a  Crucis  and  j3  Centauri,  gives  for  the  quotient  of  the  numbers 
representing  these  two  stars,  0.9452,  which,  multiplied  by  0.4137,  the  number  before  found  for 
Centauri,  gives  a  Crucis  =  0.3910,  and  taking  a  mean  between  this  and  the  result  obtained  by 
direct  comparison  with  a,  we  arrive  at  the  approximate  value  0.3923  for  the  star  in  question. 

(280)  Proceeding  in  this  way  successively  with  the  other  stars  in  the  order  of  their  import- 
ance and  frequency  of  occurrence,  and  using  in  each  case  such  combinations  as  involve  the 
greatest  mass  of  equalizations,  and  afford  the  largest  grasp  of  the  totality  of  the  observations,  we 
obtain  the  following  series  of  Provisional  or  temporary  values  for  the  intrinsic  light  of  each  star 
occurring  in  all  the  series. 


Sirius    4- 1 54 

Canopus    I-991 

a  Centauri    i.ooo 

Arcturus   0.7734 

Rigel  6502 

Procyon   5106 

a  Orionis  5106 

a  Eridani  4575 

a  Lyra?  45°6 

An  tares  4216 

/3  An  tares  4137 

a  Crucis   3923 

a  Aquilae  3587 

Spica  3147 

Fomalhaut   2768 

t)  Argus  2723 

(i  Crucis  2619 


y  Orionis    

y  Crucis    0.2066 

t  Canis  1998 

\  Scorpii  !97i 

a  Gruis  1829 

a  Trianguli  1798 

y  Argus   1740 

9  Scorpii  1600 

0  Argus  1577 

t  Argus   J55° 

8  Canis  ^46 

£  Orionis  1504 

9  Centauri  1485 

(3  Canis  1446 

a  Pavonis  '444 

£  Sagittarii  J437 

/3  Gruis  1412 

8  Argus   1382 


\  Argus    0.1 32 1 

(5  Ceti  1300 

£  Orionis  1278 

k  Orionis  1197 

£  Centauri  1 176 

<t  Sagittarii  1173 

t  Argus  1 1 16 

£  Scorpii  1084 

y  Centauri   1080 

a  Phcenicis  ......    .  1060 

a  Lupi  1048 

8  Orionis  1040 

r  Scorpii  102 1 

a  Leporis  °997 

£  Argiis   °993 

Canis  0982 

£  Centauri   0906 


y  Aquilae   0.0899 

8  Capricorni  0860 

a  Muscae  0858 

k  Argus   0842 

(i  Argus   0815 

y  Corvi  0760 

(3  Corvi  0754 

7r  Argus  0747 

i  Orionis  0727 

y  Virginis  0716 

y  Trianguli  0698 

8  Crucis   0643 

8  Corvi  0610 

/3  Trianguli  0600 

0  2  Canis  0560 

a  Circini  0544 

v  Argus   0430 


(281)  These  numbers,  as  already  observed,  are  provisional,  like  those  in  Art.  247  (B)  pro- 
visionally concluded  from  the  sequences.  They  are  derived  only  from  a  partial  reduction  of  the 
observations,  and  are  destined  merely  to  afford  a  handle  for  a  complete  and  impartial  reduction 
of  the  whole,  to  perform  which  we  proceed  as  follows.    Taking     for  the  expression  of  the  light 

of  the  compared  star,  n  will  be  a  co-efficient  which,  though  variable  from  night  to  night,  and, 
indeed,  strictly  speaking,  from  instant  to  instant,  may  yet  be  regarded  as  constant  throughout  any 

*  To  avoid  prolixity  of  arithmetical  calculation  in  these  reductions,  a  weight  =  1  is  allowed  to  every  five 
equalizations,  and  if  the  sum  of  the  numbers  be  not  divisible  by  five,  the  nearest  integer  result  has  been  used. 
This  will  explain  any  trifling  differences  which  will  appear  to  the  reader  on  repeating  the  calculations. 


BY  THE  INTERVENTION  OF  THE  MOON. 


365 


single  series.  Now,  the  immediate  object  of  inquiry  is  to  assign  for  each  series  such  a  value  of 
fj.  as  shall  give  consistent  results  when  the  individual  values  of  ^  for  any  one  star  deduced  from 

different  series  are  compared  together:  and  the  degree  of  such  consistency  will  be  the  test  of  our 
success  in  so  doing.  Now,  if  the  observations  were  perfect,  and  the  provisional  values  assigned 
to  the  stars  in  the  last  article  exact,  then  calling  these  values  S,  S',  &c,  and  denoting  by 
d,  d',  &c,  the  distances  of  equalization  of  any  number  of  the  stars  observed  in  any  series,  we 


ought  to  have  for  that  series 


and  therefore 


&c. 


=  Sd?  =  S'd~*  =  S'd"*  =  &c. 


But  this  being  only  approximately  true,  and  our  object  being  to  obtain  mean  results,  we 
determine  a  mean  value  of  \x  for  the  series  in  question,  by  taking  a  mean  of  all  these  values. 

Having  thus  obtained     we  then  recompute  the  values  of  s,  s',  s",  &c.  by  the  formula  s'  =  £- 

The  values  so  obtained  will  obviously  be  much  more  independent  of  individual  errors  of 
observation  than  those  from  which  we  set  out.  And  a  repetition  of  this  process,  should  it  appear 
necessary,  would  free  us  altogether  from  specialties,  and  bring  each  result  to  rest  on  the  whole 
mass  of  observation  for  its  co-efficient  of  reduction,  and  on  its  own  individual  accuracy  for  the 
value  of  its  result. 

(282)  Confining  ourselves,  however,  to  one  process  of  the  kind  indicated,  which  may  be 
considered  sufficient  in  the  reduction  of  observations  confessedly  imperfect,  and  in  the  nature  of 
a  first  trial,  to  be  followed  up  or  not  according  to  the  estimate  which  may  be  formed  of  its 

applicability  to  our  object:  the  following  are  the  individual  values  of  —  so  obtained  for  each 

star,  and  for  every  series  in  which  it  occurs,  without  distinction  of  good  or  bad  observations,  favourable 
or  unfavourable  circumstances.  In  taking  the  means  only  two  results  have  been  rejected,  viz.:  the 
value  1.366  assigned  to  Arcturus  in  Series  A,  and  0.612  that  of /3  Centauri  in  Series  B  :  each,  it 
should  be  observed,  resting  on  a  single  equalization  in  the  very  beginning  of  my  experience  of 
this  sort  of  observation,  and  in  the  case  of  Arcturus,  evidently  vitiated  by  the  want  of  sufficient 
altitude  of  the  moon  at  the  moment  of  comparison.  Sirius,  it  must  be  remarked,  is  too  bright  an 
object  to  admit  of  being  at  all  fairly  observed  in  comparison  with  the  other  stars,  with  a  lens  of 
the  same  focus.  The  greatest  difficulty  and  uncertainty  was  always  experienced  with  this  star, 
in  pronouncing  upon  the  point  of  equalization,  and  though  I  have  no  doubt  that  the  mean  of  its 
five  determinations  is  a  tolerable  approach  to  the  truth,  I  have  less  confidence  in  it  than  in  almost 
any  of  the  others,  except  a  Lyras,  which,  from  its  low  and  unfavourable  situation,  has  been 
necessarily  under-estimated. 


Sirius. 


A 
B 
H 
P 
R 


4.348 
2.886 
4.610 
5.320 
3.781 

4.187 


Canopus. 
P  2.060 


a  Centauri. 


0.994 
1.027 


D 

E 

F 

G 

1 

J 

K 

L 


0.930 
0.930 
1.235 
1.06 1 

l.OIO 

0.952 

1. 120 

1.095 


M         1. 014 
1.033 


Arcturus. 
A  1.366 


F  0.775 
G  0.656 
K  0.820 

0.750 
Rejecting  A. 


Rigel. 


0.702 
0.652 


0.676 


5  A 


366 


COMPARISONS  OF  LIGHT  OF  STARS 


Procyon. 

B  0.580 
H  0.495 

°-537 


a  Orionis. 


A 
Q 
R 


0.489 
0.5 1 1 
0.505 

0.502 


a  Lyrae. 
K  0.461 
(Too  low.) 


a  Eridani. 


M 
N 
P 


0.461 
0.395 
0.512 

0.456 


Antares. 

I  0.432 
M  0.405 


0.418 


/3  Centauri. 


B 

C 

D 

E 

F 

G 

I 

J 

K 

L 

M 


0.612 
0.402 
0.415 
0.440 
0.370 
0.400 
0.41 1 
0.458 
0.407 
0.423 
0.382 

0.411 


a  Crucis. 


C 

D 

E 

F 

G 

I 

J 

S 


0.332 
0.372 
0.390 
0.454 
0.409 
0.405 
0.370 
0.385 

0.390 


a  Aquilse. 


K 

0.326 

L 

0.421 

M 

0.362 

u 

0.338 

0.362 

Spica. 

B 

0.319 

G 

0.356 

H 

0.2g5 

0.320 

*> 

Argus. 

B 

0.273 

E 

0.286 

F 

0.270 

I 

0.258 

S 

0.270 

0.271 

Fomalhaut 

L 
M 
O 
P 


0.274 
0.291 
0.252 
0.268 


0.271 


0  Crucis. 


0.263 
0.274 
0.245 
0.259 
0.261 
0.277 
0.268 

0.264 


y  Orionis. 
Q  214 


A 
15 
H 
P 


Canis. 

0.216 
0.215 
0.195 
0.194 

0.205 


II 
I 


0.179 
0.188 


X  Scorpii. 


E 

0.202 

I 

0.196 

0.199 

a 

Trianguli. 

B 

0.222 

E 

0.197 

F 

0.139 

K 

0.189 

M 

0.179 

0.185 

y  Argus. 

A 

0.180 

a  Gruis. 


L 
M 
O 
P 


0.163 
0.185 
0.194 
0.160 


0.175 


6  Scorpii. 


0.150 
0.173 
0.169 

0.164 


(3  Argus. 

i  0.171 
0.156 


0.163 


t  Argus. 

B  0.160 
I  0.155 

0.157 


3  Canis. 


A 

0.151 

y  Crucis. 

B 
H 

0.163 
0.166 

D  °-237 

P 

0.147 

E  0.208 

F  0.198 

0.157 

,3  Gruis. 


M 
P 


0.142 
0.144 

0.143 


(8  Canis. 


A 
H 
P 


0.129 
0.157 
0.131 

0.139 


S  Argus. 

A  0.148 
B  0.124 
I  0.140 

0.137 


£  Orionis. 
A  0.142 
R  0.160 

0.151 

6  Ceti. 
M         0. 117 
N  °-!34 

0.126 

0  Centauri. 
J  0.147 

k  Orionis. 
A  0.124 

£  Sagittarii. 

E  0.147 
F  0.145 

0.146 

(7  Sagittarii. 

E  0.118 
F  0.122 

0.120 

0  Pavonis. 

K  °-i39 
L  0.132 
M  oiSS 
O  OI53 

0.145 

y  Centauri. 

E  0.108 
H  0.117 
K  0.107 

X  Argus. 


0.134 
0.144 
0.131 

0.136 


£  Orionis. 
A  0.121 
R  o-i34 

0.127 


£  Centauri. 

E  0.108 
H         0.1 1 1 

0.109 


$  Orionis. 
A  0.108 


£  Scorpii. 
I  0.107 


1  Argus. 

B  0.101 
I  0.1 14 

0.107 


a  Lupi. 

J  0.107 
M  0.103 


0.105 


a  Phoenicis. 

M  0.102 
N  0.107 


0.104 


£  Argus. 
A  0.104 

a  Leporis. 
A  0.103 

S  Scorpii. 
I  0.101 


t)  Canis. 

A  0.085 
P  0.107 


0.096 


y  Aquilse. 
L  0.095 


I  Capricorni. 
L  0.091 


fi  Argus. 
B  0.090 

?  Centauri. 
H  0.088 


a  Muscse. 
E  0.087 


k  Argus. 

B  0.069 
I  0.087 

0.078 


y  Com. 
F  °-°77 


7r  Argfts. 
A  0-077 


(3  Corvi. 

H  0.079 
K  0.072 

0.075 


BY  THE  INTERVENTION  OF  THE  MOON. 


367 


i  Orionis. 
A  0-075 

y  Virginis. 
F  0.072 


y  Trianguli. 

B  0.067 
I  0.071 

0.069 


/3  Trianguli. 
B  0.066 

8  Crucis. 
H  0.068 


0.061 
0.064 


8  Corvi. 
F  0.062 


o  2  Canis. 
P  0.058 

a  Circini. 
I  0.054 


v  Argus. 
B  0.047 


(283)  It  only  remains  to  reduce  all  these  results  in  the  uniform  ratio  of  1000 : 1033  so  as  to 
bring  them  to  a  scale  in  which  a  Centauri  shall  (as  originally  proposed)  be  represented  by  1.000. 
This  done,  and  the  final  values  arranged  in  order  of  magnitude,  we  get  the  following 
Table  :— 

Photometric  Determination  of  the  Comparative  Intensities  of  the  Light  of  Sixty -nine  Stars,  as  deduced 

from  the  Foregoing  Observations. 


Sirius   4.052 

Canopus    J-994 

a  Centauri   1.000 

Arcturus    0.726 

Rigel   0.654 

Procyon    0.520 

a  Orionis    0.484 

Lyra   0.446 

a  Eridani    0.441 

Antares   0.404 

(3  Centauri   °-399 

a  Crucis    0.377 

a  Aquilse    °-35° 

Spica   0.309 

t]  Argus   0.262 

Fomalhaut   0.262 

(3  Crucis    °-255 

y  Orionis    0.207 


£  Canis    0.198 

y  Crucis    °-195 

X  Scorpii    0.192 

a  Trianguli    °-i79 

y  Argus   °-!74 

a  Gruis   0.169 

9  Scorpii    °-159 

(3  Argus   0.158 

£  Argus   0.152 

8  Canis   0.152 

£  Orionis    0.146 

9  Centauri   0.142 

£  Sagittarii    0.141 

a  Pavonis   0.140 

(3  Gruis   0.138 

(3  Canis   o-!34 

8  Argus   0.132 

X  Argus   0.131 


£  Orionis    0.123 

/3  Ceti    0.122 

k  Orionis    0.120 

<j  Sagittarii    0.116 

y  Centauri   0.107 

£  Centauri   0.105 

8  Orionis    0.104 

£  Scorpii    0.103 

t  Argus   0.103 

a  Lupi    0.102 

a  Phoenicis    0.101 

£  Argus   o.ioi 

a  Leporis   0.100 

8  Scorpii    0.098 

i)  Canis   0.093 

y  Aquilse    0.092 

8  Capricorni   0.088 

H  Argus   0.087 


£  Centauri   0.085 

a  Muscse    0.084 

k  Argus   0.075 

y  Corvi   0.074 

7r  Argus   0.074 

(3  Corvi   0.073 

1  Orionis    0.073 

y  Virginis   0.070 

y  Trianguli    0.067 

(3  Trianguli    0.064 

8  Crucis   0.062 

8  Corvi   0.060 

o  2  Canis    0.056 

a  Circini    0.052 

v  Argus   0.045 


(284)  The  values  of  ju  which  have  been  computed  in  conformity  with  these  principles,  and 
which  have  served  for  the  calculation  of  the  foregoing  tables,  are  of  no  importance  except  as 
matters  of  curiosity.  Nevertheless,  as  their  consideration  leads  to  a  result  of  some  interest  in 
reference  to  the  amount  of  influence  which  the  light  of  the  moon  (or  any  other  extrinsic  light, 
as  that  of  twilight,  aurora,  &c.)  exercises  in  enfeebling  the  impression  of  the  stars  on  the  eye, 
I  subjoin  them  in  a  short  table,  arranged  according  to  the  calculated  values  of  M  (the  absolute 
quantity  of  moonlight  on  each  occasion),  on  which  they  necessarily  depend  as  their  principal 
argument.  The  logarithms  are  stated  rather  than  the  numerical  values,  for  a  reason  which  will 
presently  appear,  and  all  the  values  of  log.  fj.  are  diminished  by  0.0845  (the  logarithm  of  1.033) 
to  bring  them  to  correspondence  with  the  final  results  in  the  table  of  Art.  (283). 


Log.  M. 

Log.  /x. 

Log.  M. 

Log.  n. 

Log.  M. 

Log.  fi. 

Log.  M. 

Log.  fi. 

G 

2.7861 

2.8040 

S 

2.9048 

3.2398 

L 

2.9604 

3.3318 

D 

3.0232 

3-7I33 

K 

2.8136 

3.0060 

I 

2.9320 

3.2197 

F 

2.9815 

3.2856 

E 

3.0234 

34565 

H 

2.8676 

3.0815 

Q 

2.9334 

3.1251 

B 

2.9848 

3-i5i3 

M 

3.0298 

3.5258 

R 

2.8836 

3.0036 

N 

2.9493 

3.2936 

O 

2.9906 

3-3^2 

J 

3.0389 

3-55^9 

A 

2.8962 

2.9992 

P 

2.9519 

3.2858 

C 

3.0116 

3.5168 

368 


COMPARISONS  OF  LIGHT  OF  STARS 


(285)  It  is  evident,  on  a  mere  inspection  of  this  table,  that  /x  increases  in  a  much  higher 
ratio  than  M.  If  we  suppose  it  to  vary  as  some  indeterminate  power  of  M,  or  which  comes  to 
the  same  thing,  if  we  suppose  the  relation  between  ix  and  M  to  be  expressed  by  an  equation  of 
the  form  n  =  k.  Mp,  we  have  to  determine  the  values  of  the  constant  co-efficients  k  and  p, 
so  as  to  agree  on  the  whole  best  with  the  totality  of  these  conditions.  For  this  purpose  the 
shortest  and  most  effectual  mode  of  proceeding  is  to  project  the  corresponding  values  of  log.  M 
and  log.  \x  as  abscissae  and  ordinates  on  an  interpolating  chart,  and  pass  a  straight  line  in  the 
most  advantageous  manner  among  the  projected  points.  This  having  been  accordingly  done, 
and  the  extreme  co-ordinates  of  the  line  read  off,  its  equation  was  found  to  be 

Log  ix  =  2.98  +  Log  M  —  5.5015 

which  gives  for  the  values  of  k  and  p 

A- =  0.0000031514;        p  =  2.98 

whence  the  following  value  of  /x,  as  nearly  as  it  can  be  expressed  by  any  formula  of  this  nature, 

(]\f    \2  98 
mo)  (A) 

The  value  of  p  is  so  nearly  3,  that  the  result  arrived  at  may  be  simply  announced  by 
saying  that  the  value  of  the  co-efficient  ju  is  as  the  cube  of  the  quantity  of  moonlight. 

(286)  To  perceive  the  full  import  of  this  law,  we  must  consider  that  a  star  which,  when 
the  moonlight  is  of  the  intensity  M,  requires  to  be  placed  at  the  distance  d  to  be  judged  of  equal 
brightness  with  the  moon's  image,  necessarily  produces  an  effect  on  the  eye  which  is  measured 

by         because  the  moon's  image  is  seen  not  as  the  star  is  on  the  variably  bright  ground  of 

the  sky,  but  on  a  definitely  dark  ground,  viz.,  the  hinder  side  of  the  screen  which  carries  the 
lens,  and  similarly,  the  same  star  which  with  an  intensity  of  moonlight  =  M'  equalizes  with 

the  moon's  image  at  the  distance  d'  has  its  actual  effect  on  the  retina  truly  measured  by 
under  its  new  circumstances  of  circumambient  illumination.    The  ratio  of  these  effects,  there- 
fore, which  we  shall  call  s  and  s\  will  be  that  of  ^  :  ~,  so  that  we  have   —    =.  —.%? 

7  tP      d  '  s  M      d 2 

But  by  the  very  definition  of  the  co-efficient  p  we  have  Jjj-  =  ~-j  whence  it  follows  that 

--  =  JL  ;   which  being  substituted  in  the  former  equation,  gives 

,'_M'   P__(M\\  (B) 

by  simply  writing  for  ju  and  p'  their  values  k  M3,  and  k  M'3,  from  which  it  appears  that,  within 
the  limits  of  our  experiments,  the  effective  impression  of  a  star  on  the  retina  is  inversely  as  the 
square  of  the  illumination  of  the  ground  of  the  sky  on  which  it  is  seen  projected.  I  say  within  the 
limits  of  the  experiments,  or  within  an  illumination  not  much  exceeding  that  of  full  moonlight, 
nor  much  inferior  to  that  of  the  moon  in  her  first  quarter  ;  for  it  is  evident  that  for  much 
greater  or  much  feebler  illuminations  an  empirical  law  of  this  kind  will  require  modification, 
since  Venus  is  visible  to  the  naked  eye  with  the  sun  above  the  horizon  ;*  and  since,  moreover, 


*  General  Bell,  Secretary  to  Government  for  the  Cape  Colony,  during  the  period  of  my  residence  in  South 
Africa,  permits  me  to  state  that  in  the  year  1835,  during  the  months  of  February  and  March,  he  observed  Venus 


BY  THE  INTERVENTION  OF  THE  MOON. 


369 


in  the  total  absence  of  moonlight,  when  no  other  illumination  prevails  than  that  produced  by 
the  stars  themselves  and  some  slight  remnants  of  twilight,  the  impression  of  each  star  is  not 
so  violently  exaggerated  as  this  formula  would  then  make  it,  but  would  agree  better  with  some 
expression  of  the  form  —  =  (^qp^)"  where  m  is  some  small  constant. 

(287)  There  remains  a  very  interesting  subject  of  inquiry,  which  consists  in  comparing 
our  photometric  results  with  the  conventional  scale  of  naked-eye  magnitudes  adopted  in  our 
sequences.  To  this  end  it  is  requisite  to  project  the  two  series  of  values  (those  representing  the 
conventional  magnitude  on  the  one  hand  and  the  light  on  the  other)  as  the  abscissa  and  ordinate 
of  an  interpolating  curve,  in  the  mode  already  so  often  exemplified.  This  I  have  accordingly 
done,  and  calling  x  the  conventional  magnitude  of  any  star  (among  those  observed  in  both 
series)  and  y  its  light,  that  of  a  Centauri  being  1.000,  I  find  the  following  table  to  result  from 
reading  off  the  interpolating  curve  so  constructed  for  every  decimal  of  a  magnitude  between 
x  =  1  and  x  =  3.6.  The  earlier  magnitudes  being  purely  arbitrary  are  omitted,  and  those 
beyond  3.6  cannot  be  included  for  want  of  astrometer  observations,  which,  indeed,  already  be- 
came difficult  and  uncertain  below  the  third  magnitude. 

Readings  of  the  Interpolating  Curve,  exhibiting  the  Correspondence  between  the  Conventional  Magni- 
tude jc,  and  the  Light  y,  of  Stars  as  resulting  from  the  Sequences,  and  from  Photometric  Measures. 


X 

y 

X 

y 

X 

y 

X 

y 

X 

y 

I.O 

.500 

1.6 

.242 

2.2 

.149 

2.7 

.104 

3.2 

.075 

I.I 

.442 

*-7 

.220 

2-3 

.138 

2.8 

.097 

3-3 

.072 

1.2 

.387 

1.8 

.202 

2.4 

.129 

2.9 

.092 

3-4 

.068 

.340 

1.9 

.185 

a-S 

.120 

3.0 

.087 

3-5 

.065 

1.4 

.300 

2.0 

.171 

2.6 

.112 

.080 

3.6 

.062 

H. 

.269 

2.1 

.159 

(288)  A  very  slight  consideration  of  the  form  of  this  curve,  and  of  the  course  of  the 
numbers  in  the  above  table,  suffices  to  show  that  it  approaches  very  nearly  indeed  to  a  cubic 
hyperbola,  the  form  of  whose  equation  is  {x  +  a)*,  y  =  b,  and  it  only  remains  to  determine  the 
numerical  values  of  a  and  b,  so  as  to  represent  in  the  best  manner  possible,  the  correspondence  of 
x  and  y  throughout  the  extent  of  the  table.  To  this  end,  supposing  x,  x'  to  represent  any  two 
values  of  x  given  by  the  table,  and  y,  y'  the  corresponding  values  of  y,  we  have 

(pe  +  a)\  y  =  b;         +  «)».  y>  =  b 

whence  it  is  easy  to  obtain 

x?*/ v"  —  x  */ y  S     xr  —  x  \* 

'<■  =    ^r-  >  b  =  y  y  •  I   — -  1 . 

*/  y'  —  */  y  \  ^  y'  —  V'  yj 

with  the  naked  eye,  and  without  any  instrumental  aid  in  searching  for  her  (beyond  a  recollection  of  her  place  in 
reference  to  certain  buildings,  chimneys,  &c),  from  one  of  two  stations  in  Cape  Town,  or  from  his  country  resi- 
dence on  the  Camp  Ground,  several  hours  after  sunrise,  on  thirty-two  out  of  thirty-six  days,  among  which  were 
twenty-two  consecutive  ones.  After  some  days'  observation  in  the  country,  having  missed  the  observation  on  the 
Camp  Ground  owing  to  some  light  clouds,  he  found  the  planet  at  a  later  hour  in  town  by  sweeping,  using  an  angle 
and  cornice  of  a  church  for  a  guide  to  the  eye,  and  shifting  his  position  backwards  and  forwards  till  found. 


370  INTENSITIES  OF  LIGHT  OF  STARS 

Taking  now  the  extreme  values  set  down  in  the  above  table  for  x,  x' ,  y,  y',  we  have 

x  =  1,  y  =  0-500 ;    at  =  3  6,  y  =  0-062 
whence,  executing  the  calculations  indicated,  we  find* 

6=1,   a  =  */2—  1  =  0-4142 
and  for  the  equation  between  x  and  y 

(X+  V~2-\y.y=\.  (C) 

(289)  How  nearly  this  equation  represents  the  curve  in  question  will  appear  from  the 
following  comparison  of  the  values  of  y,  as  calculated  from  it,  and  as  read  off  on  the  curve  as 
already  stated : — 


X 

y 

X 

y 

X 

y 

X 

y 

By  Curve. 

By  Equ. 

By  Curve. 

By  Equ. 

By  Curve. 

By  Equ. 

By  Curve. 

By  Equ. 

I.O 

.500 

.500 

i-7 

.220 

.224 

2.4 

.129 

.126 

3-1 

.080 

.081 

I.I 

.442 

.436 

1.8 

.202 

.204 

2.5 

.120 

.118 

3.2 

•°75 

.077 

1.2 

.387 

.384 

1.9 

.I8S 

.187 

2.6 

.112 

.110 

3-3 

.072 

.072 

i-3 

•34° 

.340 

2.0 

.171 

.172 

2.7 

.104 

.103 

3-4 

.068 

.069 

1.4 

.300 

.304 

2.1 

.159 

.156 

2.8 

.097 

.097 

3-5 

.065 

.065 

'•5 

.269 

.273 

2.2 

.149 

.146 

2.9 

.092 

.09I 

3.6 

.062 

.062 

1.6 

.242 

.247 

2.3 

.138 

.136 

3.0 

.087 

.086 

A  better  correspondence  could  hardly  be  desired,  and  certainly  could  not  have  been 
expected.  It  is  so  complete,  that  as  a  representation  of  the  totality  of  the  observations,  the 
equation  may  be  regarded  as  a  perfect  substitute  for  the  curve,  which  latter  may  therefore  be 
dismissed  altogether  from  further  consideration. 

(290)  This  equation  once  obtained,  may  be  applied  either  to  the  numerical  estimation  of 
the  light  of  a  star  of  given  magnitude,  or  vice  versa,  from  an  experimental  determination  of  its 
light  either  by  means  of  such  an  astrometer  as  above  described,  or  any  other,  to  assign  its  place 
in  the  scale  of  conventional  magnitudes.  Let  us  now  therefore  proceed  to  determine  by  its  aid 
the  magnitudes  which  ought  to  be  assigned  to  the  several  stars  of  our  list  in  the  table  Art.  280,  and 
to  compare  them  with  those  previously  assigned  to  them  from  the  sequence  observations.  This 
is  done  in  the  subjoined  table,  in  which  it  is,  however,  to  be  borne  in  mind,  that  the  sequence 
magnitudes  of  the  larger  stars,  from  Sirius  down  to  Procyon  or  Orion,  are  purely  arbitrary,  and 
rest  on  no  other  evidence  than  a  hardly  more  than  conjectural  appergu  of  the  course  of  the 
interpolating  curve  alluded  to  in  Art.  244.  The  approach  to  agreement  between  the  two  series 
in  their  earlier  members  which  does  obtain,  is  therefore,  pro  tanto,  a  verification  of  this 

*  The  exact  arithmetical  calculation  gives  6=  1.0001,  a  =  0.4143.  The  coincidence,  which  is  a  remarkable 
one,  is  purely  accidental,  and  was  not  foreseen  when  the  data  in  the  text  were  fixed  upon.  It  is  true  that  the 
value  of  y  (0.500),  corresponding  to  x  =  1  was  designedly  chosen — the  natural  course  of  the  interpolating  curve, 
allowing  some  little  latitude  of  choice  at  this  place,  which  was  taken  advantage  of  to  give  a  round  number,  but  all 
the  rest  of  its  course  is  strictly  limited,  this  point  once  being  fixed. 


BY  THE  INTERVENTION  OF  THE  MOON. 


371 


conjecture,  and  of  the  extension  of  our  nomenclature  of  magnitudes  to  degrees  of  brightness 
higher  than  that  to  which  the  magnitude  1  is  assigned  in  the  adopted  scale.  In  this  part  of  the 
scale  the  astrometer  values  are  alone  entitled  to  any  consideration. 

Comparison  of  the  Magnitudes  of  68  Stars  as  deduced  on  the  one  hand  from  the  method  of  Sequences,  and 
on  the  other  from  Photometric  Ohservation,  by  the  aid  of  the  Astrometer. 


Star. 

Sirius 
Canopus  . 
a  Centauri 
Arcturus  . , 

Lyra  

Rigel  . . . 
Procyon  . 
a  Eridani. 
a  Orionis. 
/3  Centauri 
a  Cruris  . 
Antares  . 
a  Aquilae. 
Spica  . . . 
Fomalhaut 
(3  Cruris  . 
a  Gruis  . 
y  Cruris  . 
£  Orionis  . 
£  Canis. . . 
X  Scorpii . 
£  Orionis  . 
(3  Argus  . 


By  Seq. 


O.IO 
0.22 

°-34 
0.45 
0.66 
0.76 
0.85 
0.93 
1.00 

1. 14 

1. 21 
1.28 

i-35 
1.41 
1.47 
1.59 
1.69 
1.73 
1.84 
1.86 
1.87 
2.01 
2.03 


By  Astr. 


O.08 
0.29 
0.59 
O.77 
I.08 
O.82 
O.97 
I.09 
1.02 
1. 17 
1 .21 
1. 16 
1.28 
I.38 
I.S4 

i-57 
2.02 
1.85 
2.20 
1.83 
1.87 
2.44 
2.10 


Star. 

y  Argus  . . 
y  Orionis . . 
£  Argus  . . 
o  Trianguli 
£  Sagittarii 
6  Scorpii  . . 
d  Canis 
a  Pavonis . . 
/3  Gruis  . . 
a  Sagittarii 
h  Argus  . . 
X  Argus  . . 
/3  Ceti  .... 
9  Centauri 
(3  Canis  . . 
k  Orionis . . 
S  Orionis  . , 
y  Centauri 
£  Scorpii  . . 
£  Argus  . 

0  Phoenicis 

1  Argus. . . , 
a  Lupi 


By  Seq. 


2.08 
2.IO 
2.18 
2.23 
2.26 
2.29 
2.32 

M3 
2.36 
2.41 
2.42 
2.46 
2.46 
2.54 
2.58 
2.59 
2.61 
2.68 
2.71 
2.72 
2.78 
2.80 
2.82 


By  Astr. 


I.78 
2.15 
I.95 
2.25 
2.09 
2.15 
2.26 
2.28 
2.52 
2.34 
2.35 
2.45 
2.24 
2.32 
2.37 
2. 69 
2.64 
2.7O 
2.73 

2-73 
2.70 
2.72 


Star. 

£  Centauri  . 
r]  Canis  . .  . 
S  Scorpii  . . . 
y  Corvi  . . . 
k  Argus  . .  . 
j8  Corvi  . . . 
£  Centauri 
7r  Argus  . . . 
a  Leporis . . . 
y  Aquite  . .  . 
y  Virginis  . 
ju  Argus  . . . 
S  Capricorni 
S  Corvi 

1  Orionis  . . , 
a  Muscae . . . 
j3  Trianguli  . 
y  Trianguli  , 
v  Argus  . . , 
8  Crucis  . . . 

02  Canis  . . , 
a  Circini  . . 


By  Seq. 


82 
85 

86 
90 
94 
95 

.96 


By  Astr. 


2.67 
2.86 
2.78 
3.26 
3.24 
3.29 
3.02 
3.26 
2.75 
2.88 

3-37 
2.97 
2.96 

3-67 
3.29 
3.04 
3-5+ 
3-45 
4.30 
3.60 
3.81 
3-97 


(291)  In  judging  of  the  general  amount  of  coincidence  between  the  two  series  here  pre- 
sented, it  is  by  no  means  desired  to  under-estimate  or  unduly  palliate  the  rather  considerable  and 
numerous  cases  of  discordance  which  occur.  Out  of  sixty-three  stars  compared,  inferior  to 
Lyra  in  brightness  (for  of  the  cases  above  that  limit  no  fair  judgment  can  be  formed),  there  are  no 
less  than  eighteen  in  which  the  disagreement  of  the  assigned  values  exceeds  one-fifth  of  a  magni- 
tude, a  quantity  respecting  which  the  judgment  of  a  practised  eye  cannot  be  deceived.  Never- 
theless, it  ought  to  be  remembered  that  these  extreme  differences  are,  in  all  probability,  the  sums 
of  errors  in  opposite  directions,  of  the  values  afforded  by  the  two  methods.  And  it  must  further 
be  remarked,  that  in  a  majority  of  these  cases  the  photometric  determination  rests  on  a  single 
night's  observation,  and  not  unfrequently  on  a  single  equalization.  The  worst  case  of  all,  that  of 
v  Argus,  is  of  this  description,  and  ought  undoubtedly  to  be  rejected  as  altogether  erroneous,  and 
would  have  been  so  had  not  all  selection  been  avoided.  In  others  (such  as  those  of  a  Gruis  and 
a  Trianguli),  it  seems  extremely  probable  that  a  difference  of  colour  between  the  light  of  the 
star  and  that  of  the  moon  has  affected  the  photometric  comparisons,  leaving  them,  however, 
consistent  inter  se.  Lastly,  if  we  look  to  the  cases  of  agreement  rather  than  to  those  of  dis- 
cordance, we  shall  find  no  less  than  forty  out  of  the  sixty-three  in  question  in  which  the  results 
agree  within  one-eighth  of  a  magnitude. 

(292)  One  very  remarkable  result  of  our  equation  (C)  Art.  288,  ought  not  to  be  passed  in 
silence,  viz.,  that  if  the  numerical  values  conventionally  assigned  to  the  stars  be  all  increased  by 
the  constant  fraction  0.4142  (or  V'2  —  1)  the  new  scale  of  magnitudes  so  arising  will  represent  the 


372 


INTENSITIES  OF  LIGHT  OF  STARS  BY  THE  INTERVENTION  OF  THE  MOON. 


distances  of  the  respective  stars  to  which  they  are  ascr  ibed,  from  our  system,  on  the  supposition  of  an 
intrinsic  equality  in  the  liyht  of  the  stars  themselves;  (i.  e.  so  that  differences  of  brightness  shall  be 
merely  apparent,  and  supposed  to  arise  solely  from  differences  of  distance).  Now,  as  the  con- 
ventional scale  which  we  have  adopted  is,  after  all,  purely  arbitrary,  there  is  absolutely  no  reason 
other  than  usage,  and  (that  hitherto  a  very  vague  and  lax  one)  why  this  alteration  of  nomenclature 
should  not  be  made.  In  fact,  so  loose  is  the  present  practice,  that  it  would  hardly  be  felt  as  a 
change,  a  Centauri  would  be  our  normal  star  of  the  first  magnitude,  /3  Crucis  of  the  second, 
k  Orionis  of  the  third,*  v  Hydrae  of  the  fourth,  and  h  Volantis  of  the  fifth ;  and  these  are  the 
magnitudes  which  actually  stand  annexed  to  those  stars  in  our  catalogues  respectively.  The 
effect  of  such  a  change  would  be  to  place  the  nomenclature  of  magnitudes  on  a  natural,  or,  at  all 
events,  on  a  photometric  basis  easily  remembered,  the  relation  between  the  magnitude  and  the 
light  of  any  star  being  given  by  the  very  simple  equation 

M2  .  L  =  1  (D) 

a  Centauri  being  taken  as  the  unit  both  of  light  and  magnitude.  It  is  of  course  to  be  under- 
stood, that  in  speaking  of  a  Centauri,  which  is  a  double  star,  the  sum  of  the  two  individuals  is 
intended,  and  the  very  fact  of  its  being  double,  and  composed  of  two  very  bright  individuals, 
gives  a  sort  of  security  against  the  probability  of  its  variation  in  our  ignorance  of  the  causes  of 
the  phenomena  of  variable  stars,  inasmuch  as  there  is  a  chance  of  compensation  in  the  inde- 
pendent variations  of  two  or  more  individuals,  and  at  all  events,  the  sum  will  vary  in  a  less  ratio 
to  the  whole  if  only  one  of  the  two  be  variable. 

*  These  stars  are  those  on  our  list  (C),  in  which  the  sequence  magnitudes  are  1.59,  2.59,  3.59,  4.59.  a  Cen- 
tauri has,  properly  speaking,  no  sequence  magnitude,  and  is  our  assumed  standard.  *  Orionis  is  ill  determined 
in  the  astrometer  series,  as  are  all  stars  below  the  3rd  magnitude. 


CHAPTER  IV. 


OF  THE  DISTRIBUTION  OF  STARS  AND  OF  THE  CONSTITUTION  OF  THE  GALAXY 

IN  THE  SOUTHERN  HEMISPHERE. 

SECTION  I. — OF  THE  STATISTICAL  DISTRIBUTION  OF  STARS. 

(293)  That  the  comparative  abundance  or  paucity  of  stars  in  any  particular  region  of  the 
northern  hemisphere,  and  of  the  southern,  so  far  as  visible  in  our  latitudes,  has  reference  to  its 
situation  in  respect  of  the  Milky  Way,  is  a  proposition  which  the  researches  of  Sir  William 
Herschel  have  sufficiently  established,  not  merely  by  the  general  aspect  of  the  heavens  when 
viewed  with  the  naked  eye,  but  also  when  examined  with  powerful  telescopes  in  a  mode  which 
may  properly  be  called  statistical, — that  is  to  say,  by  counting  the  number  of  stars  in  the  field  of 
view  of  one  and  the  same  telescope  at  a  great  number  of  given  points  in  the  concave  of  the 
heavens,  and  so  estimating  their  comparative  pojmlousness  in  stars,  in  their  different  districts. 
The  results  of  a  system  of  observation  of  this  nature  have,  as  is  well  known,  conducted  him  to  the 
highly  remarkable  and  interesting  conclusion  above  mentioned,  and  to  this  further  consequence, 
that  all  the  stars  visible  to  us,  whether  by  unassisted  vision,  or  through  the  best  telescopes  (such 
at  least  as  are  scattered,  or  not  congregated  in  resolvable  nebulae,  or  globular  or  similar  highly 
condensed  clusters)  belong  to  and  form  part  of  a  vast  stratum,  or  considerably  flattened  and 
unsymmetrical  congeries  of  stars  in  which  our  system  is  deeply,  though  excentrically  plunged, 
and,  moreover,  situated  near  a  point  where  the  stratum  bifurcates  or  spreads  itself  out  into  two 
sheets.* 

(294)  It  may  easily  be  supposed  that  the  opportunity  offered  of  carrying  out  this  great 
induction  by  observations  made  with  the  same  telescope,  similarly  used  in  that  part  of  the 
heavens  inaccessible  to  its  author,  was  not  neglected.  So  soon  as  a  knowledge  of  the  regions 
where  nebula?  might  more  especially  be  expected  had  been  acquired,  so  as  not  to  hazard  too 
much  by  continually  interrupting  the  sweep  for  the  purpose  of  gauging  (i.  <?.,  counting  the 
number  of  visible  stars  in  determinate  fields  of  view),  a  system  of  star-gauges  was  set  on  foot,  at 
first  somewhat  irregularly,  but  after  a  very  few  sweeps,  more  systematically,  so  as  to  dot  over  the 
surface  of  the  heavens,  as  it  were  with  a  regular  tesseration  of  gauged  or  counted  fields,  disposed 
at  definite  and  equal  intervals  of  Right  Ascension  and  Polar  distance,  viz.,  10m  of  time  in  R  A, 
and  1°  30'  of  arc  in  N  P  D,  as  shown  in  the  following  woodcut,  where  the  circles  indicate  the 
fields  of  view,  and  the  zig-zag  lines  connecting  them,  the  course  of  a  telescope  passing  from  one 


*  Phil.  Trans.  1785,  p.  213. 


374 


OF  THE  STATISTICAL 


to  another  during  a  single  sweep,  supposing  it  devoted  only  to  this  object.  Not  that  it  was 
expected,  or,  indeed,  considered  possible  actually  to  count  so  great  a  multitude  of  fields  as  this 

plan,  completely  executed,  would  require.  But  it 
was  considered,  1st,  that  many  gauge-points  must 
escape  observation  in  consequence  of  the  inter- 
ference of  the  more  important  regular  business  of 
the  sweep ;  2dly,  that  some  system  was  necessary  to 
prevent  confusion,  and  unequal  observing,  and  that 
the  system  proposed  offered  the  advantage  of  being 
easily  carried  in  the  memory  ;*  3dly,  and  more 
especially,  that  it  was  desirable  to  ensure  an  absolute 
impartiality  in  the  selection  of  the  gauge-points, 
which  could  only  be  done  by  determining  before- 
hand where  they  should  occur,  rather  than  trust  anything  to  choice,  when,  in  all  probability, 
more  crowded  fields  might  have  obtained  an  undue  preference  in  the  richer  regions,  and  more 
empty  ones  in  the  poorer,  owing  to  the  natural  tendency  to  bring  out  into  prominence  any- 
thing which  at  the  moment  appears  a  feature. 

(295)  About  2300  gauges  have  been  thus  obtained,  which,  though  leaving  some  blanks,  in 
zones  which  had  either  been  sufficiently  swept  over  before  the  gauges  were  commenced,  or 
where,  for  other  reasons,  their  registry  was  interrupted,  yet  afford  ample  materials  for  testing  the 
validity  of  the  induction  in  question,  and  for  estimating  the  comparative  richness  of  every  con- 
siderable district  of  the  southern  heavens.  They  are  digested  and  arranged  in  the  subsequent 
synopsis,  in  which  the  following  particulars  require  to  be  noticed. 

(296)  The  setting  of  the  telescope  upon  the  gauge-points  in  P  D  was  performed  without  any 
regard  to  precision  ;  the  microscope  being  usually  brought  to  a  rough  reading  of  0°,  1°  30',  3°, 
for  the  extremes  and  middle  of  the  zone,  neglecting  the  correction  for  the  minutes  of  zero  error, 
unless  conspicuous  enough  to  be  troublesome,  in  which  cases  it  was  roughly  applied.  So,  also, 
in  R  A,  the  chronometer  error  was  habitually  neglected,  unless  unusually  great ;  and  it  would 
frequently  happen  that,  owing  to  the  interference  of  an  object,  a  delay  of  one,  two,  or  three 
minutes  beyond  the  regular  preconcerted  times  (0m,  10m,  20m,  &c.)  would  occur.  For  all  these 
reasons  it  is  probable  that  hardly  any  of  the  gauged  fields  can  be  accurately  identified,  nor  is  it  of 
the  slightest  importance  that  they  should  be  so.  It  suffices  that  they  occur  about  (i.  e.,  in  the 
immediate  neighbourhood)  of  their  intended  places — in  the  majority  of  cases,  no  doubt,  over- 
lapping them  over  some  considerable  portion  of  their  area.  This  circumstance  is  taken 
advantage  of  to  effect  a  material  saving  of  space  and  printing  in  their  synoptical  presentation,  by 
referring  each  gauge  to  its  nearest  intended  parallel  of  declination  and  decade  of  minutes  in 
Right  Ascension. 

(297)  As  a  preparation  for  this  synoptic  presentation  of  the  gauges,  each  observation  was 
first  projected  from  the  gauge-book  on  a  large  chart  constructed  for  the  purpose,  the  number  of 

*  In  the  system  of  sweeping  pursued,  where  zones  of  3°  in  breadth  from  the  equator  either  way  to  the  poles 
were  observed,  the  rule  for  the  gauge  points  adopted,  after  some  little  hesitation,  was  as  follows : — 1st,  Even  hours 
(0h,  2h,  4\  &c.)  begin  their  gauges  at  the  northern  limit  of  the  zone,  odd  hours  at  the  southern ;  2nd,  Even 
multiples  of  20"  in  R  A  correspond  to  the  northern  limit,  odd  to  the  southern;  3rd,  Odd  multiples  of  10m  (lO, 
30"',  50")  correspond  to  the  middle  of  the  zone  in  P  D. 


DISTRIBUTION  OF  STARS. 


375 


stars  in  the  gauged  fields  being  written  in  their  proper  places,  like  the  soundings  in  a  hydro- 
graphic  chart.  In  so  doing,  the  actual  observed  places  (as  nearly  as  recoverable)  of  the  gauges 
were  laid  down.  By  this  means  it  was  found,  as  expected  and  intended,  that  in  regions  swept 
over  twice  or  three  times,  blanks  left  in  one  sweep  were  very  frequently  filled  up  by  the  obser- 
vations of  another,  so  as  to  cover  the  ground  of  large  districts  with  great  regularity.  In  a  great 
multitude  of  instances,  however,  duplicates,  and  even  triplicates  of  particular  gauges  would 
occur,  seldom  exactly  coincident  in  place.  Wherever  this  happens,  neither  of  the  individual 
gauges  is  registered  in  the  synopsis,  but  a  mean  is  taken  of  all  the  numbers,  to  give  the  gauge- 
number  corresponding  to  the  gauge-point  to  which  both  the  observed  places  belong,  or  that 
nearest  to  the  mean  of  the  places.  When  the  mean  so  taken  is  a  fraction,  the  nearest  integer  is 
set  down,  and  when  the  difference  from  an  integer  is  exactly  J,  the  integer  next  less  is 
preferred. 

(298)  The  arrangement  of  the  synoptic  table  of  guages  is  as  follows  : — All  the  gauges  are 
arranged  on  meridians  and  parallels.  Under  the  heading  of  each  meridian,  denoted  by  0h  0m, 
0h  10m,  &c.  at  the  head  of  each  double  column,  are  entered,  in  the  first  column,  the  several 
parallels  on  which  gauges  have  been  observed,  and  in  the  second,  the  number  of  stars  in  the 
field  corresponding,  by  a  mean  of  the  gauges.  The  parallels  are  58  in  number,  being  numbered 
from  0  to  57  inclusive.  The  parallel  0  corresponds  to  N  P  D  90° ;  parallel  1,  to  91°  30'; 
parallel  2,  to  93°,  and  so  on,  increasing  by  1°  30'  for  each  unit,  only  that  the  last  parallel,  No.  57, 
corresponds  to  175°  0',  instead  of  175°  30',  the  interval  from  171°  to  the  South  Pole  having  been 
divided  into  two  zones  of  4°  and  5°  in  breadth  respectively.  The  dots  attached  to  the  gauge 
numbers  indicate  the  number  of  fields,  a  mean  of  which  is  taken  in  each  case. 

(299)  The  Polar  gauge  is  a  single  one,  and  contains  14  stars,  by  a  mean  of  three  ob- 
servations, in  each  of  which  the  true  pole  was  in  the  field,  though  not  exactly  central. 


Synoptic  Table  of  Southern  Star-Gauges,  arranged  on  Meridians  and  Parallels. 


Par.  Gau. 
oh.  om. 


14 
16 
26 
28 

34 
36 

38 
40 
42 

44 
48 

5° 
5* 
54 


23 
35 
37 
41 
45 


3- 

7- 
7- 
2. 

10.*, 

7  = 
*3- 

7- 
10  : 

9-- 
11. 

15- 


'3 


o  h.  10  m. 
7  4- 


Par. 

Gau. 

oh. 

20  m. 

16 

5- 

18 

2. 

20 

3- 

28 

8. 

36 

7- 

38 

7- 

42 

10  : 

44 

II. 

5° 

22. 

52 

IO. 

oh. 

30  m. 

3 

4- 

7 

1. 

15 

12. 

'9 

13- 

23 

5- 

35 

8. 

37 

8. 

39 

11. 

45 

14. 

51 

12  : 

oh. 

40  m. 

6 

5- 

20 

9- 

Par. 

Gau. 

22 

5- 

26 

6. 

34 

6. 

40 

11. 

44 

1 1. 

5° 

11. 

oh. 

50  m. 

17 

5- 

20 

3- 

23 

16. 

27 

0. 

43 

14. 

45 

5- 

ih. 

0  m. 

14 

4- 

18 

6. 

24 

3- 

28 

7- 

36 

4- 

38 

11. 

42 

10  : 

46 

9- 

5° 

15- 

52 

8. 

56 

1 1. 

Par.  Gau. 
1  h.  10m. 


7 
17 
*9 
21 
27 
31 
39 
43 
49 
51 


4 
6 

12 

14 

28 
30 
36 
38 
40 
42 
48 
5° 
52 
54 


4- 
4- 
14. 
8. 

5- 
10. 


16. 
9 


1  h.  20  m. 
4- 


11. 
6. 

6  : 
IO  : 

6. 
12  : 
17  : 


Par.  Gau. 
1  h.  30  m. 

3  5- 


7 
'3 
10 

«7 

23 
27 

3i 
37 
39 
41 
43 
49 
51 


24 
28 
32 
42 
44 


5  : 
5- 
3- 

6  : 

9- 
7- 
5- 
9- 

19. 

11. 

15- 
7- 
2. 


1  h.  40  m. 

10  6. 
12  3. 


4- 

6. 

4- 
5- 
8.- 

10. 

11. 


Par. 

Gau. 

5° 

3- 

56 

9- 

1  h. 

50  m. 

3 

1. 

7 

5- 

21 

9- 

23 

12. 

29 

3- 

3i 

7  : 

37 

8. 

4i 

6. 

43 

7- 

49 

7- 

5i 

10  : 

2h. 

0  m. 

2 

6. 

8 

5  : 

12 

7- 

14 

1. 

16 

9- 

18 

6. 

20 

5- 

22 

8. 

26 

4  = 

28 

5- 

Par. 

Gau. 

30 

10  : 

32 

9- 

36 

6. 

40 

1 1. 

42 

1 1. 

48 

14. 

5° 

10  : 

52 

10. 

54 

9- 

2h. 

10  m. 

3 

8. 

7 

10. 

9 

8. 

!3 

J3- 

15 

7- 

17 

1. 

J9 

6. 

21 

5- 

23 

4- 

27 

7- 

33 

7- 

5i 

6. 

53 

9- 

2h. 

20  m. 

IO 

5- 

Par.  Gau. 


14 
18 

22 
28 
30 
38 
42 

44 
5° 
52 
54 
56 


J3 
15 
17 
21 
23 
25 

29 
3i 
33 
37 
39 


!3- 

5- 
11  : 

7  : 
4  = 
5- 
7- 

1 1. 

10. 

16. 

21. 


2  h.  30  m. 
3  6- 


6. 

10. 

10. 
4- 
5- 

10. 
6  : 
6. 
5- 


376 


OF  THE  STATISTICAL 


Par. 

Gau. 

43 

8. 

49 

12. 

5« 

14: 

S3 

9- 

2  h. 

40  m. 

12 

6  : 

'4 

11. 

16 

4- 

22 

7- 

24 

9- 

26 

9- 

28 

8  : 

32 

7. 

36 

6. 

38 

14. 

42 

14. 

48 

18. 

5° 

14. 

5^ 

9- 

54 

J3- 

2  h. 

50  m. 

3 

7. 

7 

3- 

9 

9. 

13 

15. 

2 1 

1. 

23 

3. 

27 

6. 

29 

10. 

31 

12. 

41 

9. 

43 

6. 

48 

0. 

49 

10. 

53 

10. 

3h. 

0  m. 

4 

3. 

g 

10 

Q. 

14. 

y  ' 

l6 

y 

22 

8. 

2. 

26 

8. 

28 

2  : 

10 : 

3° 

1S- 

40 

44 

12. 

5° 

19- 

5* 

13- 

54 

17- 

56 

J3- 

3h. 

10  m. 

9 

9: 

1 1 

8. 

»3 

5: 

•5 

7  = 

2 1 

9- 

23 

9- 

^5 

1. 

*9 

»3- 

35 

26. 

41 

7- 

49 

J3- 

5i 

18. 

53 

J3- 

Par. 

Gau. 

3h. 

20  in. 

2 

5- 

6 

1. 

8 

7 ; 

10 

9 : 

12 

10 : 

22 

8. 

26 

9- 

28 

6: 

40 

12  : 

48 

«3- 

5° 

1 1. 

52 

8  : 

54 

19. 

3  h- 

30  m. 

7 

3- 

9 

6. 

1 1 

5- 

13 

8. 

15 

5- 

25 

6. 

29 

8. 

31 

13- 

33 

9- 

41 

13- 

49 

1 1. 

53 

19. 

3h. 

40  m. 

8 

6. 

10 

10 : 

12 

9- 

J4 

14. 

22 

12  : 

24 

7. 

3° 

6. 

34 

7- 

42 

9- 

5° 

5- 

5i 

10. 

56 

J 

J 

3  h. 

50  m. 

7 

10 : 

1 1 

9- 

J3 

9  : 

J7 

a 
8. 

J9 

14. 

2 1 

3- 

23 

9  = 

25 

'5- 

29 

11. 

33 

9: 

35 

5- 

36 

5- 

41 

10. 

5i 

9- 

53 

8. 

4h 

0  m. 

6 

11. 

8 

6. 

10 

6. 

12 

12.-. 

14 

9- 

16 

10. 

20 

7- 

22 

8. 

24 

10. 

26 

9  : 

Par. 

uau. 

Par. 

Gau. 

Par. 

Gau. 

Par 

Gau. 

28 

12. 

24 

16. 

32 

24. 

35 

18  : 

30 

16. 

26 

19. 

33 

17  : 

37 

16. 

32 

4- 

30 

10  : 

35 

18  : 

43 

25- 

34 

0. 

3i 

12. 

39 

22  : 

49 

25. 

40 

11. 

35 
38 

12. 
10. 

4> 

51 

18. 

IO. 

51 

28. 

44 

9- 

48 

10. 

44 

14. 

53 

8. 

6  h. 

20  m. 

52 

I  o. 

46 

12.*. 

55 

15- 

10 

18. 

54 

'5- 

5° 

28. 

5- 

12 

56 

5  h.  40  m. 

4h. 
7 

10  m. 

7  '• 

9- 

14 

27. 

4  h.  50  m. 

18 

23. 
21. 

15 
16 

35- 

41  : 

9 

10. 

7 

10. 

20 

30: 

20 

35- 

1 1 

12. 

11 

8. 

21 

23. 

22 

28. 

'3 

16. 

*5 

IO* 

22 

22. 

26 

17- 

17 

13- 

17 

14. 

28 

14. 

27 

33- 

27 

8: 

!9 

18. 

29 

22. 

28 

17- 

29 

4- 

21 

15- 

35 

25. 

31 

36. 

31 

8. 

23 

9- 

36 

13- 

34 

26. 

33 

10  : 

25 

14  : 

41 

17- 

38 

21. 

4" 

IO. 

29 

T  P 

1  5- 

42 

22. 

39 

23. 

45 

13- 
»3- 

30 
31 

8. 

52 

8. 

42 
45 

26. 

49 

9- 

24. 

5i 

16. 

35 

12  : 
J3- 

5h.  50  m. 

46 

26. 
20. 

4h. 

39 

15 
16 

14. 

37- 

5° 

20  m. 

45 

!7- 

52 
56 

17- 
6. 

8 

15  ■ 

r  Vi 

5  &. 
8 

0  iii. 

9- 

17 

J*. 

16 

15- 
»5- 

19 
21 

17- 
26. 

6  h. 

30  m. 

18 

12. 

10 

'7- 

25 

17- 

9 

39- 

22 

14: 

12 

9- 

27 

13  : 

J3 

32- 

24 

!3- 

14 

16. 

29 

12. 

15 

35  : 

26 

1 1. 

18 

13- 

3i 

>5  ■■ 

19 

37: 

30 

12  : 

22 

1 1  : 

33 

17  : 

21 

43- 

32 

8. 

24 

15- 

35 

20. 

23 

20  : 

35 

9- 

28 

17- 

4' 

20  : 

25 

25.-. 

36 

9- 

30 

13- 

5i 

16. 

27 

28  : 

42 

12. 

31 

9- 

31 

37- 

44 

19. 

35 

11. 

6h. 

0  m. 

33 

38. 

46 

20. 

42 

19. 

8 

IO  : 
19. 

20. 

35 

29. 

5° 

14. 

52 

21. 

10 
12 

37 

15- 

52 

11. 

54 

11. 

41 

20. 

54 

20. 

57 

22  : 

14 

31  : 

45 

25- 

4h.  30  m. 

5h. 

10  m. 

16 
18 

27. 
24. 
26. 
25. 

49 
5i 

22. 
17- 

9 
'5 

11. 
'5- 

9 
21 

18. 
15: 

!9 

22 

53 
55 

14. 
J5- 

21 

10. 

23 

22. 

26 

17- 

6  k. 

23 

14. 

31 

17- 

27 

26: 

40  m. 

25 

;5- 

33 

17  : 

28 

15- 

8 

35- 

17 

12  : 

35 

20. 

29 

30. 

10 

43- 

29 

13  : 

39 

17- 
11. 

34 

23. 

12 

34- 

30 

5- 

5i 

38 

8. 

14 

45- 

31 

14. 

5h. 

20  m. 

40 

19. 

15 

35- 

32 

12. 

48 

19. 

16 

58. 

33 

12  : 

6 

8. 

5° 

10  : 

18 

54- 

35 

18  : 

8 

12  : 

52 

19. 

24 

36. 

39 

9- 

20 

20. 

54 

29: 

26 

29. 

41 

16. 

24 

14. 

57 

9- 

36 
40 

25- 
20. 

45 

19  : 

35 

21  : 

6h. 

49 

10. 

38 

22. 

10  m. 

43 

17- 

5i 

15- 

5° 

5- 

9 

28. 

46 

35- 

53 

13  : 

48 

28. 

J3 

16. 

5  h.  30  m. 

5° 

20. 

15 
16 

40. 
35- 

4  h.  40  m. 

13 

'3- 

52 

16. 

6 

16. 

!5 

18. 

19 

29: 

57 

20. 

8 

10 

12. 
12. 

J9 
21 

17 ' 

22. 

21 

23 

34  •■ 
10. 

6h 

50  m. 

16 

11. 

25 

14. 

25 

28  : 

9 

43- 

20 

12. 

27 

H: 

31 

26: 

1 1 

32. 

22 

16. 

3' 

14. 

33 

18. 

13 

43- 

Par.  Gau. 

60: 
42: 
27. 
36. 
26. 

35  : 
24: 
20  : 


!5 

J9 
23 
27 
31 
33 
35 
41 
46 

49 

52 
57 


19: 
18. 


7  h.  o  m. 

ro  56  : 
63. 
60.' 
48. 

77  : 
46: 
32. 
45  ! 
4*- 
33^ 
25- 
22. 
26. 
20. 
25. 

*7- 
18. 

!3- 
22. 

17- 


7h.  10  m. 
9  60. 

80. 


*3 
J5 
»9 
21 
23 
28 
33 
35 
41 
43 
49 
51 


50. 

75- 
52. 

39- 
60. 
30.' 
30. 
20. 
24: 
19. 
10. 


7  h.  20  m. 

8  50. 
60. 
65. 

74- 
50: 
72. 
73- 
39- 
43- 
42. 
49. 
23.-. 
25. 
16. 

>5- 
21. 


10 
12 

14 
16 
18 

21 
24 
27 
29 
30 
42 

45 
48 

49 
5> 


7  h.  30  m. 
9  200. 


Par.  Gau. 
11  59. 

54- 
120. 
140. 

53- 
68. 

55- 
46. 

57- 
38: 

37- 
30. 
18. 
25  : 
31- 
24: 
25.-. 
27. 


13 
14 
15 

19 
21 

23 
25 
27 
29 

35 
39 
41 
43 
45 
47 
49 
55 


7  h.  40  m. 
10  48. 


16 

19 
21 
40 
42 
52 
53 
54 


105. 

55- 
40. 
29. 

33- 
26. 

13- 

18  : 


7  h.  50  m. 


9 

54  = 

15 

80. 

!9 

84: 

23 

36. 

25 

44- - 

27 

24. 

29 

5J-- 

31 

61  : 

33 

30: 

35 

39: 

49 

»3- 

8h. 

0  m. 

8 

41  : 

10 

66. 

12 

69. 

14 

66. 

18 

65. 

19 

80  : 

21 

82. 

22 

96. 

23 

5°- 

24 

70.- 

25 

36. 

28 

74: 

29 

64: 

32 

43  : 

34 

14: 

35 

26. 

37 

46. 

39 

33- 

42 

34- 

45 

37- 

46 

27  : 

48 

18. 

5i 

22. 

52 

35- 

54 

16: 

DISTRIBUTION  OF  STARS. 


377 


Par. 

Gau. 

Par. 

Gau. 

Par. 

Gau. 

8  h. 

10  m. 

47 

43  : 

2.  c. 

1i 

70. 
6i.\ 

51 

18. 

54 

25. 

15 

55 

22. 

57 

10. 

!9 

21 

71 : 
69: 

8h. 

40  m. 

9h. 

10  m. 

22 

200. 

8 

32: 

9 

10. 

23 

60. 

10 

37- 

J3 

20. 

24 

48. 

14 

31- 

15 

22.'. 

25 

27: 

15 

35  = 

17 

3»- 

27 

21  : 

16 

42. 

!9 

46. 

29 

49- 

18 

29. 

20 

28. 

30 

48. 

22 

30. 

25 

56. 

31 

60  : 

24 

67. 

27 

39- 

3a 

46. 

27 

21. 

31 

9- 

33 

16. 

28 

27. 

33 

49. 

35 

30  : 

32 

55- 

41 

67: 

37 

37- 

34 

48. 

51 

38. 

39 

45- 

38 

80: 

53 

41. 

41 

45.-. 

40 

46. 

55 

33- 

43 

23. 

42 

44. 

45 

28. 

44 

41  : 

9h. 

20  m. 

47 
49 
53 

37: 
17: 
12. 

45 
46 

48 
5° 
5i 

49  : 
33- 
39- 

10 
12 
16 

21. 

25. 
27. 

8h. 

20  m. 

3i- 
29. 

18 

28 

32  : 
30  : 

10 

45  • 

5* 

29. 

29 

45- 

14 
15 

48  : 
58. 

8  h. 

50  m. 

31 
32 

2S. 
12  : 

16 

C2. 

I  I 

34 

58. 

22 

70. 

22. 

36 

120. 

CO. 

*5 

28  : 

40 

68  : 

26 

45- 

17 

48.' 

42 

55- 

Jv 

•)6  : 

J9 

4U  . . 

5° 

34- 

31 

55' 

25 

42. 

1 7 
j  j 

34 

20. 
4.1. 

27 
29 

'7- 

21  . 

9  h.  30  m. 

36 

56. 

3° 

9- 

1 1 

16. 

37 

37- 

31 

41  : 

r3 

17  : 

40 

22. 

33 

DO  : 

15 

19: 

42 

24  : 

35 

70. 

17 

35  = 

44 

32  : 

37 

OS. 

*9 

21  : 

45 

37. 

39 

62  : 

21 

38: 

4° 

44. 

43 

32  : 

23 

36. 

48 

32. 

45 

54  : 

25 

48. 

5° 

20. 

47 

44: 

27 

24. 

51 

24. 

51 

i7- 

29 

59.-. 

52 

26. 

53 

47- 

31 

r5- 

54 

10. 

33 

120. 

- 

5b 

W- 

9h. 

0  m. 

35 
37 

85. 

76: 

8  h. 

30  m. 

10 
12 

24. 
19. 

39 
41 

93- 
65. 

1 1 

24. 

14 

37  : 

45 

50. 

13 

60. 

16 

28. 

53 

23. 

15 

37  = 

18 

47  •• 

55 

22. 

17 

70. 
69/. 

19 

34- 

»9 

20 

45- 

9h. 

20 

75- 

22 

31- 

40  m. 

23 

71  : 

24 

43- 

12 

21. 

H 

53- 

25 

54: 

14 

13: 

27 

5i- 

26 

75- 

15 

22. 

29 

46.-. 

27 

34- 

18 

28. 

31 

73- 

28 

33- 

20 

23  : 

33 

52. 

34 

46: 

25 

36. 

34 

15- 

36 

81  : 

28 

33- 

35 

37- 

38 

97- 

30 

85:: 

37 

54  = 

42 

42. 

32 

43- 

39 

6« 

44 

59- 

34 

125. 

41 

43  : 

46 

60. 

38 

130. 

43 

34  : 

48 

31- 

52 

14. 

45 

53- 

49 

27. 

54 

34- 

Par. 

Gau. 

9  h.  50  m. 

9 

20. 

I  I 

19. 

»3 

15- 

JS 

23  : 

17 

27. 

!9 

26. 

25 

21. 

27 

29. 

29 

54- 

31 

95 : 

33 

103. 

37 

100. 

39 

125. 

41 

150. 

A  C 

C  "3 
J  J' 

51 

19. 

53 

23. 

10  n. 

0  m. 

12 

14. 

■4 

17  : 

18 

18  : 

23 

29. 

24 

22. 

28 

30: 

30 

50. 

32 

70. 

36 

86  : 

38 

85. 

40 

200. 

42 

80. 

45 

39- 

49 

42. 

5i 

!5- 

52 

3°- 

54 

27. 

10  n. 

10  m. 

13 

1 1. 

!5 

>5  '• 

19 

!5- 

23 

26. 

25 

39- 

29 

5i  : 

3i 

90. 

106. 

41 

140. 

43 

70. 

45 

39- 

51 

21. 

52 

32. 

55 

25. 

10  h. 

20  m. 

16 

24. 

18 

27. 

20 

29. 

26 

25  : 

3° 

36. 

32 

44  = 

39 

144. 

44 

60. 

45 

69: 

48 

68. 

49 

41. 

5° 

33- 

54 

27. 

10  h. 

30  m. 

Par. 

Gau. 

J5 

23  : 

23 

29. 

25 

28. 

20 

1  T 

37 

98. 

39 

224. 

60 

AC 

go. 

40 

74- 

C  T 

3  1 

23. 

c  c 

j  J 

10  h. 

40  m. 

14 

16  : 

18 

14. 

24 

16. 

28 

20. 

29 

25. 

30 

33- 

36 

120. 

45 

81  : 

47 

63. 

4s 

38. 

5° 

42. 

10  h. 

co  m. 

9 

15. 

15 

1 1. 

23 

28. 

2C 

23  ; 

7  I 

"3  "5  : 
j3  • 

1  C 

J  J 

48. 

37 

104  : 

43 

56  : 

44 

AO. 
T/ 

45 

QO. 

47 

55. 

AO 

20. 

51 

12  : 

53 

37- 

11  h. 

0  ru . 

10 

16. 

16 

19. 

20 

17- 

29 

36. 

30 

34  : 

31 

38. 

32 

41. 

34 

4s- 

36 

68. 

38 

190  : 

44 

37- 

T) 

5° 

29.-. 

52 

i9. 

53 

37- 

54 

18. 

11  h. 

10  m. 

9 

13  : 

!5 

16. 

23 

16. 

25 

24. 

35 

67. 

37 

61. 

43 

14. 

47 

64: 

49 

36. 

51 

11. 

11  h. 

20  m. 

14 

8. 

Par.  Gau. 


23 

19. 

24 

i7- 

28 

r5- 

30 

28. 

31 

38. 

3° 

47  : 

39 

250. 

42 

40. 

45 

92. 

46 

75- 

40 

31- 

5° 

31- 

52 

56. 

56 

20. 

11  h. 

30  m. 

7 

8. 

J5 

9- 

29 

24. 

31 

46  : 

33 

D2. 

39 

14-O. 

43 

54: 

46 

53- 

48 

42. 

49 

23  : 

51 

34- 

53 

35- 

55 

22. 

11  h. 

40  m. 

6 

9. 

10 

4- 

24 

7. 

26 

26. 

32 

53- 

34 

49  : 

36 

36. 

42 

85. 

45 

80. 

48 

47- 

5° 

11. 

57 

29. 

11  h. 

50  m. 

7 

6. 

Q 

7 

12. 

23 

20. 

20 
y 

21. 

3i 

45- 

33 

5i- 

35 

43- 

43 

88. 

44 

94. 

45 

72. 

53 

35- 

55 

J5- 

57 

29. 

12  h. 

0  m. 

16 

9- 

21 

14. 

28 

33- 

3° 

38: 

34 

44. 

36 

38. 

42 

120. 

44 

61  : 

45 

89. 

+6 

98. 

Par. 

Gau. 

52 

"5  : 

54 

25. 

12  n. 

10  m. 

7 

5- 

'5 

10. 

25 

13- 

29 

22  : 

30 

29. 

31 

41.-. 

33 

53- 

37 

51- 

43 

99  : 

47 

7- 

55 

24. 

12  n. 

20  m. 

6 

9- 

20 

27. 

30 

26  : 

31 

50. 

32 

OO. 

34 

55- 

38 

67. 

42 

9- 

49 

48. 

54 

12. 

12  h. 

30  m. 

7 

6  : 

'9 

19. 

25 

11. 

29 

!3- 

31 

45- 

37 

72. 

43 

48. 

44 

7- 

47 

42. 

53 

9- 

55 

36. 

12  £1. 

40  m. 

6 

5- 

8 

10. 

18 

16. 

20 

J3- 

24 

12. 

25 

20  : 

36 

63. 

42 

38: 

A  A 
T-T 

68. 

48 

36: 

49 

20. 

5° 

17  : 

54 

24. 

12  h. 

50  m. 

7 

10. 

8 

1. 

21 

14. 

29 

5*- 

3i 

24. 

37 

80. 

47 

77- 

5i 

53 

25. 

13  h. 

0  in. 

6 

5- 

8 

7- 

Par.  Gau. 


5  D 


14 

10. 

30 

28  : 

32 

45  : 

36 

48. 

38 

115. 

40 

90. 

42 

85- 

48 

66. 

5° 

29  : 

52 

30  : 

54 

I7- 

eft 
5° 

24. 

13  h. 

10  m. 

7 

16. 

3 1 

JT 

33 

42. 

37 

62. 

39 

54- 

42 

118. 

43 

103. 

47 

95  ■■ 

5i 

40. 

53 

39- 

55 

43- 

13  h. 

20  m. 

6 

4- 

16 

12. 

28 

•  17- 

32 

46. 

36 

55- 

38 

6S. 

40 

105. 

44 

59- 

46 

100. 

48 

62  : 

5° 

44. 

52 

45- 

13  h.  30  m. 

15 

14. 

25 

18. 

29 

26. 

33 

50. 

37 

66  : 

39 

65: 

45 

35- 

47 

77- 

49 

57- 

5i 

43- 

53 

44. 

13  h. 

40  m. 

6 

6. 

8 

7- 

14 

9- 

16 

14. 

30 

30. 

32 

33- 

38 

72. 

40 

90. 

42 

105. 

44 

65. 

48 

68  : 

5° 

39- 

52 

24. 

54 

18. 

56 

24. 

378 


OF  THE  STATISTICAL 


Par. 

Gau. 

Par. 

Gau. 

13  h. 

50  m. 

16 

12. 

15 
29 

35 

18. 

3* 

53- 

30. 
30. 

36 
38 

52. 
28  : 

39 

60  : 

40 

22  : 

43 
45 

88. 

44 

93- 

55- 

48 

62: 

47 
49 

70. 
32  : 

52 
54 

52- 
26. 

5i 

53 

33- 
42. 

14  h.  50  m. 

55 

23. 

5 

«3- 
19. 

9 

14  11. 

0  m. 

15 

14. 

6 

1 1. 

27 

53- 

14 

10. 

3i 

34- 

16 

16. 

33 

50. 

24 

17- 

37 

40. 

26 

27. 

39 

20. 

28 

29. 

43 

46. 

32 

33- 

45 

78. 

36 

18. 

47 

85. 

42 

250. 

49 

53- 

44 
48 

52. 
56: 

5i 

48. 

5° 

36: 

15  h. 

0  m. 

52 

43- 

2 

'3- 

54 

23. 

6 

7- 

14  h. 

10  m 

8 

10 

14. 
17- 

7 

5- 

14 

19. 

15 

15  = 

16 

23. 

32 

36. 

24 

30. 

43 

106  .■. 

28 

45. 

45 

29. 

38 

25  .• 

47 

74- 

39 

20. 

5i 

34- 

40 

37- 

42 

44 
46 

32. 
160. 
69: 

14  h. 

20  m. 

14. 

48 

49. 

*4 

'5- 

5° 

43  •'• 

16 

9- 

53 

18. 

3° 

„  q 
25. 

54 

15- 

i'r 
36 

1  *7 

46. 

15  h. 

10  m. 

38 

41  > 

41 

87: 

5 

17- 

44 

61. 

7 

13- 

46 

53  : 

«3 

18. 

5° 

43- 

15 

8. 

53 

23. 

27 

55- 

31 

38. 

14  h. 

30  m. 

33 
35 

49. 

77: 

8 

11. 

37 

48. 

9 

21. 

39 

18. 

J5 

12  : 

41 

60. 

31 

24. 

43 

93: 

37 

38. 

45 

85: 

43 

70. 

47 

74: 

45 

49. 

5i 

57- 

47 

77- 

49 

62. 

iSh. 

20  m. 

5> 

53- 

16. 

53 

26. 

8 

12 

14- 

14  h,  40  m. 

24 
30 

20. 
38. 

7 

14. 

32 

39- 

8 

19. 

36 

47- 

14 

16. 

40 

72  : 

Par 

rur. 

Gau, 

Par. 

Gau. 

44 

74.-. 

10  n. 

10  m. 

48 

52: 

3 

14- 

8  : 

co 

41. 

7 

52 

3°- 

9 

13- 

5° 

30. 

11 

28. 

ic  h 

3  m- 

13 
15 

0. 
13  : 

3 

!3- 

23 

II  : 

9 

21. 

33 

50. 

!3 

19. 

43 

76. 

T  r 

35  •'• 

81. 

23 

24. 

49 

3i- 

33 

65. 

10  n. 

36 

54- 

20  m. 

37 

2D. 

2 

14. 

39 

IO3. 

6 

16. 

45 

69. 

10 

1 1. 

46 

67. 

1 1 

1. 

47 

65.-. 

J4 

J3- 

r  T 

i 1 

CO 

16 

4- 

c  1 
S3 

24 

17- 

lSh. 

30 

40. 

40  m. 

34 

56. 

2 

5- 

39 

49. 

6 

12. 

46 

36. 

10 

18. 

5° 

42. 

10. 

52 

29. 

16 

20. 

53 

20. 

22 

46. 

54 

24 

23. 

16  h. 

34 

30. 

30  m. 

3s 

00. 

3 

!3- 

40 

7 

i7- 

48 

54- 

9 

12  : 

5° 

41 : 

1 1 

24. 

53 

26. 

13 

12. 

54 

22. 

15 

16: 

!9 

20. 

15  h. 

50  m. 

23 

52: 

3 
7 

14. 
17- 
1S- 

T  8  • 

1 0  •  . 

31 
43 
45 

150. 
70  : 
40. 

9 

*5 

23 
27 

49 

35- 

32  : 

20. 

51 
53 

35- 
30. 

33 
37 

20. 
60. 

16  h. 

40  m. 

45 

8l. 

8 

12  .•. 

47 

54  : 

12 

17  : 

49 

32. 

1 1  : 

51 

44  ' 

20 

50. 

1  c 

j  j' 

70. 

24 

56. 

16  h. 

8 

0  m. 
17  : 

36 

44 
48 

71- 

60. 
32. 

12 

16. 

16: 
25. 

52 

32/. 

14 
16 

56 

21. 

22 
24 

45- 
10. 

16  h. 

50  m. 

26 

15- 

3 

16. 

32 

25. 

7 

22. 

36 

200. 

9 

5  : 

40 

77- 

1 1 

12. 

44 

70  : 

!3 

37- 

46 

65. 

15 

34  = 

48 

70. 

23 

45- 

52 

25  : 

35 

53- 

54 

22, 

39 

68. 

56 

24. 

45 

44. 

Par. 

(  iUU. 

47 

53- 

49 

48. 

53 

22  : 

17  h. 

0  m. 

2 

1 1. 

g 

10 

29. 

12 

60. 

14 

J  I 

16 

50. 

18 

42. 

22 

40. 

24 

30. 

28 

60. 

36 

80. 

38 

41. 

42 

61. 

4U 

45  :  : 

5° 

43- 

52 

16. 

53 

IQ. 

54 

17- 

17  h. 

10  m. 

3 

7. 

7 

25. 

9 

15. 

13 

48. 

15 

IS- 

39 

37. 

43 

58. 

A  C 
MO 

c  1 
S3- 

47 

37- 

AQ 
T7 

AC. 

51 

12  : 

17  h. 

20  in. 

6 

1. 

8 

19  : 

10 

50. 

12 

66. 

20 

0. 

22 

27. 

40 

36. 

44 

34  •*• 

48 

38. 

52 

28. 

54 

11. 

56 

*S> 

17  h. 

30  m. 

5 

6. 

6 

1. 

7 

13  : 

8 

24. 

9 

52  : 

!3 

21. 

15 

30. 

23 

59- 

31 

100. 

39 

32. 

43 

37  : 

45 

40: 

47 

38. 

49 

37- 

51 

24: 

53 

33- 

Par.  Gau. 


17  h. 

40  m. 

2 

29. 

6 

16. 

8 

21. 

10 

72. 

12 

27. 

19 

200. 

20 

130. 

22 

neb. 

38 

62. 

42 

30. 

46 

35  ••• 

5° 

3i- 

53 

12. 

55 

14. 

17  h. 

50  m. 

9 

18. 

1 1 

43- 

14 

neb. 

19  inniim. 

27 

150. 

31 

84. 

39 

37- 

41 

29. 

42 

23. 

45 

54  = 

47 

45- 

18  h. 

0  m. 

4 

12. 

6 

14: 

8 

23: 

10 

53  : 

16 

23. 

'9 

innitm. 

24 

1 10. 

26 

17- 

30 

63. 

34 

50. 

38 

36. 

40 

31  : 

42 

50. 

43 

19. 

44 

42  : 

46 

43- 

48 

26. 

52 

20. 

56 

»7- 

18  h. 

10  m. 

5 

8. 

7 

22. 

8 

50. 

9 

80. 

10 

49. 

J9 

innum. 

20 

do. 

2 1 

do. 

22 

do. 

27 

60. 

31 

76. 

43 

35- 

44 

28. 

45 

31  : 

53 

23. 

18  h. 

20  m. 

6 

18  : 

7 

I. 

Par. 

Gau. 

25 

55- 

AO 
4U. 

3° 

if, 
30. 

33* 

44 

38- 

40 

34  • 

5° 

25  : 

54 

25. 

18  h. 

30  m. 

4 

Ticfl. 

c 

j 

I  CO. 

1 

6c. 

9 

53- 

*9 

nfi 

90. 

6c 
05. 

c6 

a6  • 

3 1 

40. 

35 

6n 
09. 

37 

r  t 

5  *■ 

39 

28. 

41 

19. 

43 

28. 

47 

37- 

5» 

16. 

53 

100. 

18  h. 

40  m. 

0 

39  : 

10 

40. 

IS 

72. 

26 

29. 

36 

34- 

38 

29. 

42 

29. 

44 

3>- 

45 

22. 

48 

31- 

54 

9- 

18  h. 

50  m. 

7 

66. 

IQ 

"3Q. 

27 

36. 

31 

42. 

35 

37. 

43 

25. 

45 

27. 

AO 

28. 

52 

16. 

19  h. 

0  m. 

6 

53- 

10 

63. 

14 

72. 

28 

47  = 

32 

22. 

34 

34- 

38 

21. 

40 

!3- 

42 

23  : 

46 

31- 

48 

15- 

5° 

21. 

51 

19. 

52 

24. 

54 

17- 

56 

1 1. 

Par. 

Gau. 

19  h. 

10  m. 

7 

57- 

!3 

80. 

33 

23- 

37 

36. 

41 

!5- 

45 

18  : 

19  h. 

20  m. 

g 

39* 

12 

6S. 

32 

32. 

36 

31  : 

38 

20. 

42 

23. 

44 

20  : 

46 

20  : 

48 

25. 

5° 

26. 

19  h. 

30  m. 

«3 

31- 

33 

33- 

35 

21. 

43 

20. 

49 

20. 

51 

23. 

53 

1 1. 

55 

*3- 

19  h. 

40  m. 

J4 

29. 

22 

'7- 

34 

27  : 

42 

12. 

44 

2  . 

19  h. 

50  m. 

13 

24. 

35 

25- 

43 

18. 

47 

29. 

49 

14. 

20  h 

0  m. 

12 

3*' 

28. 

24 

18. 

IQ 
J 

1  c. 

36 

17: 

40 

16. 

44 

16. 

48 

18  : 

49 

18. 

52 

19. 

54 

IO. 

20  h. 

10  m. 

»3 

19. 

21 

29. 

27 

22. 

3i 

»3- 

41 

18. 

45 

17- 

47 

12. 

49 

19. 

53 

17- 

DISTRIBUTION  OF  STARS. 


379 


Par. 
20  h. 

20 
26 
32 
34 
38 
40 

42 
46 

5° 
54 

20  h. 

'3 
21 

25 
27 

43 
45 
47 

53 


Gau. 


20. 
22. 

!3- 

16. 

15- 
22. 
17  : 
20. 
20  : 
17- 


30  m. 

14. 

23  : 
8. 

9- 
14: 

9- 
16. 
21. 


20  h.  40  m. 


20 
24 
36 
48 
5° 
5i 
52 


11  : 
14. 
21  : 
14. 
19. 

13- 
14. 


Par. 

Gau. 

20  h. 

50  m. 

25 

16. 

27 

9* 

29 

21. 

35 

21. 

43 

15- 

48 

J3- 

49 

12. 

21  h 

0  m 

4 

12. 

22 

II  : 

26 

II. 

28 

12. 

30 

15- 

38 

17- 

42 

15- 

44 

13- 

46 

19. 

5° 

!3- 

21  h. 

10  m. 

3 

12. 

21 

is- 

25 

7- 

4i 

9- 

43 

10. 

45 

'3- 

49 

22. 

5i 

14. 

52 

16. 

Par. 

Gau. 

u 

21  D. 

20  m. 

2 

12. 

20 

19. 

24 

6. 

26 

18. 

40 

17- 

44 

20. 

48 

19. 

5° 

12. 

53 

14- 

2 1  n. 

30  in. 

3 

11. 

21 

18. 

25 

9- 

27 

15- 

29 

14. 

35 

7- 

43 

19: 

45 

10. 

47 

18. 

49 

13- 

51 

7- 

53 

10. 

21  h. 

40  m. 

22 

17- 

26 

12. 

30 

10. 

40 

10. 

41 

7- 

Par. 

Gau. 

42 

10. 

5° 

*4- 

52 

9- 

54 

22. 

21  h. 

50  m. 

25 

4- 

27 

14. 

35 

'3- 

41 

13. 

49 

J5- 

51 

9- 

22  n. 

0  m. 

2 

12. 

24 

5- 

34 

5- 

40 

12. 

42 

10. 

44 

14. 

48 

9- 

5° 

9- 

52 

18. 

22  h. 

10  m. 

21 

15- 

27 

10. 

29 

18. 

39 

14. 

4i 

8. 

53 

18. 

Par. 

Gau. 

Par. 

Gau. 

Par. 

Gau. 

22  h. 

20  m. 

22  h. 

50  m. 

47 

9- 

4 

6. 

3 

-  # 
7- 

53 

20. 

28 

30 

3- 
7- 

25 
29 

7- 
6. 

21  h. 

20  m. 

36 

6. 

35 

9- 

6 

2. 

40 

17- 

4i 

6. 

16 

6. 

*3- 

45 

10  : 

22 

4- 

CO 

I  C  ! 

47 

9- 

24 

4- 

52 

13- 

49 

10. 

30 

7  : 

54 

6. 

51 

VI  • 

34 

6. 

r5- 

23  n. 

30 

22  h. 

30  m. 

0  m. 

40 

14. 

8 

5- 
1. 

44 

7- 

3 

9. 

y 

18 

4° 

21 

8. 

22 

2. 

25 
35 

7- 
11. 

24 
26 

2. 
8. 

52 
54 

*3- 
r3- 

41 

45 
47 

14. 

6. 
14. 

'5  : 

*3- 

28 
38 

23  h. 

30  m. 

49 

14. 

40 

J3- 

3 

1 1. 

53 

14. 

42 

10. 

13 

0. 

46 

5  = 

17 

6. 

22  h. 

5° 

'5  s 

21 

10. 

40  m. 

52 

10  : 

27 

7- 

2 

5- 

54 

10. 

29 

6: 

20 

17- 

56 

10. 

35 

3- 
6. 

26 

8  : 

23  h. 

37 

36 

5- 

10  m. 

39 

14. 

38 

9- 

17 

7- 

41 

18. 

44 

»3- 

35 

1 1. 

45 

11. 

48 

'3  : 

37 

14. 

47 

8. 
16. 

5° 

9- 

41 

26. 

49 

52 

9- 

45 

8: 

5i 

14. 

Par. 

Gau. 

23  h. 

40  m. 

4 

13- 

8 

7- 

18 

7- 

26 

7- 

28 

8. 

30 

4- 

38 

7  : 

40 

12. 

42 

12. 

44 
46 

12. 

8. 

5° 

10  : 

54 

II. 

56 

18. 

23  h. 

50  m. 

7 

3- 

'3 

8. 

15 

9- 

17 

5- 

2 1 

5- 

35 

9- 

37 

7- 

39 

10. 

41 

7- 

43 

8. 

45 

12. 

49 

1 1. 

53 

19. 

(300)  In  order  to  examine  how  far  the  induction  alluded  to  in  Arts.  (293)  and  (294)  is  borne 
out  by  the  system  of  observations  above  described,  the  following  process  was  instituted.  The 
poles  of  the  great  circle  marking  on  a  celestial  globe  the  medial  line  of  the  Milky  Way,  which 
may  be  called  the  Galactic  circle,  were  found,  and  their  places  ascertained  to  be  in  0h  47m  R  A 
and  116°  0'  N  P  D  for  the  southern  pole,  and  12h  47m  R  A,  64°  O'NPD  for  the  northern. 
With  these  poles,  a  series  of  parallels  to  the  Galactic  circle  were  described  on  an  18-inch 
celestial  globe,  dividing  the  heavens  into  zones  15°  each  in  breadth,  six  on  the  south,  and  six  on 
the  north  side  of  the  Milky  Way ;  and  the  points  of  intersection  of  these  with  the  meridians  of 
0h  0m,  0h  20m,  0h  40m,  &c.  being  read  off  in  N  P  D,  by  the  aid  of  the  brass  meridian  arc  (a  process 
quite  accurate  enough  for  the  purpose),  every  such  point  was  transferred  to  the  chart  mentioned 
in  Art.  (297),  containing  the  actual  projections  of  all  the  observed  gauges.  These  points  were 
then  connected  by  regular  curves,  which  are,  consequently,  the  projections  of  the  galactic 
parallels  in  question,  the  spaces  between  them  being  the  projections  of  the  zones  into  which  they 
divide  the  surface  of  the  sphere. 

(301)  This  done,  the  next  step  consisted  in  counting  the  number  of  fields  of  view  actually 
laid  down  on  the  charts  in  the  region  occupied  by  each  zone,  seriatim ;  and  in  adding  together 
into  one  sum  the  numbers  of  stars  therein  observed,  or  the  gauge  numbers  as  they  actually 
occurred  on  the  chart,  and  the  following  are  the  results  obtained : — 

(302)  In  the  oval  representing  the  circle  of  15°  radius  surrounding  the  southern  pole  of  the 
Galactic  circle,  were  found  to  have  been  observed  forty-three  fields,  containing  in  all  260  stars, 
which  gives  for  the  average  density  of  stars  in  this  region  of  the  heavens  6-05  stars  to  a  field  of 
15'  in  diameter,  visible  in  the  20-feet  reflector  with  the  usual  sweeping  power  180. 


380 


OF  THE  STATISTICAL 


(303)  In  the  zone  comprised  between  the  parallels  of  15°  and  30°  Galactic  south  polar  dis- 
tance 144  gauges  were  found  to  occur,  containing  an  aggregate  of  953  stars,  or  6*62  stars  to  a 
field. 

(304)  In  the  zone  comprised  between  30°  and  45°  were  observed  218  gauges  containing 
1980  stars,  which  gives  an  average  of  9-08  stars  to  a  field. 

(305)  In  the  zone  from  45°  to  60°  were  found  375  gauges  containing  5060  stars,  being 
13  49  stars  to  a  field. 

(306)  From  60°  to  75°  are  found  to  have  been  observed  472  gauges  containing  12409 
counted  stars,  whence  the  average  of  26*29  stars  to  a  field. 

(307)  From  75°  to  90°,  being  the  zone  immediately  adjacent  to  the  Milky  Way  on  the  south 
side,  and  containing  half  its  breadth,  442  gauges  are  registered  containing  26105  stars.  Among 
these  occur  some  gauges  in  which  the  stars  are  set  down  as  "  innumerable,"  or  so  crowded  as  to 
be  impossible  to  count  them  without  bestowing  more  time  and  care  than  the  nature  of  the  object 
in  view  was  judged  to  require.  These  are  taken  when  they  occur  at  200  stars  to  the  field,  which 
is  certainly  not  an  excessive  estimate.  There  are,  however,  not  above  five  or  six  gauges  in  this 
predicament.  The  average  density  of  stars  in  this  zone,  according  to  the  numbers  above  stated, 
is  5 9 '06  stars  to  a  field. 

(308)  A  zone  of  3°  in  breadth  bisected  throughout  by  the  Galactic  circle,  or  extending  1^° 
on  its  north,  and  as  much  on  its  south  side,  was  found  to  include  eighty-four  gauges  containing 
6258  stars,  giving  an  average  of  74*50  stars  to  a  field.  The  average  wrould  have  been  much 
higher  if,  instead  of  following  the  course  of  this  circle,  a  zone  of  equal  breadth  pursuing  the 
irregular  line  of  maximum  intensity  of  the  Milky  Way  had  been  chosen,  which  in  some  places 
deviates  by  several  degrees  from  the  great  circle  which  expresses  its  general  situation.  Judging 
from  the  course  of  the  counted  gauges  only,  the  mean  density  of  stars  in  the  medial  line  of  the 
actual  galaxy  in  that  part  I  have  observed  would  be  somewhere  about  ninety  stars  to  the  field, 
but  this  must  be  considered  as  exclusive  of  the  more  densely  clustering  masses. 

(309)  On  the  northern  side  of  the  Galactic  circle,  the  numbers  of  gauges  registered  in  my 
observations,  with  their  respective  aggregates  and  averages  of  stars,  run  as  follows  : — 


Number 

Aggregate 

Average  of 

of  Gauges 

of  stars 

stars  in 

Zone. 

observed. 

counted. 

a  field. 

90° 

to 

105°  Galactic  S  P  D 

321 

16461 

51.28 

105° 

to 

120°      „       „       .       .  . 

195 

4576 

23.47 

120° 

to 

135°  „   

G8 

982 

14.46 

135° 

to 

150°      „      „      .      .  • 

21 

162 

7.71 

(310)  Nothing  can  be  more  striking  than  the  gradual  but  rapid  increase  of  density  on  either 
side  of  the  Milky  Way  as  we  approach  its  course,  and  the  reproduction  of  nearly  the  same  law  of 
graduation  on  the  north  side  which  holds  good  on  the  south,  so  far  as  the  comparative  paucity  of 
the  gauges  taken  in  that  direction  allow  us  to  judge.  On  the  whole,  this  induction,  founded  as 
it  is  on  the  actual  enumeration  of  68948  stars  contained  in  2299  fields,  must  be  admitted  as 
decisive  of  the  specific  point  in  question,  and  as  completing  the  evidence  to  the  same  effect 
afforded  by  Sir  William  Herschel's  observations*  in  the  northern  hemisphere. 


*  I  have  purposely  abstained  from  mixing  up  in  any  way  the  gauges  observed  by  myself  with  those  recorded 


DISTRIBUTION  OF  STARS. 


381 


(311)  Were  we  to  calculate  upon  these  averages  the  number  of  stars  visible  enough  to  be  dis- 
tinctly counted  in  the  20-feet  reflector  in  one  hemisphere,  throwing  together  into  one  the  gauges 
observed  in  corresponding  zones  north  and  south  of  the  Galactic  circle,  by  way  of  obtaining  a 
broader  average,  we  should  find  it  to  be  2665786  ;  and  for  the  two  hemispheres,  supposing  them 
equally  rich  5331572,  or  somewhat  less  than  5|  millions.  That  the  actual  number  is  much 
greater  there  can  be  little  doubt,  when  we  consider  that  large  tracts  of  the  Milky  Way  exist  so 
crowded  as  to  defy  counting  the  gauges,  not  by  reason  of  the  smallness  of  the  stars,  but  their 
number.  As,  for  example,  in  the  zone  141°. . .  .143°,  between  the  15th  and  16th  hour  of  R  A 
(/599);  in  the  rich  masses  of  Sagittarius  and  Antinous  mentioned  in  Arts.  (321),  (322);  and 
in  many  other  localities. 

(312)  It  will  of  course  be  understood,  and  a  very  superficial  inspection  of  the  synopsis  of 
gauges  above  given,  suffices  to  show  that  great  local  departures  from  the  general  law  of  distribu- 
tion indicated  in  this  table  occur,  and  that  nowhere  more  remarkably  than  in  the  Milky  Way 
itself,  whose  inequalities  of  density  and  irregularities  of  breadth  and  structure  are  most  conspi- 
cuous and  singular.  On  this  head  I  shall  presently  have  more  to  say.  But,  with  exception  of 
these  portions  of  the  galaxy  itself,  I  find  nothing  in  the  smallest  degree  meriting  to  be  regarded 
as  systematic  in  any  part  of  the  heavens  which  I  have  examined,  as  respects  these  deviations  from 
perfect  regularity.  On  the  contrary,  so  purely  local  are  they,  that  on  a  careful  revisal  of  the 
whole  chart,  I  find  it  difficult  to  specify  any  considerable  areas  over  which  an  average  density  of 
stars  prevails  materially  differing  from  what  might  be  expected  from  the  law  of  density  (regarded 
as  a  function  of  the  Galactic  polar  distance)  indicated  in  the  last  article.  As  respects  mere  local 
inequalities,  the  occasional  occurrence  of  clusters  of  stars  of  the  7th  and  8th  classes  remote  from  the 
Milky  Way,  may  be  regarded  as  fully  compensated  by  the  occurrence  (almost  as  rare)  of  fields  of 
view  totally  devoid  of  any  perceptible  star.  When  such  a  field  has  occurred  in  sweeping,  it  has 
usually  been  noticed  as  a  thing  worthy  of  special  remark,  and  its  place  taken  and  registered  as  an 
object.    The  following  is  a  list  of  places  where  such  blanks  occur. 


h. 

R  A. 
ra. 

s. 

N  P  D. 

0  / 

Sweep. 

h. 

R  A. 
m. 

s. 

N  P  D. 
0  / 

Sweep. 

h. 

R  A. 
m. 

s. 

N  P  D. 

0  / 

Sweep. 

o 

5° 

129 

32  - 

638 

2 

29 

126 

4  — 

635 

16 

8 

24 

114. 

...117 

453 

I 

3 

45 

129 

45  - 

638 

5° 

96 

1  — 

739 

16 

10 

Ill . 

...114 

588 

I 

8 

44 

123 

3  - 

494 

2 

57 

14 

131 

3  - 

638 

16 

10 

34 

126 

59  *5 

460  i 

I 

35 

94 

42  - 

739 

9 

34 

36 

72 

3i  - 

688T 

47 

60  25 

462  5 

I 

38 

125 

23  - 

635 

10 

5° 

32 

166 

15  40 

548 

16 

12 

45 

109 

7  — 

722 

I 

46 

100 

53  - 

650 

16 

6 

0 

126 

39  57 

461 

16 

12 

45 

113 

34 

793+ 

I 

58 

125 

37  - 

635* 

16 

6 

27 

126 

59  35 

462 

16 

12 

112 

55 

588 

by  him,  in  order  to  give  the  corroboration  of  his  views  on  this  important  subject  the  force  of  a  perfectly  inde- 
pendent result,  obtained  from  a  diametrically  opposite  point  of  view,  and  resting  on  a  series  of  observations 
hardly  less  extensive  than  his  own. 

*  Totally  blank,  not  the  smallest  star,  and  the  heavens  here  are  singularly  void  of  stars :  many  fields  are 
blank  all  but  one  or  two  stars  15m.  N.B. — In  this  zone  also  from  O'1  30"  to  1"  39™  occur  many  fields  with  one  cr 
two  stars  only,  of  the  1 5th  or  16th  magnitude. 

t  In  this  zone  (72°. . .  .75°  N  P  D)  between  IO  and  llh  40m  occur  several  blank  fields. 

t  This  blank  extends  from  113°  52'  to  113°  25'  in  P  D,  and  over  a  considerable  space  in  R  A. 

5  E 


382 


OF  THE  STATISTICAL  DISTRIBUTION  OF  STARS. 


h. 

R  A. 
m. 

8. 

N 

0 

P  D. 
/ 

Sweep. 

h. 

It  A. 
m. 

S. 

N  P  D. 

0  / 

Sweep. 

h. 

R  A. 
m. 

s. 

N  P  D. 
0  t 

Sweep. 

16 

J4 

1 

"3 
114 

3  to 

1 1 

! 

588* 

16 

30 

O 
22 

113 

S3 
48 

793  ) 
474  * 

17 
17 

23 
23 

1 

98 

"5 

45 
40 

30 

721 
474 

16 

21 

"3 

IO  — 

588 

16 

37 

1 10 

58 

588 

17 

23 

41 

115 

57 

453 

16 

21 

15 

113 

25  - 

793 

16 

43 

105 

17 

699 

17 

24 

40 

"5 

5° 

30 

474 

16 

23 

9 

114 

24  23 

474 

17 

1 1 

45 

116 

42 

723 

17 

29 

99 

22 

721+ 

z6 

23 

9 

114 

4  S3 

474 

17 

17 

30 

116 

46 

723 

17 

S3 

28 

94 

46 

57 

608 

16 

23 

1 

112 
113 

51  to 

I 
S 

588 

17 

18 

30 

f  116 
I  116 

38 
54 

to  | 

723 

18 
18 

7 

"3 

4 

27 

97 
97 

44 

9 

18 

609 
609 

16 

*5 

32 

114 

14  23 

474 

17 

*9 

IO 

116 

1 1 

453 

23 

43 

127 

29 

636 

16 

27 

113 

0  — 

588f 

17 

2 1 

9 

116 

7 

46 

453 

23 

44 

128 

3 

636 

16 

27 

21 

113 

59  24 

474 

(313)  Hitherto  we  have  considered  merely  the  total  numbers  of  stars  in  our  gauged  fields, 
without  reference  to  their  classification  by  magnitudes.  In  counting  the  gauges,  however,  not 
only  the  total  numbers  were  set  down,  but  those  of  all  the  several  magnitudes  down  to  the  11th 
inclusive,  and  even  of  the  estimated  half  magnitudes  intermediate,  so  that  we  are  not  left  without 
data  for  entering  with  considerable  detail  into  this  part  of  the  general  inquiry.  To  this  end 
the  numbers  of  all  the  stars  of  the  several  magnitudes  below  specified,  occurring  in  the  registered 
gauges,  distributed  in  the  respective  zones  of  Galactic  polar  distance,  have  been  added  together 
and  collected  into  sums :  and  the  following  table  offers  a  synoptic  view  of  the  results  of  this 
operation,  in  which  also  (for  comparison's  sake)  those  which  have  reference  to  stars  of  mixed 
magnitudes  are  inserted. 


Zones 

22 

Total  Number  of  Stars  Registered. 

Deduced  Number  of  Stars  per  100  Fields. 

of  Galactic 

0^  3 

.  T)  ° 

S  P  D. 

O  0)  N 

t  a 

0 

Above 
8  m. 

8  m. 
and 
8' m. 

9  m. 
and 
9  m. 

10  m. 

and 
10' m. 

1 1  m. 

and 
1 1'  m. 

12  m. 

and 
under. 

Above 
8  m. 

8  m. 
and 
8' m. 

9  m. 
and 
9' m. 

10  m. 

and 
10' m. 

11  m. 

and 
1 1'  m. 

12  m. 

and 
under. 

o°  to 

i5° 

43 

2 

0 

3 

20 

31 

204 

S 

7 

47 

72 

474 

15  .. 

30 

144 

7 

9 

32 

54 

80 

771 

5 

6 

22 

38 

56 

535 

30  .. 

45 

218 

10 

16 

38 

86 

165 

1665 

S 

7 

17 

39 

76 

764 

45  •• 

60 

375 

1 1 

22 

68 

158 

410 

439i 

3 

6 

18 

42 

109 

1171 

60  .. 

75 

472 

13 

3° 

109 

268 

758 

1 123 1 

3 

7 

23 

57 

161 

2378 

75  •• 

90 

44a 

28 

48 

170 

391 

1096 

24372 

6 

1 1 

38 

88 

248 

5515 

90  .. 

105 

321 

12 

26 

90 

234 

689 

15410 

4 

9 

28 

70 

215 

4802 

105  .. 

120 

195 

12 

13 

40 

90 

236 

4185 

6 

8 

21 

46 

121 

2145 

120   . . 

i35 

68 

2 

1 

14 

35 

102 

828 

3 

i 

21 

5i 

130 

1240 

135  .. 

150 

21 

0 

1 

1 

5 

17 

138 

5 

S 

*4 

81 

656 

(314)  On  a  general  view  of  this  table  it  appears  that  the  tendency  to  greater  frequency,  or 
the  increase  of  density  in  respect  of  statistical  distribution,  in  approaching  the  Milky  Way,  is  quite 

*  In  all  this  interval  of  P  D  (besides  the  radius  of  the  field  at  either  end),  not  the  smallest  star.  Sky  per- 
fectly pure  and  superb. 

t  Many  other  blank  fields  hereabouts, 
t  One  star  l/m  seen  with  long  attention. 


TELESCOPIC  CONSTITUTION  OF  THE  MILKY  WAY  IN  THE  SOUTHERN  HEMISPHERE.  383 


imperceptible  among  stars  of  a  higher  magnitude  than  the  8th,  and  except  on  the  very  verge  of  the 
Milky  Way  itself,  stars  of  the  8th  magnitude  can  hardly  be  said  to  participate  in  the  general  law 
of  increase.  For  the  9th  and  10th  the  increase,  though  unequivocally  indicated  over  a  zone 
extending  at  least  30°  on  either  side  of  the  Milky  Way,  is  by  no  means  striking.  It  is  with  the 
11th  magnitude  that  it  first  becomes  conspicuous,  though  still  of  small  amount  when  compared 
with  that  which  prevails  among  the  mass  of  stars  of  magnitudes  inferior  to  the  11th,  which  con- 
stitute sixteen-seventeenths  of  the  totality  of  stars  within  30°  on  either  side  of  the  Galactic 
circle. 

(315)  Two  conclusions  seem  to  follow  inevitably  from  this;  viz. — 1st,  That  the  larger  stars 
are  really  nearer  to  us  (taken  en  masse,  and  without  denying  individual  exceptions)  than  the 
smaller  ones.  Were  this  not  the  case,  were  there  really  among  the  infinite  multitude  of  stars, 
constituting  the  remoter  portions  of  the  galaxy,  numerous  individuals  of  extravagant  size  and 
brightness,  as  compared  with  the  generality  of  those  around  them,  so  as  to  overcome  the  effect 
of  distance  and  appear  to  us  as  large  stars,  the  probability  of  their  occurrence  in  any  given  region 
would  increase  with  the  total  apparent  density  of  stars  in  that  region,  and  would  result  in  a  pre- 
ponderance of  considerable  stars  in  the  Milky  Way,  beyond  what  the  heavens  really  present,  over 
its  whole  circumference.  2dly,  That  the  depth  at  which  our  system  is  plunged  in  the  sidereal 
stratum  constituting  the  galaxy,  reckoning  from  the  southern  surface  or  limit  of  that  stratum,  is 
about  equal  to  that  distance  which  on  a  general  average  corresponds  to  the  light  of  a  star  of  the 
9th  or  10th  magnitude,  and  certainly  does  not  exceed  that  corresponding  to  the  11th. 


SECTION  II.— OF  THE  GENERAL  APPEARANCE  AND  TELESCOPIC  CONSTITUTION  OF  THE  MILKY 

WAY  IN  THE  SOUTHERN  HEMISPHERE. 

(316)  The  Milky  Way,  where  it  passes  through  the  constellation  Monoceros,  is  of  great 
breadth  ;  and  is  uniform  and  starless  in  appearance.  Its  axis  nearly  bisects  the  interval  between 
Sirius  and  Procyon,  as  it  does  also  the  smaller  intervals  between  f  and  h  Monocerotis,  between 
s  and  m  of  the  same  constellation,  and  (less  exactly)  between  y  Canis  and  n  Monocerotis.  It 
crosses  the  equinoctial  in  6h  54m  R  A  (for  1800).  The  uniform,  and  (to  the  naked  eye)  starless 
portion  continues  to  about  the  southern  tropic,  in  the  parallel  of  £  Argus.  At  this  point  of  its 
course,  it  subdivides,  sending  off,  in  the  first  instance,  a  narrow  and  winding  branch  on  the  pre- 
ceding side,  which  may  be  considered  as  originating  at  m  Puppis,  and  whose  course  may  be 
traced  nearly  along  its  medial  line  by  the  stars  p,f,  e,  c,  a,  N  Puppis,  as  far  as  y  Argus,  which  it 
involves,  and  where  it  terminates  rather  abruptly.  £  Argus  is  involved  in  this  branch  near  its 
following  border,  where  it  makes  an  elbow,  and  acquires  considerable  intensity.  See  Plate 
XIII.  fig.  1. 

(317)  After  sending  off  this  branch,  the  main  body  of  the  Milky  Way  pursues  its  course 
southwards  to  the  parallel  of  o>  Puppis  and  a  Mali,  where  it  diffuses  itself  broadly,  and  again  sub- 
divides, the  preceding  stream  going  on  with  a  great  increase  of  intensity  to  q  Puppis,  where  it  is 
suddenly  broken  off,  but  resuming,  continues  more  feebly  till  it  finally  terminates  in  a  rounded 
mass,  in  which  are  involved  the  stars  a,  b,f,g,  Velorum.    The  following  stream,  which  is  faint 


384 


GENERAL  APPEARANCE  AND  TELESCOPIC  CONSTITUTION  OF  THE 


and  indefinite,  attains  and  involves  A  Argus,  where  it  also  terminates.  Some  faint  traces  of  a 
fourth  branch  extending  to  and  involving  ^r,  may  also  be  suspected. 

(318)  At  this  part  of  its  general  course,  the  continuity  of  the  Milky  Way  may  be  said  to  be 
almost  entirely  broken  off,  insomuch  that  a  line  may  be  drawn  through  x  Argus,  E,  D,  e  and 
y  Velorum,  cutting  across  its  whole  extent,  and  hardly  perceptibly  affected  by  its  light,  and 
forming,  as  it  were,  a  gap  between  each  of  the  branches  above  specified,  and  their  further 
continuation. 

(319)  On  the  following  side  of  this  gap,  viz.,  at  8  Argus,  at  M,  L  Velorum,  and  at  U  Velorum, 
streams  originate,  more  or  less  corresponding  to  the  aforesaid  branches,  but  more  diffused,  faint, 
and  indefinite,  forming  altogether  a  broad  and  fan-shaped  effusion,  whose  widest  opening 
extends  from  8  Argus  to  q  Velorum,  or  about  18°  in  breadth,  and  which  converges,  increasing  in 
intensity  as  it  narrows  (evidently  indicating  a  foreshortening  by  perspective),  till  it  attains  a 
minimum  of  breadth  between  z  1  +  z  2  Carina:  and  A  Centauri,  which  stars  form  the  promon- 
tories or  head-lands  (so  to  speak)  of  a  small,  but  very  strongly  marked  and  sharply  cut  semi- 
circular bay,  half  way  between  ??  Argus  and  a  Cruris,  on  the  southern  side  of  the  Milky  Way, 
whose  breadth  here  does  not  exceed  4  or  5  degrees,  or  even  less,  if  measured  across  to  the 
concavity  of  a  corresponding  but  less  conspicuous  indentation  on  the  north  side,  having  8  Cruris 
for  the  centre  of  curvature  of  its  contour.  In  all  the  region  from  rj  Argus  to  this  point,  the  Milky 
Way  is  exceedingly  intense.  From  the  star  last  named  it  throws  off  a  short  spur  towards 
i  Argus,  which  terminates  in  a  very  intense  rounded  nebulous  knot,  at  a  point  marked  o,  in 
Bode's  map,  which  is  the  cluster  h.  3224  =  A  297,  in  which  are  the  small  stars  Nos.  3441,  3445, 
3447  of  the  B.  A.  Catal.,  unless,  indeed,  a  faint  effusion  involving  i  Argus,  and  stretching 
onwards  towards  e,  be  regarded  as  connecting  the  Milky  Way  with  the  cluster  h.  3111,  near 
B  Carina,  which  is  very  conspicuous  to  the  naked  eye  as  a  round  nebulous  patch,  and  which 
includes  the  stars  Nos.  2686,  2687,  2694,  and  2695  B.  A.  C. 

(320)  Immediately  after  the  contraction  between  A  Centauri  and  8  Cruris,  the  Milky  Way 
suddenly  expands  so  as  to  include  the  southern  half  of  the  cross  and  the  northern  portion  of 
Musca,  whence  it  proceeds  to  /3  Centauri,  embracing  in  this  wide  expansion  that  singular  vacuity 
on  the  south  following  side  of  the  cross,  called  the  "  Coal-sack,"  a  pear-shaped  oval,  whose 
greatest  length  is  about  8°,  and  breadth  5°,  the  longer  axis  being  nearly  parallel  to  the  line 
joining  a  and  (3  Crucis,  which  line  is  very  nearly  a  tangent  to  the  north-preceding  portion  of  its 
circumference.  As  this  is  always  regarded  by  voyagers  and  travellers  as  one  of  the  most  con- 
spicuous features  of  the  southern  sky,  it  may  not  be  irrevelant  to  state  a  few  particulars  as  to  its 
telescopic  constitution.  It  is  by  no  means  entirely  devoid  of  stars,  the  lowest  gauges  recorded 
being  9  and  7,  and  no  blank  fields  being  specified  as  occurring  in  it.  The  cluster  of  telescopic 
stars  h.  3407  =  A.  272,  is  actually  contained  within  its  area;  and  even  in  the  middle  of  its 
extent  gauges  of  29,  and  48  stars  are  noted.  Its  striking  blackness  is,  therefore,  by  no  means 
owing  to  an  absolute  want  of  telescopic  stars,  but  rather  to  its  contrast  with  the  very  rich  portion 
of  the  Milky  Way  adjacent,  where  the  gauges  run  up  to  98,  100,  120,  and  even  200  on  the  pre- 
ceding side, — to  65,  103,  108,  on  the  following;  68  on  the  south,  and  90  on  the  north.  The 
contrast  is  enhanced  by  the  suddenness  of  the  transition.  The  gauge  65,  occurs  immediately  on 
the  following  edge  of  the  Coal-sack.  In  sweep  778,  the  northern  border  was  definitely  observed 
in  R  A  12h  46m,  NPD  150°  13',  with  the  remark,— "  The  transition  from  rich  Milky  Way  to 


MILKY  WAY  IN  THE  SOUTHERN  HEMISPHERE. 


385 


almost  complete  darkness  is  here  very  sudden ;"  while,  on  the  preceding  edge,  the  gauge  9 
occurs  almost  immediately  on  entering  within  its  precincts. 

(321)  It  is  about  this  region,  or,  perhaps,  somewhat  earlier,  in  the  interval  between 
r)  Argus  and  a  Crucis,  that  the  Galactic  Circle,  or  medial  line  of  the  Milky  Way  may  be  con- 
sidered as  crossed  by  that  of  the  zone  of  large  stars  which  is  marked  out  by  the  brilliant  con- 
stellation of  Orion,  the  bright  stars  of  Canis  Major,  and  almost  all  the  more  conspicuous  stars  of 
Argo — the  Cross — the  Centaur,  Lupus,  and  Scorpio.  A  great  circle  passing  through  e  Orionis 
and  a  Crucis  will  mark  out  the  axis  of  the  zone  in  question,  whose  inclination  to  the  galactic 
circle  is  therefore  about  20°,  and  whose  appearance  would  lead  us  to  suspect  that  our  nearest 
neighbours  in  the  sidereal  system  (if  really  such),  form  part  of  a  subordinate  sheet  or  stratum 
deviating  to  that  extent  from  parallelism  to  the  general  mass  which,  seen  projected  on  the 
heavens,  forms  the  Milky  Way. 

(322)  From  the  Coal-sack,  over  /3,  and  almost  up  to  a  Centauri,  the  Milky  Way  continues 
broad,  unbroken,  and  uniform,  but  just  before  arriving  at  a,  it  divides  into  two  great  and  conspicuous 
streams  (See  PI.  XIII.  fig.  2.),  the  preceding  of  which  passes  over  B  A  C  4977  (miscalled  by  Bode 
i  Lupi),  and  -n  (Bode)  Norma;  =  B  A  C  5136,  its  axis  passing  centrally  between  these  two  stars ; 
thence  to  d  Lupi  (Bode)  =  B  A  C  5123,  which  its  preceding  border  just  attains,  and  from  which 
point  its  intensity,  hitherto  very  great,  rapidly  degrades.  Holding  on  its  course,  it  passes 
centrally  over  -q  Lupi,  and  finally  loses  itself  in  a  faint  effusion,  which  skirts  the  following  side  of 
the  line  of  stars  p,  tt,  8,  /3  Scorpii.  This  branch  is  indicated  in  Bode's  chart  as  terminating  before 
it  reaches  77  Lupi,  near  a  star  there  marked  k. 

(323)  The  following,  or  main  stream,  setting  out  from  a  Centauri  (having  a  Circini  in  the 
middle  of  its  breadth,  and  extending  nearly  to  y  Trianguli),  proceeds  northwards  in  a  very  vivid 
stream  till  it  almost  attains  y  Norma,  including  within  its  breadth  in  the  earlier  part  of  this  its 
course,  a  rather  remarkable  lacuna  of  an  elongated  form,  parallel  to  its  general  direction,  about 
5°  in  length  and  1^°  in  breadth,  commencing  near  a  Circini.  Before  attaining  y  Norma,  this 
branch  is  connected  with  the  preceding  one  described  in  the  last  article  by  a  narrow  and  pretty 
conspicuous  bridge,  which  covers  the  stars  marked  in  Bode's  map  as  1,  a,  and  77  Norma  (B  A  C 
5283,  5209,  5136),  and  which  insulates  a  long  and  somewhat  triangularly  formed  dark  space 
between  the  streams,  having  a  Centauri  at  its  southern  extremity,  and  just  included  within  it. 

(324)  At  y  Norma,  the  main  branch  of  the  Milky  Way  suddenly  makes  an  abrupt  bend  at 
an  angle  of  about  120°  to  the  following  side,  passing  over  two  stars  dignified  in  Bode  by  the 
Greek  letters  p  1  and  p  2  Ara,  but  which  are  invisible  to  the  naked  eye — over  1  Ara,  6  and 
t  Scorpii,  and  y  Tuhi  to  an  exceedingly  bright  and  conspicuous  round  mass  1^°  in  diameter, 
which  is  (or  rather  contains)  the  great  cluster  h.  3706,  and  thence  to  y  Sagittarii,  about  which  it 
forms  one  of  the  most  intense  and  striking  developments  in  the  form  of  an  oval  luminous  mass 
about  6°  in  length  and  4°  in  breadth,  and  in  which,  intermixed  with  gauges  of  200  stars  in  the 
field,  occur  portions  of  such  richness  that  it  was  found  impossible  to  count  the  gauges,  and  that 
in  a  zone  3°  in  breadth,  over  an  interval  of  R  A  from  17h  45m  to  18h  30m  (sweep  723).  A  very 
moderate  calculation  indeed,  would  make  the  number  of  stars  in  this  mass  upwards  of  100,000. 

(322)  From  this  mass  northward,  across  the  ecliptic,  in  the  bow  of  Sagittarius,  and  as  far  as 
Antinous,  the  broken  and  irregular  aspect  of  the  Milky  Way  is  familiar  to  every  European 
observer,  though  much  better  seen  in  southern  latitudes.     On  its  following  side  it  graduates 

5  F 


386 


GENERAL  APPEARANCE  AND  TELESCOPIC  CONSTITUTION  OF  THE 


away  insensibly  ;  but  along  its  preceding  border  it  is  occasionally  very  definitely  terminated,  and 
especially  it  is  broken  by  three  deep  sinuses,  separated  from  each  other  by  conspicuous  pro- 
tuberances, the  one  about  the  star  s  Scuti  (B  AC  6279),  and  the  other  a  most  remarkable, 
regularly  formed,  and  considerably  well  defined  paraboloidal  mass,  projecting  boldly  between  n 
and  /  Scuti  (Fl.  3  and  6  Aquil.),  and  of  an  intensity  and  richness  hardly  inferior  to  that 
adjoining  y  Sagittarii.  From  I  Scuti  a  deep  hollow  extends  to  A  Aquila,  after  which  this  branch 
(which  must  certainly  be  considered  the  main  stream  of  the  Milky  Way,  as  its  continuity  alone 
is  unbroken),  runs  northward  through  Aquila,  without  any  further  distinguishing  feature  to  the 
junction  of  the  two  great  streams  in  Cygnus. 

(325)  Bode's,  and  most  other  celestial  charts,  make  the  Milky  Way  bifurcate,  in  Cygnus  and 
the  tail  of  Scorpio,  into  two  great  streams,  both  of  which,  the  preceding  and  the  following,  preserve 
their  continuity,  from  point  to  point,  unbroken.  This,  however,  is  the  case  only  with  the  fol- 
lowing, or  main  stream,  whose  course  we  have  just  traced.  The  preceding  is  discontinuous. 
Its  northern  portion  (from  Cygnus  southwards)  terminates  precisely  at  the  equator,  just  beyond 
the  bisection  of  a  line  joining  y\  Serpentis  and  (3  Ophiuchi,  and  from  this  to  the  nearest  point  of 
its  southern  continuation  (if  it  can  be  so  considered),  there  is  a  break  of  14°  in  extent  to  the 
star  o  Serpentis,  totally  devoid  of  all  appearance  of  it.  In  order  to  trace  this  southern  portion, 
let  us  return  to  our  point  of  divergence  (Art.  321)  at  y  Norma.  Here,  as  we  have  stated,  the 
following,  or  main  stream,  makes  an  abrupt  elbow,  and  from  this  point  (but  on  the  other  side  of 
y  Normcp,  and  completely  cut  off  it  by  a  narrow  and  strongly  marked  dark  channel,  in  whose 
middle  that  star  is  situated),  this  preceding  stream  sets  off,  running  through  (and  ^  to  e  Scorpii, 
in  a  very  irregular  and  patchy  course.  Northwards  from  e,  it  expands  into  a  vast  effusion,  filling 
nearly  the  whole  area  enclosed  by  e,  1,  Scorpii,  -q  Ophiuchi,  o  Serpentis,  E,  D,  tt  (Bode)  Ophiuchi, 
and  u  Scorpii,  Beyond  o  Serpentis  (as  above  stated),  it  cannot  be  traced  northwards.  It  rather 
sweeps  round  to  the  following  side,  as  if  to  re-unite  itself  with  the  main  stream,  from  which  it 
can,  in  fact,  hardly  be  said  to  be  separated  by  a  dark  interval,  in  which  are  three  lucid  patches 
or  islands,  situated  in  a  line  drawn  from  \x  Sagittarii  towards  i]  Serpentis,  the  southern  and 
brighter  being  near  /x,  the  northern  and  fainter  opposite  to  s  Scuti.  This  tendency  to  a  reunion 
with  the  main  stream,  indeed,  is  conspicuous  in  other  parts  of  its  course.  Thus,  at  \x  Scorpii,  it 
sends  out  a  strong  offset  which  crosses  the  interval  between  the  two  streams  like  a  bridge,  and 
joins  the  following  one  at  6,  i,  k  Scorpii.  So,  also,  another  similar  bridge  crosses  the  interval 
from  u  Scorpii  to  the  conspicuous  round  mass  near  y  Tubi,  mentioned  in  Art.  321,  passing 
between,  and  slightly  involving  the  star  I  (Bode)  Tubi  =  B  A  C  5925,  and  the  place  of  a  star 
marked  f  in  Bode's  constellation  Tubus,  not  visible  to  the  naked  eye. 

(326)  If  we  now  consider  the  telescopic  structure  of  the  region  spread  over  by,  and  enclosed 
between  the  effusions  of  the  Milky  Way  in  the  body  and  tail  of  Scorpio,  the  hand  and  bow  of 
Sagittarius,  and  the  following  leg  of  Ophiuchus,  we  shall  find  it,  in  the  highest  degree,  interesting 
and  complex.  No  region  of  the  heavens,  in  fact,  is  fuller  of  objects,  beautiful  and  remarkable  in 
themselves,  and  rendered  still  more  so  by  their  mode  of  association,  and  by  the  peculiar  features 
assumed  by  the  Milky  Way,  which  are  without  a  parallel  in  any  other  part  of  its  course. 

(327)  To  begin  with  the  preceding  offset  of  all,  which  takes  its  origin  at  a  Centauri.  This 
offers  nothing  peculiar  in  its  internal  constitution,  but  is  separated  from  the  others  by  a  very 
poor  region,  in  which  several  blank  fields  occur  between  the  126th  and  129th  degree  of  P  D,  and 


MILKY  WAY  IN  THE  SOUTHERN  HEMISPHERE. 


387 


so  numerous  are  these  from  the  111th  to  the  117th  in  the  region  adjacent  to  Antares,  as  to  make 
it  doubtful  whether  the  faint  apparent  illumination  between  (3  and  p  Scorpii  be  not  a  mere  effect 
of  contrast  with  the  intense  darkness  on  which  it  borders,  the  more  so  as  the  gauges  in  that 
region,  ranging  only  from  10  to  20  stars  per  field,  indicate  rather  a  poor  than  rich  scattering  of 
stars  thereabouts. 

(328)  The  preceding  stream,  diverging  from  y  Norma,  presents  in  the  more  southern  part  of 
its  course,  as  far  as  Cana"  e  Scorpii,  a  succession  of  rich  clusters  of  the  7th  and  8th  classes.  In  the 
bridge  connecting  e  with  6  Scorpii,  occur  a  globular  cluster,  and  one  of  the  only  two  annular 
nebulae  in  the  southern  hemisphere  (h.  3680).  But  in  the  northern  portion,  from  the  120th  to 
the  108th  degree  of  P  D,  this  branch  is  thickly  set  with  fine  globular  clusters,  all  of  which  occur 
within  its  starry  area,  and  none  in  the  dark  region  intervening  between  the  streams.  Immediately 
on  the  following  edge  of  this  stream,  between  the  113th  and  114th  parallel  of  P  D,  occurs  the 
other  annular  nebula  (h.  3686).  The  richest  portion  of  this  stream  is  between  the  118th  and 
and  119th  parallel,  when  the  gauge  indicates  120  stars  per  field,  from  which  point  northwards  they 
decrease  to  42,  60,  40,  37,  48,  &c,  and  finally  again  attain  60  and  66.  Following  e  Scorpii,  in 
the  interval  between  that  star  and  A,  this  branch  first  presents  the  phenomenon  of  nebulosity 
irresolvable  in  the  20-feet  reflector.  "  Sweep  791,  16h  48m.  The  northern  part  of  the  zone 
(P  D  122°  52')  is  Milky  Way,  but  strangely  mixed,  of  patches  of  stars,  and  starless  space,  and 
light  in  the  field  without  stars  enough  to  account  for  it,"  an  appearance  which  ceases,  however, 
when  we  leave  this  branch  and  enter  on  the  region  intervening  between  the  streams  where  it  is 
noticed  in  the  same  sweep,  that  at  17h  13m  "  the  northern  end  of  the  zone,  though  pretty  rich  in 
sta?s,  is  yet  quite  free  from  brightness  of  ground.    It  is  as  black  as  a  coal." 

(329)  The  constitution  of  the  following,  or  main  stream,  is  much  more  intricate  and  various. 
Besides  being  thickly  set  with  superb  globular  clusters,  from  y  Tuhi  to  the  113th  degree  of  P  D, 
its  course  from  the  126th  to  the  117th  degree  is  broken  up  into  a  succession  of  nebulous  and 
semi-nebulous  or  barely  resolvable  masses,  of  small  extent,  and  singularly  insulated  from  each 
other,  and  from  the  starry  portions.  The  superb  nebulas  8  Messier  and  H.  IV.  41,  with  its  trifid 
companion,  which  occur  on  or  near  its  anterior  border,  seem  to  be  only  intense  exaggerations  of 
these  nebulous  appearances  and  patches,  of  which  a  large  catalogue  might  easily  be  made.  In 
describing  the  nature  of  these  appearances,  and  the  general  telescopic  aspect  of  this  region,  it  will 
be  better  to  let  the  observations  speak  for  themselves,  as  actually  recorded. 

(330)  In  sweeps  791,  792,  after  passing  across  the  dark  interval  between  the  two  streams  of 
the  milky  way,  comprised  between  the  two  connecting  streaks  or  bridges  mentioned  in  Art.  322, 
in  the  zone  of  Polar  distance  between  123°  and  126°,  the  coming  on  of  the  great  stream  is  thus 
described: — "  17h  32m  124°  16'  the  northern,  and  124°  55'  the  southern,  edge  of  a  great  nebulous 
projection  of  the  Milky  Way  of  great  extent  running  horizontally.  At  the  former  Polar  distance, 
the  northern  half  of  the  field  of  view  has  stars  on  a  black  ground.    After  this  the  Milky  Way 

becomes  very  nebulous,  in  great  cirrous  masses  and  streaks."  "17h  31m  ±.  Hereabouts 

begins  a  series  of  great  nebulous  and  semi- nebulous  milky  way  patches  over  the  whole  breadth 
of  the  zone  from  123°  31'  downwards  to  126°."  At  I7h  34m  31.4s  occurs  (as  a  highly  character- 
istic specimen)  the  mass  figured  in  PI.  V.  Fig.  1,  and  described  in  the  Catalogue  of  Nebulae, 
where  it  will  be  found  under  its  proper  R  A,  and  in  due  succession  the  analogous  masses 
described  in  the  Catalogue  as  h.  3704,  3708,  3709,  which,  it  is  remarked,  occur  "  among  alterna- 


3S8 


GENERAL  APPEARANCE  AND  TELESCOPIC  CONSTITUTION  OF  THE 


tions  of  vacuity  and  richness  most  surprising,  and  baffling  all  description."  As  the  main  body  of 
the  Milky  Way  comes  on,  the  frequency  and  variety  of  these  masses  increases.  At  17h  50m,  the 
following  remarks  occur  in  the  sweeps  specified.  "  Here  the  Milky  Way  is  composed  of  separate, 
or  slightly,  or  strongly,  connected  clouds  of  semi-nebulous  light ;  and,  as  the  telescope  moves, 
the  appearance  is  that  of  clouds  passing  in  a  scud  as  the  sailors  call  it."  "  I  could  fill  a  cata- 
logue with  the  clusters  of  the  6th  class  which  are  here.  The  Milky  Way  is  like  sand,  not  strewed 
evenly  as  with  a  sieve,  but  as  if  flung  down  by  handfuls  (and  both  hands  at  once),  leaving  dark 
intervals,  and  all  consisting  of  stars  14...16...20m,  down  to  nebulosity,  in  a  most  astonishing  man- 
ner." Again,  at  17h  53m,  "After  an  interval  of  comparative  poverty,  the  same  phenomenon, 

and  even  more  remarkable.  I  cannot  say  it  is  nebulous.  It  is  all  resolved,  but  the  stars  are 
inconceivably  numerous  and  minute.  There  must  be  millions  on  millions,  and  all  most  unequally 
massed  together,  yet  they  nowhere  run  to  nuclei  or  clusters  much  brighter  in  the  middle.''''  This 
extraordinary  exhibition  terminates  about  the  eighteenth  hour  of  R  A  (where  the  Milky  Way 
resumes  its  usual  appearance),  with  the  planetary  nebula  h.  3734. 

(331)  In  the  zone  next  adjacent  (120°...  123°),  the  nebulous  appearance  of  the  anterior  edge 
of  the  great  stream  comes  on  later,  and  is  less  broken  into  distinct  masses.  In  some  places  it  is 
even  sharply  defined,  a  specimen  of  which  (at  17h  43m  40s)  is  figured  in  PI.  V.  Fig.  2,  and 
described  in  the  Catalogue.  (See  the  above  R  A,  and  the  description  of  the  objects  immediately 
following  it.)  Towards  the  end  of  the  seventeenth  hour,  the  globular  clusters  begin  to  come  on. 
They  consist  of  stars  of  excessive  minuteness,  but  yet  not  more  so  than  the  ground  of  the  Milky 
Way  on  which  not  only  they  appear  projected,  but  of  which  it  is  very  probable  that  they  really 
form  a  part.  (See  the  descriptions  of  h.  3720,  3723,  3731,  3736,  and  of  the  Milky  Way  at 
lgh  8m  10s  p  D  121o  59/  55f,  under  that  R  A  in  the  Catalogue,  as  also  the  remark  in  Art.  105). 

(332)  In  the  zone  from  117°  to  120°,  the  commencement  of  the  Milky  Way  in  17h  40m  is  by 
a  crowd  of  stars  beyond  counting,  but  which  speedily  becomes  mingled  with  nebulous  masses,  as 
at  h.  3712,  which  is  the  commencement  of  a  series  of  such  masses.  At  17h  45m  30s,  119°  2',  a  field 
of  view  is  thus  described : — "  Here  is  a  field,  the  preceding  half  of  which  is  clear  of  nebula,  the 
last  patch  having  disappeared,  but  the  following  is  densely  filled  with  Nebulous  Milky  Way  !  ! 
(f  723.)"  At  17"  49m,  118°  7',  is  noted  the  northern  limit,  and  at  17h  47m  58s,  119°  22'  the 
southern,  of  a  great  nebulous  or  almost  nebulous  protuberance  or  promontory,  "  which  projects 
into  the  field  of  view  as  the  Cape  of  Good  Hope  on  a  map  does  into  the  Southern  Ocean." 
(/723,  478.)  At  17"  50m,  118°  59',  "the  density  of  the  nebula  is  extraordinary,  and  the  stars 
are  by  no  means  sufficient  to  make  glare  enough  to  account  for  it."  h.  3732  is  evidently  a  nebu- 
loid  of  the  same  nature,  but  more  resolvable. 

(333)  Proceeding  still  northwards,  in  the  zone  114°. ..117°,  presently  after  quitting  the 
preceding  stream  of  the  Milky  Way,  we  fall  upon  a  series  of  blank  fields,  and  exceedingly  poor 
spaces,  extending  in  R  A  from  17h  10m  to  I7h  25m,  and  from  P  D  115°  40'  to  116°  54',  forming 
a  dark  patch  which  corresponds  in  a  remarkable  way  to  that  near  Antares  on  the  opposite  side  of 
the  preceding  stream,  already  noticed  in  Art.  324.  The  place  of  this  void  space  corresponds  to 
the  following  foot  of  Ophiuchus  nearly  on  Bode's  Chart,  south  following  the  star  marked  tt  in  that 
chart,  but  which  is  called  9  in  B  A  C.  Immediately  after  this,  between  the  right  ascensions 
17h  28m  and  17h  35m,  we  come  upon  the  returning  portion  of  the  broad  effusion  of  the  preceding 
branch  of  the  Milky  Way,  where  it  makes  a  sweep  round  tt  (0)  Ophiuchi,  and  which  is  thus 


MILKY  WAY  IN  THE  SOUTHERN  HEMISPHERE. 


389 


characterized  in /723  "  17h  25m,  116°  52',  a  field  selected  among  many  nebulous  ones"  (after  a 
starless  and  perfectly  dark  space)  "  for  having  very  few  stars,  and  yet  being  so  bright  that  I  see  all 
the  wires."  Again,  in  /724  "  17h  28m  16.7s,  114°  27'  1",  the  Milky  Way  comes  on  in  large  milky 
nebulous  irregular  patches  and  banks,  with  few  stars  of  visible  magnitude.  After  a  succession  of 
blank  fields,  and  a  region  of  extremely  rare  stars  above  18m,  I  do  not  remember  ever  seeing  the 

Milky  Way  so  decidedly  nebulous  (or  indeed  at  all  so)  before."  '*  17h  35m  18s,  114°  25'  32", 

the  southern  edge  of  the  Milky  Way,  terminated  by  an  irregular  nebulous  fringe  as  if  lacerated. 
The  body  of  it  towards  the  north  is  very  decidedly  nebulous."  Quitting  here  this  curl  of  the 
preceding  branch,  and  traversing  the  interval  which  separates  it  from  the  following  or  main  stream 
we  come  in  the  first  instance  on  Messier's  eighth  nebula  (PI.  I.  Fig.  1),  which  may  probably  be 
regarded  as  one  of  the  nebulous  outliers  of  that  stream,  since  it  is  hardly  passed,  when  at 
18h  2m  55s,  116°  49',  "  the  Milky  Way  comes  on  suddenly,  the  commencement  being  in  streaky  or 
riband-shaped  masses  of  stars  so  small  as  to  be  almost  nebulous,  yet  when  well  examined  it  is  all 
resolved."  At  its  immediate  preceding  border  occurs  the  fine  globular  cluster  h.  3730  (VI.  12), 
which  partakes  of  the  same  character,  as  regards  the  excessive  minuteness  of  its  stars ;  and  the 
same  remark  applies  to  two  other  similar  clusters  h.  3743  (M.  28),  and  h.  3748,  which  occur 
further  on  in  R  A. 

(334)  In  the  next  zone  (111°  .  .  .  114°)  at  I7h  37m  R  A,  P  D  112°  56',  we  find  still  the 
same  phenomenon  of  irresolvable  nebulosity  thus  described.  "  This  is  about  the  middle  of  a 
very  large  space  in  the  Milky  Way  which  is  completely  nebulous,  like  the  diffused  nebulosity  of 
the  Magellanic  Cloud,  with  a  tolerable  abundance  of  very  small  stars  also  scattered  in  it."  And 
again,  "  17h  48m,  111°  2',  the  apparent  top  of  the  field  (the  real  bottom)  is  full  of  faint  nebulous 
light  without  stars  :  the  rest  of  the  zone  is  blank."  At  18h  8m  "  the  real  Milky  Way  is  just  come 
on  in  great  cloudy  semi-nebulous  masses  running  into  one  another,  heaps  on  heaps."  This  again 
corresponds  to  a  portion  of  the  preceding  effusion.  Before  we  reach  the  following  stream  an 
interval  has  to  be  traversed  in  which  (again  as  a  premonitory  outlier)  occurs  the  great  "  trifid 
nebula"  figured  in  PL  II.  Fig.  2. 

(335)  From  the  foregoing  analysis  of  the  telescopic  aspect  of  the  Milky  Way  in  this  interesting 
region,  I  think  it  can  hardly  be  doubted  that  it  consists  of  portions  differing  exceedingly  in  dis- 
tance, but  brought  by  the  effect  of  projection  into  the  same  or  nearly  the  same  visual  line :  in 
particular,  that  at  the  anterior  edge  of  what  we  have  called  the  main  stream,  we  see,  foreshortened, 
a  vast  and  illimitable  area  scattered  over  with  discontinuous  masses  and  aggregates  of  stars  in  the 
manner  of  the  cumuli  of  a  mackerel  sky,  rather  than  of  a  stratum  of  regular  thickness  and  homo- 
geneous formation :  and  that  in  the  enclosed  spaces  insulated  from  the  rest  of  the  heavens  by  the 
preceding  and  following  streams,  and  the  "bridges"  above  spoken  of  as  connecting  them  (as,  for 
instance,  in  that  which  includes  A.  Scorpii),  we  are,  in  fact,  looking  out  into  space  through  vast 
chimney-form  or  tubular  vacancies  whose  terminations  are  rendered  nebulous  by  the  effect  of 
their  exceeding  distance,  and  at  the  same  time  are  brought  by  that  of  perspective  to  constitute 
the  interior  borders  of  the  apparent  vacuities.  It  is  possible  that  the  globular  clusters  we  see 
scattered  over  it  are  nothing  more  than  such  masses  in  a  higher  state  of  aggregation,  to  which 
perhaps  the  others  are  by  slow  degrees  advancing.  Yet  in  that  case  we  should  certainly  be  pre- 
pared to  expect  specimens  of  an  intermediate  character  to  occur  in  considerable  numbers,  scat- 
tered among  them,  whereas  in  fact  it  would  be  difficult  to  particularize  any  objects  in  the  region 

5  o 


390 


SOME  INDICATIONS  OF  VERY  REMOTE  TELESCOPIC 


in  question  which  can  be  quite  fairly  so  considered.  The  intermediate  stages  of  central  conden- 
sation between  the  highly  compressed  globular  cluster,  and  the  dilute  and  nearly  uniform 
nebuloid  patch,  if  not  altogether  wanting,  are,  at  all  events,  feebly  represented. 


SECTION  III.— OF  SOME  INDICATIONS  OF  VERY  REMOTE  TELESCOPIC  BRANCHES  OF  THE  MILKY 
WAY,  OR  OF  AN  INDEPENDENT  SIDEREAL  SYSTEM,  OR  SYSTEMS,  BEARING  A  RESEM- 
BLANCE TO  SUCH  BRANCHES. 

(336)  I  find  frequent  mention  made  in  the  course  of  sweeping,  of  a  phenomenon  which 
would  appear  to  indicate  the  existence  of  starry  regions  of  great  extent  and  excessive  remoteness, 
disconnected,  or  at  least  in  no  traceable  connexion  with  any  part  of  the  Milky  Way  except  in 
some  particular  localities,  but  which  yet  may  possibly  be  branches  or  outlying  portions  of  that 
system.  This  phenomenon  consists  in  an  exceedingly  delicate  and  uniform  dotting  or  stippling 
of  the  field  of  view  by  points  of  light  too  small  to  admit  of  any  one  being  steadily  and  fixedly 
viewed,  and  too  numerous  for  counting,  were  it  possible  so  to  view  them.  Of  the  reality  of  this 
phenomenon  (which  has  occurred  in  parts  of  the  heavens  far  remote  from  the  Milky  Way,  or  from 
any  large  nebula  or  cluster)  I  have  always  felt  satisfied  at  the  moment  of  observation.  But  that 
conviction  has  not  been  permanent.  The  idea  of  illusion  has  continually  arisen  (subsequently), 
partly  owing  to  the  extreme  delicacy  of  the  points  of  light  so  seen  or  suspected,  but  chiefly  from 
the  circumstance  that  when  noticed  (usually  in  taking  the  gauges)  it  has  been  almost  invariably  in 
the  first  quarter  or  half  an  hour  from  the  commencement  of  sweeping ;  often  in  the  first  gauge 
taken,  and  in  that  only ;  occasionally  later  in  the  sweep,  but  after  an  interval  of  rest.  To  this, 
however,  there  is  here  and  there  an  exception.  Pointed  mention  is,  moreover,  not  unfrequently 
made  of  the  perfect  darkness  of  the  ground  of  the  sky  in  some  regions  ;  which  would  appear  to 
indicate  that  light  had  prevailed,  without  stars  being  seen,  in  the  parts  viewed  previously.  I  think 
it  right,  therefore,  not  to  suppress  all  mention  of  the  phenomenon  in  question,  which,  if  it  arise 
from  physiological  causes  is  at  least  curious  and  remarkable  as  a  case  of  optical  illusion. 

(337)  The  following  is  a  list  of  the  places  in  the  heavens  where  this  phenomenon  has  been 
remarked,  with  the  sweeps  in  which  they  have  been  noted.  Col.  1  contains  a  reference  number ; 
col.  2,  the  R  A  of  the  place  observed ;  col.  3,  the  polar  distance  of  the  zone  affected  or  the 
middle  of  the  field  of  view  gauged ;  col.  4,  the  sweep.  An  asterisk  (*)  affixed  to  this  number 
denotes  that  the  phenomena  was  noted  only  in  the  first  half-hour  of  sweeping,  or  within  the  same 
limit  of  time  after  an  interruption  of  the  sweep  by  an  interval  of  rest  and  absence  from  the 
telescope.  The  letter  M  similarly  attached  indicates  that  the  place  set  down  is  in  the  neighbour- 
hood of  the  Milky  Way. 


No. 

R.  A. 
h.  m. 

N  P  D. 
0  / 

Sweep. 

No. 

R.  A. 
h.  m. 

N  P  D. 

0  / 

Sweep. 

I 

3 

47 

99°  •• 

.101° 

758 

* 

6 

4 

29 

124 

28 

663 

2 

3 

5° 

124. 

28 

663 

7 

4 

30 

148 

28 

665 

* 

3 

4 

1 1 

156°. 

159° 

653 

* 

8 

5 

24 

1230  . 

1260 

S3S 

* 

4 

4 

16 

156 

10 

653 

* 

9 

5 

39 

124 

28 

535 

* 

5 

4 

19 

125 

58 

663 

10 

5 

45 

1 12 

27 

532 

* 

BRANCHES  OF  THE  MILKY  WAY. 


391 


No. 

E. 

A. 

N  P  D. 

Sweep. 

No. 

R. 

A. 

N  PD. 

Sweep. 

h. 

m. 

0 

/ 

h. 

m. 

0 

/ 

I 1 

5 

49 

151 

27 

682 

* 

2  ? 

10 

160 

28 

604 

* 

12 

7 

14 

139 

29 

526 

* 

26 

19 

59 

119 

56 

620 

7 

19 

I52 

57 

682 

* 

27 

20 

9 

121 

26 

620 

8 

0 

148 

24 

543 

*  M 

28 

20 

59 

121 

56 

620 

15 

8 

53 

109 

24 

561 

* 

29 

21 

0 

152 

57 

613 

* 

16 

10 

5° 

142 

35 

576 

* 

30 

21 

1 

165°.. . 

.168° 

627 

*  ? 

17 

13 

48 

163 

28 

606 

*  M 

31 

21 

9 

120 

26 

620 

18 

14 

5° 

144°.. 

.146° 

694 

M 

32 

21 

1 1 

166 

26 

627 

*  ? 

'9 

15 

0 

ISO 

7 

575 

M 

33 

21 

21 

164 

56 

627 

20 

iS 

20 

134 

53 

695 

M 

34 

21 

24 

118 

56 

620 

21 

IS 

39 

168 

2 

592 

*  M 

35 

22 

49 

127 

33 

636 

* 

22 

iS 

40 

I47°... 

.150° 

575 

M 

36 

23 

30 

145 

24 

629 

* 

23 

iS 

40 

125 

5* 

791 

M 

37 

23 

44 

150.. 

•153 

736 

* 

24 

16 

41 

122 

5* 

79i 

M 

(338)  In  f  663  (Nos.  2,  5,  6),  the  appearance  in  question  continued  during  forty  minutes, 
after  which  it  ceased  to  attract  attention.  In  f  526  (No.  12),  it  occurred  after  twenty  minutes' 
sweeping,  preceded  by  an  interval  of  forty  minutes'  rest.  The  observation  No.  18,  is  thus  re- 
corded :  "  A  very  remarkable  change  in  the  ground  of  the  sky.  From  being  light  and  dotty,  it 
is  now  become,  all  over  the  zone,  clear  black,  on  which  the  stars  stand  as  on  a  black  ground : 
Nos.  19,  22,  are  almost  upon  the  Milky  Way,  and  indicate  a  transition  to  its  nebulous  state.  In 
the  latter  entry  especially  it  is  stated,  that  "  over  the  whole  zone,  the  Milky  Way  is  very  remark- 
able, consisting  of  large  and  small  stars  loosely  scattered  over  a  brilliant  and  closely  stippled 
reticulated  ground  of  stars,  say  17  m.  With  attention  they  are  insulable  and  innumerable."  The 
"stippling  of  the  ground  of  the  sky"  to  which  attention  is  intended  to  be  drawn  in  these  notices, 
seems  to  be  one  step  farther  in  the  progress  towards  milky  nebulosity  than  this  observation 
records.  In  the  observation  No.  20,  twenty-eight  stars  12  and  13  m  were  counted  "on  a  field 
uniformly  stippled  over.  A  remarkable  field."  This  occurred  after  two  hours  fifty  minutes  of 
continuous  sweeping,  in  the  course  of  which,  at  13h  0m,  the  ground  of  the  sky  is  expressly  stated 
to  have  been  quite  black.  In  f  620,  which  is  far  enough  from  the  borders  of  the  Milky  Way  to 
be  fairly  out  of  its  ordinary  influence,  the  notices  of  the  stippling  are  very  strongly  expressed, 
thus:— "19h  59m,  field  distinctly  stippled  all  over  uniformly;"  "  20h  9m,  I  feel  satisfied  the 
stippling  is  no  illusion,  as  its  dark  mottling  moves  with  the  stars  as  I  move  the  tube  to  and  fro  ;" 
«  20h  29m,  stippling  no  longer  seen ;  20h  39m,  the  stippled  appearance  is  gone  ;  20h  59m,  query,  if 
not  a  feeble  stippling ;"  and  so  on  to  22h  29m,  where  the  ground  was  observed  perfectly  dark, 
and  this  remark  added,  "  Hitherto  there  has  been  light  in  the  field,  especially  when  faint  or 
doubtful  stippling  has  been  recorded."  In  /  627  the  entries  of  stippling  are  only  in  the  first  three 
gauges  (Nos.  30,  32,  34),  but  it  is  not  till  R  A  22h  lm,  or  after  a  full  hour  from  the  commence- 
ment that  it  is  declared  to  be  "gone."  In  /  629  (No.  36)  the  phenomenon  is  noted  as  "feeble." 
On  this  occasion  the  entry  occurs  after  nearly  an  hour's  sweeping;  but  this  had  been  interrupted 
from  23h  5m  to  23h  18m,  during  which  the  eye  of  a  friend  replaced  my  own  at  the  telescope  while 
I  stood  by,  without,  however,  quitting  the  platform,  or  going  into  the  light.    This  was  twelve 


392 


TELESCOPIC  BRANCHES  OF  THE  MILKY  WAY. 


minutes  before  the  entry  in  question,  and  a  gauge  taken  at  23h  20m,  only  two  minutes  after 
resuming  the  observations,  mentions  no  stippling. 

(339)  In  order  to  throw  as  much  light  upon  this  subject  as  possible,  I  have  projected  all 
these  recorded  points  on  a  chart,  with  a  view  to  see  whether  they  group  themselves  in  any 
consistent  manner.  One  group  occurs  tolerably  compact,  occupying  the  arms  and  fore-legs  of 
the  Centaur,  and  this  seems  pretty  evidently  connected  with  the  Milky  Way,  which  runs  directly 
across  it.  Another  more  loosely  occupies  the  constellations  Lepus,  Columba,  and  Pictor,  while  a 
third  straggles  over  a  region  including  Pavo,  Grus,  and  the  hind  part  of  Sagittarius.  These 
include  all  the  recorded  fields  but  three,  which  are  outlying  and  disconnected. 

(340)  The  following  is  a  list  of  points  recorded  as  having  the  ground  of  the  sky  particularly 
black,  and  certainly  devoid  of  any  such  stippling  or  nebulous  phenomenon. 


R.  A. 

N  P  D. 

Sw. 

B.  A. 

N  P  D. 

Sw. 

R.  A. 

N  P  D. 

Sw. 

h.  m. 

0  1 

h.  m. 

0  / 

h.  ra. 

0  / 

o  39 

123  1 

635 

9  9 

173  O 

779 

17  3 

"7  35 

723 

2  O 

134  49 

634 

9  28 

120  29 

678 

17  13 

123  — 

79 1 

2  30 

136  19 

634 

13  0 

137  53 

695 

17  18 

116  45 

723 

4  IO 

129  32 

638 

14  50 

145  29 

694 

19  II 

160  28 

604 

7  3 

104  59 

757 

16  IO 

123  126 

791 

21  23 

157  30 

610 

7  36 

"3  57 

677 

(341)  I  shall  close  this  chapter  by  a  general  reference  to  Plate  XIII.  Figs.  1,  2,  which 
represent  the  cause  and  aspect  of  the  Milky  Way,  from  Antinous  to  Monoceros,  delineated  with  as 
much  precision  as  the  nature  of  such  work  admits,  i.  e.  with  the  naked  eye  by  faint  lamplight,  in 
the  open  air.  In  the  projection,  the  Galactic  Circle  or  medial  line  of  the  entire  galaxy  is  extended 
into  a  straight  line  which  is  divided  into  hours  of  right  ascension  at  the  points  where  the  meridians 
of  those  hours  cross  it.  The  figures  are  reduced  from  drawings  on  a  larger  scale,  viz.  that  formed 
by  pricking  off  the  stars  from  Bode's  charts,  on  blank  paper,  to  serve  as  skeleton  charts  for  that 
purpose  as  well  as  for  a  general  triangulation  of  the  whole  heavens  (northern  as  well  as  southern) 
in  which  it  was  proposed  to  lay  down  every  star  visible  to  the  naked  eye.*  From  these  charts 
the  Milky  Way  has  been  transferred  by  laying  down  (from  a  good  celestial  globe,  by  Bardin,  for 
1800)  the  chief  stars,  as  a  skeleton — inserting  others  from  the  maps  by  the  aid  of  proportional 
compasses,  and  then  working  over  it  an  accurate  resemblance  of  the  forms,  and  as  near  as  possible 
of  the  intensities,  of  the  several  parts  in  the  originals.  The  reader  may  perhaps  be  surprised  by 
differences  which  occur  in  very  obvious  features  between  this  and  former  representations,  as,  for 
instance,  in  the  great  embranchment  at  a  Centauri,  which  both  in  Bode's  chart  and  in  Mr. 
Dunlop's  figure  is  made  to  take  place  at  or  near  /3,  and  in  several  other  points  which  it  is  not 
worth  while  to  particularize. 

*  This  operation,  I  may  as  well  mention,  has  been  very  nearly  completed  in  the  Southern  Hemisphere  (a  few 
triangles  only  having  escaped),  and  quite  so  in  the  Northern ;  just  as  the  elaborate  charts  of  Argelander  and 
Schwink,  aiming  at  and  accomplishing  the  same  objects  for  that  part  of  the  heavens  visible  in  Europe,  have 
satisfied,  at  least  to  that  extent,  the  present  wants  of  astronomers. 


CHAPTER  V. 


OBSERVATIONS  OF  HALLEY'S  COMET,  WITH  REMARKS  ON  ITS  PHYSICAL 
CONDITION,  AND  THAT  OF  COMETS  IN  GENERAL. 

(342)  It  was  not  before  the  28th  of  October  (1835)  that  I  obtained  a  view  of  this  long 
expected  and  anxiously  looked  for  member  of  our  system.  On  the  21st  and  following  days  of 
March,  guided  by  Mr.  R'umker's  ephemeris,  which  fortunately  came  to  hand  in  time,  I  had 
examined  both  with  the  equatorial  and  with  the  20-feet  reflector  the  places  set  down  in  that 
ephemeris  for  the  days  of  observation,  and  the  whole  adjacent  region  of  the  heavens,  with  all  pos- 
sible attention,  but  without  success.  Nor  was  I  more  fortunate  in  the  end  of  August  and  the 
beginning  of  September,  when,  on  several  occasions,  in  the  morning  before  sunrise,  I  swept  over 
the  places  given  in  the  Nautical  Almanac  for  1835,  which  it  is  now  known  were  not  far  from  the 
true  ones.  On  these  occasions,  however,  my  search  was  uniformly  baffled  by  a  drift  of  light,  low, 
scudding  vapour,  hurried  rapidly  along  by  the  south-east  wind  of  the  season,  and  forming  con- 
stantly anew  nearly  on  the  spot  to  which  the  telescope  was  directed.  The  local  situation  of  the 
observatory  exempts  it  from  this  annoyance  (which  is  a  consequence  of  the  greater  proximity  of 
Feldhausen  to  the  slope  of  the  Table  Mountain,  the  great  rendezvous  of  the  south-east  cloud- 
drift);  and,  in  consequence,  I  am  informed  by  Mr.  Maclear  that,  on  the  morning  of  the  1st 
September,  he  succeeded  in  obtaining  a  satisfactory  observation. 

(343)  On  the  24th  October  the  comet  was  seen  by  several  persons  in  Cape  Town  with  the 
naked  eye;  but  even  so  early  as  the  22nd,  my  own  servants  had  obtained  a  sight  of  it  for  a  few 
minutes  (but  without  informing  me  at  the  time)  during  a  casual  and  transient  removal  of  the 
vast  pile  of  clouds  which  then,  and  for  many  evenings  subsequent,  congregated  over  the  summits 
of  the  Table  and  Devil  Mountains.  This  obstruction  continued  till  the  28th,  in  the  afternoon  of 
which  day,  despairing  of  success  at  home,  and  impatient  of  repeated  disappointments,  I  dismounted 
the  equatorial  telescope,  and  having  constructed  for  it  a  convenient  temporary  stand  transported 
it  to  a  station  on  the  Cape  Flats,  five  or  six  miles  to  the  eastward  of  Feldhausen,  where  a  clear  sky 
might  be  depended  on.  There,  sheltered  by  a  range  of  low  sand-hills  from  the  violence  of  the 
south-east  wind,  and  freed  by  distance  from  the  obstruction  produced  by  the  Table  Mountain 
with  its  superposed  mass  of  cloud  (which  at  that  time  extended  over  the  zenith  of  Feldhausen). 
the  instrument  was  erected  about  sunset,  and  before  the  termination  of  the  twilight  I  had  the 
gratification  to  obtain  an  excellent  view  of  the  comet. 

(344)  Its  appearance  on  that  evening,  to  the  naked  eye,  was  about  that  of  a  star  of  the  3rd 
magnitude,  which,  as  the  darkness  increased,  appeared  somewhat  hazy,  and  accompanied  by  a 

5  H 


394 


OBSERVATIONS  OF  HALLEY'S  COMET. 


scarcely  perceptible  tail.  In  a  night-glass,  however,  the  tail  was  conspicuous  enough  and  3°  in 
length,  extending  to,  and  just  perceptibly  involving,  a  star  of  the  6th  magnitude,  afterwards  iden- 
tified by  reference  to  Bode's  Atlas  as  No.  217  of  his  Catalogue,  =  A.  31816,  the  comet  itself 
holding  the  situation  and  presenting  the  appearance  represented  in  Fig.  1,  PI.  XIV.,  in  which 
figure  the  star  a  is  that  marked  in  Bode's  Chart  as  n  Ophiuchi  (B  A  C.  5890),  b  =  I  (Bode 
Ophiuchi),*  c  =  A.  31592,  d  =  A.  31485,  and  f  =  A.  31699. 

(345)  Fig.  2,  PI.  XIV.,  represents  its  appearance  on  the  same  evening  in  the  7-feet  achro- 
matic, with  its  ring  micrometer  eye-piece  magnifying  about  seventy  times.  It  was  that  of  a 
nebula  very  suddenly  and  highly  condensed  in  the  centre,  to  so  great  a  degree  indeed  that  I 
would  not  (from  this  observation  alone)  have  ventured  to  deny  the  existence  of  a  solid  nucleus. 
No  phase,  however,  was  perceptible  on  that  central  mass  which  might  have  been  so  regarded. 
Neither  was  any  other  remarkable  peculiarity  about  the  head,  nucleus,  or  tail,  noticed  on  this 
occasion. 

(346)  The  following  evening  (the  29th)  proved  very  clear  at  Feldhausen,  and  having  cut 
down  several  trees  which  obstructed  the  view  of  that  part  of  the  sky  where  the  comet  would  set 
(and  which  had  already  been  partially  cleared  for  the  comet  of  Encke),  the  20-feet  reflector, 
armed  with  an  excellent  mirror,  recently  and  brilliantly  polished  for  this  express  service,  was 
directed  on  it  as  soon  as  it  became  visible  in  the  finder  in  the  strong  twilight.  Under  these  cir- 
cumstances its  appearance  was  most  singular,  and  such  as  I  had  never  observed  and  do  not 
remember  to  have  seen  described  in  any  previous  comet.  Its  nucleus,  small,  bright,  and  highly 
condensed,  was  shielded  or  capped  on  the  side  next  the  sun  by  a  vivid  but  narrow  crescent  of 
nebulous  light,  Fig.  3,  PI.  XIV.,  the  front  of  which  presented  an  outline  nearly  circular,  having 
an  amplitude  of  somewhat  more  than  90°  from  horn  to  horn.  Within  this  was  situated  the 
nucleus,  but  at  a  distance  behind  the  front  or  vertex  of  the  crescent,  considerably  less  than  its 
venedsine,  so  that  the  horns  of  the  crescent  extended  a  good  way  behind  the  nucleus  on  either 
side.  On  the  other  hand,  the  nucleus  lay  somewhat  behind  the  interior  boundary  (if  it  could 
properly  be  said  to  have  a  boundary,  shading  off  insensibly  though  rapidly)  of  the  crescent ;  and, 
not  being  itself  a  well  defined  planetary  body,  but  apparently  only  a  spherical  nebula  in  a  state 
of  high  central  condensation.  The  exterior  portions  of  its  nebulosity  appeared  to  blend  with  the 
interior  border  of  the  crescent,  in  such  a  manner  as  to  give  the  impression  of  a  compounded  out- 
line, consisting  of  two  slight  concavities  meeting  in  a  sort  of  blunted  cusp  at  the  nucleus.  This 
is  no  doubt  Mr.  Cooper's  fan,  and  M.  Arago's  sector,  or  at  least  their  denser  portion — such  as  the 
twilight  could  not  obliterate — or  at  all  events  a  modification  of  those  phenomena  induced  by 
lapse  of  time.  There  can  consequently  be  little  doubt  of  its  existence  on  the  preceding  evening, 
so  that  its  escaping  notice  in  the  former  observation  can  only  be  ascribed  to  want  of  sufficient 
light  in  the  instrument  employed — a  defect  which  no  degree  of  distinctness  under  magnifying 
power  can  compensate  in  the  examination  of  nebulous  phenomena. 

(347)  In  the  state  above  described,  and  shorn  of  its  exterior  envelopes,  the  distance  of  the 
central  point  of  the  nucleus  from  the  vertex  of  the  crescent  was  estimated  at  45",  and  the  breadth 
of  the  latter  from  horn  to  horn  at  2'  30"  or  3'  at  most.    The  nucleus  was  decidedly  not  planetary, 


*  This  star  does  not  occur  either  in  B  AC  or  in  X.  It  is,  however,  visible  to  the  naked  eye  as  a  star  5^m., 
and,  as  such,  was  observed  by  me  on  June  2, 1842,  in  Chart  Triangle  No.  620. 


OBSERVATIONS  OF  HALLEY'S  COMET. 


395 


and  as  decidedly  exhibited  no  phase.  As  the  evening  advanced,  the  exterior  strata  of  the  cres- 
cent— the  coma  and  the  tail  which  were  before  obliterated  by  the  twilight — became  visible,  and  the 
whole  finally  put  on  the  appearance  represented  in  Fig.  4,  PI.  XIV.  The  tail,  however,  was 
never  very  apparent,  and  the  magnifying  power  (180),  the  lowest  I  could  then  apply,  was  still  too 
high  to  give  its  feeble  light  sufficient  concentration  to  enable  me  to  trace  its  course,  and  say  with 
confidence  whether  the  chord  of  the  crescent  was  or  was  not  perpendicular  to  the  general  direc- 
tion of  the  tail.    Certainly  at  the  time  I  had  no  suspicion  of  its  being  otherwise. 

(348)  The  next  day  (the  30th)  I  visited  the  Observatory,  and  as  the  clouds  towards  evening 
covered  the  whole  Table  Mountain  in  such  a  manner  as  to  preclude  any  hope  of  an  observation 
at  Feldhausen,  I  remained,  and  was  indulged  by  Mr.  Maclear  with  a  view  of  it  through  the  14-feet 
Newtonian  reflector  of  my  father's  construction — an  instrument  of  great  optical  capacity,  both  as 
regards  light  and  distinctness.  In  this,  the  appearance  was  very  different  from  what  was  observed 
on  the  previous  night.  I  could  discern  no  distinct  crescent,  but  in  its  place  a  strongly  marked 
arc  in  the  bend  of  the  tail  round  the  head,  which  was  decidedly  most  luminous  at  the  north  pre- 
ceding side  of  the  vertex. 

(349)  On  the  31st,  the  general  appearance  of  the  comet  was  not  materially  different.  The 
diameter  of  the  head  or  more  concentrated  part  around  the  nucleus,  distinguished  sufficiently  by 
its  spherical  form  to  admit  of  measurement,  was  found  to  be  80  parts  of  the  equatorial  micrometer, 
corresponding  to  19". 2.  On  this  occasion,  also,  the  comet  was  compared  micrometrically  with  a 
star  of  the  7th  magnitude  just  outside  of  the  following  border  of  its  tail  as  under,  viz.,  s  T 
22h  25m  40"  north  of  star  479  Micr  Pts  =  1'  55".2  and  s  t  22h  28m  40s  a  =  preceded  star  46s.5  in 
time.  Previous  to  the  perihelian  passage,  however,  I  did  not  think  it  necessary  to  pay  regard  to 
exact  determinations  of  its  place,  which  would  have  demanded  the  exclusive  use  of  the  equa- 
torial, and  involved  the  loss  of  opportunities  for  examining  its  physical  construction  with  the 
20-feet. 

(350)  On  the  evening  of  the  31st,  the  crescent  was  less  remarkable  than  on  the  29th,  and  on 
the  following  evening  (Nov.  1st),  still  less  so  ;  its  appearance  on  that  evening  was  as  represented 
in  Fig.  5,  PI.  XIV.  in  which  the  only  feature  deserving  especial  notice  consists  in  the  extension 
of  the  feeble  light  of  the  coma,  considerably  beyond  the  general  parabolic  sweep  of  the  denser 
portion  of  the  tail  around  the  head. 

(351)  By  this  time  the  observation  of  the  comet  with  the  20-feet  was  growing  difficult,  and 
confined  to  a  brief  interval  before  its  disappearance  behind  local  obstacles.  I  therefore  regretted 
the  less  the  necessity  of  leaving  home  for  some  days  on  the  2nd  November.  On  my  return  on  the 
10th,  it  was  still  visible  by  climbing  above  the  nearer  trees,  in  the  strong  twilight,  as  a  star  of  the 
2.3  or  3rd  magnitude,  though  out  of  the  reach  of  any  instrument  but  a  night-glass  held  in  the 
hand,  through  which  its  tail  was  seen,  at  the  instant  of  disappearance  of  the  head  behind  the 
Table  Mountain,  extending  over  just  one  radius  of  the  field,  or  about  2|°. 

(352)  On  the  return  of  the  comet  from  the  sun,  it  was  carefully  swept  for  before  sunrise, 
on  several  occasions,  about  the  end  of  December,  especially  on  the  21st  and  26th,  which  days  I 
particularize  on  account  of  the  perfect  clearness  of  the  horizon  down  to  the  summits  of  the 
Hottentot  Holland  Mountains,  a  range  of  hills  to  the  south-east,  about  3,000  or  4,000  feet  in  height, 
and  distant  25  to  30  miles.  On  these  occasions,  Antares  was  taken  as  a  point  of  departure,  and 
azimuthal  sweeps  made  on  either  side,  from  the  horizon  upwards,  but  without  perceiving  it.  By 


396 


OBSERVATIONS  OF  HALLEY'S  COMET, 


Mr.  Stratford's  elaborate  ephemeris  (which  of  course  had  not  then  come  to  hand),  it  now  appears 
that  the  comet  in  all  this  interval  must  have  occupied  a  situation  so  near  Antares,  that  its 
escaping  observation  at  that  time,  although  in  strong  twilight,  seems  not  a  little  remarkable, 
though  in  great  measure  explained  by  the  course  of  the  subsequent  phenomena.  Cloudy 
mornings,  and  other  occupations,  then  intervened ;  indeed,  I  had  begun  to  despair  of  its  re- 
appearance. On  the  25th  of  January,  however,  notice  was  received  from  Mr.  Maclear  of  his 
having  rediscovered  it  on  the  morning  of  that  day,  or,  more  properly  speaking,  the  night  of  the 
24th,  astronomical  reckoning.  This  intelligence  set  everything  once  more  on  the  alert ;  and  so 
soon  as  Scorpio  became  visible  on  the  subsequent  night  (or  morning  of  the  26th),  it  was  con- 
spicuously seen  somewhat  above  the  star  p  of  that  constellation,  as  a  bright  star  of  the  4th,  or 
small  one  of  the  3rd  magnitude.  Trees  not  yet  allowing  it  to  be  taken  up  in  the  20-feet,  the 
equatorial  was  turned  upon  it  in  the  first  instance  until  it  had  attained  altitude  enough  to  be 
visible  in  the  former  instrument ;  and  this  was  the  course  of  proceeding  on  subsequent  mornings, 
until  the  advance  of  the  season,  and  the  progress  of  the  comet  in  its  orbit,  rendered  it  equally 
convenient  for  either  instrument  at  an  earlier  hour. 

(353)  To  the  naked  eye  it  now  offered  the  aspect  of  a  star,  a  very  little  dim  and  hazy ;  but 
no  tail  was  visible,  neither  was  any  seen  in  the  night-glass,  in  which  its  appearance  was  that  of  a 
highly  condensed  globular  nebula.  In  the  equatorial  it  appeared  as  a  bright,  round,  and  very 
nearly  uniform  nebulous  disc,  little  condensed  towards  the  centre,  but  decidedly  more  sharply 
defined  on  the  following  than  on  the  preceding  side.  Scarcely  any  nucleus  was  to  be  seen, 
except  that  by  glimpses  some  small,  ill-distinguished  object  was  perceived  near  the  centre.  No 
trace  of  a  tail  was  observed  with  this  instrument,  but  a  considerable  coma  enveloped  the  disc 
above  mentioned,  extending  to  nearly  the  same  distance  on  all  sides,  and  giving  to  the  whole 
object  a  strong  resemblance,  though  on  a  greatly  enlarged  scale,  to  those  singular  nebulae  which 
are  described  as  at  first  very  gradually,  then  very  suddenly,  much  brighter  towards  the  middle, 
up  to  a  uniform  disc  of  sensible  diameter. 

(354)  Viewed  through  the  20-feet  reflector  (which  on  this  as  on  the  former  occasion  I  had 
taken  care  to  provide  with  a  mirror  freshly  polished  and  in  the  highest  possible  condition,  which 
had  been  kept  in  readiness  for  its  return  from  the  sun)  the  comet  now  was  indeed  a  most  singular 
and  remarkable  object,  PI.  XV.  Fig.  1.  Certainly  nothing  could  be  more  surprising  than  the 
total  change  which  had  taken  place  in  its  appearance  since  the  observations  of  October.  Not  to 
speak  of  the  extraordinary  sharpness  of  termination  of  the  head,  especially  towards  the  following 
side,  for  which  I  can  find  no  comparison  so  apt  as  the  ground-glass  shade  of  an  Argand  lamp ;  a 
new  and  perfectly  unexpected  phenomenon  had  developed  itself,  a  phenomenon,  I  believe,  quite 
unique  in  the  history  of  comets.  Within  the  well-defined  head,  and  somewhat  excentricallv 
placed  (being  rather  nearer  to  its  southern  than  to  its  northern  edge),  was  seen  a  vividly  lumi- 
nous nucleus,  or  rather  an  object  which  I  know  no  better  way  to  describe  than  by  calling  it  a 
miniature  comet  having  a  nucleus,  head  and  tail  of  its  own,  perfectly  distinct  and  considerably 
exceeding  in  intensity  of  light,  the  nebulous  disc  or  envelope  which  I  have  above  called  the 
"  head."  As  the  comet  gained  altitude,  a  minute  bright  point  like  a  very  small  star,  or  rather 
like  the  nucleus  of  the  nebula  in  Andromeda,  only  smaller,  came  to  be  distinctly  perceived.  It 
is  this  point  which  I  shall  henceforward  term  the  nucleus,  and  which,  according  to  the  state  of  the 
atmosphere  at  the  time  of  observation  (and  perhaps  also  that  of  the  comet  itself)  was  subsequently 


OBSERVATIONS  OF  HALLEY'S  COMET. 


397 


seen  sometimes  more,  sometimes  less  sharply  concentrated,  and  stellar — but  always  of  excessively 
minute  dimension,  certainly  on  no  occasion  subtending  an  angle  of  4",  and  never  quite  so  well 
denned  as  give  a  positive  assurance  of  the  existence  of  a  solid  sphere — much  less  could  any  phase 
be  at  any  time  discerned  on  it.  The  whole  was  encircled  with  a  strong  coma  which  nearly  filled 
the  field  of  view  (15'  diameter),  dying  away  insensibly  but  rapidly  at  the  edges.  When  the 
nucleus  was  brought  to  any  part  of  the  circumference  of  the  field,  the  border  of  the  coma  fell 
little  short  of  the  centre.  On  the  south  preceding  side,  however,  its  extent  was  somewhat 
greater,  projecting  in  that  quarter  into  a  feeble  and  irregular  appendage,  which  might  be  regarded 
as  a  rudimentary  tail. 

(355)  From  the  25th  January,  whenever  the  weather  would  permit,  till  the  final  disap- 
pearance of  the  comet,  it  was  observed  constantly  with  the  equatorial,  and,  as  often  as  the  other 
indispensable  duties  of  the  20-feet  would  permit,  with  that  instrument.  My  last  observation  of 
it  dates  on  the  5th  of  May,  on  which  day  it  was  still  visible,  though  with  great  difficulty,  in  the 
equatorial ;  so  conspicuous  was  it  on  the  4th,  in  the  20-feet,  that  I  fully  expected  to  have  kept  it 
in  view  at  least  another  fortnight.  In  this,  however,  I  was  disappointed.  Cloudy  nights  pre- 
vented further  operations  till  the  11th.  Late  on  that  night  the  clouds  dispersed,  and  sweeping 
for  it  out  of  the  meridian  over  its  presumed  place  three  nebulae  were  encountered,  one  of  which 
(I.  163)  was  at  once  recognised  by  its  form,  and  as  being  far  too  bright ;  a  second,  not  occurring 
in  the  catalogues,  was  considered  too  faint,  as  well  as  too  far  from  the  expected  place,  to  be  the 
comet ;  a  third  was  then  found,  and  although  from  the  first  it  was  suspected  not  to  be  the  comet, 
not  having  sufficient  central  condensation,  yet  as  the  place  seemed  to  agree  tolerably,  and  no 
other  object  offering  the  same  degree  of  probability  had  presented  itself,  I  identified  it  by  means 
of  surrounding  stars,  and  then  had  recourse  to  the  equatorial  to  determine  its  place,  when  it 
proved  to  be  the  nebula  II.  305.  The  opportunity  of  further  examination  was,  however,  lost  for 
that  night. 

(356)  On  the  12th  of  May  a  sweep  was  set,  including  the  96th,  97th,  and  98th  degrees  of 
N  P  D,  within  which  it  was  certain  the  comet  must  lie,  and  to  pass  over  the  two  stars  marked  in 
Bode's  Atlas  as  g  Sextantis  (Fl.  17  and  18),  the  nearest  lettered  stars  to  its  expected  place  as 
laid  down  in  the  chart  by  the  last  obtained  daily  motion  in  R  A  and  N  P  D.  As  the  time  of 
transit  approached  the  sweep  was  interrupted  by  clouds,  between  which,  however,  the  nebula 
I.  163  was  seen,  and  its  place  taken,  R  A  9h  56ra  44M,  N  P  D  96°  54'  13"  (1830).  From  that 
time  till  llh  5m  it  continued  cloudy,  admitting  only  momentary  glimpses,  during  which  whole 
interval,  nevertheless,  the  sweeping  was  continued,  that  no  chance  might  be  missed.  The 
moment  it  cleared,  the  transit  being  long  past,  the  telescope  was  directed  out  of  the  meridian 
on  g  Sextantis  as  a  point  of  departure  to  sweep  from.  It  was  now  perfectly  clear,  and  to  mv 
surprise,  but  at  the  time  to  my  great  satisfaction,  in  the  field  with  g1  the  brighter,  and  preceding 
of  the  two  stars  of  g,  an  object  was  seen  which  at  once  impressed  me  with  a  full  conviction  of 
its  being  that  I  was  in  search  of,  no  catalogued  nebula  occurring  in  that  place.  In  my  sweeping- 
journal  it  stands  described  as  "  A  faint  nebula  of  the  2nd  class,  but  very  suddenly  brighter  in 
the  middle  to  a  stellar  point,  equal  to  a  star  16  m.  Diameter  about  1'  or  1^'.  The  star 
prevents  it  being  seen  of  its  full  size  and  brightness,  but  the  observations  are  unexceptionable. 
I  showed  it  to  my  attendant,  who  saw  it  as  described."    This  nebula  (for  such  it  proved  to  be) 

5  i 


398 


OBSERVATIONS  OF  HALLEY'S  COMET. 


preceded  the  star  gx  by  0s. 8 7 ;  and  its  difference  of  declination,  as  determined  by  an  oblique 
transit  across  a  wire  45°  inclined  to  the  parallel,  was  found  to  be  4/  36"  south  of  the  star. 

(357)  The  next  night  the  telescope  was  again  turned  on  g  Sextantis  as  a  starting  point, 
whence,  by  the  easy  transition  of  a  day's  motion,  the  comet  might  be  readily  taken  up,  the  state 
of  the  weather  precluding  a  regular  sweep,  though  admitting  excellent  views  in  brief  intervals. 
To  my  mortification,  however,  on  the  first  view  of  gl  it  was  seen  accompanied  by  the  same 
nebula,  in  the  same  precise  situation  as  the  previous  night.*  Clouds  prevented  all  further 
search  on  that  and  several  subsequent  nights ;  and  when  at  length  the  weather  became  favourable 
no  trace  of  the  comet  could  be  found,  after  most  patient  and  persevering  search.  Thus,  by  a 
most  inopportune  discovery  of  a  nebula,  otherwise  interesting  enough,  I  found  myself  deprived 
of  the  opportunity  I  should  doubtless  have  otherwise  enjoyed,  of  accompanying  this  remote 
denizen  of  our  system  a  few  steps  farther  on  his  journey. 

(358)  On  account  of  the  interest  which  may  be  considered  to  attach  to  the  final  disappear- 
ance of  this  comet,  it  has  been  thought  right  to  state  the  above  circumstances.  I  proceed  now 
to  detail  the  observations  made  in  the  interim,  and  endeavour  to  present  a  connected  view  of  the 
various  remarkable  changes  the  comet  underwent  in  its  figure,  dimensions,  and  in  the  relative 
degrees  of  illumination  of  its  constituent  parts,  viz.,  the  coma,  the  tail,  the  head,  and  the 
nucleus,  with  its  ray  or  tail.  As  respects  the  micrometric  comparison  of  its  places  with  those 
of  neighbouring  stars,  from  January  25  to  May  5,  both  inclusive,  I  have  already  published  them 
in  the  "  Transactions  of  the  Astronomical  Society,"  vol.  x.  p.  325,  et  seq.,  which  volume  also 
contains  the  far  more  elaborate  observations  of  Mr.  Maclear,  extending  over  the  whole  of  that 
interval  of  time,  and  given  with  all  possible  circumstantial  detail.  These,  therefore,  I  pretermit 
as  unnecessary ;  reserving,  however,  a  few  remarks  at  the  end  of  this  chapter  in  explanation  of 
some  artifices  employed  in  the  management  of  the  equatorial  to  insure  exactness  when  the 
comet  grew  very  faint,  which  may  be  useful  to  others  under  similar  circumstances. 

(359)  The  appearance  of  the  comet  on  the  25th  January  has  been  already  described,  and  is 


represented  in  Fig.  1,  PI.  XV.  Before  turning  the  20-feet  upon  it,  the  following  measures  were 
procured  with  the  equatorial  : — 

M  T  13h  38m— Diameter  of  the  head  in  Right  Ascension   229".4 

Distance  of  the  nucleus  from  the  vertex  (uncertain)       ....       1 18".3  : : 
14''  15" — Diameter  of  the  head  in  Declination   237".3 

Returning  to  this  instrument  after  the  20-feet  observations  were  terminated,  I  repeated  these 
measures,  and  was  not  a  little  surprised  to  find  the  results  most  materially  different,  viz. : — 

M  T  16"  25m— Diameter  of  the  head  in  Right  Ascension  196"./ 

16"  29m— Diameter  of  the  head  in  Declination   252".0 


These  measures  having  been  performed  in  strong  morning  twilight,  the  deficiency  in  the  measure 
in  R  A  was  easily  accounted  for  by  the  action  of  the  twilight  on  the  ill-defined  and  graduating 
posteriorf  portion  of  the  head.    But  how  to  account  for  the  increased  result  of  the  measurement 

*  I  find  a  loose  memorandum,  dated  February  2  (which  must  have  been  1837),  to  the  following  effect — 
"  Viewed  g  Sextantis.    The  nebula  stands  as  before,  viz.,  exactly  south  of  gl  and  about  4'  distant." 

f  Posterior,  in  reference  to  the  vertex,  which,  as  fronting  the  sun,  is  considered  as  the  anterior  portion  of  the 
comet,  without  regard  either  to  its  diurnal  or  orbitual  motion. 


OBSERVATIONS  OF  HALLEY'S  COMET. 


399 


across  the  axis,  where  the  edges  of  the  portion  measured  were  both  well  defined  ?  A  difference 
of  14". 7  between  the  measurements  of  the  same  dimension  taken  within  two  hours  and  a  quarter 
of  each  other,  and  in  opposition  to  the  tendency  of  the  twilight,  seemed  inconceivable,  and  threw 
a  momentary  doubt  on  the  exactness  of  the  earlier  measure.  That  measure  had,  however,  been 
taken  and  read  off  with  all  possible  care,  and  in  short,  nothing  remained  but  the  conclusion  that 
the  change  was  real,  and  that  the  comet  was  actually  increasing  in  dimensions  witli  such  rapidity  that  it 
might  almost  be  said  to  be  seen  to  grow  ! 

(360)  Here  was  a  phenomenon  of  a  new  and  startling  kind.  The  increase  in  the  dimensions 
of  comets  in  their  recess  from  the  sun,  had,  it  is  true,  been  pointed  out  and  dwelt  upon  by  M. 
Valz,  as  an  effect  due  in  his  opinion  to  the  relief  of  pressure  of  the  aether  upon  them,  and  as 
following  a  certain  direct  ratio  of  distance  from  the  sun,  such  as  might  be  conceived  to  correspond 
to  the  supposed  density  of  the  aether  at  that  distance.  But  in  this  case,  in  so  small  an  interval  of 
time,  the  change  of  distance  from  the  sun  is  altogether  trifling  compared  with  the  change  of 
dimension.  If  the  above  measures  were  correct,  the  bulk  of  the  head  (supposing  its  posterior 
part  to  have  participated  in  the  increase)  must  have  enlarged  in  the  ratio  of  1  :  1.198  or  5  :  6,  a 
quantity  out  of  all  proportion  to  the  increase  of  its  radius  vector  in  the  interval.  Subsequent 
observations,  it  will  be  seen,  show  the  change  not  to  have  been  indeed  quite  so  rapid,  while  they 
confirm  its  reality,  and  lead  to  conclusions  of  the  most  singular  nature,  as  will  be  shown  when  we 
come  to  consider  a  resume  of  the  results. 

(361)  On  this  night  the  position  of  the  axis  of  the  nuclear  ray,  taken  with  the  20-feet  micro- 
meter, was  276°. 9,  and  its  length,  from  the  nucleus  to  a  small  star,  which,  at  15h  40m  M  T,  hap- 
pened to  be  situate  precisely  in  the  axis,  and  at  the  extremity,  came  out,  by  a  difference  of  R  A, 
=  91". 75,  which,  however,  is  probably  rather  too  small.  The  nucleus  itself  was  somewhat 
excentrically  placed,  with  respect  to  the  line  of  symmetry  of  the  head  being  nearer  to  its  southern 
than  to  its  northern  limb.    Its  distance  from  the  vertex  at  15h  23m  =  7S.00  A  R  A  =  95".0. 

(362)  On  the  next  night,  the  26th,  the  increase  of  dimension  of  the  comet  was  evident  at 
the  first  glance.  Its  form,  too,  had  undergone  a  change,  being  more  elongated  in  proportion  in 
the  direction  of  its  axis,  and  materially  less  definite  in  its  posterior  region.  Its  appearance  in  the 
20-feet  and  proportional  size  (being  drawn  on  the  same  scale  as  Fig.  1),  are  represented  in 
Fig.  2,  PI.  XV.  The  coma  also  had  undergone  a  great  and  remarkable  change — not  so  much  in 
dimension  (which  had  not  indeed  increased  proportionally,  extending  still  to  a  distance  from  the 
vertex  only  0.8  of  a  radius  of  the  field  or  6')  as  in  brightness ;  being  very  much  enfeebled.  The 
small  protuberance,  however,  to  which  allusion  has  already  been  made,  on  the  south  preceding 
side,  had  extended  into  a  sort  of  wing  towards  a  star  of  the  9th  magnitude  s  p,  to  a  distance 
nearly  twice  as  great  as  in  any  other  quarter.  The  head  or  envelope  had  begun  to  assume  an 
evident  tendency  to  a  paraboloidal  form,  the  posterior  portion  being  terminated,  however,  by  an 
outline  of  an  oval  or  nearly  semicircular  figure.  The  nucleus  appeared  as  a  star  about  the  11th 
magnitude,  not,  however,  sharp  and  sparkling  like  a  true  star,  but  furred  and  nebulous,  so  that, 
with  its  ray,  it  presented  exactly  the  appearance  of  a  miniature  comet,  having  a  head  and  tail  of 
its  own. 

(363)  The  dimensions  of  the  comet  obtained  on  this  night,  with  the  equatorial,  were  as 
follows  : — 


400 


OBSERVATIONS  OF  HALLEY'S  COMET. 


M  T  14''  21"'— Length  of  the  Paraholoid  from  vertex,  or  Diameter  of  the  head  in  R  A     .  31 1" A 

14'  25"'— Diameter  in  Declination   328".9 

14"  27"' — Diameter  across  the  axis,  or  greatest  breadth  of  the  well-defined  portion   .  333".5 

14'' 31"' — Distance  of  Nucleus  from  vertex   110".9 

Differences  of  R  A,  and  measures  with  the  20-feet  position  micrometer,  gave  for 

M  T  15h  40"— Diameter  in  R  A  (23!.625  =  A  R  A)   308".9 

16h  2m — Distance  of  Nucleus  from  vertex  in  parallel  (9«.28)   121".3 

15"  51 '—Length  of  Ray  in  R  A  (12 .19)   159".5 

15>.  24m— Position  of  Ray,  276°.3. 


The  total  bulk  of  the  comet  (exclusive  of  the  coma)  had  therefore  considerably  more  than 
doubled  within  the  twenty-four  or  twenty-five  hours  elapsed  since  the  measurements  of  the 
previous  night ! 

(364)  On  the  27th  January,  the  appearance  in  the  20-feet  was  as  represented  (on  the  same 
scale)  in  Fig.  3,  PL  XV.  The  head  or  envelope  with  its  enclosed  nucleus  and  ray,  still  more 
dilated  than  last  night,  but  the  coma  was  grown  extremely  thin  and  faint,  still,  however,  extending 
to  about  the  same  distance  from  the  well  defined  outline  of  the  vertex.  It  had  lost,  however,  all 
regularity  of  form.  A  considerable  ragged  protuberance  appeared  in  front,  in  the  nf  region, 
while  the  wing  on  the  s  p  side  seemed  to  have  attached  itself  to  the  arc  of  the  paraboloid, 
prolonging  it  as  a  kind  of  one-sided  and  false  tail.  During  the  whole  of  this  night's  observations, 
the  southern  arc  of  the  paraboloid  appeared  larger  than  the  northern.  The  nucleus  presented 
less  of  a  stellar  aspect  than  heretofore,  and  more  that  of  the  head  of  an  ordinary  comet,  its 
denser  portion  being  estimated  at  12"  in  diameter.  Measures  of  the  several  parts  were  taken 
on  this,  and  on  all  other  occasions,  so  long  as  it  continued  practicable  to  do  so ;  but,  not  to 
interrupt  the  course  of  our  statement  with  a  mass  of  figures,  they  are  reserved  to  be  presented 
synoptically  in  tabular  form. 

(365)  Jan.  28.  20  feet.  "  Most  astonishing !  the  coma  is  all  but  gone,  but  there  are 
long  irregular  nebulous  tails  in  various  directions."  (In  the  night-glass,  before  this  observation, 
there  appeared  distinctly  a  forked  swallow-tailed  appendage  going  off  from  the  head,  the 
branches  being  of  unequal  length  and  brightness,  and  making  an  angle  of  about  45°  with  each 
other.  These,  as  is  evidently  seen  in  Fig.  4,  PI.  XV.,  are  the  remains  of  the  coma,  the  portion 
of  which,  to  the  s  p  side,  formed  the  nearest  approach  to  a  tail  which  the  comet  exhibited  after 
its  perihelion.) — "  Twenty  feet.  The  nucleus  is  now  no  longer  a  dim,  misty  speck,  but  a  sharp 
brilliant  point.  I  cannot,  however,  '  raise  a  disc^  on  it,  at  least  not  a  well-defined  one  ;  but  the 
light  comes  on  so  suddenly,  it  is  like  a  planetary  nebula  a  little  hazy  at  the  edges,  2"  or  2\" 
in  diameter,  16h  0m  M.  T.  Being  now  high,  and  the  telescope  acting  to  admiration  (nothing 
ever  equalled  the  definition  of  stars  to-night),  I  see  a  sharp,  all  but  planetary  disc,  diameter 
fully  \^",  quite  distinct  from  the  haze  about  it.  Power  320  shows  it  well.  It  is  like  one  of  Jupi- 
ter's satellites  in  a  thick  fog  of  hazy  light.  Nothing  can  be  more  delicate  and  regular  than  the 
curve  of  the  head  and  the  symmetry  of  the  whole  upper  part  of  the  figure."  The  continued 
dilatation  of  the  comet  on  this  and  the  subsequent  nights  is  well  exhibited  in  the  figures  of 
Plates  XV.  and  XVI.,  which  are  all  on  the  same  scale.  The  observations  of  this  night 
conclude  with  the  following  memorandum : — "  So  ended  a  most  memorable  night.     I  can 


WITH  REMARKS  ON  ITS  PHYSICAL  CONSTITUTION. 


401 


hardly  doubt  that  the  comet  was  fairly  evaporated  in  perihelio  by  the  heat,  and  resolved  into 
transparent  vapour,  and  is  now  in  process  of  rapid  condensation  and  re-precipitation  on  the 
nucleus." 

(366)  The  29th  of  January  was  cloudy,  and  my  observations  on  the  30th  were  cut  short 
by  clouds,  after  procuring  a  few  equatorial  measures.  The  nucleus  and  interior  comet  were, 
however,  now  much  more  developed,  so  as  to  be  well  seen  in  this  instrument  with  its  power 
170,  which  had  not  hitherto  been  the  case.  On  the  31st,  the  20  feet  was  again  brought  into 
action,  when  the  comet  appeared  as  in  Fig.  1,  PL  XVI.  It  was  now  so  much  dilated  as  more 
than  to  fill  the  field  of  view  (15')  in  length,  and  nearly  so  in  breadth;  the  right,  or  southern 
side,  however,  being  still  the  longer  and  brighter,  and  the  termination  irregular  and  indistinct. 
Every  trace  of  coma  had  disappeared,  as  had  also  the  false  tail  or  appendage  to  the  southern 
arc  of  the  parabolic  envelope.  The  clear  parabolic  outline  of  the  head  was  seen  free  from  any 
mistiness  or  vaporous  appearance,  and  in  its  full  beauty,  and  certainly  a  more  delicately  formed 
and  soft,  yet  well  defined,  outline  than  it  presented  on  this  night,  could  not  be  imagined.  It 
was  indeed  a  charming  object.  My  journal  compares  the  rounding  off  of  its  edges  to  that  of  the 
wane-cloud,  occasionally  seen  on  the  Table  Mountain  in  certain  stages  of  a  south-east  gale. 
The  simile,  though  apposite,  conveys  no  illustration  to  a  European  reader.  That  of  a  trans- 
parent gauze  or  alabaster  vase  illuminated  from  within  may  be  more  successful.  All  idea  of 
vagueness  or  confusion  connected  with  an  ill  defined  and  fluctuating  coma  being  now  absent,  an 
impression  of  regularity  of  structure  and  of  precise  and  definite  laws  obeyed  in  its  constitution, 
was  no  less  strongly  conveyed  by  this  view  of  it  than  by  that  of  the  body  of  Jupiter  or  Saturn. 
From  this  night  may  be  dated  the  commencement  of  the  development  of  the  true  tail,  viz.,  the 
prolongation  into  a  regular  train  of  the  parabolic  envelope,  aided  in  its  general  effect  by  the 
similar  prolongation  of  the  ray  or  internal  comet,  which  had  now  become  very  conspicuous. 
The  coma  from  this  time  appeared  no  more,  but  in  the  progress  of  the  comet  towards  its  final 
extinction,  the  semblance  of  a  new  coma  arose  from  the  dilatation  of  the  mass  of  internal  light 
immediately  surrounding  the  nucleus,  after  the  final  dissipation  of  the  envelope,  and  which,  from 
being  at  first  a  subordinate  and  inconspicuous  part  of  the  phenomenon,  became  by  degrees  a 
leading  feature,  and  at  last  may  be  said  to  have  constituted  the  whole  visible  comet,  the 
infinitely  minute  and  hardly  perceptible  nucleus  excepted. 

(367)  The  comet  on  this  night  (January  31)  was  full  of  small  stars,  and  in  its  course  passed 
tangentially  over  one  at  the  edge  of  the  densest  part  of  the  paraboloid,  while  another  was 
swept  across  by  the  axis  of  the  Ray.  And  I  may  here  mention,  once  for  all,  that  among  the 
innumerable  stars  of  all  magnitudes,  from  the  ninth  downwards,  which  at  various  times  were  seen 
through  it,  and  some  extremely  near  to  the  nucleus  (though  none  exactly  on  it),  there  never 
appeared  the  least  ground  for  presuming  any  extinction  of  their  light  in  traversing  it.  Very 
minute  stars  indeed,  on  entering  its  brighter  portions,  were  obliterated,  as  they  would  have 
been  by  an  equal  illumination  of  the  field  of  view ;  but  stars  which  before  their  entry  appeared 
bright  enough  to  bear  that  degree  of  illumination,  were  in  no  case,  so  far  as  I  could  judge, 
affected  to  a  greater  extent  than  they  would  have  been  by  so  much  lamp-light  artificially 
introduced. 

(368)  February  1.  Under  the  joint  influence  of  a  moon  nearly  full  and  the  morning 
twilight,  the  comet  was  much  enfeebled.    Its  outline,  however,  continued  quite  distinct;  so 

5  K 


402 


OBSERVATIONS  OF  HALLEY'S  COMET, 


that,  when  brought  up  to  the  edge  of  the  field  of  view  of  the  20  feet,  the  want  of  fitting  of  its 
convexity  into  the  concavity  of  the  field  circumference  was  apparent  by  a  narrow  darker  lunule 
at  the  sides  of  the  vertex.  The  nucleus  was  grown  more  bulky,  hazy,  and  ill  defined,  and 
its  tail  very  strong.  From  this  time  till  the  11th  February,  the  moon  approaching  and  passing 
the  place  of  the  comet,  caused  the  20  feet  observations  to  be  suspended — the  equatorial  only 
being  used  for  determinations  of  its  place,  and  for  such  measurements  of  dimension  as  could 
be  procured,  which,  however  (for  the  cause  assigned),  ceased  to  be  practicable  after  the  4th, 
though  it  still  continued  to  present  a  perceptible  and  constantly  dilating  outline.  On  the 
removal  of  the  moon  the  dilatation  had  become  so  great,  and  the  envelope  so  faint,  that  no  more 
mierometric  measures  of  dimension  could  be  procured.  The  20  feet  observations  were  resumed 
on  the  11th,  on  which  day  it  was  seen  as  in  Fig.  2,  Plate  XVL,  omitting  most  of  the  stars  of 
which  a  great  multitude  bespangled  it,  and  is  described  as  "  a  superb  object,  but  grown  much  too 
large  for  the  grasp  of  this  telescope  with  its  sweeping  power.  Tried  it  with  the  Huygenian  eye- 
piece of  the  night-glass,  which  improves  it  much.  The  nucleus  now  is  the  most  conspicuous 
part,  being  vastly  brighter  than  the  rest,  psvmbM  almost  to  a  star.  I  see  no  increase  of 
brightness  at  the  edges  as  if  it  were  a  shell.  The  outline  is  that  of  a  planetary  nebula,  somewhat 
hazy  at  the  edges  with  this  low  power.  With  180  much  less  definite  :  A  R  A  between  nucleus 
and  vertex  =  35s. 50  (almost  exactly  occupying  the  interval  between  the  wires)  =  452'/.7."  The 
elongation  of  the  paraboloid  was  now  such  as  to  merit  its  being  regarded  as  a  true  tail,  and  from 
this  time  forward  its  appearance  in  the  night-glass,  finder,  &c,  was  that  of  an  ordinary  comet, 
with  a  short,  broad,  parabolic  tail,  which  on  the  15th  Feb.  occupied  f  the  radius  of  the  field  of 
the  equatorial  finder,  or  about  40'. 

(369)  On  the  17th,  in  the  20  feet,  with  the  above  mentioned  Huygenian  eye-piece,  it  was 
"  dilated  to  a  vast  size,  and  no  longer  sharply  defined,  but  yet  the  outline  well  made  out,  the 
nucleus  pretty  sharp,  all  but  stellar,  and  much  brighter  than  ever  seen  before,  but  the  interior 
cometic  tail  hardly  perceptibly  brighter  than  the  general  tail."  On  the  19th,  "The  nucleus  and 
its  coma  very  bright,  and  highly  condensed.  The  parabolic  envelope  hardly  to  be  made  out,  and 
evidently  distorted.  The  right  (south)  side  of  the  envelope  is  best  defined,  and  tolerably  sharp. 
The  left,  especially  towards  the  vertex,  is  very  irregular  in  shape,  and  extends  far  out  to 
near  a  star  7  m."  See  Fig.  6,  PI.  XIV,  of  which  the  scale  is  much  reduced  in  proportion  to  the 
other  figures. 

(370)  From  this  time  forward,  the  envelope  continued  still  to  dilate,  becoming,  however, 
worse  defined  and  fainter,  till  at  length,  on  the  18th  of  March,  all  trace  of  a  visible  outline  had 
disappeared.  "  20  feet — the  nucleus  is  singularly  bright  compared  with  the  nebula,  which  is 
diffused,  and  loses  itself  insensibly.  An  immense  region  around  it  is  dimly  lighted  with  a  nebulous 
light,  but  no  form  is  traceable  with  the  sweeping  power."  On  the  22d  March  it  was  taken  in  a 
regular  sweep  on  the  meridian,  and  is  described  as  "vvvsvvmbM  to  a  well  concentrated 
but  not  stellar  nucleus,  4"  diam.  R  A  11"  45m  25\4 ;  N  P  D  114°  41'  22"  (for  1830)."  The 
tail  of  the  nucleus  or  the  "Ray"  had  entirely  disappeared,  and  henceforward  it  presented  only 
the  appearance  of  a  round  nebula,  highly  and  very  suddenly  condensed  in  the  middle  (in  which 
state  it  is  figured  in  Fig.  7,  PI.  XIV,  on  May  3),  gradually  dying  away  till  finally  lost. 

(371)  Four  things  in  the  post-perihelion  history  of  this  comet  are  especially  remarkable: 
1st,  The  astonishingly  rapid  dilatation  of  the  visible  dimensions ;  2d,  The  preservation  of  the  same 


WITH  REMARKS  ON  ITS  PHYSICAL  CONSTITUTION. 


403 


regular  geometrical  form  of  the  dilated  and  dilating  envelope ;  3dly,  The  rapid  disappearance  of 
the  coma;  and,  lastly,  the  increase  in  density  and  relative  brightness  of  the  nucleus.  As  regards 
the  dilatation,  the  following  synoptic  table  of  the  measures  of  the  several  parts  as  taken  with  the 
equatorial  by  direct  micrometric  measurement,  or  with  the  20  feet  by  differences  of  R  A 
and  angles  of  position,  will  best  express  the  fact.  In  this  table,  letters  of  reference  are 
attached  to  each  observation,  capitals  denoting  equatorial  measurements,  and  small  letters 
20  feet  determinations. 


Date. 
1836. 

Distance 
of  Nucleus 
from 
Vertex. 

11 

Mean 
Time  of 
Observ- 
ation, 
h.  m. 

Length 

of 
Para- 
boloid. 

// 

Mean 
Time  of 
Observa- 
tion, 
h.  m. 

Breadth 
of 
Para- 
boloid. 

11 

Mean 
Time  of 
Observa- 
tion, 
h.  m. 

Length 
of 
Ray. 

11 

Mean 
Time  of 
Observa- 
tion, 
h.  m. 

Position 
of  Axis  of 
Ray. 

0 

Jan.  25  . . 

A 

118. 3:: 

C 

229.4 

13  38 

E 

237.3 

14  15 

g 

91.7 

15  40 

k 

276.8 

b 

9S-o 

15  23 

D 

196.7:: 

16  25 

F 

252.O 

16  29 

Jan.  26  . . 

A 

1 10.9 

14  31 

C 

311.4 

14  21 

E 

328.9 

14  25 

S 

'59-5 

15  51 

k 

276.3 

b 

121. 3 

16  2 

d 

308.9 

15  40 

F 

333-5 

14  27 

Jan.  27  . . 

A 

160.4:: 

H  45 

C 

400.6 

14  42 

E 

422.2 

14  40 

k 

^77-3 

b 

154.0 

15  27 

d 

472.7 

15  29 

Jan.  28  . . 

A 

164.5 

14  53 

c 

482.3 

14  51 

E 

497.2 

14  46 

G 

291.2 

b 

171. 1 

16  12 

h 

381.4 

Jan.  30  . . 

A 

207.0 

14  31 

Jan.  31 

A 

218.2 

14  45 

c 

739.6 

14  50 

Feb. 1  

A 

230.1 

14  55 

d 

900.0 

«5  15 

E 

823.3 

14  5° 

F 

668.4:: 

14  55 

Feb. 2  

A 

258.4 

14  57 

E 

939.2 

15  5 

G 

561.7 

K 

282.0 

F 

835-3 

15  3 

Feb. 4.... 

A 

287.6 

15  0 

F 

937-7 

Feb.  11  .. 

a 

452.7 

13  56 

Notes. — January  25 — A,  very  uncertain,  owing  to  the  difficulty  of  seeing  the  nucleus ;  D,  in  strong  morning  twilight,  too 

small ;  g  by  A  R  A  of  nucleus  and  extremity  of  Ray. 
January  26 — b,  by  a  mean  of  two  differences  of  R  A  of  nucleus  and  vertex,  mean  9'. 28  ;  d,  by  A  R  A  =  23  .63  ;  E,  diameter  in 

declination  of  the  best  defined  oval  portion  ;  F,  ditto  ditto,  perpendicular  to  axis  of  the  comet ;  g.  A  R  A  =  12s.  125. 
January  27 — A,  very  difficult,  uncertain  measure;  b,  A  R  A  =  13s.  125;  d,  A  R  A=  36.19;  k,  by  two  measures  exactly 

agreeing. 

January  28 — b,  by  A  R  A  =  13M25  ;  C,  cutting  deep  into  the  thin  base  of  the  paraboloid;  E,  diameter  in  declination  of  the 

most  spherical  mass. 
January  31 — C,  by  A  R  A  =  57'.o. 

February  1 — C,  length  just  contained  in  field  15' diameter;  E,  greatest  breadth  of  paraboloid;  F,  breadth  across  nucleus,  or 
apparent  parameter.    The  same  is  also  indicated  by  these  letters  on  February  2  and  February  4. 

(372)  The  only  element  in  these  measurements  which  is  sufficiently  definite  and  com- 
parable throughout  the  series,  and  at  the  same  time  little  affected  by  the  unequal  lights  of  the 
telescope  used,  is  the  distance  of  the  nucleus  from  the  vertex  of  the  paraboloid.  Calculating  on 
this  element,  and  rejecting  the  equatorial  measures  of  Jan.  25  and  Jan.  27,  on  which,  from  the 
circumstances  of  the  measures,  no  dependence  can  be  placed,  and  taking  means  of  those  of 
Jan.  26  and  28,  we  find  the  following  extraordinary  series  of  values  of  the  apparent,  and  real  bulk 
of  that  definite  segment  of  the  paraboloid,  which  may  be  conceived  cut  off  at  its  vertex  by  a  plane 


404 


OBSERVATIONS  OF  HALLEY'S  COMET, 


at  right  angles  to  its  axis  passing  through  the  nucleus.  The  real  bulk  is  derived  from  the 
apparent,  by  multiplying  it  by  the  cube  of  the  distance  from  the  earth,  as  given  by  Mr.  Stratford's 
ephemeris    In  both,  the  volume  for  Jan.  25  is  taken  as  unity. 


Date. 

Apparent 
Volume. 

Heal 
Volume. 

Date. 

Apparent 
Volume. 

Real 
Volume. 

Date. 

Apparent 
Volume. 

Real 
Volume. 

January  25 . . 

1. 000 

1,000 

January  28 . . 

5.511 

5-»79 

February  1 . . 

14.010 

12.242 

„  26.. 

1.825 

I.789 

„  30.. 

10.345 

9.314 

,,       2. . 

20. 125 

16.953 

„  27.. 

4.260 

4.089 

„  31" 

12. 1  13 

10.672 

,1  4-- 

27-743 

22.343 

„  11.. 

108.210 

74-3°3 

From  which  it  appears,  that  although  the  approach  of  the  comet  to  the  earth  accounts  for 
some  considerable  part  of  the  apparent  dilatation  of  volume,  yet,  allowing  for  the  full  effect  of 
this  cause,  the  definite  segment  in  question  had  actually  enlarged  to  74  times  its  original  bulk  in 
the  17  days  elapsed  between  the  extreme  observations.  The  total  volume,  however,  or  the  solid 
content  of  the  whole  visible  paraboloid,  had  increased  in  a  much  greater  proportion,  viz.,  in  the 
interval  from  Jan.  25  to  Feb.  1,  (the  last  day  on  which  measures  of  the  total  length  and  breadth 
were  procured),  in  the  ratio  of  1  to  41.605,  instead  of  1  :  12.242,  as  in  the  table. 

(373)  A  most  singular  consequence  follows  from  this.  If  we  project  the  measured  distance 
of  the  nucleus  from  the  vertex  on  a  chart  of  engraved  squares,  taking  the  time  elapsed  in  days 
since  a  given  date  (say  Jan.  0),  for  the  abscissa,  and  the  distance  in  question  for  the  ordinate,  we 
shall  find  the  locus  of  the  interpolating  curve  to  be  very  nearly  a  straight  line,  and  the 
ordinate  to  be  expressed  very  nearly  by  the  equation. 

(t  -   21.07)   x    21"  =  y 

and,  in  fact,  if  we  compare  the  distance  in  question  as  calculated  from  this  formula  with  that 
resulting  from  actual  measurement,  we  find  them  to  correspond  as  follows: — 


Jan. 

25 
26 


27 
28 


Date  =  t. 


h. 
15 
14 
16 

15 
14 
16 


23     =  25.64  . 

31  \  =  26.64  • 
2  5 


(mean) 
27  =  27.64  . 
53*=. 
12  5  /, 


30  14 


28. 69  . 

(mean) 
31     =  30.60  . 


Nucleus  from  Vertex. 


Measured.  Calculated 


95.0 
116. 1 

154.0 
167.8 

207.0 


96.0 
1 1 6.9 

138.O 
160.0 


Date  =  t. 


Jan.  h.  m. 
3i     H  45 


31.61 


Feb. 
1 

2 

4 
1 1 


14  55  =  32-62 

'4  57  =  33-62 

15  0  =  35.63 
13  56  =  42.58 


Nucleus  from  Vertex. 


Measured. 


218.2 


230.1 
258.4 
287.6 
452.7 


Calculated. 


221.3 


242.5 
263.5 
307.0 
45J-7 


(374)  We  see  by  this  comparison,  that  the  apparent  linear  dilatations  of  the  envelope  was 
nearly  uniform  during  the  whole  interval  embraced  by  my  observations,  so  long,  at  least,  as  it 
continued  measurable,  and  that  the  mean  rate  of  that  dilatation  was  21"  per  diem  on  the  vertical 
distance.  Now,  if  we  calculate  backwards,  on  the  hypothesis  of  this  rate  having  been  previously 
observed,  i.  e.,  if  we  resolve  the  equation  t  —  21.07  =0,  or  take  t  =  21.07  =  21d  0h  10m,  we 


WITH  REMARKS  ON  ITS  PHYSICAL  CONSTITUTION. 


405 


arrive  at  the  singular  conclusion  that  on  the  21st  of  January,  at  0h  10m  p.m.,  the  envelope  had  no 
magnitude,  that  in  short,  at  that  moment,  a  most  important  physical  change  commenced  in  the 
comet's  state.  Previous  to  that  instant,  it  must  have  consisted  of  a  mere  nucleus,  a  stellar  point, 
more  or  less  bright,  and  a  coma  more  or  less  dense  and  extensive.  At  that  instant,  the  formation 
of  the  envelope  commenced,  and  continued  in  the  manner  and  at  the  rate  above  described. 
The  "  Ray,"  or  internal  comet,  no  doubt,  also  commenced  its  existence  at  the  same  instant. 

(375)  Laying  aside  for  a  moment  all  speculation  as  to  the  physical  interpretation  of  this 
strange  fact,  I  must  now  notice  a  most  remarkable  observation  (unknown  to  me  at  the  time  of 
drawing  the  above  conclusion),  which  corroborates  in  a  striking  and  unexpected  manner  the  result 
arrived  at.  On  the  night  of  the  22nd  January,*  M.  Boguslawski,  Professor  of  Astronomy  at 
Breslau,  actually  observed  the  comet  as  a  star  of  the  6th  magnitude,  a  bright,  concentrated  point, 
which  showed  no  disc  with  a  magnifying  power  of  140  :  and  that  it  actually  ivas  the  comet,  and 
no  star,  he  assured  himself  by  turning  the  telescope,  the  next  night,  on  the  place  where  he  saw 
it.  It  was  gone.  Moreover,  he  had  taken  care  to  secure,  by  actual  observation,  the  place  of  the 
star  he  had  observed.  That  place  agreed  with  the  calculated  place  of  the  comet.  Certainly 
better  evidence  could  not  be  had. 

(376)  The  above  statement  rests  on  the  authority  of  a  letter  from  M.  Boguslawski  to  the  late 
Dr.  Olbers,  which  that  venerable  astronomer  had  the  goodness  to  show  me  on  the  occasion  of  a 
visit  I  made  to  him  at  Bremen  on  July  27,  1838.  Not  having  a  copy  of  that  letter,  and  wishing 
for  more  precise  information,  I  wrote  to  M.  Boguslawski  on  the  subject,  and  was  favoured 
by  him  with  a  reply,  dated  Breslau,  Sept.  20,  1838,  of  which  the  following  is  an  extract: — 

"I  saw  the  comet  without  any  diameter,  not  on  the  night  of  Jan.  21-2,  but  of  Jan.  22-3, 
between  17h  36m.8  and  18h  3m.7  m  t  at  Breslau.  But  this  very  circumstance  agrees  better  with 
your  observation  and  measurements  than  you  have  found  yourself.  One  need  only  derive  from 
your  observations  another  very  plain  curve,  which  will  bend  still  closer  to  your  measurements 
than  yours,*f-  viz. : — 


Date. 

Your  measurements. 

Your  Curve. 

The  New  Curve. 

1836.  Jan. 

25-5 

// 

93 

// 
93 

// 
93.0 

26.5 

119 

114 

1 19.0 

27.5 

144 

135 

142.8 

28.5 

168 

156 

164.4 

3°-5 

201 

198 

201.0 

3i-5 

216 

219 

216.0 

"  and  this  prolonged  backwards  gives  : — 

Date  January  25.5;  24.5;  23.5;  22.5;  22.45. 

Ordinate   93-°;  64.8;   34.4;     1.8;  0.0. 

*  In  a  statement  of  this  curious  fact  to  the  British  Association,  at  Newcastle,  printed  in  their  Report  for 
1838-9,  the  date  is  given  as  the  21st,  but  erroneously. 

t  This  is  perfectly  correct.  The  interpolating  curve  drawn,  as  I  had  drawn  it,  does  actually  deviate  from  the 
straight  line  assumed  as  its  mean  representative,  in  the  manner  M.  Boguslawski  indicates.  It  is  concave  towards 
its  abscissa  from  January  25  to  January  31,  and  convex  towards  the  same  line  from  that  epoch  to  February  11  : 

5  L 


406 


REMARKS  ON  ITS  PHYSICAL  CONSTITUTION, 


"  The  zero  point  of  the  abscissa  and  of  the  dilatation  of  the  nebula  of  the  comet  will  be 
Jan.  22.45  =  Jan.  22  10h48m.  I  observed  the  comet,  like  a  star,  at  17h  50m,  therefore  7h  2m  after 
that  calculated  catastrophe.  It  follows,  indeed,  that  the  radius  of  the  comet  according  to  the 
curve  must  have  been  then  already  9//.5,  and,  therefore,  the  diameter  19".  But,  having  not  the 
slightest  diameter,  although  one  of  3".45  (that  of  Uranus),  by  a  magnifying  power  of  140,  was 
lately  sufficiently  evident — one  is,  perhaps,  obliged  to  believe  that  the  motion  of  the  dilatation  at 
the  beginning  was  still  faster  than  the  equation  of  this  curve  expresses." 

(377)  Mr.  Maclear  observed  the  comet  on  the  24th  of  January,  and  assigns  2'  11"  for  the 
diameter  of  the  disc  on  that  day.  It  was  then  so  nearly  circular  (see  the  beautiful  engravings 
accompanying  his  paper),  that  the  half  of  this,  or  65". 5  may  very  properly  be  taken  for  the 
distance  from  the  nucleus  to  the  vertex  on  that  night.  A  decrease  of  21"  on  93,  would  give  72" 
for  this  distance.  This  observation,  therefore,  corroborates  the  idea  of  a  more  rapid  rate  of 
increase  in  the  earlier  stages,  and  agrees  very  closely  with  M.  Boguslawski's  curve. 

(378)  It  will  not  be  necessary  to  enter  into  any  calculation  of  the  comet's  distance  from  the 
sun  at  the  moment  of  these  observations,  to  warrant  our  rejection  of  an  hypothesis  such  as  that  of 
M.  Valz,  which  makes  the  volume  depend  directly  on  that  distance.  Undoubtedly,  its  recess 
from  the  sun  is  ultimately,  but  indirectly,  the  cause  of  the  observed  increase.  The  question  is 
only  as  to  the  modus  operandi.  The  perihelion  passage,  it  will  be  borne  in  mind,  took  place  on 
the  loth  of  November,  and  it  was  therefore  not  till  the  83rd  day  after  that  event  that  the 
formation  of  the  envelope  commenced.  Now,  during  these  83  days,  it  is  certain  that  a  process 
of  refrigeration  had  been  going  on,  both  in  the  nucleus,  and  in  the  transparent  and  vaporous 
matter,  if  any,  with  which  it  was  surrounded.  It  is  hardly  possible  to  imagine  a  case  more 
corroborative  of  the  view  taken  of  this  subject  in  my  paper  on  Biela's  comet  (Mem.  Ast.  Soc. 
Vol.  VI.  pp.  104,  105).  According  to  the  theory  there  suggested,  the  surface  of  the  nucleus 
must  be  supposed  to  have  cooled  down  at  this  precise  epoch  to  the  dew-point  (granting  the 
extension  of  such  a  time  to  the  point  of  condensation  of  the  vapour,  whatever  its  nature,  present 
in  the  cometary  atmosphere,  but  not  constituting  the  whole  of  it).  At  this  instant,  therefore, 
according  to  that  theory  and  in  conformity  with  all  we  know  of  the  laws  of  vaporous  con- 
densation, must  have  commenced  the  formation  of  a  mist,  first,  precisely  in  contact  with  the 
radiating  surface,  and,  by  degrees  more  or  less  rapid,  ascending  above  it,  and  limited  (as  we 
actually  see  radiation  fogs  in  our  valleys  or  on  extensive  plains  in  very  calm  nights),  by  a 
definite  upper  surface,  the  seat  of  a  fresh  process  of  radiation.  As  this  superior  vapour-plane 
attains  a  higher  and  higher  level,  corresponding  to  a  less  and  less  actual  density,  both  of  the 
atmosphere  and  vapour,  its  surface,  without  losing  its  geometrical  form,  necessarily  becomes  less 
and  less  visible  and  conspicuous  ;  acquiring  as  it  were,  a  greater  tenuity,  and  becoming  more 
filmy  in  its  texture ;  being,  in  fact,  nothing  else  than  a  boundary  surface  between  a  transparent 
medium  above,  and  a  misty  one  diminishing  in  opacity  as  the  level  rises,  below. 

(379)  It  is  this  superior  vapour  plane  which  constitutes,  in  our  conception  of  the  matter, 
the  visible  surface  of  the  envelope.  As  the  envelope  increases  in  dimension,  that  surface,  for 
the  reason  adduced,  must  continually  become  more  faintly  outlined,  and  at  length  disappear 


indicating  a  more  rapid  approach  to  the  abscissa  previous  to  January  25  than  the  straight  line  would  give.  Hav- 
ing no  observations,  I  did  not  think  it  necessary  to  go  into  the  minutiae  of  its  flexure. 


AND  THAT  OF  COMETS  IN  GENERAL. 


407 


altogether ;  an  additional  cause  for  which  will  be  the  removal  of  reflective  matter  from  below, 
by  subsidence  into  the  nucleus  or  into  the  axis  of  the  paraboloid  (according  to  the  peculiar  laws 
of  cometic  aggregation,  of  which  more  presently),  as  we  see  a  cloud  subsiding  in  rain  beneath, 
and  accumulating  in  visible  volume  above. 

(380)  If  the  condensible  vapour  were  everywhere  distributed  spherically  around  the 
nucleus,  so  as  to  have  equal  density  at  equal  distances,  the  form  of  the  envelope  would 
necessarily  be  spherical,  because,  on  account  of  the  exceeding  tenuity  of  the  cometic  atmo- 
sphere, its  posterior  portion  is  no  way  shaded  by  its  anterior,  but  every  part,  interior  and 
exterior,  equally  exposed  to  the  sun's  influence,  or  very  nearly  so.  That  the  form  is  in  fact 
not  spherical,  but  paraboloidal,  or  very  eccentrically  elliptic,  instructs  us  in  an  important  and 
truly  wonderful  fact,  viz.,  that  the  surfaces  of  equilibrium  of  the  vapour  in  its  transparent  state 
are  so;  that  in  fact,  although  not  seen,  the  envelope  existed  as  a  transparent  atmosphere  — a  tail 
in  posse,  though  not  to  our  eyes  in  esse,  and  of  its  full  extent,  prior  to  the  epoch  of  its  com- 
mencing visibility,  and  probably  prior  to  the  perihelion  passage. 

(381)  If  we  now  inquire  by  what  forces  it  is  possible  that  such  a  form  of  equilibrium  can 
be  maintained,  we  shall  at  once  perceive  that  the  laws  of  gravitation,  as  at  present  recognized, 
are  altogether  insufficient  to  account  for  it.  Such  a  form,  as  one  of  equilibrium,  is  incon- 
ceivable without  the  admission  of  repulsive  as  well  as  attractive  forces.  But,  if  we  admit  the 
matter  of  the  tail  to  be  at  once  repelled  from  the  sun  and  attracted  by  the  nucleus,  it  no  longer 
presents  any  difficulty.  It  is  evident,  without  going  into  any  geometrical  calculations,  that 
the  effect  of  the  sun's  repulsion  on  such  an  atmosphere  must  be  to  distort  it  from  the  spherical 
form  it  would  assume  in  virtue  of  its  gravitation  to  the  nucleus  alone — to  press  the  particles 
on  the  side  of  the  sun  nearer  to,  and  to  drive  those  on  the  opposite  side  farther  from  it,  so 
as  to  give  rise  to  an  oval  form,  the  length  of  which  will  be  the  greater  in  proportion  to  its 
breadth  the  more  energetic  the  repulsive  force  is  supposed ;  and  that  by  assigning  to  that 
force  a  sufficient  energy,  the  oval  in  question  may  be  prolonged  to  any  length,  or  the  remoter 
particles  even  driven  altogether  beyond  the  coercive  range  of  the  nucleus,  and  carried  out  into 
space.* 


*  The  resultant  of  the  two  forces  in  question,  the  one  directed  from  the  sun,  or  in  the  direction  P  X  in  the 
figure  (where  S  is  the  sun  and  C  the  nucleus),  and  the  other  to  the  nucleus,  or  in  the  direction  P  C,  will  neces- 
sarily lie  in  a  direction  P  0,  inter- 
mediate between  them,  which,  if  pro- 
longed, must  cut  the  axis  in  some  point 
N  further  from  the  sun  than  C.  Now, 
if  A  P  B  be  the  surface  of  the  comet's 
atmosphere,  this  resultant  must  neces- 
sarily be  in  the  direction  of  a  normal 
to  it,  supposing  it  in  equilibrio.  The 
angle  C  P  Y,  therefore,  will  necessarily 
be  less  than  a  right  angle,  so  that  the 
portion  P  D  A  of  the  surface  will  lie 
wholly  within,  and  P  E  B  wholly  with- 
out a  circle,  having  C  for  a  centre,  and 
C  P  for  a  radius.    The  for  m,  therefore 


408 


REMARKS  ON  ITS  PHYSICAL  CONSTITUTION, 


(382)  Nor  let  any  one  be  startled  at  the  assumption  of  such  a  repulsive  force  as  here  sup- 
posed. Let  it  be  borne  in  mind  that  we  are  dealing  (in  the  tails  of  comets)  with  phenomena 
utterly  incompatible  with  our  ordinary  notions  of  gravitating  matter.  If  they  be  material  in  that 
ordinary  received  sense  which  assigns  to  them  only  inertia  and  attractive  gi-avitation,  where,  I 
would  ask,  is  the  force  which  can  carry  them  round,  in  the  perihelion  passage  of  the  nucleus,  in 
a  direction  continually  pointing  from  the  sun — in  the  manner  of  a  rigid  rod  swept  round  by  some 
strong  directive  power,  and  in  contravention  of  all  the  laws  of  planetary  motion,  which  would 
require  a  slower  angular  movement  of  the  more  remote  particles,  such  as  no  attraction  to  the 
nucleus  could  give  them,  supposing  it  ever  so  intense?  The  tail  of  the  comet  of  1680,  in  five 
days  after  its  perihelion  passage,  extended  far  beyond  the  earth's  orbit,  having  in  that  brief  interval 
shifted  its  angular  direction  nearly  150°.  Where  can  we  find,  in  its  gravitation  either  to  the  sun 
or  to  its  nucleus,  any  cause  for  this  extravagant  sweep  ? 

(383)  But  again,  where  are  we  to  look  (if  only  gravity  be  admitted)  for  any  reasonable 
account  of  its  projection  outwards  from  the  sun,  putting  its  angular  motion  out  of  the  question? 
Newton  calculates  that  the  matter  composing  its  upper  extremity  quitted  the  nucleus  only  two 
days  previous  to  its  arrival  at  this  enormous  distance.  A  projectional  velocity  much  exceeding 
that  of  the  comet  itself  in  perihelio  (i.  e.  exceeding  that  which  the  sun's  attraction  would  generate 
in  a  body  falling  from  infinit}')  would  be  necessary  for  this  purpose.  If  the  motion  of  matter  be 
a  criterion  of  the  direction  and  intensity  of  the  forces  acting  upon  it,  assuredly  we  can  look 
nowhere  but  to  a  force  directed  from  the  sun,  and  that  of  an  intensity  far  exceeding  its  gravitating 
energy  on  ordinary  planetary  matter,  for  the  origin  of  such  a  movement  (supposing  it  real). 

(384)  The  manner  in  which  Newton  deals  with  this  phenomenon  is  somewhat  unac- 
countable. Discussing  the  various  hypotheses  advanced  on  the  subject,  this,  among  others, 
presents  itself  as  a  speculation  of  Kepler.  "  Alias  particulas  tam  leves  quam  graves  dari  posse 
existimat,  et  materiem  caudae  levitare,  perquc  levitatem  suam  a  sole  ascendere." — Princip.  III. 
prop.  41,  Leseur  and  Jacquier,  iii.  652.  But  he  dismisses  it  summarily  on  the  ground  of  the 
induction  of  a  gravity  proportional  to  inertia  in  all  terrestr  ial  bodies,  and  substitutes  in  its  place  a 
theory  of  the  ascent  of  matter  rarefied  by  heat  in  the  solar  atmosphere  or  the  ether  itself,  in  a 
mode  precisely  analogous  to  a  suggestion  of  Fresnel  respecting  the  cause  of  the  ascent  of  clouds 
in  our  atmosphere.  It  is  surprizing  that  a  mind  so  penetrating  as  Newton's  should  not  have  felt 
the  inadequacy  of  the  means  to  the  end  in  this  account  of  the  matter.  Granting  all  the 
machinery  of  this  hypothesis,  ether,  solar  atmosphere,  and  rarefaction,  still  the  ascent  has  to  be 
effected  ultimately  by  the  sun's  attraction,  i.  e.,  by  the  difference  of  the  gravitations  towards  it  of 
the  displaced  and  displacing  masses ;  and  this  difference  has  to  effect  at  once  the  descent  of  the 
displacing,  and  the  ascent  of  the  displaced  ether  (the  latter  loaded  with  matter  heavier  than 
itself) ;  the  difference  of  the  moving  forces  acting  on  more  than  the  sum  of  the  masses  put  in 
motion ;  as  in  the  case  of  two  unequal  weights  suspended  on  the  arms  of  a  balance  in  which  the 
sum  of  the  bodies  has  to  be  set  in  motion  by  the  difference  of  their  weights.  And  even  granting 
that  from  such  a  combination  an  ascending  velocity  could  be  generated  greater  than  any 

(whatever  be  the  laws  of  the  two  forces,  provided  only  their  directions  be  as  supposed)  will  necessarily  be  such  an 
elongated  or  oval  figure  as  described  in  the  text. 

Where  the  form  is  described  as  paraboloidal,  this  is  of  course  to  be  understood  not  as  designating  strictly  a 
conic  parabola,  but  only  a  form  having  a  general  resemblance,  in  the  neighbourhood  of  its  vertex,  to  such  a  solid. 


AND  THAT  OF  COMETS  IN  GENERAL. 


409 


descending  velocity  which  the  sun's  attraction  could  directly  produce  under  any  circumstances  on 
a  body  falling  freely  (a  thing  clearly  impossible),  it  is  still  only  the  dilated  aether  which  is  so 
driven  upwards,  and  we  are  called  upon  further  to  admit  the  possibility  of  its  carrying  up  with  it 
the  matter  of  the  tail,  while  yet,  on  the  other  hand,  the  same  aether  is  throughout  assumed  to  be 
incapable  (owing  to  its  excessive  tenuity),  of  resisting,  when  itself  quiescent,  the  motion  of 
cometary  matter,  however  rapid.  And  all  this  in  the  face  of  the  resistance  of  the  aether  to  the 
motion  of  an  upward  current  of  its  own  substance  still  more  attenuated.  What  follows,  respecting 
the  angular  motion  of  the  tail  when  so  produced,  is  even  more  difficult  to  reconcile  with  the 
exceeding  clearness  and  precision  of  Newton's  views  in  general. 

(385)  Kepler's  hypothesis  of  a  simply  levitating  matter  as  the  constituent  substance  of  the 
tail  is,  however,  insufficient.  Supposing  the  tail  to  have  no  attraction  for  the  nucleus,  and  to  be 
merely  projected  with  it  into  the  sphere  of  the  sun's  action,  they  would  at  once  part  company, 
the  tail  describing  an  hyperbola  convex,  and  the  nucleus  a  parabola  concave  towards  the  sun.  To 
make  the  hypothesis  available,  it  is  indispensable  to  superadd  that  of  nuclear  attraction.  Taken 
then  as  a  whole,  the  compound  mass  of  the  comet  is  urged  towards  the  sun  by  the  difference  of 
the  total  attractive  and  repulsive  forces,  and  so  long  as  the  repulsive  power  is  insufficient  to 
separate  them,  or  analyse  the  compound,  they  will  revolve  together  as  one  body,  continually 
elongating  itself  as  it  approaches  the  sun,  and  on  the  position  of  whose  larger  axis  the  sun 
exercises  a  directive  power,  as  it  would  on  a  magnet,  if  itself  magnetic;  or  rather,  as  a  positively 
electrified  body  would  on  a  non-conducting  body  of  elongated  form  having  one  end  positively,  the  other 
negatively  excited* 

*  It  is  prudent,  to  say  the  least,  in  such  hypotheses  to  keep  clear  of  specialties,  yet  I  cannot  help  remarking 
that  the  conception  of  a  high  degree  of  electrical  excitement  in  the  matter  of  the  tail  (of  the  same  chai-acter  with 
that  of  a  permanent  electrical  charge  supposed  to  be  resident  in  the  sun),  superadded  to  the  ordinary  conception 
of  a  gravitating  nucleus  would  satisfy  most  of  the  essential  conditions  of  the  problem.  That  the  sun's  heat 
in  perihelio  does  actually  vaporize  a  portion  of  the  cometic  matter,  there  can  no  longer,  I  think,  be  any  reason- 
able doubt.  That  in  such  vaporization,  a  separation  of  the  two  electricities  should  be  effected,  the  nucleus 
becoming  (suppose)  negative,  and  the  tail  positive  is  in  accordance  with  many  physical  facts.  The  circumstances 
of  this  vaporization,  as  they  were  seen  to  take  place  in  Halley's  comet,  were  highly  favourable  to  such  separation. 
The  matter  of  the  tail  seemed  to  be  emitted  in  violent  jets  and  streams,  as  if  from  orifices  or  fissures  in  the 
anterior  part  of  the  nucleus  (See  M.  Struve's  extraordinary  drawings  in  his  Beobachtungen  des  Halleyschen 
Cometen),  a  state  of  things  productive  (as  recent  experiments  have  shown)  of  powerful  electrical  excitement. 
Moreover,  it  is  worthy  of  notice  that  these  jets,  instead  of  continuing  their  course  forwards  towards  the  sun, 
appeared,  in  many  instances,  to  have  been  driven  back,  in  curved  forms,  towards  the  tail,  as  if  unable,  by  reason 
of  some  opposing  power,  to  advance  in  their  original  direction.  That  no  such  tumultuous  phenomena  should 
have  taken  place  after  the  perihelion  passage,  when  the  tail  was  quietly  subsiding  under  the  cooling  process,  is 
precisely  what  might  be  expected ;  and,  in  short,  I  see  no  part  of  the  phenomena  of  a  comet  which  appears  to 
stand  out  as  irreconcilable  with  this  view  of  the  subject.  The  exceeding  energy  of  the  electric  in  comparison 
with  the  gravitating  force  as  exerted  on  matter  of  equal  inertia  is  strongly  in  its  favour. 

Should  it  be  objected  to  this  theory,  that  it  supposes  the  sun  to  be  in  a  permanently  excited  electrical  state, 
and  that,  therefore,  thunder-clouds  in.  our  atmosphere  ought  to  be  attracted  to  or  repelled  from  it,  and  move 
accordingly,  I  would  observe,  in  reply, —  1st,  That  the  matter  of  a  cloud  is  almost  infinitely  denser  than  that  of  a 
comet's  tail,  and  probably  in  a  far  less  powerful  state  of  electrical  excitement,  so  that  the  inertia  bears  an  incom- 
parably greater  ratio  to  the  moving  force :  2ndly,  That  our  clouds  float  in  a  medium  capable  of  resisting,  effec- 
tually, any  independent  movement  so  generated  in  them,  and  of  commanding  completely  their  movements  by  its 
own :  3rdly,  That  we  are  by  no  means  certain  that  other  phenomena  in  meteorology,  referable  to  this  cause,  may 

5  M 


410 


REMARKS  ON  ITS  PHYSICAL  CONSTITUTION, 


(386)  Supposing  the  approach  of  a  comet  to  the  sun  to  be  such  as  to  enable  the  repulsive 
force  to  overcome  the  attractive  in  those  portions  of  its  tail  remote  from  the  nucleus,  they  would, 
of  course,  be  driven  off  irrecoverably.  But  what  would  now  be  the  state  of  the  remaining  mass? 
Inertia  and  repulsion  have  been  subtracted :  of  course,  what  is  left  has  become  pro  quantitate 
materia,  on  both  accounts  more  attractively  disposed  as  a  whole ;  the  dimensions  of  the  orbit  must, 
therefore,  contract.  The  periodic  time  will  diminish.  We  have  here  presented  to  us  a  series  of 
consequences  identical  in  some  of  their  leading  features  with  those  which,  observed  in  the  case 
of  Encke's  comet,  have  been  attributed  to  resistance  of  the  aether.  Pursued  into  all  their 
consequences,  no  doubt  the  two  explanations  diverge.  For  example,  in  the  case  supposed,  the 
diminution  of  the  periodic  time  will  be  more  than  in  proportion  to  the  diminution  of  the  major 
axis  of  the  orbit.  But  it  may  be  doubted  whether  observation  of  a  body  so  ill  defined  is  yet 
precise  enough  to  decide  between  them. 

(387)  The  separation  of  a  portion  of  the  tail  here  contemplated  could  hardly  be  accom- 
plished without  carrying  off  some  portion  of  the  gravitating  matter.  Supposing  the  excess  of 
repulsive  power  anyhow  got  rid  of,  a  new  comet  might  be  formed.  But  there  is  another  mode 
in  which,  without  having  recourse  to  a  direct  divellent  action  of  the  sun  on  the  materials  of  a 
comet  in  perihelio,  its  separation  into  two  may  be  accomplished,  and  a  phenomenon  produced 
like  that  presented  in  the  early  part  of  the  present  year  (1846)  by  Biela's  comet,  which  was 
actually  seen  to  subdivide  ;  the  two  portions  subsequently  journeying  along  quietly  side  by  side 
in  orbits  differing  very  slightly  from  each  other,  and  apparently  quite  undisturbed  by  any  mutual 
attraction.  It  will,  of  course,  have  been  noticed  that,  although  (for  the  sake  of  simpler 
illustration),  we  have  supposed,  in  what  has  been  said  above,  the  form  of  equilibrium  of  our 
envelope  or  tail  to  be  assumed  at  every  instant,  yet  in  this,  as  in  the  theory  of  the  tides  (to 
which  it  properly  belongs,  and  may  be  considered  as  in  some  sort  a  supplement),  the  true 
problem  is  a  dynamical,  not  a  statical  one.  The  oscillations  of  a  fluid  covering  a  central  body, 
may,  as  is  well  known  to  those  who  are  conversant  with  the  theory  of  tidal  movements,  under 
certain  conditions  as  to  the  coercive  power  of  that  central  mass,  cease  to  continue  of  small 
extent,  and  may  increase  in  magnitude  beyond  any  limit  which  analysis  is  capable  of  assigning 

not  exist  and  come  to  be  observed.  A  sun  so  electrically  charged,  would  induce  opposite  electrical  states  in  the 
two  hemispheres  of  day  and  night,  the  intensity  of  those  states  defending  greatly  on  the  degree  of  conductibility  to 
be  attributed  to  the  earth  as  a  mass.  The  electrical  meteorology  of  day  and  night,  indeed  all  electrical  meteorology 
is  in  a  state  too  little  advanced  to  admit  of  satisfactory  answers  to  a  crowd  of  queries  which  here  suggest  them- 
selves. Lastly,  there  may,  after  all,  exist  in  nature  other  repulsive  forces,  whose  existence  can  only  be  known  to 
us  by  studying  their  "instantire  lucifera." 

Without  at  all  going  into  the  question  raised  by  Prof.  Mosotti,  whether  gravitation  be  not  a  manifestation 
of  statical  electrical  action  (or  rather,  without  here  explaining  the  arguments,  which  seem  to  me  opposed  to 
such  an  idea),  one  thing  is  physically  certain,  viz. :  That,  the  laws  of  the  two  powers  being  the  same,  the  apparent 
gravitation  of  one  spherical  body  on  another,  supposing  their  diameters  very  minute,  compared  with  their  mutual 
distance,  may  be  increased  or  diminished  in  any  ratio,  or  changed  into  an  apparent  repulsion  (still  following  the 
same  law),  by  communicating  to  them  electrical  charges  of  similar  or  opposing  characters,  and  of  a  proper 
intensity.  It  thus  becomes,  at  least,  conceivable  how  the  stars  of  a  globular  cluster  may  have  their  mutual 
gravitation — their  tendency  to  collapse  and  produce  a  general  catastrophe — counteracted,  while  yet  each  might 
have  planets  revolving  within  its  own  sphere  of  attraction  (which  would  not  be  in  the  smallest  appreciable 
degree  affected  by  any  charge  permanently  resident  in  their  central  body,  provided  their  own  state  were  that  of 
neutrality).    It  will  of  course  be  understood  that  I  attach  no  importance  to  such  a  speculation  as  this  last. 


AND  THAT  OF  COMETS  IN  GENERAL. 


411 


even  to  the  extent  of  destroying  the  continuity  of  the  fluid,  and  separating  it  into  distinct 
masses.  Now,  if  the  conditions  of  such  an  extreme  case  can  ever  be  approached  at  all,  it  must 
be  in  that  of  a  comet  like  Biela's,  in  which  the  coercive  power  of  the  nucleus  is  reduced  in  the 
utmost  conceivable  degree ;  it  being  a  mere  vaporous  mass  devoid  of  all  cohesion  or  consistency, 
and  mixed  up,  and  probably  almost  coextensive  with  the  tail.  Its  return  to  the  perihelion  will 
be  watched  with  intense  interest. 

(388)  That  comets  undergo  a  change  of  some  kind  in  their  perihelion  passage,  was  a 
favorite  speculation  of  Sir  William  Herschel.  He  considered  this  change  to  consist  in  a  loss  of 
some  portion  of  their  more  elastic  matter  by  which  the  remainder  acquired  a  higher  degree  of 
consolidation.    Thus,  in  Phil.  Trans.  1812,  p.  141,  he  says,  "That,"  besides  light,  "many 

other  elastic  volatile  substances  may  escape  in  so  high  a  degree  of  rarefaction,  is  far 

from  improbable."  "  Then,  since  light  certainly,  and  very  likely  other  subtle  fluids,  also 

escape  in  great  abundance  during  a  considerable  time  before  and  after  a  comet's  nearest 
approach  to  the  sun,  I  look  upon  a  perihelion  passage  as  in  some  degree  an  act  of  consolidation." 
If  this  language  be  considered  (as  no  doubt  it  is),  somewhat  vague,  we  are  now  at  least  prepared 
to  assign  a  more  definite  meaning  to  it. 

(389)  The  preservation  of  the  geometrical  form  of  the  envelope  of  our  comet  (to  return  to 
Art.  371.),  is  undoubtedly  indicative  of  a  high  degree  of  tranquillity,  the  definite  action  of 
perfectly  regular  forces,  and  at  least  a  near  approach  to  a  state  of  equilibrium  in  the  strata  of 
which  the  mass  consists.  It  proves  also,  if  taken  in  conjunction  with  what  has  been  said 
respecting  its  apparent  dilatation,  similarity  of  external  and  internal  strata,  precisely  such  as  the 
laws  of  equilibrium  would  lead  us  to  expect  in  an  elastic  fluid  mass  subjected  to  such 
forces. 

(390)  The  rapid  disappearance  of  the  coma  would  seem  to  be  referable  neither  to  dis- 
sipation nor  absorption  into  the  head,  but  rather  to  its  being  swept  off  into  the  tail  by  the  sun's 
action,  and  there  deposited  as  part  thereof.  The  "wing"  of  the  26th,  and  the  "false  tail"  of  the 
27th  January  would  seem  to  have  been  the  matter  of  the  coma  thus  drifted  off.  To  trace  the 
complete  history  of  the  coma,  however,  it  would  be  necessary  to  have  before  us  observations  of 
its  appearance  in  the  months  of  December  and  the  early  part  of  January,  which  I  am  not  aware 
of  having  been  obtained. 

(391)  The  ray  or  tail  of  the  nucleus  is  also  a  highly  instructive  phenomenon.  As  the 
envelope  dilated  and  grew  fainter,  this,  on  the  contrary,  while  also  dilating  at  the  same  rate, 
grew  more  intense  up  to  the  1st  February,  after  which  time  it  faded,  while  the  nucleus  with  its 
coma  rapidly  increased  in  comparative  brightness.  It  seems  hardly  possible  not  to  recognize  in 
these  changes  the  effect  of  the  gradual  deposition  of  the  matter  of  the  envelope  ;  choosing 
the  line  of  its  axis  as  the  course  of  the  deposited  particles  in  their  progress  to  rejoin 
the  nucleus. 

(392)  Mention  is  made  in  Art.  358,  of  certain  artifices  employed  in  the  management  of  the 
equatorial,  to  ensure  exactness,  when  the  comet  was  growing  faint.  These  consisted  chiefly  in 
the  mode  of  using  the  thick  pair  of  wires  with  which  the  micrometer  was  furnished,  so  as  to  take 
advantage  of  their  visibility,  under  the  faintest  possible  illumination,  without  interfering  with  the 
exactness  of  observation,  so  far  as  the  stars  of  comparison  (not  unfrequently  themselves  faint 
objects)  were  concerned.    This  latter  condition,  it  was  found,  could  be  secured  by  placing  the 


412 


REMARKS  ON  ITS  PHYSICAL  CONSTITUTION, 


two  wires  side  by  side,  not  exactly  in  contact,  but  with  the  narrowest  possible  chink  or  interval 
between  thern.  Thus  disposed,  in  a  dark  field,  the  broad  space  covered  by  the  wires,  enabled 
them  to  be  seen  upon  the  comet,  as  if  they  formed  a  single  dark  line,  while,  on  the  other  hand, 
the  star,  after  disappearing  behind  the  first  wire,  would  be  seen  to  glimmer  for  a  moment  through 
the  chink  and  again  to  disappear  previous  to  its  final  emergence,  in  the  operation  for  determining 
the  difference  of  right  ascensions ;  and  the  momentary  glimpse  thus  obtained  of  it  between  the 
wires,  was  taken  as  the  instant  of  its  transit.  When  "oblique  transits"  are  to  be  taken,  the 
same  principle  is  equally  applicable,  and  I  can  recommend  it  as  very  serviceable  in  all  such 
cases. 

(393)  In  taking  differences  of  declination  between  the  comet  and  the  star  of  comparison, 
three  methods  were  followed:  1st,  The  wires  (A  B)  were  roughly  set  on  the  comet  and  star,  by 
passing  from  one  to  the  other  by  the  right  ascension  motion,  then  placing  the  instrument  in 
advance  of  both,  and  clamping  it,  the  first  in  order  of  R  A  was  bisected  by  the  wire  A,  and  the 
other  (on  its  coming  up)  by  B.  A  second  observation  was  then  similarly  made,  only  crossing 
the  wires,  and  using  B  to  bisect  the  first  in  order,  and  A  the  second,  and  so  on  alternately  ;  or, 
2ndly,  supposing  the  comet  to  pass  first,  the  wire  A  being  placed  at  zero,  was  exactly  covered  by 
B,  and  the  comet  bisected  by  them  as  by  a  single  wire,  by  the  declination  motion ;  then,  on  the 
star  coining  up,  B  was  opened  out  till  it  bisected  the  star.  This  method  could,  of  course,  not 
be  applied  when  the  star  preceded.  3rdly,  The  instrument  being  clamped,  so  as  to  allow  both 
objects  to  pass,  conveniently  situated,  through  the  field  of  view,  both  were,  in  succession, 
bisected  by  one  and  the  same  wire.  In  either  of  these  modes  of  using  the  micrometer,  the  zero 
correction  of  the  wires  is  eliminated,  but  the  latter  is  undoubtedly  preferable. 

(394)  In  identifying  the  star  compared,  a  conspicuous  zero  or  fiducial  star  was  always 
chosen,  as  near  its  place  as  possible,  to  be  compared  with  it  by  differences  of  R  A  and  N  P  D 
read  off  on  the  hour  and  declination  circles  of  the  instrument.  In  so  doing,  it  was  often  neces- 
sary, in  order  to  read  off  the  latter  circle,  to  shift  the  whole  instrument  through  several  hours 
of  right  ascension.  Either  owing  to  some  instability  in  the  support  of  the  polar  axis,  or  to  the 
effect  of  sand  blown  into  the  Y,  and  adhering  to  that  portion  of  the  axis  resting  on  it,  which 
seldom  came  into  use  (a  thing  impossible  to  avoid  in  consequence  of  the  nature  of  the  soil  and 
the  violent  and  searching  winds),  it  was  often  found  that  on  restoring  the  instrument  to  a  star 
after  reading  off,  the  bisection  of  the  latter  would  be  found  materially  deranged.  This  could 
always  be  prevented,  indeed,  by  several  times  swinging  the  instrument  to  and  fro  over  a  larger  arc 
in  R  A  previous  to  commencing,  and  by  very  gentle  handling  afterwards,  but  the  inconvenience 
was  entirely  done  away  with  as  a  cause  of  error  by  proceeding  as  follows.  The  star  first  to  be 
taken  was  brought  into  the  centre  of  the  field  and  bisected,  and  the  declination  circle  (being  of 
course  clamped)  was  read  off,  by  bringing  the  instrument  round  to  the  eye  in  R  A.  It  was  then 
restored  to  the  star,  which,  if  not  found  bisected,  was  now  rebisected  by  the  micrometer  screio  without 
altering  the  declination  circle.  The  instrument  was  then  transferred,  by  the  regular  application 
of  both  its  tangent  screws,  to  the  other  star,  which  was  bisected  by  the  same  wire,  but,  this  time, 
not  by  the  micrometer  screw,  but  by  the  declination  motion.  The  difference  of  declination  was 
now,  of  course,  secured  on  the  limb,  and  could  be  read  off  at  leisure,  without  regard  to  any  possible 
shift  of  bearing  in  the  act  of  bringing  it  into  a  situation  convenient  for  so  doing. 

(395)  I  will  take  this  opportunity  to  mention,  that  the  formulas  for  computing  the  corrections 


AND  THAT  OF  COMETS  IN  GENERAL. 


413 


for  parallax  and  refraction  (for  the  latitude  of  Feldhausen)  given  in  my  paper  above  cited, 
Mem.  Ast.  Soc.  x.  p.  326,  are  entirely  vitiated  by  typographical  errors.  The  correct  formula; 
are  as  follows  (a  being,  in  addition  to  the  notation  there  explained,  the  co-latitude):  — 

tan  n  =  tan  a  .  cos  h 

D  '  sin  p  '      y  ~      D  '     cos  n 

P,  =    _  ,d(/-,).sin  ^coS^.cos(2^-/t) 
xr      r/         sin  p  .  cos  (p  —  ny 

0'  =  +  $  .  (p'  —  p)  .  sec  (p  — 


5  v 


CHAPTER  VI. 
OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 

(395)  During  the  years  1835,  1836,  and  1837,  the  ring  of  Saturn,  and  the  orbits  of  its 
satellites  were  sufficiently  open  to  permit  the  accumulation  of  a  considerably  extensive  series  of 
their  angles  of  position  with  the  meridian,  or  with  the  longer  axis  of  the  ring  so  disposed  as  to 
be  available  towards  the  more  exact  determination  of  their  orbits ;  of  which  little  is  known  with 
exception  of  the  sixth,  which  is  the  largest  and  most  easily  observable,  and  whose  elements  and 
perturbations  have  been  made  the  subject  of  elaborate  investigation  by  Bessel.  I  consider, 
therefore,  that  the  observations  I  have  been  able  to  make  of  these  bodies,  though  confessedly 
imperfect,  owing  to  their  extreme  faintness  in  the  equatorial,  and  to  the  difficulty  of  obtaining 
any  measures  at  all  of  position  with  the  20-feet  reflector  out  of  the  meridian,  may  not  be  wholly 
without  interest  as  a  contribution  to  their  theory. 

(396)  All  the  measures  of  position,  whether  obtained  with  the  one  or  the  other  instrument, 
were  taken  with  reference  to  the  estimated  centre  of  the  body  of  the  planet.  In  the  equatorial, 
the  use  of  a  single  thin  thread  placed  across  the  satellite  and  the  estimated  centre  was  abandoned 
at  an  early  period  of  the  measurement,  and  the  far  preferable  method  of  placing  both  the 
satellite  and  the  whole  body  of  the  planet  between  the  two  thick  wires  opened,  so  as  rather  more 
than  to  include  the  latter,  adopted.  This  mode  of  observing,  which  is  excellently  well  adapted 
to  the  measurement  of  very  unequal  double  stars,  requires  some  little  practice  and  familiarity  to 
be  equally  satisfactory  on  the  satellites  of  Saturn.  Attention  must  be  directed  entirely  to  the 
globe  and  the  satellite,  studiously  disregarding  the  ring,  and  filling  up  by  imagination  the 
contour  of  the  globe  where  covered  by  the  ring.  This,  if  at  first  the  cause  of  some  hesitation 
and  uncertainty,  soon  becomes  familiar  ;  the  ring  ceasing  to  offer  any  disturbance  to  the  judg- 
ment, or  to  produce  any  bias  in  the  measurement.  The  position  of  the  wires  is  then  only  to  be 
judged  correct  when  a  perfect  symmetry  of  situation  of  the  globe  and  satellite  with  respect  to 
them  is  attained.  To  show  the  nature  and  extent  of  the  discordances  which  exist  in  the  mea- 
surement so  conducted,  I  subjoin,  as  specimens,  a  few  instances,  selected  impartially  from  the 
mass  on  record,  of  the  individual  measures  of  each  satellite  equatorially  measured. 


Satellite 

Date. 

Individual  measures,  including  zero. 

Mean. 

VII. 

o  / 
212  5 
240  55 

0  / 
212  50 
24I  20 

0  / 
211  50 

0  ' 

0  / 

0  / 
212  l6 

241  8 

OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


415 


VII. 
VI. 


IV. 


1837, 
1835, 

1836, 
1837. 

1835. 
1836, 
1837. 


1836, 


April  24 
May  27 
June  10 
March  6 
April  9 . 
May  21 
July  21 
April  27 
April  1 . 
April  7 . 
April  9  . 
May  21 
April  27 


Individual  measures,  including  zero. 


Mean. 


0 

0  / 

O 

0  / 

0 

/ 

O  / 

323 

30 

323  15 

323  23 

245 

30 

245  10 

245 

15 

244  45 

244  45 

245  5 

113 

33 

115  8 

113 

38 

113  48 

114 

18 

114  5 

IOI 

IS 

102  30 

IOI 

42 

101  15 

IOI 

35 

101  39 

103 

*3 

103  5 

103 

20 

102  55 

102 

5° 

103  5 

319 

10 

319  30 

317 

30 

318  10 

318 

'5 

318  31 

79  48 

78  28 

78 

13 

78  43 

78 

23 

78  43 

IOI 

25 

100  55 

100 

45 

IOI  2 

in 

27 

112  37 

in 

57 

1 12  0 

266 

0 

265  35 

266 

5 

265  55 

266 

5 

265  56 

77 

25 

77  25 

77 

15 

77  20 

77 

45 

77  26 

131 

5° 

129  40 

128 

35 

131  10 

130  19 

85 

5° 

84  30 

85  10 

(397)  Measures  of  the  fourth  satellite  could,  however,  very  rarely  be  procured  so  as  to  be 
in  any  degree  satisfactory  with  the  equatorial — of  the  third,  never.  The  former,  however,  was 
often  seen,  and  the  latter  also  occasionally,  though  rarely.  As  to  the  two  interior  satellites, 
it  is  needless  to  state  that  no  glimpse  of  either  of  them  was  ever  obtained  with  this 
instrument. 

(398)  In  the  nomenclature  above  used,  the  satellites  reckon  outwards  from  the  centre,  seven 
in  number  ;  but  as  this  practice  is  even  yet  not  become  general  among  astronomers,*  and  as  I 
have  found  the  equivoque  practically  annoying,  and  a  source  of  frequent  error  and  mistake,  I 
have  used  for  my  own  convenience,  and  shall  continue  to  do  so  in  what  follows,  a  mythological 
nomenclature,  which,  however,  I  do  not  presume  to  recommend  to  the  adoption  of  others,  though 
I  am  persuaded  that  some  nomenclature  other  than  the  equivocal  one  in  actual  use,  will  be 
found  necessary  by  all  who  observe  these  bodies.  The  names  I  have  selected  are  as  follows  :f 
viz.,  for 


The  exterior  satellite,  discovered  by  Cassini 

The  bright  satellite,  discovered  by  Huyghens 

The  exterior  of  the  three  satellites,  discovered  by  Cassini 

The  intermediate  of  these  three,  discovered  by  Cassini 

The  interior  of  them,  discovered  by  Cassini 

The  exterior  of  the  two,  discovered  by  Sir  W.  Herschel 

The  interior  and  smallest  of  all  


Iapetus. 

Titan. 

Rhea. 

Dione. 

Tethys. 

Enceladus. 

Mimas. 


*  See  Dr.  Lamont's  paper  and  tables  of  the  "sixth"  satellite  (Astronom.  Nachr.  No.  316),  meaning  the 
second. 

t  As  Saturn  devoured  his  children,  his  family  could  not  be  assembled  round  him,  so  that  the  choice  lay 
among  his  brothers  and  sisters,  the  Titans  and  Titanesses  {vide  Lempriere).  The  name  Iapetus  seemed 
indicated  by  the  obscurity  and  remoteness  of  the  exterior  satellite,  Titan  by  the  superior  size  of  the  Huygenian, 
while  the  three  female  appellatives  class  together  the  three  intermediate  Cassinian  satellites.  The  minute 
interior  ones  seemed  appropriately  characterized  by  a  return  to  male  appellatives,  chosen  from  a  younger  and 
inferior  (though  still  superhuman)  brood.  Should  an  eighth  satellite  exist,  the  confusion  of  the  old  nomen- 
clature will  become  quite  intolerable.  I  am  not  aware  that  a  distant  satellite  of  Jupiter  (analogous  to  Iapetus 
and  our  moon)  has  ever  been  looked  for.    Would  it  not  be  worth  a  search  ? 


416 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


(399)  It  was  not  until  Feb.  28,  1837,  that  the  single  position  wire  of  the  20-feet  micrometer 
was  exchanged  for  a  double  one,  composed  of  two  pretty  thick  glass  threads  (the  perfect 
straightness  of  which  can  always  be  depended  on  if  kept  in  a  state  of  tension  in  a  vertical  position 
while  cooling  from  fusion),  well  smoked  to  render  them  opaque  and  non-reflective.  Until  that 
date  (that  is  to  say,  during  all  the  series  of  measures  recorded  for  1835  and  1836  with  the 
reflector),  the  positions  taken  with  it  are  open  to  all  the  objections  against  the  use  of  a  single 
thread  for  this  especial  purpose.  The  positions  in  these  years  are,  moreover,  liable  to  an 
additional  source  of  uncertainty,  which  has,  no  doubt,  vitiated  them  materially — the  difficulty, 
indeed,  almost  impossibility,  of  well  adjusting  the  fixed  wire  to  the  parallel  out  of  the  meridian 
with  an  instrument  suspended  after  the  manner  of  the  20-feet  reflector.  This  difficulty  did  not 
fail  to  make  itself  felt  in  the  first  attempt  to  take  measures  of  the  satellites.  It  was  endeavoured 
to  be  overcome  by  adjusting  the  fixed  wire  to  the  line  of  Ansae,  and,  in  one  instance,  to  the 
position  of  the  great  satellite  (Observation  of  June  2,  1836).  But  the  mode  of  doing  this  was 
not  well  considered.  The  wire  once  so  adjusted  was  left  unaltered  during  the  whole  of  a  set 
of  measures  (lasting,  it  is  true,  not  many  minutes),  which,  of  course,  inflicts  a  permanent  error  on 
each  reading  off.  For  these  reasons,  I  place  but  little  reliance  on  the  20-feet  measures  of  the 
two  first  years  in  question. 

(400)  On  the  28th  of  April  1837,  however  (the  first  occasion  of  using  this  instrument  on 
Saturn  after  the  change  of  wires),  a  mode  of  observation  was  adopted  free  from  all  objection 
of  this  kind.  The  line  of  Ansae  was  chosen  as  a  fiducial  line,  for  which  the  moderate  opening  of 
the  ring  in  that  year  did  not  yet  unfit  it,  whatever  it  might  have  done  a  year  or  two  later  (in 
which  case  the  great  satellite  must  have  been  resorted  to  as  a  fiducial  object,  and  its  position 
otherwise  determined).  The  zero,  or  single  wire,  was,  however,  not  adjusted  to  the  "apparent  line 
of  Ansae,  nor,  indeed,  adjusted  at  all,  but  set  at  random,  or,  rather,  so  as  to  be  most  out  of  the 
way  of  the  measures  to  be  taken.  The  positions  of  the  line  of  Ansae,  and  of  whichever  satel- 
lite was  under  measurement,  were  then  alternately  taken  between  the  double  wires,  and  read 
off,  beginning  and  ending  in  each  set  of  measures  with  the  Ansa.  Means  then  being  taken  of  the 
readings,  not  the  angle  of  position  of  the  satellite,  but  the  difference  of  its  position  and  that  of 
the  Ansae  was  obtained ;  and  as  the  situation  of  the  Ansae  is  given  to  great  accuracy  in  both  the 
Nautical  Almanac  and  the  Berlin  Ephemeris,  it  is  easy  thence  to  derive  the  true  position  of  the 
satellite.  In  setting  the  moveable  wires  to  the  line  of  Ansae,  exactly  the  same  mode  of  pro- 
ceeding was  adopted  as  in  the  case  of  a  double  star,  only  that  in  this  case  the  body  of  the  planet 
was  disregarded,  and  the  whole  attention  directed  to  the  ellipse  of  the  ring,  so  as  to  place  it 
symmetrically  between  the  thick  wires.  The  following  specimen  of  a  series  of  observations 
executed  in  this  way  on  May  4,  1837,  will  serve  to  explain  the  details  of  the  procedure.  A 
night  of  observation  is  purposely  chosen,  in  which  Enceladus  was  well  seen  and  measured,  and 
in  which  Tethys  was  observed  through  its  inferior  conjunction,  without  the  least  hinderance  from 
its  extreme  apparent  proximity  to  the  ring  and  body  of  the  planet. 


S.  T. 

Ansee  or 
Satellite. 

Microm. 
reading. 

S.  T. 

Ansae  or 
Satellite. 

Microm. 
reading. 

S.  T. 

Ansa?  or 
Satellite. 

Mieiom. 
reading:. 

h.  in. 
13  42 

13  45 

Ansae  .... 
Tethys    . . 
Ansae  .... 

0  d- 

59  5 
12 1.7 

65.4 

1 

fa.  m. 
13  47 

J3  49 

Ansae  .... 
Tethys    . . 
Ansae  .... 
Tethys  .. 

0  d. 

70.0 
127.2 

67.8 
133.0 

h.  m. 

»3  53 
13  55 

Ansae  .... 
Tethys  .. 
Ansae  .... 
Tethys    .  . 

0  d. 

72.1 
129.0 

6S.9 
137.O 

1  1 

OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


417 


S.  T. 


h.  m. 
13  57 


H  7 

1+  9 

14  11 

14.  12 

14  14 


14  14 

14  15 

14  17 

14  18 


14  20 
14  22 


Ansse  or 
Satellite. 


Tethys 
Ansae  . . 


Ansae  . . 
Titan  . . 
Ansae  . . 
Titan  . . 
Ansae  . . 
Titan  . . 
Ansae  . . 
Titan  . . 
Ansae  . . 


Ansa? 
Rhea 
Ansae 
Rhea 
Ansae 
Rhea 
Ansae 


Ansae  . 
Dione . 
Ansae  . 
Dione . 


Microm. 
reading. 


o  d. 

137-5 
70.3 


76.1 
278.8 

79.0 
278.4 

80.3 
279.0 

78.5 
278.2 

79-5 


79-5 
252.5 

78.6 
249.5 

78.0 
25 1.0 

78.4 


85.1 
56.5 
89.1 
57.0 


1  0 

I  ON 

d 

Pi  cn 


Interrupted  the  measures  to  note 
(Enceladus)  which  is  perfectly  dis- 
tinct, and  equal  to  a  star  15.16m. 
From  its  situation  I  can  hardly 
have  a  doubt  of  its  being  a  satellite. 
It  is  beautifully  defined.  Yet,  N.B. 
there  is  a  great  number  of  stars 
about  this  part  of  the  sky.  Sent 
for  *  *  *  who  after  a  few  trials 
saw  it  well.  Put  on  a  field-bar 
eye-piece.  Perfectly  well  seen  by 
both  of  us.  Its  distance  from  the 
ring's  edge  is  i£  its  breadth. 


S.  T. 


li.  m. 

14  48 

14  49 

14  51 

14  52 


Ansse  or 
Satellite. 


Ansae  . 
Dione. 
Ansae  . 
Dione . 
Ansae  . 
Dione . 
Ansae  . 


14    52    Ansae  ....     102. 1 
Iapetus  ?  84.2 
Ansae  ....  101.0 
Iapetus  ?  95.4 
Ansae  ....  103.0 
[The  first  of  the  objects  here  taken 
proved  to  be  the  true  satellite,  the 
other  a  star.] 


Microm. 
reading. 


o  d. 
104.0 

71.0 
103.7 

69.2 
102.8 

71.0 
102. 1 


14  55  (Enceladus)  is  now  fully  as 
far  from  the  edge  of  the  Ansae  as  that 
edge  is  from  the  limb  of  the  planet. 
When  first  seen  it  was  somewhat 
south  of  the  line  of  Ansae.  It  is 
now  just  on  the  axis.  Never  was 
anything  more  perfect  than  the  de- 
finition of  Saturn  to-night. 


'5 

3 

Ansae  .... 

108.5 

Tethys  .. 

188.0 

15 

4 

Ansae  .... 

1 12.0 

Tethys   . . 

185.4 

15 

6 

Ansae  .... 

109.4 

Tethys  ... 

187.2 

15 

8 

Ansae  .... 

109.5 

I 

Perfectly  satisfactory  measures  of 
Tethys  in  or  very  near  its  inferior 
conjunction.  Quite  easy,  though 
very  close  to  the  edge  of  the  ring. 


S.  T. 


1).  m. 
15  14 


15  17 


lS  34 


15  35 


15  37 


41 


Ansa;  or 
Satellite. 


Ansae 
Enceladus 
Enceladu; 
Enceladu 
Ansae  . . . 


Ansae  .. 
Tethys 
Ansae  ., 
Tethys 
Ansae  . 
Tethys 
Ansae  . , 


Microm. 
reading. 


o  d. 
1 14.2 

298.2 

295-3 
297.3 

1 16.0 


124.8 
218.8 
127.2 
219.6 
127.0 
222.4 
125.4 
in  all  sorts  of 
12  inches  aper- 


;    4 1  )  Examined 
;    56  S  ways. 

ture  and  power  240  suits  it  best. 
At  16  h.  3  m.  S.  T.,  Enceladus  is 
somewhat  nearer  to  Saturn,  and 
very  decidedly  north  of  the  axis  of 
the  ring  Ellipse. 


16 


16  22 


16 


16 


24 
28 


Ansae 

Enceladus 

Ansae 

Enceladus 

Ansae 


Ansae  . , 
Tethys 
Ansae  . 
Tethys 
Ansae  . 


143.0 
3*5-8 
142.8 
326.2 
142.0 


Hi-5 
260.0 
142.8 
262.4 
142.6 


15 


Ansae 

Enceladus 

Ansae 


109.0 
290.9 
108.5 


Perfectly    sharp  distinct 
Shifted  micrometer. 


16  41  Left  off  having  first  seen  En- 
celadus still  nearly  at  the  same 
distance,  or,  if  any  thing,  a  very  little 
nearer,  but  decidedly  advanced  in 
position  in  its  orbit.  By  this  time 
the  planet,  were  it  a  star,  must 
have  occulted  it,  as  the  motion  was 
full  upon  it  at  the  rate  of  nearly  a 
semidiameter  of  the  globe  of  Saturn 
per  hour  in  right  ascension. 


(401)  The  following  table  exhibits  a  synopsis  of  all  the  measured  (and  some  of  the 
estimated)  positions  of  the  satellites  as  taken  with  both  the  equatorial  and  the  reflector  during 
the  three  years  in  question.  No  correction  for  Bias  (See  Art.  168),  has  been  applied  to  the 
measures  taken  with  the  latter  instrument,  it  being  by  no  means  clear  that  any  such  correction 
is  needed  in  the  mode  of  observing  finally  adopted,  and  in  the  earlier  measures ;  it  being  quite 
uncertain  whether  it  can  be  applied  correctly.  It  will,  of  course,  be  understood  that  the 
estimated  positions  have  no  further  use  than  to  determine  whether  the  object  seen  was  or 
was  not  a  satellite,  and  which.  The  list  of  measures,  as  originally  drawn  out  from  the 
registered  observations  was  considerably  more  extensive,  but  has  been  reduced  by  striking 
out  numerous  observations  of  stars  taken  at  the  time  for  satellites,  or  at  least  possibly  such 
(especially  for  Iapetus),  but  since  ascertained  not  to  have  been  so. 

(402)  In  this  table,  the  first  column  contains  the  date  of  the  observation;  the  second 
indicates,  by  the  letter  E  or  R,  whether  the  equatorial  or  the  reflector  was  used ;  column  3 
contains  the  name  of  the  satellite  observed  ;  column  4,  the  estimated  magnitude ;  column  5,  the 

5  o 


418 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


mean  time  at  Feldhausen ;  column  6,  its  angle  of  position  finally  resulting  from  the  means  of 
the  measures  (to  which  the  mean  time  always  corresponds),  being  the  due  application  of  zeros 
in  the  one  instrument,  and  the  appropriate  modes  of  treatment  in  the  other ;  lastly,  column  7 
contains  the  number  of  observations  on  the  mean,  of  which  the  results  in  column  6  relies ;  the 
letter  d  in  this  column  indicates  that  the  position  in  column  6  is  not  the  result  of  a  micrometrical 
measure,  but  of  the  configuration  as  laid  down  in  a  diagram  made  at  that  time,  and  liable 
therefore  to  very  great  errors. 


SYNOPSIS  OF  THE  OBSERVED  ANGLES  OF  POSITION  OF  THE  SATELLITES  OF  SATURN. 


Date. 

Inst. 

Satellite. 

Mag. 

M.  T. 

Position. 

Xo. 

Date. 

Inst. 

Satellite. 

Mag. 

M.  T. 

Position. 

No. 

183S 

h. 

m. 

0 

1 

1835 

Rhea  

h. 

m. 

0 

/ 

May  18 

£ 

lapetus  .  . 

1 1 

10 

?2 

8; 

0  3 

33 

1 

7 

jj 

211 

4.8 

4 

Titan  

9' 

10 

46 

i  J" 

t  r 
*5 

5 

8 

A  A 
TT 

225 

•7  A 
T 

3 

12 

O 

344 

3 

Dione    . . 

7 

/ 

1% 

y° 

^S/ 

?  A 
Z  + 

3 

Dione .... 

12 

2  I 

33 

2 

Tethys  .. 

7 

1A. 

263 

JU 

1 

E 

lapetus  . . 

11 

1 1 

2  1 
j 

87 

-+- 

d 

Enceladus 

8 

c 
j 

87 

Titan  

9 

j  j 

0 1 

.  / 

60 

49 

5 

June  25 

R 

lapetus  . . 

7 

CA 

j^r 

6 

42 

1 

Rhea  

9' 

1 1 

1 1 
6  5 

88 

23 

3 

Titan  

g 

I 

07 

42 

3 

20 

E 

lapetus  .. 

9 

7 

91 

A  fi 

4» 

2 

Rhea  

g 

5 

5 

Titan  

9 

8 

75 

44 

5 

Tethys  .. 

g 

Vi 

J 1 

271 

4a 

6 

23 

E 

lapetus  . . 

1 1 

9 

42 

93 

55 

2 

26 

R 

lapetus  . . 

7 

53 

l8 

1 

Titan  .... 

8' 

9 

93 

2 

6 

Titan  

7 

49 

116 

° 

3 

Rhea  .... 

1 1 

9 

28 

7° 

7 

5 

Rhea  

7 

24 

2 

24 

E 

lapetus  . . 

8 

95 
98 

_l_ 

d 

Dione    . . 

) 

Titan  

8 

9 

46 

2 

5 

+ 

{ 

7 

5° 

97 

0 

2 

Rhea  .... 

10 

10 

4. 

Q2 
J 

10 

5 

Tethvs  .. 

s 

25 

E 

lapetus  . . 

8 

40: 

IOO 

d 

27 

E 

Titan  

8 

55 

196 

4 

6 

Titan  

8' 

8 

42 

I  I  I 

33 

5 

Rhea  

9 

4 

275 

5° 

2 

Rhea  .... 

8 

49 

240 

± 

d 

July  13 

E 

Titan  

7 

43 

'97 

10 

5 

27 

E 

Titan  

9 

47 

245 

5 

5 

J5 

E 

lapetus  . . 

1 1 

6 

44 

290 

20 

1 

29 

E 

Titan  

8 

9 

9 

263 

17 

5 

Titan  

9 

6 

17 

257 

47 

5 

31 

E 

Titan  

8' 

7 

33 

270 

36 

5 

Rhea  .... 

12 

6 

40 

274 

45 

2 

June  1 

E 

Titan  

8' 

8 

26 

276 

23 

5 

Dione 

6 

44 

93 

-1- 

d 

4 

E 

Titan  

10 

8 

62 

10 

4 

21 

E 

lapetus  . . 

10 

7 

6 

302 

48 

3 

5 

E 

Titan  

10 

1 1 

77 

1 1 

5 

Titan  

10 

6 

53 

344 

3 

12 

6 

E 

Titan  

8' 

9 

17 

84 

0 

6 

Rhea  

10' 

6 

5i 

78 

43 

5 

Rhea  .... 

io' 

38 

86 

9 

2 

4 

7 

E 

Titan  

7 

25 

87 

5° 

5 

1836 

8 

E 

Titan  

8 

7 

22 

92 

7 

5 

Jan.  10 

E 

Titan  

10 

15 

36 

278 

4 

5 

9 

E 

Titan  

8' 

9 

35 

98 

58 

5 

Feb.  1 

E 

Titan  

9' 

15 

14 

85 

8 

3 

10 

E 

Titan  

9 

8 

58 

114 

55 

10 

4 

E 

Titan  .... 

15 

39 

112 

*5 

5 

12 

E 

Titan  

9 

5 

56 

244 

27 

6 

5 

E 

Titan  

14 

49 

138 

38 

3 

E 

lapetus  . . 

1 1 

10 

9 

156 

45 

1 

9 

E 

Titan  

9 

16 

6 

265 

J3 

5 

Titan  

10 

10 

2 

268 

28 

3 

Rhea  .... 

11 

16 

24 

74 

52 

2 

Rhea  

9 

9 

57 

85 

5 

4 

Mar.  6 

E 

Titan  

15 

1 1 

IOI 

39 

5 

16 

E 

lapetus  . . 

11 

9 

52 

172 

45 

1 

.  27 

E 

Titan  

12 

41 

257 

5i 

5 

Titan 

9' 

9 

41 

272 

28 

3 

April  7 

E 

lapetus  .. 

12 

'3 

31 

98 

20 

2 

Dione 

»3 

10 

± 

268 

± 

d 

Titan  

12 

13 

25 

IOI 

3i 

5 

E 

lapetus  . . 

12 

8 

9 

189 

40 

1 

14 

E 

Titan  

9 
8' 

1 1 

16 

271 

36 

2 

Titan 

8' 

7 

44 

277 

17 

5 

21 

E 

Titan  

13 

12 

87 

30 

2 

Rhea  

10' 

7 

5° 

260 

5 

4 

2  5 

E 

lapetus  . . 

9 

13 

23 

124 

10 

2 

18 

E 

lapetus  .. 

7 

7 

212 

15 

3 

Titan  

13 

15 

159 

17 

8 

Titan  

9 

19 

289 

6 

13 

26 

E 

lapetus  . . 

10' 

12 

5i 

126 

10 

1 

Rhea 

8 

24 

276 

45 

7 

Titan  

8' 

12 

!9 

225 

31 

5 

19 

E 

lapetus  . . 

12 

6 

26 

228 

20 

2 

Rhea  

10 

12 

40 

78 

23 

3 

Titan  

10 

7 

26 

337 

5^ 

1 1 

27 

E 

lapetus  .. 

11' 

12 

28 

130 

5° 

2 

11 

2 

356 

20 

8 

Titan  

8' 

12 

1 1 

250 

45 

4 

Rhea  . .  . 

1 1 

9 

33 

70 

56 

5 

Rhea  

10' 

12 

16 

IOI 

2 

3 

20 

E 

lapetus  . 

12 

8 

58 

241 

8 

1 

Dione    . . 

12 

12 

26 

85 

10 

2 

Titan  . .  . 

9' 

8 

5° 

62 

0 

5 

May  3 

E 

lapetus  . . 

11' 

>3 

6 

206 

8 

2 

R 

Rhea  . .  . 

10 

8 

56 

90 

47 

3 

Titan  

9 

13 

0 

326 

24 

4 

21 

lapetus  . 

7 

36 

251 

18 

2 

Rhea 

11 

13 

4 

264 

18 

2 

Titan  . . . 

7 

42 

81 

36 

1 

12 

R 

Titan  

9' 

,0 

28 

222 

48 

1 

OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN.  419 


Date. 

Inst. 

Satellite. 


Mag. 

M.  T. 

Position. 

No. 

Date. 

Inst. 

satellite. 

Mag 

M.  T. 

Position. 

No. 

1836 

h. 

m. 

0 



1837 

h. 

m. 

0 

Rhea  .... 

10' 

10 

29 

260 

18 

I 

April  7 

E 

Titan  

9 

J4 

8 

86 

17 

5 

Dione 

1 1 

10 

30 

259 

18 

I 

Rhea  .... 

1 1 

'4 

16 

265 

56 

5 

Tethys  .. 

1 1 

10 

40 

105 

12 

I 

Dione 

12 

'4 

22 

92 

15 

1 

Enceladus 

15 

10 

41 

81 

18 

I 

Tethys   . . 

13 
9' 

'4 

22 

92 

15  : 

1 

May  13 

R 

Titan  

10 

-1- 

252 

-+- 

d 

8 

E 

Titan  

12 

J3 

93 

58 

5 

Rhea  

10 

± 

291 

-+- 

d 

Rhea  

12 

12 

30 

3°5 

53 

2 

Dione 

10 

■+• 

3.5 

-+- 

d 

9 

E 

Titan  .... 

8' 

'4 

5 

103 

5 

5 

Tethys   .  . 

10 

■+- 

296 

■+- 

d 

Rhea  

10' 

'4 

12 

77 

26 

5 

*9 

E 

Iapetus  . . 

9 

56 

279 

28 

2 

Tethys   . . 

'3 

'4 

28 

100 

25  : 

1 

Titan  

1 1 

9 

49 

322 

42 

5 

10 

E 

Titan  .... 

9 

12 

26 

116 

20 

5 

22 

E 

Iapetus  . . 

10' 

10 

5a 

282 

5 

2 

Rhea  

1 1 

12 

37 

108 

28 

5 

Titan  

9, 

10 

32 

80 

37 

5 

1 1 

E 

Titan  

8' 

13 

55 

144 

1 5 

5 

24 

E 

Iapetus  . . 

10' 

10 

20 

285 

5° 

1 

Rhea  

11 

'4 

7 

241 

37 

3 

Titan  .... 

9, 
10 

10 

9 

95 

0 

3 

12 

E 

Iapetus  . . 

10' 

*4 

10 

289 

26 

4 

Rhea  

9 

52 

97 

55 

3 

Titan  

9 

J3 

53 

200 

27 

6 

Tethys   . . 

10 

40 

270 

+ 

d 

Rhea  

12 

J4 

5 

275 

35 

2 

June  1 

R 

Titan  

9 

5° 

270 

56 

1 

13 

E 

Iapetus  . . 

15 

10 

290 

0 

1 

Rhea  

9 

32 

68 

5° 

2 

Titan  

'4 

5° 

238 

22 

5 

Dione 

9 

48 

325 

44 

3 

14 

E 

Titan  

9 

10' 

r3 

28 

255 

53 

5 

Tethys   . . 

9 

30 

316 

26 

1 

Rhea  

!3 

26 

92 

10 

3 

Enceladus 

9 

42 

268 

26 

2 

15 

E 

Iapetus  . . 

10' 

12 

37 

294 

I  c 

J 

2 

2 

R 

Rhea  

8 

42 

84 

39 

2 

Titan  

9' 

1 1 

26 

264. 

22 

5 

Dione 

8 

42 

85 

± 

20 

E 

Titan  

12 

18 

12 

4.7 

7 

Tethys  .. 

8 

37 

152 

27 

3 

Rhea  

12 

32 

214 

10  ; 

1 

3 

R 

Titan  

1 1 

6 

289 

37 

1 

24 

E 

Iapetus  . . 

10' 

14 

16 

111 
j  j 

27 
J 

2 

Rhea  

10 

8 

221 

29 

1 

Titan  

9 

14 

6 

0  ? 

1 1 
j  J 

2 

Dione 

10 

10 

262 

35 

1 

27 

E 

Iapetus  .. 

12' 

13 

57 

jj) 

r 

? 

2 

Tethys  .. 

9 

39 

14 

32 

1 

Titan  

9' 
1 1' 

1 3 

37 

14.8 

6 

5 

10 

36 

42 

2 

1 

Rhea  

1 3 

5 1 

11 

1  J 

<;6 

5 

11 

0 

56 

50 

1 

28 

R 

Iapetus  . . 

12 

7.7 

6 

18 

5 

Enceladus 

11 

0 

85 

8 

1 

Titan  

1 1 

57 

196 

20 

16 

Mimas   . . 

9 

50 

85 

+ 

Rhea  

12 

12 

IOC 

j 

2, 

4 

8 

R 

Iapetus  . . 

11 

34 

325 

1 1 

1 

Dione 

12 

9 

299 

49 

8 

Titan  

1 1 

•JO 

j 

88 

CO 

1 

Tethys  .. 

12 

2.Q 
J 

06 

^  *7 

*/ 

2 

Rhea  

1 1 

27 

26 1 

C 

J 

28 

E 

Iapetus  . . 

1 1 

1 7 

Z  7 

I O 

27 

3 

Dione 

1 1 

24 

2T1 

j  j 

5Q 

1 

Titan  

9 

11 

4.7 

2o6 

i  / 

3 

Tethys 

1 1 

27 

266 

2Q 

y 

Rhea  

10 

11 

j 

c  1 

I07 

3 

11 

R 

Iapetus  . . 

10 

36 

7 

20  : 
j 

1 

Tethys  .. 

12 

13 

S.2 

07 

y  1 

± 

d 

Titan  .... 

10 

30 

II5 

47  : 

1 

29 

R 

Iapetus  . . 

12 

20 

2 1 

4 

Rhea  

10 

1 1 

02 

7 

2*2  : 

1 

Titan  .... 

14. 

CJ. 
j<r 

242 

27 

4 

Dione 

10 

1& 

JT 

2  c6 

; 

1 1  : 

1 

Rhea  

12 

16 

237 

C7 

7 

E 

Tethys  .. 

10 

32 
J 

8q 

Co  * 

jy  • 

1 

Dione 

12 

6 

93 

J3 

5 

27 

Titan  

7 

47 

117 

10 

y 

Tethys  .. 

12 

Q 

282 

1 

6 

July  12 

R 

Rhea  

7 

S3 

272 

55 

1 

29 

E 

Iapetus  . . 

13 

54 

27 

5 

2 

Iapetus  . . 

12 

7 

48 

120 

22 

1 

Titan  

!3 

48 

240 

3 

3 

Titan  

9 

7 

32 

100 

22 

2 

Rhea  

r3 

52 

242 

35 

2 

Rhea  

11 

7 

35 

80 

22 

2 

30 

R 

Iapetus  . . 

1 1 

24 

35 

49 

4 

Dione 

J3 

7 

37 

296 

1 

2 

Titan  

10 

8 

256 

21 

3 

R 

x  cinys    .  . 

J3 

7 

39 

257 

58 

3 

1  >  1  

i\  lit  a  .... 

1 1 

15 

277 

42 

3 

Iapetus  . . 

6 

32 

131 

3 

1 

Dione 

12 

39 

254 

56 

4 

Titan  .... 

6 

34 

167 

39 

4 

Tethys  .. 

12 

3i 

104 

0 

3 

Rhea  .... 

6 

23 

244 

3 

2 

May  1 

E 

Iapetus  . . 

1 1 

13 

5° 

5i 

55 

3 

Dione 

6 

30 

256 

57 

1 

Titan  

8' 

r3 

44 

265 

20 

4 

Aug.  11 

E 

Tethys  .. 
Titan  

9 

6 
6 

31 

26 

265 
88 

*5 

!3 

1 

3 

3 

E 

Rhea  

Iapetus  . . 

*3 
12 

5° 
20 

20 
69 

± 

5 

d 
1 

Rhea  .... 

12 

6 

34 

274 

15 

1 

R 

Titan  

Iapetus  . . 

12 

14 

280 

36 

4 

1837 

4 

12 

2 

73 

5 

1 

Titan  

Titan  

1 1 

21 

290 

5° 

4 

Mar.  12 

E 

12 

5° 

232 

46 

5 

Rhea  

1 1 

26 

263 

18 

3 

Rhea  

«3 

1 

324 

5 

1 

Dione 

1 1 

46 

59 

21 

5 

E 

Dione 

!3 

0 

272 

d 

Tethys  .. 

11 

2 

'53 

5° 

5 

*3 

Titan  

15 

1 

253 

*9 

5 

12 

16 

167 

56 

3 

26 

Rhea  

15 

9 

83 

48 

2 

12 

45 

,8S 

r5"> 

3 

£ 

E 

Titan  

J3 

4 

137 

36 

5 

13 

35 

209 

49 

28 

E 

Titan  

!4 

21 

236 

53 

10 

Enceladus 

12 

33 

273 

15 

6 

April  1 

E 

Titan  

8' 

'4 

5 

280 

37 

5 

5 

R 

Iapetus  . . 

12 

26 

75 

17 

1 

Rhea  .... 

1 1 

14 

16 

1 12 

0 

3 

Titan  

1 1 

54 

317 

58 

4 

420 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


Date. 

lust. 

Satellite. 

Mag. 

If.  T. 

Position. 

No. 

Date. 

Inst. 

Satellite. 

Mag. 

M.  T. 

Position. 

No. 

i8-?7 

w  j  / 

h 

0 

1837 

Ii 

0 

Rhea  .... 

206 

6 

May  21 

E 

Titan  

8 

3s 

318 

31 

5 

Dione 

42 

118 

4> 

7 

Rhea  

12 

10 

53 

130 

>9 

4 

Tethys  .. 

7 

343 

a8 
40 

3 

June  5 

R 

lapetus  . . 

J4 

I»5 

52 

I 

19 

37 

2 

Titan  .... 

9 

42 

293 

2 

3 

May  6 

R 

lapetus  . . 

12 

17 

80 

8 

3 

Rhea  .... 

9 

49 

27O 

30 

2 

Titan  

I  I 

46 

17 

32 

6 

Dione 

12 

9 

53 

27  I 

4.2 

2 

Rhea  .... 

I  I 

'9 

71 

57 

4 

Tethys  .. 

12 

10 

0 

113 

56 

3 

Dione 

12 

1 

281 

47 

5 

6 

R 

lapetus  . . 

9 

21 

205 

48 

5 

Tethys  .. 

I  I 

56 

219 

5 

7 

Titan  

9 

1 

319 

13 

4 

Enceladus 

1 1 

47 

83 

45 

4 

Rhea  

9 

3 

327 

48 

4 

12 

59 

87 

22  : 

3 

Dione 

9 

10 

68 

5 

5 

7 

R 

lapetus  .. 

12 

1 

82 

56 

2 

Tethys  .. 

9 

23 

306 

47 

6 

Titan  

I  I 

36 
8 

60 

1 1 

3 

Enceladus 

10 

28 

276 

3 

7 

Rhea  .... 

12 

102 

5 

3 

24 

E 

Titan  

9 

42 

63 

15 

5 

Dione 

1 1 

56 

81 

15 

3 

25 

R 

lapetus  . . 

10 

10 

44 

284 

10 

2 

Tethys  .. 

12 

6 

57 

9 

7 

Titan  

9' 

10 

39 

80 

0 

2 

S 

R 

lapetus  . . 

12 

87 

25 

1 

Rhea  .... 

12 

10 

33 

82 

9 

3 

Titan  

I  I 

33 

70 

± 

d 

Dione    . . 

13 

10 

3 

51 

4 

6 

Rhea  

I  I 

43 

232 

1 1 

3 

Tethys  .. 

*4 

9 

47 

343 

12 

3 

Dione 

I  I 

48 

225 

1 

4 

10 

26 

2 

*9 

2 

Tethys  .. 

II 

48 

251 

3 

4 

Enceladus 

15 

10 

*3 

261 

55 

2 

Enceladus 

12 

1 1 

263 

3 

3 

28 

R 

lapetus  . . 

9 

28 

82 

5i 

2 

9 

R 

lapetus  . . 

*3 

21 

88 

59 

3 

Titan  

9 

24 

87 

29 

2 

Titan  

I  I 

3 

85 

13 

3 

Rhea  

9 

140 

52 

3 

Rhea  

1 1 

12 

274 

32 

3 

Dione 

9 

17 

57 

56 

4 

Dione 

»3 

9 

3°9 

15 

2 

Tethys  .. 

9 

6 

"5 

29 

4 

Tethys  .. 

i3 

14 

78 

5° 

2 

29 

R 

Titan  

9 

56 

97 

0 

2 

Enceladus 

13 

34 

119 

8 

2 

Rhea  .... 

9 

5i 

262 

35 

2 

(403)  To  render  these  observations  available  for  the  purpose  of  affording-  epochs  by  which 
to  correct  the  received  periodic  times,  and  obtaining  a  knowledge  of  the  ellij>ticities  of  the 
orbits  (so  far  as  they  may  be  adequate  to  that  purpose),  it  will  be  necessary  to  convert  the 
observed  angles  of  position  into  Saturnicentric  longitudes,  for  which  the  following  formulae  and 
elements  are  used,  the  Ascending  node  of  the  ring  being  the  zero  point  of  longitude. 

tan  <p  =  sin  I  .  tan  (0  —  p) ;  v  =  <p  +  X  ;  (A) 

The  Berlin  Ephemeris  contains  the  values  of  p,  I,  and  A  (there  called  u'),  for  intervals  of  forty 
days,  as  also  of  a,  the  major  axis  of  the  ring-ellipse ;  p  representing  the  angle  of  position  of  the 
northern  semi-minor  axis  of  the  ring,  I  the  angle  of  elevation  of  the  earth  (northwards)  above  the 
plane  of  the  ring,  and  A  the  Saturnicentric  longitude  of  the  earth,  reckoned  in  the  plane  of  the 
ring  from  the  ascending  node  of  the  ring  on  the  ecliptic.  These  elements  are  interpolated 
(graphically  by  interpolating  curves),  for  the  days  of  observation,  in  the  following  table,  where 
also  are  added  the  values  of  r,  the  time  occupied  by  light  in  its  passage  from  the  planet  to  the 
earth. 


Date. 

P 

I 

\ 

a 

T 

Date. 

P 

\ 

a 

T 

+ 

+ 

1835 

0  / 

0  / 

n 

m. 

1835 

0  / 

0 

m. 

May  18 

2  23 

11  20 

208  8 

42.85 

73.2 

May  24 

•2  25 

1 1 

13 

207  5'5 

42-55 

73-7 

'9 

2  23 

11  19 

208  5 

42.80 

73-3 

25 

2  25 

1 1 

12 

207  52 

42.50 

73-8 

20 

2  24 

11  18 

208  2 

42.75 

73-4 

27 

2  26 

1 1 

10 

207  48 

42.40 

74.0 

23 

2  24 

11  14 

207  56 

42.60 

73.6 

28 

2  26 

1 1 

9 

207  44 

42.35 

74.1 

OBSERVATIONS  OF  THE  SATELLITES  OP  SATURN. 


421 


Date 

X 

a 

T 

Date. 

F 

\ 

T 

+ 

— 

+ 



26 

11 

June  1 

0  / 

O 

0 

it 

m. 

May  29 

2 

11 

8 

207 

42 

42.30 

74.2 

0  58 

16 

6 

219 

33 

42.43 

74.2 

31 

2 

27 

7 

207 

38 

42.25 

74-4 

3 

0  59 

16 

4 

219 

28 

42.33 

74-5 

June  1 

2 

27 

7 

207 

37 

42.20 

74.6 

8 

1  0 

16 

0 

219 

8 

41-97 

74-9 

4 

2 

28 

5 

207 

31 

41.90 

74-9 

1 1 

1  1 

15 

58 

219 

3 

41.83 

75.2 

c 
3 

2 

28 

4 

207 

29 

41.85 

75.0 

27 

1  4 

15 

53 

218 

45 

40.80 

77.1 

6 

2 

28 

4 

207 

27 

41.80 

75-i 

July  12 

1  4 

15 

59 

218 

46 

39.80 

79.0 

7 

2 

20 

3 

207 

25 

41-75 

75.2 

'4 

1  3 

16 

1 

218 

5° 

39-7° 

79-4 

8 

2 

20 

3 

207 

24 

41.70 

75-4 

Aug.  1 1 

0  56 

16 

37 

220 

4 

37.70 

83.1 

2 

20 

2 

207 

23 

41.65 

75-5 

9 

10 

2 

20 

7 

2 

207 

22 

4r-57 

75.6 

1837 

+ 

+ 

12 

2 

29 

2 

207 

21 

41.44 

75-9 

Mar.  12 

121 

21 

48 

237 

6 

41.37 

76.2 

15 

2 

29 

2 

207 

18 

41.25 

76.2 

13 

1  21 

21 

47 

237 

4 

41.42 

76.1 

16 

2 

29 

2 

207 

18 

41.19 

76.4 

26 

1  17 

21 

36 

236  31 

42.08 

74.8 

17 

2 

20 

7 

2 

207 

18 

41.22 

76.5 

28 

1  16 

21 

34 

236  24 

42.14 

74-5 

18 

2 

29 

2 

207 

17 

41.06 

76.6 

April  1 

1  14 

21 

30 

236 

12 

42.37 

74-3 

'9 

2 

20 
7 

3 

207 

17 

41.00 

76.8 

7 

1  11 

21 

24 

235 

49 

42.85 

73-9 

20 

2 

•JO 
j 

3 

207 

17 

40.92 

76.9 

8 

1  11 

21 

23 

235 

46 

42.63 

73.8 

21 

2 

30 

3 

207 

17 

40.84 

77.0 

9 

1  10 

21 

21 

235 

43 

42.67 

73-7 

24 

2 

30 

4 

207 

18 

40.62 

77-5 

10 

1  10 

21 

20 

235 

39 

42.70 

73-7 

25 

2 

30 

4 

207 

19 

40.55 

77.6 

1 1 

1  9 

21 

19 

235 

35 

42.72 

73.6 

27 

2 

20 

7 

5 

207 

21 

40.48 

77.8 

12 

1  9 

21 

18 

235 

30 

42.75 

73.6 

July  13 

2 

28 

20 

207 

41 

39-3° 

79-4 

J3 

1  8 

21 

16 

235 

23 

42.78 

73-5 

'5 

2 

27 

23 

207 

44 

39.20 

79-7 

14 

1  8 

21 

15 

235 

20 

42.80 

73-5 

21 

2 

25 

3i 

208 

1 

38.80 

81. 1 

15 

1  7 

21 

14 

235 

17 

42.83 

73-4 



20 

21 

234 

54 

42.93 

73.2 



1  4 

9 

1836 

+ 

16 

82.0 

24 

1  2 

2 1 

4 

234  36 

43.01 

73.1 

Jan.  10 

0 

21 

18 

4 

224 

38-53 

27 

1  0 

2 1 

1 

234 

24 

43.03 

73.0 

Feb.  1 

0 

15 

18 

17 

225 

9 

39.87 

78.9 

28 

0  59 

21 

0 

234 

20 

43-°5 

.0 

4 

0 

»4 

18 

18 

225 

14 

40.00 

78.5 

29 

0  58 

20 

59 

234 

16 

43.07 

.0 

S 

0 

14 

18 

18 

225 

15 

40.07 

78.4 

30 

0  57 

20 

58 

234 

12 

43.07 

.0 

9 

0 

14 

18 

17 

225 

17 

40.27 

77.8 

May  1 

0  57 

20 

56 

234 

6 

43.08 

.0 

Mar.  6 

0 

15 

18 

4 

224 

48 

42.11 

74.8 

3 

0  56 

20 

54 

233 

58 

43.10 

.0 

26 

0 

24 

17 

38 

223 

48 

43.03 

73-i 

4 

0  55 

20 

53 

233 

53 

43.11 

.0 

April  7 

0 

31 

17 

19 

223 

3 

43-37 

72.5 

5 

0  54 

20 

52 

233 

48 

43.11 

.0 

14 

0 

35 

17 

9 

222 

34 

43-47 

72.3 

6 

0  53 

20 

5i 

233 

44 

43.11 

.0 

21 

0 

39 

16 

58 

222 

3 

43-53 

72.2 

7 

0  52 

20 

49 

233 

39 

43.11 

.0 

0 

41 

16 

5» 

221 

46 

43.52 

72.3 

8 

0  51 

20 

48 

233 

30 

43.10 

.0 

26 

0 

41 

16 

5° 

221 

43 

43.52 

72.3 

9 

0  50 

20 

46 

233 

26 

43.09 

73.0 

27 

0 

42 

16 

48 

221 

40 

43.50 

72.3 

21 

0  43 

20 

33 

232 

32 

42.87 

73-3 

May  1 

0 

45 

16 

43 

221 

23 

43-47 

72.4 

June  5 

0  36 

20 

19 

23 1 

38 

42-33 

74.2 

3 

0 

46 

16 

41 

221 

*3 

43-43 

72.5 

6 

0  35 

20 

18 

23 1 

36 

42.28 

74-3 

12 

0 

5i 

16 

28 

220 

37 

43.22 

72.8 

24 

0  29 

20 

7 

230 

40 

41.38 

76.0 

J3 

0 

52 

16 

27 

220 

33 

43.10 

72.8 

25 

0  29 

20 

7 

230  38 

41-33 

76.1 

'9 

0 

54 

16 

T9 

220 

12 

42.97 

73.2 

July  28 

0  28 

20 

21 

231 

0 

39.22 

80.3 

22 

0 

55 

16 

16 

220 

1 

42.87 

73-4 

29 

0  29 

20 

22 

23 1 

2 

39.11 

80.4 

24 

0 

56 

16 

14 

219 

54 

42.77 

73.6 

(404)  The  use  of  these  elements  supposes  the  orbits  of  the  satellites  coincident  with  the 
plane  of  the  ring.  They  are,  therefore,  inapplicable  to  the  reduction  of  the  observations  of 
Iapetus,  the  deviation  of  whose  orbit  from  that  plane  is  very  considerable,  and  which  will 
require  special  elements  adapted  to  its  own  case. 

(405)  For  the  other  satellites  the  following  tables  exhibit  the  Saturnicentric  longitudes,  from 
the  descending  node  of  the  ring,  calculated  from  these  formulae  and  elements  for  each  of  the 
times  of  observation  as  above  stated,  and  for  each  satellite  drawn  out  seriatim.  They  are  found 
in  the  column  headed  Observed  Longitudes  :  annexed,  in  the  column  headed  Mean  Longitudes, 
are  the  mean  longitudes  (reckoned  in  the  same  way  on  the  ring,  and  from  the  same  node),  as 
calculated  from  the  following  assumed  epochs  of  longitude  and  mean  motions. 

5  p 


422 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


Titan. 

Rhea. 

Dione. 

Tethjs. 

Enceladus. 

Mimas. 

Epochs. 

0  / 

0  / 

0  / 

0  / 

0  1 

0  / 

1835.0 

321  58.2 

346  33.4 

65  54.6 

358  16.6 

29  26.4 

1836.0 

3°5  9-3 

3  53 

327  40.8 

313  43.8 

67  36.6 

16  34.2 

1837.0 

265  45.8 

280   11. 1 

97  55-2 

78  28.8 

203  3.0 

Mean  motion 

22  Rev.  + 

80  Rev.  + 

133  Rev.  4- 

193  Rev.  + 

266  Rev.  + 

387  Rev.  + 

in  365  days. 

320  36.5 

286  58.2 

130  14.4 

124  45.0 

135  26.4 

95  58.8 

The  other  column  contains  the  excess  of  the  observed  true  over  the  calculated  mean  longi- 
tudes, and  exhibits  the  joint  effect  of  error  of  observation,  equation  of  the  centre,  and  error  of 
epoch,  the  mean  motions  assumed  being  so  nearly  correct  as  to  render  any  small  error  thence 
arising  of  no  account.  In  this  table,  estimated  angles,  and  those  resulting  from  measurement  of 
diagrams  are  omitted. 


TABLE  A.    SYNOPSIS  OF  OBSERVED  TRUE  AND  CALCULATED  LONGITUDES  OF  TITAN. 


Date. 

Observed  Long. 

Mean  Long. 

Difference. 

Date. 

Observed  Long. 

Mean  Long. 

Difference. 

1835 

/ 

0 

/ 

0 

1835 

0 

348 

0 
346 

0 

/ 

May  18 

203 

44 

206 

35 

—  2 

51 

April  7 

40 

16 

+ 

2 

24 

205 

26 

207 

54 

—  2 

28 

14 

139 

57 

142 

18 

2 

21 

!9 

229 

!9 

229 

47 

—  0 

28 

21 

306 

18 

302 

9 

+ 

4 

9 

20 

251 

2 

249 

5° 

+  1 

12 

25 

35 

44 

32 

30 

+ 

3 

14 

23 

323 

57 

3J7 

56 

+  6 

1 

26 

58 

3' 

54 

12 

+ 

4 

l9 

24 

341 

23 

34i 

5 

+  0 

18 

27 

82 

24 

76 

39 

+ 

5 

45 

25 

4 

16 

3 

40 

+  0 

36 

May  3 

210 

43 

213 

!3 

2 

30 

27 

52 

52 

48 

5° 

+  4 

2 

8 

329 

48 

322 

42 

+ 

7 

6 

29 

96 

30 

93 

23 

+  3 

7 

12 

55 

45 

54 

1 

+ 

1 

44 

31 

132 

25 

*37 

2 

—  4 

37 

*9 

208 

30 

211 

27 

2 

57 

June  1 

156 

30 

160 

26 

-  3 

56 

22 

282 

2 

279 

5i 

+ 

2 

1 1 

4 

229 

35 

229 

46 

—  0 

1 1 

24 

33° 

18 

324 

47 

+ 

5 

31 

5 

253 

24 

252 

23 

+  1 

31 

June  1 

136 

22  : 

144 

57 

8 

33  = 

6 

279 

37 

274 

7 

+  5 

30 

3 

183 

6  : 

191 

"7 

8 

II  : 

7 

299 

4 

294 

56 

+  4 

8 

8 

309 

5 

304 

32 

+ 

4 

33 

8 

320 

10 

317 

28 

+  2 

42 

1 1 

10 

29 

1 1 

20 

0 

51 

9 

344 

0 

342 

7 

+  1 

53 

27 

1 1 

53 

9 

59 

+ 

1 

54 

10 

7 

6 

4 

7 

+  2 

59 

July  12 

345 

4 

348 

22 

3 

18 

12 

5i 

33 

46 

25 

+  5 

8 

H 

35 

41 

32 

36 

+ 

3 

5 

15 

122 

15 

118 

0 

+  4 

15 

Aug.  1 1 

307 

6 

304 

35 

+ 

2 

31 

16 

141 

39 

140 

14 

+  1 

25 

17 

159 

16 

160 

59 

—  1 

43 

J«37 

18 

181 

28 

184 

59 

—  3 

31 

Mar.  12 

82 

1 1 

79 

36 

+ 

2 

35 

'9 

203 

20 

205 

51 

—  2 

3« 

13 

105 

48 

104 

14 

+ 

1 

34 

207 

4 

209 

14 

—  2 

10 

26 

37 

9 

35 

56 

+ 

1 

'3 

20 

229 

1 1 

229 

44 

—  0 

33 

28 

84 

39 

82 

18 

+ 

2 

21 

21 

208 

57 

251 

15 

+  17 

42 

April  1 

170 

28 

172 

3i 

^ 

3 

25 

340 

27 

340 

51 

—  0 

24 

7 

312 

36 

308 

2 

+ 

4 

34 

26 

7 

51 

3 

14 

+  4 

37 

8 

333 

22 

328 

49 

+ 

4 

33 

27 

3i 

0 

27 

5i 

+  3 

9 

9 

355 

47 

353 

9 

+ 

2 

38 

July  13 

3i 

41 

29 

55 

+  1 

46 

10 

17 

54 

'4 

10 

+ 

3 

44 

»5 

76 

39 

7i 

43 

+  4 

56 

1 1 

40 

19 

38 

9 

+ 

2 

10 

21 

205 

16 

207 

44 

—  2 

28 

12 

62 

45 

60 

41 

+ 

2 

4 

»3 

84 

47 

84 

10 

+ 

37 

0 

1836 

H 

108 

53 

105 

26 

+ 

3 

27 

Jan.  10 

J59 

46 

161 

25 

—  1 

39 

15 

127 

1 1 

126 

6 

+ 

1 

5 

Feb.  1 

300 

43 

298 

8 

+  2 

35 

20 

239 

1 1 

239 

48 

0 

37 

4 

8 

16 

6 

16 

+  2 

0 

24 

336 

59 

331 

49 

+ 

5 

10 

5 

29 

55 

27 

35 

+  2 

20 

27 

41 

20 

39 

5 

+ 

2 

15 

9 

121 

5 

119 

35 

+  1 

30 

28 

59 

56 

60 

7 

0 

1 1 

Mar.  6 

349 

0 

345 

46 

+  3 

14 

64 

8 

61 

5° 

+ 

2 

18 

27 

99 

20 

97 

34 

+  1 

46 

29 

87 

40 

82 

39 

+ 

5 

1 

OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


423 


Date. 

Observed  Long. 

Mean  Long. 

Difference. 

Date. 

Observed  Long. 

Mean  Long. 

Difference. 

1837 

0 

/ 

0 

0 

1837 

0 

/ 

0 

/ 

0  / 

85 

9 

84 

26 

+  0 

43 

May  9 

307 

55 

307 

37 

+  0  18 

April  30 

108 

9 

104 

30 

+  3 

39 

21 

214 

53 

218 

8 

-  3  15 

May  1 

128 

46 

129 

21 

—  0 

35 

June  5 

191 

34 

195 

54 

—  4  20 

3 

169 

29 

173 

6 

-  3 

37 

6 

214 

37 

217 

49 

-  3  12 

4 

189 

21 

194 

5i 

-  5 

30 

24 

264 

25 

264 

5° 

—  0  25 

5 

215 

28 

217 

56 

—  2 

28 

25 

292 

21 

288 

34 

+  3  47 

6 

239 

56 

240 

33 

—  0 

37 

July  28 

312 

28 

3 12 

26 

+  0  2 

7 

264 

35 

262 

59 

+  1 

36 

29 

339 

12 

335 

3° 

+  3  42 

TABLE  B.    SYNOPSIS  OF  OBSERVED  TRUE  AND  CALCULATED  MEAN  LONGITUDES  OF  RHEA. 


Date. 

Observed  Long. 

Mean  Long. 

Difference. 

Date. 

Observed  Long. 

Mean  Long. 

Difference. 

1835 

0 

0 

0 

/ 

1836 

0 

0 

O 

May  19 

301 

29 

297 

39 

+ 

3 

5° 

Aug.  11 

147 

40 

141 

•9 

+ 

6 

21 

23 

25I 

44 

249 

52 

+ 

1 

52 

24 

322 

21 

331 

20 

8 

59 

1837 

June  6 

289 

4i 

285 

48 

+ 

3 

53 

Mar.  12 

221 

*9 

217 

12 

+ 

4 

7 

15 

284 

47 

284 

0 

+ 

0 

47 

13 

307 

25 

303 

58 

+ 

3 

27 

17 

80 

1 

76 

21 

+ 

3 

40 

April  1 

12 

10 

15 

16 

3 

6 

18 

157 

38 

157 

55 

0 

17 

7 

131 

42 

133 

26 

1 

44 

19 

240 

3 

241 

24 

1 

21 

8 

208 

0 

207 

15 

+ 

0 

45 

20 

3*3 

57 

319 

2 

5 

5 

9 

29I 

5i 

292 

36 

0 

45 

21 

34 

44 

34 

8 

+ 

0 

36 

10 

6 

'3 

9 

48 

3 

35 

39 

16 

38 

4 

+ 

1 

12 

1 1 

88 

16 

91 

43 

3 

27 

a5 

348 

53 

356 

38 

7 

45 

12 

157 

33 

171 

17 

r3 

44 

26 

84 

20 

73 

32 

+  10 

58 

14 

328 

1 1 

329 

4 

0 

53 

27 

r54 

36 

r57 

14 

2 

38 

20 

68 

8  : 

83 

41 

'5 

33  : 

July  15 

150 

21 

r43 

46 

+ 

6 

45 

27 

283 

5° 

285 

54 

2 

4 

21 

260 

1 

262 

17 

2 

16 

28 

359 

16 

0 

6 

0 

5° 

56 

35 

39 

1836 

3 

5 

1 

29 

83 

8 

80 

1 

+ 

3 

7 

Feb.  9 

274 

59 

271 

17 

+ 

3 

32 

87 

51 

85 

20 

+ 

2 

31 

April  26 

278 

1 

275 

22 

+ 

2 

39 

30 

162 

30 

156 

20 

+ 

6 

10 

27 

347 

22 

353 

44 

6 

22 

May  4 

123 

20 

JI5 

42 

+ 

7 

38 

May  3 

114 

29 

114 

48 

0 

l9 

5 

196 

34 

192 

24 

+ 

4 

10 

12 

IOI 

5° 

103 

7 

1 

17 

6 

279 

48 

274 

4i 

+ 

5 

7 

24 

339 

1 

337 

20 

+ 

1 

41 

7 

352 

48 

357 

5 

4 

17 

June  1 

256 

33 

253 

43 

+ 

2 

5° 

8 

77 

26 

75 

24 

+ 

2 

2 

2 

329 

3 

331 

5 

2 

2 

9 

153 

46 

153 

22 

+ 

0 

24 

3 

53 

4i 

55 

4 

1 

23 

21 

29 

33 

28 

35 

+ 

0 

58 

8 

IOI 

22 

97 

51 

+ 

4 

31 

June  5 

141 

21 

140 

22 

+ 

0 

59 

1 1 

321 

14  : 

333 

49 

12 

35  : 

6 

219 

0 

217 

30 

+ 

1 

30 

*7 

r43 

1 

160 

1 

17 

0 

25 

297 

37 

296 

30 

+ 

1 

7 

July  12 

280 

5 

275 

16 

+ 

4 

49 

July  28 

34 

14 

41 

40 

7 

26 

'4 

69 

34 

69 

38 

0 

4 

29 

120 

1 1 

123 

24 

3 

13 

TABLE  C.    SYNOPSIS  OF  OBSERVED  TRUE  AND  CALCULATED  MEAN  LONGITUDES  OF  DIONE. 


Date. 

Observed  Long. 

Mean  Long. 

Difference. 

Date. 

Observed  Long. 

Mean  Long. 

Difference. 

1835 
May  18 
June  21 

26 

0  / 
277  39 
45  35 
338  23 

0  ; 

278  44 
44  43 
343  26 

0  / 

-  1  5 
+  0  52 

-  4  53 

1836 
June  3 
8 
1 1 

July  12 
14 

0  / 
107    18  : 

60  22 

89  29 
190  28 

91  11 

0  / 
112  58 

57  22 

87  22 
188  27 
85  22 

0  / 
-  S    40  : 
+  3  0 
+   2  7 
+   2  I 

+  5  49 

1836 
April  27 
May  12 
June  1 

297  38 
99  8 
209     14  : 

298  47 

IOI  II 

207  55 

-  1  9 

-  2  3 
+  1     19  : 

1837 
April  7 

328  44 

328  47 

-  0  3 

424 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


Date. 

Observed  Long. 

Mean 

Long. 

Difference. 

Date. 

Observed  Long. 

Mean  Long. 

Difference. 

1837 

0 

/ 

0 

0 

1837 

0 

/ 

0 

0  y 

April  28 

20I 

16 

198 

58 

+  2 

18 

May  8 

72 

32 

72 

23 

+  °  9 

29 

330 

32 

330 

13 

+  0 

*9 

9 

209 

20 

211 

'9 

-  1  59 

30 

105 

28 

99 

»7 

+  6 

1 1 

June  5 

144 

48 

I44 

45 

+  0  3 

May  4 

264 

0 

266 

4 

—  2 

4 

6 

271 

33 

272 

21 

—  0  12 

5 

35 

56 

37 

14- 

—  1 

18 

*5 

253 

20 

256 

1 1 

-  2  51 

6 

172 

9 

170 

31 

+  1 

38 

July  28 

259 

36 

272 

17 

— 12  41 

7 

298 

10 

301 

35 

-  3 

35 

TABLE  D.    SYNOPSIS  OF  THE  OBSERVED  TRUE  AND  CALCULATED  MEAN  LONGITUDES  OF 

TETHYS. 


Date. 

Observed  Long. 

Mean  Long. 

Difference. 

Date. 

Observed  Long. 

Mean  Long. 

Difference. 

1835 

0 

/ 

0 

/ 

0 

1837 

0 

1 

0 

0 

June  21 

97 

14 

88 

15 

+  8 

59 

April 

29 

173 

9 

178 

24 

5 

15 

25 

138 

42 

141 

10 

—  2 

28 

30 

357 

8 

4 

3 

6 

55 

43 

33 

43 

+ 

0 

33 

May 

4 

0 

1836 

49 

1 1 

52 

49 

3 

38 

May  12 

357 

20 

0 

59 

-  3 

39 

55 

22 

56 

39 

1 

17 

June  1 

205 

14  : 

205 

29 

—  0 

15  : 

65 

1 

63 

16 

+ 

1 

45 

2 

31 

38 

29 

43 

+  1 

58 

5 

227 

33 

226 

26 

+ 

1 

7 

3 

223 

55 

225 

1 

—  1 

6 

240 

4i 

241 

32 

0 

5' 

233 

56 

235 

35 

—  1 

39 

6 

69 

23 

71 

33 

2 

1 1 

243 

12 

248 

45 

-  5 

33 

7 

261 

42 

263 

35 

1 

53 

8 

120 

1 

115 

44 

+  4 

17 

8 

98 

8 

9' 

54 

+ 

6 

14 

11 

312 

4« 

320 

5° 

-  8 

9 

9 

292 

32 

294 

59 

2 

37 

July  12 

93 

28 

88 

45 

+  4 

43 

June 

5 

12 

48 

17 

0 

4 

12 

14 

I!5 

38 

101 

5 

+  14 

33 

6 

206 

14 

202 

47 

+ 

3 

27 

25 

224 

228 

22 

58 

4 

36 

1837 

236 

55 

234 

8 

+ 

2 

47 

April  7 

328 

44  = 

320 

32 

+  8 

12  : 

July 

28 

18 

36 

0 

21 

42 

9 

349 

49  : 

342 

46 

+  7 

3  : 

24 

26  : 

39 

27 

»s 

1  : 

28 

339 

17 

35° 

21 

—  1 1 

4 

TABLE  E.    SYNOPSIS  OF  THE  OBSERVED  TRUE  AND  CALCULATED  MEAN  LONGITUDES  OF 

ENCELADUS. 


Date. 

1835 
June  21 

Observed  Long. 

0  / 
297  17 

Mean  Long. 

0  / 
292  58 

Difference. 

0  / 
+  4  19 

Date. 

1837 
May  4 

6 

8 
9 

June  6 

25 

Observed  Long. 

0  / 
150  25 
304  22 
313  56: 
122  24 

20  34 
157  I 
Il6  59 

Mean  Long. 

0  / 
145  18 
302  22 
315  29 
112  12 

3°  3 

152  15 

IOI  0 

Difference. 

0 

+  5  7 

4-2  0 

-  1  33 
+  10  12 

-  9  29 
4-  4  46 
+  15  59 

1836 
May  12 
June  1 

3 

284  41 

127    23  : 
295    41  : 

290  47 
134  4S 
314  26 

-  6  6 

-  7     25  : 
-18    45  : 

PRESUMED  SINGLE  OBSERVED  TRUE  LONGITUDE  AND  CALCULATED  MEAN  LONGITUDE  OF  MIMAS. 


1836,  June  3  ;  Observed  Long.  2950  24' ;  Mean  Long.  295°  24';  Difference  =  o. 


(406)  Whatever  errors  we  attribute  to  our  assumed  epochs,  and  whatever  values  we  assign 
to  the  equations  of  the  centres  in  these  series,  there  will  still  remain  large  outstanding  diffe- 
rences, which  can  only  arise  from  error  of  observation.    It  must  be  borne  in  mind,  however,  that 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


425 


any  error  committed  in  the  measurement  of  the  angle  of  position  at  or  near  the  greatest  elon- 
gations, are  violently  exaggerated  when  reduced  to  longitude,  since  they  become  multiplied  (as 
the  effect  of  that  reduction)  by  a  factor  nearly  equal  to  cosec  /,  the  average  values  of  which,  in 
the  respective  years  1835,  6,  and  7,  are  5.13,  3.42,  and  2.79.  Now,  very  nearly  all  the  worst 
cases  of  apparent  discordance  fall  within  a  measured  angle  of  15°,  one  way  or  other,  of  the  line 
of  Ansae,  and  therefore  originate  (in  so  far  as  they  are  really  erroneous)  in  errors  of  measure- 
ment very  much  less  than  their  apparent  amount,  and  which  in  fact  fall  within  limits  even  less 
wide  than  might  be  expected  under  all  the  circumstances.  Some  observations,  no  doubt,  ought 
to  be  rejected.  Such  are  those  of  Titan  for  June  21,  1835,  and  June  1  and  3,  1836 ;  of  Rhea, 
for  June  26,  1835,  June  11  and  27,  1836,  and  April  12  and  20,  1837;  of  Dione,  for  July  28, 
1837  ;  and  of  Tethys  for  the  same  day.  Now  there  is  not  one  of  these  whose  rejection,  on 
referring  to  the  original  observations,  is  not  justified  on  good  and  obvious  grounds.  Thus  the 
observations  of  June  21  and  26,  1835,  and  June  11,  1836,  were  made  with  the  reflector  out 
of  the  meridian  by  adjusting  the  fixed  wire  as  well  as  might  be  to  the  parallel — a  proceeding 
especially  open  to  error,  from  the  mode  of  suspension  of  the  telescope,  and  the  difficulty  of 
keeping  it  steady  when  deprived  of  the  firm  support  of  the  side  ladder.  Those  of  June  1  and  3, 
1836,  were  altogether  irregular  and  tentative  :  reference  being  had,  indeed,  to  the  Ansae,  but 
in  the  insufficient  and  unsatisfactory  manner  alluded  to  in  Art.  (399).  Again,  the  equatorial 
measures  of  Rhea  for  June  27,  1836,  and  April  20,  1837,  are  merely  superficial,  hurried  and 
single  measures  without  any  weights  attached  to  them;  while  on  Ajiril  12,  1837,  occur  the 
remarks  : — "  Definition  for  the  most  part  dreadfully  bad."  And  again,  "  Every  possible  annoy- 
ance from  cloud  and  bad  definition."  Lastly,  the  observations  of  July  28,  1837,  besides  the  evil 
of  bad  definition,  which  disturbed  and  prematurely  broke  off  the  observations,  some  other 
especial  cause  would  appear  to  have  acted  to  disturb  the  judgment  in  respect  of  all  the 
satellites  observed  (except  Titan),  the  measures  of  all  being  affected  with  unusually  large 
negative  error,  and  that  in  the  proportion  of  their  proximity  to  the  planet. 

(407)  In  the  mode  of  treatment  by  graphical  projection  to  which  these  observations  have 
been  subjected,  considerations  of  this  kind  may  in  great  measure  be  disjjensed  with.  It 
is  certainly  satisfactory  to  see  good  reason  for  rejecting  discordant  measures  ;  but  in  such 
projections  bad  observations  at  once  proclaim  themselves,  and  drop  out  of  consideration. 
Each  of  the  foregoing  series  has  been  so  projected,  and  the  following  are  the  results  of  the 
operation : — 


Deduced  Elements. 

Titan. 

Rhea. 

Dione. 

Tethys. 

Enceladus. 

O.02385 

O.02269 

0.02066 

0.04217  : 

Equation  of  centre   . . 

2°  44' 

2°  36' 

2°  22' 

4°  5°'  : 

270  0 

95  0 

42  30 

53    4°  : 

Correction  of  epochs 

+0  30 

+0  30 

0  0 

0  0 

+o°  5' 

Corrected  epochs  : — 

1^35   

322  28.2 

347  3-4 

65  54.6 

358  16.6 

29  31.4 

1836   

305  39.3 

353  44-° 

327  40.8 

313  43.8 

67  41.6 

1837   

266  15.8 

280    41. 1 

97  55-2 

78  28.8 

203  8.0 

(408)  Comparing  these  results  in  the  case  of  Titan  with  those  of  Bessel,  we  find  as  near 

5  Q 


426 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


an  agreement  as,  from  the  apparently  rough  data  from  which  we  set  out,  and  the  brief  interval 
embraced  by  my  observations,  could  be  expected.  The  excentricity  assigned  by  him  as  his 
final  result  for  1830  (Astron.  Nachr.  214)  is  0.029314,  and  his  perisaturnium  for  the  same  epoch 
244°  17'  36"  from  his  point  of  departure,  which,  reduced  to  the  descending  node  of  the  ring 
by  adding  12°  20'  35",  and  further  corrected  by  +  3°  13'  19",  the  motion  of  the  perisaturnium 
for  the  six  years  from  1830  to  1836  gives  259°  4'  30"  in  our  mode  of  reckoning:  differing  by 
10°  18'  30"  from  that  above  concluded — a  quantity  not  large,  considering  the  near  approach  of 
the  orbit  to  a  circle,  and  the  consequent  delicacy  of  this  element.  The  most  important 
difference  is  the  correction  of  0°  30'  in  the  epochs,  which  is  in  effect  a  deviation  to  that  precise 
amount  from  Bessel's  :  those  epochs,  and  the  tables  of  mean  motions  given  by  him  in  Astron. 
Nachr.,  No.  195,  having  been  used  in  calculating  the  mean  longitudes  in  Table  (A).  Though 
this  correction  is  more  considerable  than  could  be  wished,  I  feel  disposed,  on  a  mature  con- 
sideration of  the  whole  series  of  projected  results,  to  insist  on  the  necessity  of  some  correction  in 
this  direction,  though  perhaps  not  to  quite  so  great  an  extent. 

(409)  The  excentricities  and  perisaturnia  of  Rhea  and  Dione,  especially  the  latter,  are 
indicated  with  considerable  decision  by  the  projections,  and  I  have  no  doubt  are  respectable 
approximations  to  the  truth.  The  epochs  of  both  are  undoubtedly  correct  to  within  a 
degree,  and  afford  the  means  of  testing,  and,  if  need  be,  of  correcting,  their  periods  and  mean 
motions  by  comparison  with  earlier  observations.  Thus,  in  the  case  of  Rhea,  if  we  calculate  by 
the  tables,  epochs,  and  precepts  given  in  Phil.  Trans.  1790,  p.  488... 495,  its  mean  longitude  for 
Aug.  23,  1789,  mean  noon  at  Slough  (on  which  day  the  earth  was  exactly  or  very  nearly  in 
the  plane  of  the  ring*),  we  find  it  to  have  been  36°.64,  as  seen  from  Slough,  the  equation  of 
light  being  neglected  in  the  precept  alluded  to ;  and  since  noon  at  Slough  corresponds  to 
+  lh  16m  19s  at  Feldhausen,  which  is  partly  counteracted  by  the  equation  of  light  —  lh  10m  at 
the  date  in  question,  if  we  calculate  by  the  same  tables  of  mean  motion,  but  by  our  epoch  for 
1836,  the  mean  longitude  for  1836,  Aug.  23,  0h  6m  19s  (tabular  date),  we  get  1°.30  for  the 
actual  mean  longitude,  after  a  lapse  of  17166  exact  days.  In  this  interval  there  must  have 
been  described,  over  and  above  an  integer  number  of  revolutions,  a  fractional  part  =  361°.30 
—  36°.64  =  324°. 66.  Now,  the  mean  motion  assumed  gives  for  that  number  of  days 
3799  revol.  +  324°.18,  differing  only  by  —  0°.48  from  observation,  a  degree  of  precision 
which  could  by  no  means  have  been  looked  for,  and  which  authorizes  our  regarding  our 
assumed  mean  motion  of  80  revol.  +  286°.97  in  365  clays  as  exceedingly  accurate.  An 
error  of  a  whole  revolution  would  entail  a  deviation  of  7°. 66  per  annum,  and  would  therefore 
produce  on  the  whole  period  embraced  by  my  observations  a  regularly  progressive  dis- 
cordance, amounting  in  the  whole  to  between  16°  and  17°. 

(410)  If  we  institute  a  similar  calculation  for  Dione,  we  find  that  the  mean  longitude 
actually  described  in  our  interval  of  17166  days  is  15°.47  in  excess  of  an  integer  period;  and 


*  The  mean  motions  of  these  tables,  for  the  live  older  satellites,  are  Lalande's,  from  the  Connaiss.  des 
Temps,  1791-— The  23rd  of  August  is  chosen  because,  under  the  circumstances  of  that  date,  the  precept  alluded 
to  in  the  text  is  rigorously  exact,  the  reduction  of  Saturn's  geocentric  longitude  (or  rather  of  the  portion  of  that 
longitude  between  Saturn  and  the  node  of  the  ring)  to  the  plane  of  the  ring  being  then,  and  then  only, 
negligible. 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN.  427 

if  we  calculate  by  the  tabular  mean  motion,  the  mean  motion  for  that  interval,  we  find  it  to 
come  out  6272  rev.  +  8°.16.  Here,  again,  the  difference  (7°.31)  is  so  small,  that  we  cannot 
hesitate  to  accept  6272  as  the  true  number  of  revolutions;  and  calculating  on  this,  we 
obtain  for  a  corrected  mean  motion,  for  1  day,  131°.5353296,  and  for  365  days,  133  rev. 
+  130°.3953040. 

(411)  So,  again,  forTethys.  The  mean  longitude  really  described  in  the  same  interval  was 
49°. 30  in  excess  of  a  whole  number  of  revolutions,  while  that  calculated  from  our  assumed 
mean  motion  is  9093  rev.  +  40°.93.  The  difference,  again,  is  so  small  a  fraction  of  a  circum- 
ference, that  we  are  authorized  to  assume  9093  for  the  true  number,  and  to  assign  190°.6984330 
for  the  corrected  mean  motion  in  1  day,  and  193  rev.  +  124°.9280450  in  365. 

(412)  With  Enceladus  the  discordance  is  greater;  the  observed  motion  being  337°.32  in 
excess  of  whole  revolutions,  and  the  calculated  being  12527  rev.  +  255°.68.  The  difference 
is  81°. 64,  which,  being  still  less  than  a  quadrant,  would  appear  to  authorize  our  assuming 
12527  as  the  true  number  of  revolutions,  since  the  assumption  of  the  nearest  less  integer  would 
produce  the  intolerable  error  of  nearly  6°  per  annum.  Taking,  therefore,  12527  as  the  true 
number,  we  get  262°.7319889  and  266  rev.  +  137°. 1759485  for  the  mean  motions  in  1  and  365 
days  respectively. 

(413)  From  the  single  observation  of  Mimas  (if  really  such)  of  course  nothing  can  be 
concluded.  It  is  necessary  to  state  the  circumstances  of  this  observation.  On  the  3rd  of  June, 
1836,  at  9h  38m  M.  T.,  the  satellites  A  North. 

(Titan),   B   (Rhea),   C   (Dione),   D  A» 
(Tethys),  were  seen,  and  a  diagram 
made  of  them  as  here  represented. 
Jupiter,  though  of  course  visible,  was 

not  noted,  being  much  more  distant  in  D 
the  direction  nearly  of  A,  as  appears  p  /  f 

by  referring  to  its  table  of  observed  c  %   vQ^L-      >-<^)  ''  E 

angles  of  position.*     At  9'1  50m  the 

following  memorandum  occurs:  —  "I  B 
now  see  another  satellite,  E"  (this  was 

Enceladus).     "  Showed    the 

above.  She  could  not  see  E."  (The 
party  here  referred  to  is  very  short-sighted.)  "  As  she  was  going,  looking  again,  I  now  see  that 
E  is  double,  and  F  by  glimpses  very  discernible. '  At  10h  25m  it  is  remarked,  "The  lineE  F  is 
more  oblique,  and  jioints  very  nearly  towards  B."  After  taking  several  measures,  among  which 
is  that  of  Enceladus  at  1 1 h  0m,  recorded  in  the  synoptic  table  (p.  419),  and  which  is  characterized 
as  "  a  satisfactory  measure,  steadily  contemplated  in  an  interval  of  unexampled  tranquillity,"  the 
following  remarks  occur:  "llh  6m  M.  T.  Planet  getting  low,  and  frequent  intervals  of 
confusion  coming  on.    Of  the  existence  of  E  there  can  be  no  doubt ;  but  when  I  got  my  best 


South. 


*  There  is  in  the  original  diagram  a  small  star  marked  y  beyond  A,  but  not  far  enough  for  the  satellite  in 
question.  Its  situation,  however,  is  correct  as  regards  position,  and  it  may  have  been  the  satellite  misplaced  in 
distance  to  keep  the  figure  within  bounds.    A  in  the  figure  is  represented  too  distant. 


428 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


views  of  E,  I  did  not  see  F  ;  and  though  I  have  no  doubt  F  was  a  real  object,  I  could  not  see 
it  again  after  the  planet  began  to  grow  furry.  Tried  the  field  bar,  but  it  proved  of  no  service." 
It  is  to  be  remarked,  that  during  the  35  minutes  between  the  two  recorded  notices  of  F,  the 
planet  had  moved  3".8  westward,  and  F'.OS  northward,  which  would  be  nearly  counteracted 
by  the  apparent  southward  motion  of  E ;  so  that,  had  F  been  a  star,  the  objects  would  have 
been  brought  into  conjunction,  instead  of  remaining,  as  they  appeared  to  do,  nearly  at  the 
same  mutual  distance.  Should  it  be  contended,  from  the  invisibility  of  F  at  1  lh  0m,  when  E 
teas  best  seen,  that  such  was  really  the  case,  and  that  it  was  then  actually  covered  by  Enceladus, 
I  can  only  remark  on  the  improbability  of  such  an  occultation ;  which  yet  certainly  may 
have  happened.  If  so,  I  have  been  defeated  in  every  attempt  to  observe  this  satellite.  Mr. 
Lassel  has  been  more  fortunate,  having,  as  he  informs  me,  obtained  three  sure  observations  of 
it,  on  Aug.  25,  30,  and  Sept.  1,  1846,  with  his  large  equatorial  reflector,  power  567. 

(414)  For  the  determination  of  the  mean  distances  or  major  semiaxes  of  the  orbits,  measures 
at  or  near  the  greatest  elongation  of  the  satellites  can  alone  be  advantageously  employed,  espe- 
cially in  considerable  oblicpiities  of  the  ring  where  the  foreshortening  of  the  radius  vector 
renders  every  error  committed  unduly  influential.  In  the  course  of  the  observations  in  which 
the  foregoing  positions  were  accumulated,  a  good  many  measures  of  distance  were  also  taken 
in  all  angles  of  position,  and  all  taken  from  the  apparent  centre  of  the  planet  for  the  sake  of 
uniformity  of  calculation.  On  reducing  them,  however,  I  find  that  even  at  moderate  inclinations 
to  the  line  of  Ansae,  not  only  do  the  discordances  between  individual  results  increase  rapidly 
(as  might  be  expected),  but  that  a  general  cause  appears  to  have  acted,  rendering  the  results 
progressively  more  and  more  erroneous  in  defect  of  the  truth  with  the  increase  of  inclination. 
This  cause  can  be  no  other  than  the  want  of  symmetry  of  the  upper  and  lower  portions 
of  the  outline  of  the  visible  part  of  the  body — the  one  circular  and  protuberant,  jjrojecting 
upon  and  beyond  the  ring  and  uninterrupted — the  other  cut  across  by  the  ring,  and  thereby 
deprived  of  its  due  influence  on  the  judgment.  This,  of  course,  makes  the  apparent  centre 
more  difficult  to  fix  upon,  and  is  therefore  far  more  influential  here  than  in  measures  of 
position  where  general  symmetry  alone  is  aimed  at,  and  the  imagination  has  only  to  fill  up  the 
circular  outline,  not  at  the  same  time  to  decide  upon  its  centre.  In  situations  very  near  the  line 
of  Ansae,  this  disturbing  influence  does  not  act ;  the  diameter  of  the  planet  presenting  itself 
unbroken  and  similarly  terminated  at  both  extremities  as  a  line  for  bisection.  I  shall,  tberefore, 
set  down  only  those  measures  of  distance  which  have  been  procured  at  apparent  inclinations  to 
the  line  of  Ansae  within  10°  one  way  or  other  (a  situation,  however,  it  must  be  recollected, 
still  unfavourable  for  exactness  without  the  advantage  of  a  clock-work  movement).  For  Titan 
these  distances  are  as  follows  : — 


Date. 

-9o° 

P 

r 

Date. 

0  +p 

—  90? 

P 

r 

i83S 

0  / 

Pts. 

a 

1835 

0  / 

Pts. 

n 

May  23 

f 

+  5  28 

695.30 

167.75 

in 

June  7 

f 

+  0  12 

737.10 

I7O.29 

m 

29 

P 

-4  9 

71 1.90 

176.65 

111 

8 

f 

+4  36 

673.90 

166.15 

m 

31 

June  1 

P 
P 

+  3  9 
+  9  5° 

736.80 
589.00 

178.65 
182.17 

m 
ni 

iS 

P 

+  0  57 

779-5° 

182.25 

S  m 
I  A 

6 

f 

-3  32 

684.10 

170.43 

m 

16 

P 

+4-  57 

706.70 

»79-75 

m 

OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN.  429 


Date. 

e  +P 

-90° 

P 

r 

Date. 

e+P 

-  90° 

P 

r 

1835 

0  / 

Pts. 

1836 

0  / 

Pts. 

June  17 

P 

+9  46 

577-9° 

186.54 

m 

May  24 

f 

+  5  56 

725.80 

169.42 

m 

Aug.  1 1 

f 

-0  51 

676.70 

173.65 

A 

1836 

Jan.  10 

P 

+  8  25 

656.60 

183.17 

m 

1837 

Feb.  1 

f 

-4-  37 

695.20 

174.41 

m 

Apr.  7 

f 

-4  54 

77 1.20 

181.30 

A 

9 

P 

-4  39 

745-5° 

184.13 

m 

8 

f 

+2  47 

791.44 

179.33 

A 

Apr.  14 

P 

+  2  11 

821.00 

184.71 

A 

15 

P 

-6  45 

763.53 

179.26 

A 

21 

f 

-1  51 

804.30 

180.32 

A 

24 

f 

+4  31 

787.22 

178.01 

A 

May  22 

f 

-8  28 

670.00 

171.04 

m 

May  1 

P 

-5  37 

761.10 

178.54 

A 

The  letters  p  and  f  in  the  second  column  of  this  table  indicate  whether  the  measures  were 
taken  at  the  preceding  or  following  elongation,  and  m  and  A  in  the  last  whether  between  the 
wires  or  by  differences  of  right  ascension  (duly  reduced),  both  expressed  in  micrometer  parts  in 
the  column  headed  p.  The  angles  set  down  under  the  heading  0  +  p  —  90°  are  the  apparent 
inclinations  of  p  to  the  line  of  Ansae.  Lastly,  under  the  heading  r  are  stated  the  ellijitic  values 
of  the  radius  vector  calculated  from  p  by  the  formulas. 

cos  <//  =  cos  I  .  cos  (v  —  \)  ;    r  =  [0.98410]  .  ^-  cosec  ip 

where  v  is  the  calculated  mean  longitude  for  the  moment  of  observation  (which  is  sufficiently 
approximate  for  the  purpose),  and  a,  I,  and  A  are  given  by  the  table  in  Art.  403.  The  numerical 
quantity  0.98410  is  the  logarithm  of  40".095,  the  mean  value  of  a  multiplied  by  0.24044,  the 
reducing  factor  of  the  micrometer  parts  for  conversion  into  seconds.  The  auxiliary  angle  \j/ 
represents  the  angular  saturnicentric  elongation  of  the  satellite  from  the  earth. 

(415)  To  obtain  from  these  elliptic  distances  the  mean  distance  or  semiaxis  of  the  orbit, 
we  must  consider  that  in  an  ellipse  whose  excentricity  is  A  e  (the  semiaxis  being  A),  the  greatest 
possible  difference  between  two  chords  passing  through  the  focus  is  2  A  es ;  and,  consequently, 
that  the  semi-sum  of  any  two  opposite  radii  vectores  cannot  differ  from  the  major  semiaxis  by 
more  than  A  e2,  which  in  the  present  case  hardly  exceeds  0".l.  In  the  actual  state  of  the  data, 
owing  to  the  situation  of  the  perisaturnium,  whose  average  distance  in  longitude  from  the  Ansa 
during  the  period  embraced  by  the  observations  is  about  52°  (using  Bessel's  place),  it  is  still 
less.  Taking,  therefore,  the  means  of  the  results  for  the  preceding  and  following  Ansae  respec- 
tively, which  we  will  call  r  and  r',  we  get  r=  181.44  (eleven  observations),  and  r  =  173.51 
(twelve  observations),  from  which  we  obtain — 

A  =   r  +        |l   +  e1.  (sin  52-)*  |  =  177". 53 

(416)  I  have  no  confidence  in  any  of  the  distances  of  Rhea  measured  with  the  equatorial 
micrometer,  the  faintness  of  the  object  not  permitting  it  to  be  satisfactorily  covered  with  the 
wire,  while  the  attention  was  necessarily  divided  between  it  and  the  apparent  centre  of  the  planet. 
On  reducing  those  which  have  been  procured,  I  find  them  so  far  from  satisfactory  that  it  is 
needless  to  state  them,  inasmuch  as  they  give  for  their  ultimate  result  a  mean  distance  of  73". 86, 

5  R 


430 


OBSERVATIONS  OF  THE  SATELLITES  OF  SATURN. 


being  2\"  less  than  would  be  consistent  with  Kepler's  law,  and  are  otherwise  very  discordant  both 
with  each  other  and  with  the  ellipticity  and  situation  of  the  orbit  as  above  determined.  Those  of 
Iapetus,  though  not  numerous,  and  for  the  most  part  taken  merely  for  the  purpose  of  identifying 
the  satellite  and  distinguishing  it  from  a  star,  presented  less  difficulty;  for  which  reason,  and 
because  they  may  not  prove  altogether  valueless,  they  are  here  set  down,  distinguishing  by 
m  measures  taken  between  the  wires,  by  A  those  calculated  from  differences  of  R  A,  and  by  8 
those  obtained  by  oblique  transits,  and  also  annexing  the  number  of  individual  measurements  on 
which  each  relies. 


Time  of  Obs. 

Dist. 

Time  of  Obs. 

Dist. 

Time  of  Obs. 

Dist. 

1835 

h. 

m. 

1836 

h. 

m. 

1837 

h. 

m. 

May  1 8 

10 

55 

315.02 

I  A 

April  27 

12 

3° 

255-54 

2  A 

April  12 

20 

522.15 

5 

A 

23 

9 

47 

494.83 

1  A 

May  3 

!3 

15 

142.22 

3  m 

15 

12 

45 

497.69 

3 

A 

June  15 

10 

1 1 

148.95 

3  A 

!9 

10 

4 

546.89 

3  A 

24 

14 

28 

228.73 

4 

d 

18 

7 

15 

120.48 

1  m 

22 

1 1 

0 

553-93 

2  A 

May  1 

14 

7 

197.40 

5 

July  21 

7 

1 1 

254.92 

6  A 

14 

10 

40 

549.22 

2  A 

7 

12 

5 

37°-45 

1 

A 

The  observed  greatest  elongation,  for  such  it  appears  by  a  projection  of  all  the  angles 
and  distances  to  have  really  been,  of  May  22,  1836,  of  553".93,  if  reduced  to  the  mean 
distance  of  Saturn,  corresponds  to  a  radius  vector  of  8'  38. "07,  which  (considering  that  we  have 
no  knowledge  of  the  excentricity  of  the  orbit)  agrees  sufficiently  well  with  the  mean  elongation 
(8'  34". 8)  calculated  from  the  distance  of  Titan,  by  comparison  of  their  mean  motions.  In  this 
table  two  very  rude  measurements  under  most  unfavourable  circumstances,  on  April  25  and  26, 
1836,  have  been  rejected;  and  that  of  May  7,  1837,  ought  probably  to  be  so,  being  the  result 
of  a  single  difference  of  R  A  awkwardly  taken  with  the  20-feet. 


CHAPTER  VII. 


OBSERVATIONS  OF  THE  SOLAR  SPOTS. 

(417)  At  the  latter  end  of  1836,  and  during  the  first  half  of  1837,  the  spots  on  the  surface 
of  the  sun  were  extremely  remarkable,  not  only  for  number  and  size,  but  also  in  their  arrange- 
ment and  forms.  In  consequence,  during  the  interval  above  mentioned,  a  great  number  of 
drawings  were  made  of  the  sun's  disc,  by  projecting  the  image  formed  in  the  focus  of  an 
achromatic  finder  attached  to  the  equatorial,  for  which,  after  a  few  trials,  a  perspective  day 
telescope  of  twenty  inches  focus,  and  1.4  in.  aperture,  was  substituted  as  more  convenient. 
The  image  was  received  on  paper  pinned  on  a  screen  of  wood,  and  traced  with  pencil  with  one 
hand,  the  other  managing  the  right  ascension  handle  so  as  to  keep  the  preceding  limb  of  the 
sun  on  a  fiducial  line,  previously  drawn  on  the  paper,  and  the  centre  of  some  small  and  well 
defined  spot  on  a  fiducial  dot.  Where  the  right  ascension  motion  was  allowed  to  rest,  the  image 
of  this  spot  of  course  travelled  away  from  the  dot,  and  after  allowing  it  to  do  so  till  near  the 
edge  of  the  paper,  another  dot  was  made,  marking  its  new  place,  and  these  two  dots  being 
joined  by  a  straight  line,  gave  the  direction  of  the  diurnal  parallel  on  the  paper.  The  minuter 
details  necessary  to  effect  a  complete  resemblance  of  the  projection  to  the  actual  appearance  of 
the  spots,  with  their  penumbras,  &c,  were  then  worked  in  with  the  aid  of  the  telescope,  by 
hand,  as  an  eye-draft ;  as  well  as  magnified  representations  of  remarkable  spots,  faculse,  and 
other  particulars. 

(418)  I  consider  it  unnecessai'y  here  to  engrave  and  publish  all  these  drawings,  which 
would  entail  a  great  additional  cost  and  bulk  on  the  present  volume ;  but  in  case  it  should  ever 
be  considered  necessary  to  appeal  to  any  of  them  as  records  of  the  state  of  the  sun's  surface  at 
that  time,  I  annex  a  list  of  the  days  on  which  such  drawings  were  made  as  are  now  before  me. 
These  are  as  follows : 

1836—  Dec.  27,  31. 

1837—  Jan.  9,  10,  11,  12,  13,  14,  15,  16,  18,  19,  21,  23,  29;  Feb.  1,  2,  3,  5,  6,  7,  9,  10,  12,  13,  15,  20,  21,  22, 
23,  24,  26,  27, 28 ;  March  1,  3,  4,  6,  10,  12,  13,  14,  18,  19,  21,  22,  26,  27,  29,  31 ;  April  2,  3,  8,  10,  11,  13,  19,  21, 
25,  29 ;  May  5,  7,  9,  20,  21,  24,  25,  29  ;  June  8,  18,  25  ;  July  10,  12,  13,  14,  17,  19,  20,  25,  26,  28,  29 ;  August  4, 
7  ;  October  9,  10,  11,  17,  18,  24. 

It  were  much  to  be  wished  that  all  who  habitually  make  similar  projections,  would,  in  like 
manner,  place  at  least  on  record,  the  days  on  which  they  possess  drawings  of  the  spots,  in  order 
that  it  may  be  rendered  possible  (by  taking  a  certain  moderate  amount  of  trouble)  to  ascertain 
the  state  of  the  sun  by  actual  observation  on  any  given  day.    In  all  probability,  such  drawings 


* 


432  OBSERVATIONS  OF  THE  SOLAR  SPOTS. 

exist,  scattered  throughout  the  world,  if  not  for  every  day  of  every  year  for  some  years  past, 
yet,  for  a  much  greater  number  of  days  than  in  any  single  accessible  collection ;  and  next  to 
bringing  them  together,  and  forming  a  complete  history  of  the  changes  of  the  solar  surface,  the 
course  recommended  appears  the  most  advantageous. 

(419)  In  the  delineation  of  very  remarkable  spots,  a  magnified  image,  accompanied  and 
crossed  by  the  black  images  of  the  threads  of  the  micrometer  (adjusted  to  zero  of  position,  and 
opened  to  five  revolutions  of  the  screw,  or  2'  0".22),  was  formed  on  a  screen,  at  a  convenient 
distance  from  the  eye-piece  of  the  7-feet  achromatic,  and  brought  to  sharp  definition  by  properly 
adjusting  the  moveable  lens  of  the  eye-piece.  Thus,  the  form  of  the  spot,  its  dimensions,  and 
true  situation  as  respects  the  parallel  were  secured,  and  its  delineation  was  then  completed  by 
eye-draft,  under  a  magnifying  power  of  105  or  179,  as  the  state  of  the  atmosphere  would  allow. 
Several  of  these  delineations  are  presented  in  Plate  XVII.,  their  dates  being  as  follows  : — 

Jan.  18  . .  fig.  13  Feb.  20  .  fig.  2  Mar.  29  . .  fig.  3  July  26  . .  fig.  6. 
Jan.  29  . .  fig.  10  Feb.  28  . .  fig.  11  May  25  ..  fig.  9  July  28  . .  fig.  5. 
Feb.  5  . .  fig.  12  Mar.  19  . .  fig.  8  July  19  . .  fig.  4  July  29  . .  fig.  7- 
Feb.   9  . .  fig.  1 

(420)  These  figures  are  not  all  on  the  same  scale.  Not  having  been  so  drawn  originally 
(which  might  have  been  done,  but  would  have  recpiired  a  special  apparatus),  it  was  thought 
better  not  to  risk  their  correctness  in  copying  by  any  subsequent  alteration.  The  scale  of  each 
figure,  however,  is  sufficiently  indicated  by  the  distance  of  the  parallel  lines  representing  the 
micrometer  threads  crossing  it,  which  in  all  alike  is  2'.  As  these  drawings  sufficiently  express 
the  objects  they  are  intended  to  represent,  I  shall  only  draw  attention,  1st,  to  the  forms  of  those 
in  figs.  8  and  10,  as  highly  characteristic,  and  frequently  reproduced  on  the  sun's  surface  (as  it 
was  in  perfection  on  the  25th  of  May,  in  the  same  year)  ;  2ndly,  to  the  remarkable  radiated  or 
striated  apparent  structure  of  the  penumbra  in  that  of  fig.  9,  an  appearance  which  occurs  in 
many  of  M.  PastorfF's  engravings,  and  which  is  obviously  connected  very  intimately  with  the 
physical  cause  of  the  spots ;  3dly,  to  the  total  absence  of  all  penumbra  in  the  spots  adjacent  to 
the  large  one  in  fig.  1 2  ;  4thly,  to  the  occurrence  of  distinct  shades  in  certain  parts  of  the 
penumbrae  in  figures  1,  5,  7,  12,  and,  lastly,  to  the  immense  area  occupied  by  some  of  the  spots 
with  their  penumbrse  here  represented.  That  of  March  29,  for  instance,  in  fig.  3,  occupies 
(without  the  outlying  spots  at  the  tail  of  the  figure),  an  area  (such  as  may  fairly  be  included 
within  the  general  outline),  of  nearly  five  square  minutes.  Now  a  minute  in  linear  dimension 
on  the  sun  being  27,500  miles,  and  a  square  minute  756,000,000,  we  have  here  an  area  of 
3,780,000,000  square  miles  included  in  one  vast  region  of  disturbance,  and  this  requires  to  be 
increased  for  the  effect  of  foreshortening.  The  black  centre  of  the  spot  of  May  25  (fig.  9), 
would  have  allowed  the  globe  of  the  earth  to  drop  through  it,  leaving  a  thousand  miles  clear  of 
contact  on  all  sides  of  that  tremendous  gulph. 

(421)  We  are  naturally  led  to  inquire  for  an  efficient  cause — for  a  vis  motrix — to  give  rise 
to  such  enormous  dynamical  phenomena,  for  such  they  undoubtedly  are.  The  efficient  cause  of 
fluctuations  in  our  atmosphere,  in  terrestrial  meteorology,  is  apparent  enough;  viz.,  external 
agency— the  heating  power  of  the  sun.  Without  this,  all  would  be  tranquil  enough.  But  in 
the  solar  meteorology  we  have  no  such  extraneous  source  of  alternate  elevations  and  depressions 


OBSERVATIONS  OF  THE  SOLAR  SPOTS.  433 

of  temperature  altering  the  specific  gravity  and  disturbing  the  equilibrium  of  its  atmospheric 
strata.  The  cause  of  such  movements  as  we  observe,  and  upon  so  immense  a  scale,  must  there- 
fore reside  within  the  sun  itself,  and  it  is  there  we  must  seek  it. 

(422)  Now,  whatever  be  the  physical  cause  of  the  spots,  one  thing  is  certain,  that  they 
have  an  intimate  connection  with  the  rotation  of  the  sun  upon  its  axis.  The  absence  of  spots 
in  the  polar  regions  of  the  sun,  and  their  confinement  to  two  zones  extending  to  about  35° 
latitude  on  either  side,  with  an  intermediate  equatorial  belt  much  more  rarely  visited  by  spots, 
is  a  fact  notorious  in  their  history,  and  which  at  once  refers  their  cause  to  fluid  circulations, 
modified,  if  not  produced,  by  that  rotation,  by  reasoning  of  the  very  same  kind  whereby  we 
connect  our  own  system  of  trade  and  anti-trade  winds  with  the  earth's  rotation.  Having  given 
any  exciting  cause  for  the  circulation  of  atmospheric  fluids  from  the  poles  to  the  equator,  and 
back  again,  or  vice  veisa,  the  effect  of  rotation  will  necessarily  be  to  modify  those  currents 
as  our  trade  winds  and  monsoons  are  modified,  and  to  dispose  all  their  meteorological 
phenomena  on  a  great  scale  which  accompany  them  as  their  visible  manifestations,  in  zones 
parallel  to  the  equator,  with  a  calm  equatorial  zone  interposed.  It  only  remains,  therefore,  to 
inquire,  Whether  any  such  cause  of  circulation  can  be  found  in  the  economy  of  the  sun,  so 
far  as  we  know  and  can  understand  it  ?" 

(423)  Before  attempting  any  reply  to 
this  question,  I  would  observe  that  the  fact 
above  mentioned  —  the  distribution  of  the 
spots  in  two  moderately  broad  zones  parallel 
to  the  equator,  leaving  the  equator  itself  and 
the  poles  free — was  most  unequivocally  and 
beautifully  marked  during  a  great  part  of 
the  interval  embraced  by  my  observations. 
In  the  last  days  of  December  1836,  indeed, 
and  throughout  January  1 837,  as  also  from 
the  21st  to  the  26th  of  February,  both  in- 
clusive, even  the  most  unpractised  eye  could 
not  fail  to  perceive  by  the  mere  allineation 
of  the  spots,  the  situation  of  the  poles  and 
equator  of  the  sun,  without  watching  from 
day  to  day  their  progress  across  the  disc. 

See  marginal  fig.  which  represents  their  arrangement  on  Jan.  10,  1837. 

(424)  Recurring  now  to  the  question  whether  any  probable  or  possible  cause  can  be  assigned, 
from  what  we  know  of  the  sun's  economy,  capable  of  giving  rise  to  circulatory  movements  to  and 
from  its  poles,  in  the  fluids  which  cover  its  surface,  and  having  at  the  same  time  a  dependency  on 
its  rotation ;  it  may  be  observed  that  if  any  physical  difference  in  the  constitution  or  circum- 
stances of  its  polar  and  equatorial  regions  tend  to  repress  the  escape  of  heat  in  the  one,  and  to 
favour  it  in  the  other  of  these  regions,  the  effect  will  be  the  same  as  if  those  regions  were  un- 
equally heated  from  without,  and  all  the  phenomena  of  trade  winds,  mutatis  mutandis,  must  arise. 

(425)  It  has  been  a  matter  of  doubt  among  astronomers,  whether  the  sun  be  or  be  not 
surrounded  by  a  transparent  atmosphere  extending  beyond  its  luminous  surface.  Numerous 

5  s 


434  OBSERVATIONS  OF  THE  SOLAR  SPOTS. 

observations  made  under  the  most  favourable  circumstances  while  employed  in  these  delineations 
have  appeared  to  myself  quite  conclusive  as  to  its  reality.  The  deficiency  of  light  at  the  borders 
of  the  visible  disc  is  in  fact  so  striking,  whether  viewed  through  coloured  glasses  or  without 
their  intervention,  by  projecting  its  image  through  a  good  achromatic  telescope  on  white  paper, 
that  it  seems  surprising  it  should  ever  have  been  controverted.  The  extraordinary  phenomenon 
of  the  rose-coloured  solar  clouds  witnessed  during  the  total  eclipse  of  July  8,  1842,  which  must 
have  floated  in  and  been  sustained  by  an  exterior  transparent  atmosphere,  must  also  be  regarded 
as  definitively  settling  this  question  in  the  affirmative.  To  what  distance  beyond  the  visible  disc 
this  atmosphere  may  extend,  we  have  no  means  of  judging  accurately ;  but,  from  the  manner  in 
which  the  deficiency  of  light  alluded  to  comes  on,  being  by  no  means  sudden  on  approaching 
the  edge,  but  extending  to  some  distance  within  the  disc,  it  would  seem  to  be  considerable,  not 
merely  in  absolute  measure,  but  as  an  aliquot  part  of  the  sun's  radius.  Now,  granting  the 
existence  of  such  an  atmosphere,  its  form  in  obedience  to  the  laws  of  equilibrium  must  be  that 
of  an  oblate  spheroid,  the  ellipticities  of  whose  strata  differ  from  each  other  and  from  that  of 
the  nucleus.  Consequently,  the  equatorial  portions  of  this  envelope  must  be  of  a  thickness 
different  from  that  of  the  polar,  density  for  density,  so  that  a  different  obstacle  must  be  thereby 
opposed  to  the  escape  of  heat  from  the  equatorial  and  the  polar  regions  of  the  sun.  The  former, 
therefore,  ought,  according  to  this  reasoning,  to  be  habitually  maintained  at  a  different  tempe- 
rature from  the  latter. 

(426)  The  spots  in  this  view  of  the  subject  would  come  to  be  assimilated  to  those  regions  on 
the  earth's  surface  in  which,  for  the  moment,  hurricanes  and  tornadoes  prevail — the  upper 
stratum  being  temporarily  carried  downwards,  displacing  by  its  impetus  the  two  strata  of 
luminous  matter  beneath  (which  may  be  conceived  as  forming  an  habitually  tranquil  limit  between 
the  opposite  upper  and  under  currents),  the  upper  of  course  to  a  greater  extent  than  the  lower, 
and  thus  wholly  or  partially  denuding  the  opaque  surface  of  the  sun  below.  Such  processes 
cannot  be  unaccompanied  with  vorticose  motions,  which,  left  to  themselves,  die  away  by  degrees 
and  dissipate,  with  this  peculiarity,  that  their  lower  portions  come  to  rest  more  speedily  than 
their  upper,  by  reason  of  the  greater  resistance  below,  as  well  as  the  remoteness  from  the  point 
of  action,  which  lies  in  a  higher  region,  so  that  their  centre  (as  seen  in  our  water-spouts  which 
are  nothing  but  small  tornadoes)  appears  to  retreat  upwards.  Now  this  agrees  perfectly  with 
what  is  observed  during  the  obliteration  of  the  solar  spots,  which  appear  as  if  filled  in  by  the 
collapse  of  their  sides,  the  penumbra  closing  in  upon  the  spot  and  disappearing  after  it. 

(427)  An  appearance  frequently  noticed  in  the  course  of  these  observations,  but  which  I  do 
not  know  to  be  of  general  occurrence,  may  seem  at  first  sight  to  militate  against  this  idea. 
Lines  of  spots  of  more  or  less  extent,  or  connected  with  penumbral  trains  more  or  less  beset  with 
spots,  have  been  frequently  noticed  (as  in  the  annexed  figure,  which  represents  the  appearance 
in  question  on  Feb.  12,  1837,)  oblique  to  the  direction  of  parallels  of  latitude  on  the  sun's  surface, 
and  converging  on  both  sides  of  the  equator  towards  the  preceding  side  of  the  disc.  Again, 
instances  have  occurred  within  the  same  period,  frequent  enough  to  be  remarked,  of  the  peuum- 
brae  of  great  spots  in  what  may  be  considered  a  tumultuary  state  of  the  atmosphere,  being 
rounded  and  well  terminated  on  the  preceding  side,  but  ragged  and  ill-defined,  as  well  as  more 
extensively  effused  on  the  following,  where  they  would  often  take  the  form  of  great  trains,  and 
ultimately  in  the  progress  of  their  changes,  before  they  become  obliterated,  affect  the  form  of 


OBSERVATIONS  OF  THE  SOLAR  SPOTS. 


435 


pretty  long,  straight,  parallel  bands,  having 
the  same  obliquity  to  the  sun's  equator  and 
its  parallels  as  the  lines  of  spots  above  men- 
tioned. The  great  spot  of  March  29  (fig. 
3),  affords  a  tolerable  example  of  this,  though 
less  strongly  marked  than  in  some  other 
instances.  Now,  the  direction  of  such  bands 
and  lines  is  transverse  to  the  course  of  the 
currents  which  the  dynamical  theory  above 
suggested  supposes.  They  must,  therefore, 
be  assimilated  rather  to  ripple  marks  which 
are  transverse  to  the  direction  of  the  general 
movement  to  which  they  owe  their  origin, 
than  to  trails  drawn  out  by  a  current  in 
its  own  direction,  if  indeed  the  appearances 
in  question  be  anything  more  than  acci- 
dental. 

(428)  It  may,  perhaps,  be  allowed  me  here  to  remark  on  a  character  of  the  solar  spots  in 
general,  which,  though  so  universal  and  so  striking  as  to  be  perfectly  familiar  to  every  observer, 
and  to  form  in  fact  an  essential  and  integrant  part  of  their  phenomena,  has  not  yet,  nevertheless, 
so  far  as  I  am  aware,  had  drawn  from  it  exactly  that  conclusion  which  seems  to  me  inevitably  to 
follow  from  it.  I  allude  to  the  definite  and  intense  blackness  of  the  spot 11  nucleus'''  or  "opening," 
as  it  has  been  termed,  as  contrasted  with  the  Penumbra  or  "  Shallow"  surrounding  it.*  This  want 
of  graduation — this  sharply  marked  suddenness  of  transition,  is  altogether  opposed  to  the  concep- 
tion of  a  susceptibility  of  indefinite  and  easy  mixture  in  the  luminous,  non-luminous,  and  semi- 
luminous  constituents  of  the  solar  envelope.  Were  they  so  susceptible  there  seems  no  reason 
why  spots  should  not  be  seen  of  every  possible  shade  of  darkness,  from  a  barely  perceptible 
deficiency  of  light  to  absolute  blackness,  or  why  one  stage  of  mixture  should  be  more  habitually 
prevalent  than  another.  It  is  true  we  see  bridges  of  light,  as  it  were,  across  the  spots,  and  these 
may  sometimes,  though  very  rarely,  form  so  fine  a  net-work  as  here  and  there  to  give  the 
appearance  of  a  partial  illumination,  and  on  very  rare  occasions  the  spots  have  been  described  as 
nebulous  or  hazy.f  But,  looking  to  the  broad  fact — the  spots  are  black — the  penumbra  a  nearly 
uniform  half  shadow,  with,  however,  here  and  there,  undeniable  definite  spaces  of  a  second  depth 


*  The  great  importance  of  a  systematic  and  continuous  series  of  observations  of  the  solar  spots  cannot  be 
too  strongly  insisted  on.  One  observer,  though  gifted  with  the  diligence  and  perseverance  of  a  Pastorff,  is  not 
enough.  Many  are  necessary — and  especially  in  habitually  sunny  regions  of  the  globe — to  secure  an  unbroken 
history  of  their  appearances.  And  now  that  clock- movements  have  been  applied  to  our  equatorials,  and  that 
photographic  delineation  can  supply,  in  the  utmost  perfection,  the  talent  of  the  draftsman,  it  were  much  to  be 
wished  that  the  subject  were  seriously  taken  up  as  part  of  the  regular  business  of  observatories.  An  interchange 
of  copies  might  perhaps  take  place,  without  recourse  to  the  engraver,  by  the  aid  of  the  Kalotype  process  of  Mr. 
Talbot,  to  any  moderate  and  useful  extent. 

t  See  Phil.  Tr.  1795,  p.  57- — But  as  on  this  occasion  all  the  spots,  indiscriminately,  are  declared  to  be  so 
affected,  there  is  room  to  apprehend  some  instrumental  or  atmospheric  cause  of  illusion  to  have  prevailed. 


436 


OBSERVATIONS  OF  THE  SOLAR  SPOTS. 


of  shade,  as  shown  in  some  of  the  figures  annexed.  There  is  no  gradual  melting  of  the  one 
shade  into  the  other — spot  into  penumbra — penumbra  into  full  light.  The  idea  conveyed  is 
more  that  of  the  successive  withdrawal  of  veils — the  partial  removal  of  definite  films,  than  the 
melting  away  of  a  mist,  or  the  mutual  dilution  of  gaseous  media.  Films  of  immiscible  liquids 
having  a  certain  cohesion,  floating  on  a  dark  or  transparent  ocean  and  liable  to  temporary 
removal  by  winds,  would  rather  seem  suggested  by  the  general  tenor  of  the  appearances,  though 
they  are  far  from  being  wholly  explicable  by  this  conception,  at  least  if  any  considerable  degree 
of  transparency  be  allowed  to  the  luminous  matter. 

(429)  In  delineating  the  spots  here  figured,  the  7-feet  achromatic  only  was  used ;  and 
although,  generally  speaking,  the  definition  of  the  sun  with  this  instrument  is  much  inferior  to 
that  afforded  by  a  Newtonian  reflector  of  equal  focus  and  6  inches  aperture,  yet,  on  many  occa- 
sions, the  distinctness  of  vision  obtained,  under  what  might,  a  priori,  be  considered  very  unfavour- 
able circumstances,  has  been  not  a  little  remarkable.  Looking  northward,  over  a  burning  tract 
of  many  miles  in  extent  (often  heated  to  140°  or  150°  Fahr.),  and  on  some  occasions  with  a  hot 
wind  from  the  north-west  of  extreme  aridity,  a  tranquillity  and  perfection  of  vision  was  expe- 
rienced which  was  never,  or  very  rarely  indeed,  obtained  at  nigkt  at  the  same  altitude  in  that 
direction  (as  has  been  already  remarked  on  the  occasion  of  the  observations  of  y  Virginis). 

(430)  The  combination  of  coloured  glasses  employed  in  these  delineations  was  a  triple  one, 
consisting  of  two  green  glasses,  between  which  a  blue  one  coloured  by  cobalt  is  interposed.  This 
I  can  recommend  as  by  far  the  most  agreeable  of  any  which  I  have  tried  for  long-continued 
inspection  of  the  sun.  Occasionally  (but  not  for  purposes  of  delineation)  I  may  mention  having 
at  various  times  employed  with  a  6-inch  Newtonian  reflector,  in  place  of  the  ordinary  small 
metallic  speculum,  one  of  plate  glass,  with  good  effect.  A  6-inch  glass  speculum  (the  same 
mentioned  in  Phil.  Trans.,  1803,  p.  214)  has  proved  less  advantageous  than  I  should  have,  a 
priori,  expected,  the  cause  of  which,  however,  would  appear  to  arise  from  the  circumstance  of 
its  posterior  surface  being  roughened  and  blackened  to  take  off  any  disturbing  reflexion.  In  conse- 
quence, a  great  distortion  of  figure  arises,  owing  to  that  surface  becoming  speedily  and  strongly 
heated.  This  inconvenience  might  doubtless  be  entirely  done  away  with,  by  grinding  and  polish- 
ing that,  as  well  as  the  anterior  surface,  to  a  concave  spherical  curve  of  a  considerably  smaller 
radius  of  curvature  than  the  focal  length  of  the  effective  reflecting  surface.  In  this  arrangement 
about  95  per  cent,  of  the  light  would  be  freely  transmitted  (and  ought  not  to  be  stopped 
by  any  back  to  the  speculum  or  even  to  the  tube  of  the  telescope,  but  permitted  to  escape  into 
the  air).  As  regards  the  portion  (about  2|  per  cent,  of  the  incident  beam)  reflected  from  the 
posterior  surface,  being  incident  on  a  convex  internal  surface  of  considerable  curvature,  these  rays 
would  be  dispersed  and  so  enfeebled  as  to  have  no  material  influence  on  the  distinctness  of  the 
image  formed  in  the  focus  of  the  first  surface,  a  result  greatly  favoured  by  both  the  refractions  at 
that  surface  which  they  have  to  undergo,  as  a  very  little  consideration  of  the  course  of  the  rays 
suffices  to  show.  The  image  formed  by  the  first  surface,  being  received  by  a  small  plane  glass 
reflector,  will  (if  the  reflexion  from  the  second  surface  of  that  mirror  be  also  got  rid  of*)  be 


*  To  do  this,  the  small  mirror  should  hy  no  means  he  roughened  or  blackened  at  the  hack.  It  should  be  in 
fact  a  prism  of  crown  glass  with  a  refracting  angle  of  at  least  28°  8',  the  edge  heing  towards  the  eye —  and  set 
transparent  (<'.  e.  without  a  metal  hack  to  arrest  the  transmitted  light).    In  this  arrangement,  no  ray  but  those 


OBSERVATIONS  OF  THE  SOLAR  SPOTS. 


437 


finally  reduced  before  reaching  the  eye-glass  to  little  more  than  -g^th  part  of  their  original 
intensity,*  and  will  therefore  require  no  darkening  glass,  or  but  a  very  slightly  tinted  one ;  and 
all  danger  of  its  cracking  will  be  completely  obviated.  This  arrangement  I  have  not  had  an 
opportunity  to  put  to  the  test  of  experience,  but  it  appears  very  well  worthy  of  trial. 

(431)  During  the  months  embraced  by  these  observations,  the  state  of  the  sun  seemed 
evidently  undergoing  a  gradual  alteration,  in  the  nature  of  a  subsidence  from  violent  agitation 
to  comparative  tranquillity.  Although  rich  in  spots  during  the  whole  of  January,  it  was  only 
from  the  23rd  of  that  month  to  the  end  of  March,  that  these  large  effused  spots  of  complex 
structure  and  great  penumbral  trains  (specimens  of  which  are  figured  in  figs.  1,  2,3,  8,  10,  11, 
12)  continued  to  be  formed  in  copious  succession.  From  that  date  forward,  the  character,  as 
well  as  the  abundance  of  spots,  was  greatly  changed.  During  April  and  May,  rounded  and 
well-defined  forms  were  chiefly  affected,  one  spot  only  of  the  very  peculiar  character  of  fig.  10 
being  exhibited  (May  5-7),  which,  however,  broke  up  into  round  spots  without  any  great 
penumbral  effusion ;  and  one  considerable  group  from  the  19th  to  the  25th  of  April,  which 
may  be  considered  as  belonging  to  and  terminating  the  series  of  "  confluent  spots,"  as  those  in 
question  may  be  termed.  During  April  and  May,  the  spots  were  also  fewer  in  number.  In 
June  and  July  they  became  again  more  abundant ;  but  the  character  they  then  affected  was 
rounded  and  compact,  without  any  tendency  to  those  broadly  effused  irregular  penumbrae  which 
formed  so  very  remarkable  a  feature  in  February  and  March ;  while  in  August  and  October, 
so  far  as  observed,  the  sun  seemed  to  have  passed  into  a  quiescent  state,  the  spots  being  few, 
small,  and  irregularly  disposed. 


regularly  reflected  from  its  first  surface  at  45°  going  to  form  the  useful  image,  could  find  its  way  to  the  eye-piece, 
all  other  would  pass  out  into  the  air  at  the  mouth  of  the  tube,  or  be  returned  to  the  sun  by  re-reflection  at  the 
great  speculum,  &c.  No  care  need  be  bestowed  on  figuring  the  posterior  surfaces  of  either  speculum.  It  suffices 
that  both  be  well  polished. 

*  Adopting  Bouguer's  estimates  of  the  light  reflected  from  glass  at  different  incidences. —  Traite  cTOpttque, 
page  137. 


APPENDIX. 


APPENDIX  A. 

On  the  Numerical  Magnitudes  of  certain  Stars,  as  obtained  by  subsequent  Observation  on  the 
principle  of  Sequences,  in  the  Northern  Hemisphere,  compared  and  combined  with  those 
of  the  same  Stars  as  observed  in  the  Southern ;  and  of  some  others  lohose  Places  in  the 
scale  of  Magnitudes  are  directly  deducible  from  these  by  interpolation  of  the  Sequences. 

(432)  Circumstances  rendering  it  highly  improbable  that  the  series  of  northern  sequences 
alluded  to  in  Art.  255  will  be  further  prosecuted  (at  least  by  myself),  I  have  thought  it 
advisable  here  to  annex  so  much  of  the  results  of  those  observations  as  shall  serve  for  an 
effectual  basis  of  connexion  between  the  northern  and  southern  numerical  nomenclature,  and 
at  the  same  time  afford  more  dependable  values  to  several  stars  which  are  very  imperfectly 
determined  in  our  Synoptic  Table  C,  p.  341,  being  there  concluded  from  single  observations, 
or  in  that  imperfect  manner  which  is  indicated  by  the  annexation  of  one  or  two  asterisks 
(see  Art.  254).  The  following  list  of  139  stars  above  the  4th  magnitude  is  arranged  in  order 
of  apparent  magnitude,  solely  by  the  result  of  the  northern  sequences  in  question.  The  first 
column  contains  the  name  of  the  star ;  the  second,  its  magnitude  in  the  Astronomical  Society's 
Catalogue;  the  third,  its  magnitude  in  our  Synoptic  Table  C,  derived  from  the  southern 
sequences ;  the  fourth,  the  result  of  a  graphical  interpolation  conducted  on  a  principle  explained 
below ;  and  the  fifth,  the  magnitude  finally  to  be  adopted,  in  preference  to  and  exclusion  of  any 
magnitude  previously  assigned  to  the  same  star  in  any  of  the  previous  sequences  and  lists  in  this 
work,  where  they  differ.  Notes  of  interrogation  (?)  annexed  to  the  numbers  in  column  3, 
indicate  that  the  stars  in  question  belong  to  the  imperfectly  determined  ones  in  Table  C, 
as  above  alluded  to. 


440 


APPENDIX. 


Star's  Name. 


Sirius   

Arcturus  

Capella   

a  Orionis  (max)  

Rigel   

Lyra   

Procyon   , 

Aldebaran   

Antares   

a  A c  | in U ■  

Spica   

Pollux  

Fomalhaut   

Regulus   

a  Cygni   

Castor  

a  Ursa?  (var.)   

t  Ursa?  (var.)  

a  Persei   

t  Orionis  

£  Orionis  , 

il  Ursa?  (var.  ?)   

(3  Tauri   

y  Orionis   

(3  Ursae  Minoris  (var.) 

a  Polaris  

y  Leonis  

£  Ursa;   

a  Hydra;  

a  Arietis  

(3  Andromedae   

/3  Auriga;   

y  Andromeda;  

y  Cassiopeia;   

a  Andromeda;  ., 

a  Cassiopeia;   

y  Geminorum  

(3  Leonis  

Algol  (max.)  

y  Draconis  

a  Ophiuchi  

(i  Cassiopeia;   

r  Cygni   

(3  Canis   

k  Orionis  

a  Ceti  

a  Pegasi  , 

(3  Pegasi  

8  Orionis  

£  Pegasi   , 

a  Corona;   

y  Ursae   i 

j3  Ursae   , 

S  Scorpii  

£  Bootis  , 

a  Sagittarii  

£  Cygni   

"  a  Cephei  

a  Serpentis  

8  Leonis  

7]  Bootis  

y  Aquilse   

8  Cassiopeia;   

8  Ophiuchi  , 

r)  Draconis  , 

tj  Ophiuchi  

0  Draconis  , 

j3  Arietis  

y  Pegasi  


Mag. 
A  S  C. 


i.o 
3.0 

1-  5 

3.0 
2.5 

2-  5 

3-  o 

a-S 
2.0 
2.0 
3.0 
2.5 
2.0 
3.0 
4.0 

3° 
2.0 
2.0 

3-5 
3.0 
1.0 
3.0 
3.0 

*-5 
2.5 
2.0 
2.0 
2.5 
3.0 
2.5 
3.0 

2-5 
2.0 
2.0 
2.0 

2-  5 

2.0 
2.0 
2.0 

3-  ° 
3.0 

3-° 
3.0 
3.0 

2-5 
3.0 
3.0 
3.0 
3.0 
3.0 
3.0 
2.5 
2.0 
3.0 
2-5 


Mag. 
Table  C. 


1.95  ? 
1.99 
1.94 
1.88 


2.01 
2.13  ? 
2.34 
2.10 
2.46 

2-59 
2.34 
2.50 
2.30 
2.40 

2.51  ? 


2.25  ? 

2.51 
2.63 


2.67 


2.58 
2.59 
3.14? 
2.65  ? 
2.78  ? 

2. 6l 
2.56 
2.63  ? 
2.71 
2.77 

2.86 
2.71 
2.41 


3.14? 
2.92 
3.06 
3.07  ? 

3.00  ? 

2.89  ? 

3  -49  ? 
3.05  .' 


Interp. 
Mag. 


1.90 
1.94 
I.98 
2.02 
2.07 
2.10 
2.14 
2.l8 
2.22 
2.26 
2.28 
2.30 

2-34 
2.37 
2.41 
2.43 
2.45 
2.48 
2.50 
2.52 
2.54 
2.57 
2.59 
2.61 
2.62 
2.62 
2.63 
2.63 
2.63 
2.63 
2.64 
2.64 
2.65 
2.65 
2.66 
2.67 
2.69 
2.71 
2.76 
2.78 
2.80 
2.84 
2.88 
2.90 
2.92 
2.94 
2.96 
2.98 
2.99 
3.00 
3.02 
3.04 
3.06 
3.09 
3. 11 


Adopted 
Mag. 


1.90 
I.94 
1.96 
I.95 
2.07 
I.97 
2.07 
2.18 
2.28 
2.18 
2.28 
2.30 
2.34 
2.43 
2.30 
2.40 

2-45 
2.48 
2.50 
2.52 
2.54 
2.57 
2.59 
2.63 
2.62 
2.62 
2.63 
2.63 
2.63 
2.58 
2.59 
2.82 
2.65 
2.65 
2.61 
2.62 
2.69 
2.71 
2.77 
2.86 
2.80 
2.41 
2.88 
2.90 
2.92 
2.94 
3.01 
2.98 
2.99 
3.00 
3.02 
3.04 
3.06 
3.09 
3. 11 


Star's  Name. 


y  Corvi   

(3  Corvi   

6  Auriga; 
(3  Herculis  .... 
y  Virginis  .... 
£  Ophiuchi  ... . 
a  Cor  Caroli  . . 
(3  Ophiuchi .... 

8  Cygni   

8  Capricorni  . . 

£  Persei   

£  Persei   

£  Herculis 

1  Aurigae  

y  Ursae  Minoris 

tj  Pegasi  

£  Aquilae  .... 

P  Cygni  

y  Persei  

j3  Trianguli .... 

8  Persei   

a  Aquarii  .... 
(3  Aquarii  .... 
8  Aquarii  .... 
£  Draconis  .... 
7r  Herculis  .... 
8  Draconis  .... 

y  Bootis  

8  Herculis  .... 

f3  Cephei  

(3  Capricorni  . . 

r  Lyrae   

y  Cephei  

£  Cassiopeia;  . . 
6  Aquilae  .... 
8  Andromeda; . . 

£  Pegasi  

£  Cygni   

a  Trianguli  Bor. 

X  Aquilae  

t  Draconis  .... 

fi  Pegasi  

X  Draconis  .... 
■q  Cassiopeiae  . . 

6  Pegasi  

8  Aquilae  .... 
7r  Sagittarii  .... 

£  Cephei  

t)  Cephei  

X  Sagittarii  .... 
(3  Delphini  .... 
a  Delphini  .... 
1  Herculis  .... 
a  Draconis  .... 

1  Cephei  

tj  Serpentis .... 
t  Sagittarii  .... 

e  Aquarii  

y  Ophiuchi  .... 

y  Delphini  .... 

£  Sagittarii  .... 

£  Aquarii ...... 

y  Capricorni  . . 
y  Aquarii  .... 

y  Piscium  .... 

I  Draconis  .... 

(3  Aquilae  

X  Draconis  . . . . 


Mag. 
A  S  C. 

Mag. 
Table  C. 

Interp. 
Mag. 

Adopted 
Mag. 

3.0 

2.90 

3.13 

2.90 

2-5 

2.95 

315 

2.95 

4.0 



3.17 

3-17 

2.5 

3.02 

3.18 

3.18 

4.0 

3.08 

3.20 

3.14 

3-5 

2.97  ? 

3.21 

3.21 

2-5 

3.22 

3.22 

3.22 

3.0 

.... 

3.23 

3.23 

3-5 

3.24 

3.24 

3-5 

3.20  ? 

3.25 

3.25 

3-5 

3.26 

3.26 

3-5 

3.27 

3.27 

3.0 

3.28 

3.28 

4.0 

3.29 

3.29 

3-5 

3.30 

3.30 

3.0 

.... 

3-3» 

3-31 

3.0 

3-45  ? 

3.32 

3-32 

3.0 

3-33 

3-33 

4.0 



3-34 

3-34 

4.0 

3-35 

3-35 

3-5 

.... 

3.36 

3.36 

3.0 

2.97  ? 

3-37 

3.2  ? 

3.0 

2.85  ? 

3.38 

3.2? 

3.0 

3.80 

3-39 

3.60 

3.0 

.... 

3.40 

3.40 

3-5 

3.41 

3.41 

3.0 

3.3V? 

3.42 

3.42 

35 

3-43 

3-43 

4.0 

3-44 

3-44 

3.0 



3-45 

3-45 

3-5 

3.32? 

3.46 

3.40 

3.0 

3-47 

3-47 

3.0 

.... 

3.48 

3.48 

3-5 

.... 

3-49 

3-49 

3.5 

3-57  ? 

3.50 

3.50 

3.0 

.... 

3Si 

3Si 

3.0 

3.52 

5.32 

3.0 

.... 

3-53 

3-53 

3-5 

3-54 

3-54 

3.0 

3-57  •' 

3-55 

3-55 

3.0 

.... 

3.56 

3.56 

4.0 

.... 

3-57 

3-57 

4-5 

3-58 

3.58 

4.0 

3-57 

3-57 

4.0 

3.60 

3.60 

3-5 

3.64? 

3.61 

3.61 

4-5 

3.40 

3.62 

3.40 

4.0 

3.64 

3.64 

3-5 

3-65 

3-65 

4.0 

3-»3? 

3.66 

3.2  ? 

4.0 

3.67 

3.67 

3-5 

3.68 

3.68 

4.0 

3.70 

3.70 

3-5 

3.71 

3.71 

4.0 

3-73 

3-73 

4.0 

3-sV? 

3-74 

3.6? 

4.0 

3.76 

3.76 

4-5 

3-77 

3-77 

4.0 

3-79 

3-79 

4.0 

3.80 

3.80 

5.0 

2.82 

3.82 

4.0 

3.83 

3.83 

4.0 

3.98? 

3.86 

3.86 

4.0 

3.88 

3.88 

4-5 

3.89 

3.89 

3-5 

3.91 

3.91 

3-5 

3.92 

3.92 

3-5 

3-94 

3-94 

APPENDIX. 


441 


(433)  It  cannot  be  expected  that  two  lists  arranged,  the  one  in  the  northern  and  the 
other  in  the  southern  hemisphere,  should  agree,  except  in  respect  of  stars  which  attain  a 
considerable  altitude  at  either  station  ;  and  we  accordingly  find  that  low  stars  (in  our 
latitudes),  such  as  a  Hydra,  8  Scorpii,  /3  and  y  Corvi,  a-,  -n,  and  A.  Sagittarii,  stand  lower  in 
this  list  than  they  undoubtedly  ought,  and,  vice  versa,  that  some  stars,  high  in  our  horizon, 
but  low  in  respect  of  that  of  the  southern  station  of  observation,  such  as  Polaris,  a  Andromeda?, 
j3  Pegasi,  /3  Arietis,  higher  in  comparison  with  the  general  mass.  In  the  column  of  adopted 
magnitudes,  regard  is  had  to  this  by  the  preference  of  the  result  obtained  at  the  most 
favourable  station,  wherever  cases  of  conflict  arise  between  values  without  a  ?  attached. 

(434)  In  the  interpolation  of  these  values,  the  values  of  Table  C  have  been  used  so  far 
as  they  could  be  used  with  perfect  security — that  is,  as  far  as  about  the  magnitude  3.3. 
Beyond  this  point  they  have  been  (not  supplanted,  but)  aided  by  the  catalogued  magnitudes, 
in  the  manner  explained  in  Art.  243,  with  whose  indications  they  coincide  very  well,  except 
in  the  cases  of  low  stars.  And,  on  the  whole,  I  doubt  not  that,  within  the  range  of  magni- 
tudes embraced  in  this  list,  the  connexion  of  the  northern  with  the  southern  nomenclature 
will  be  found  practically  established  to  the  satisfaction  of  astronomers. 


APPENDIX  B. 

On  the  Difference  of  Level  between  the  Royal  Observatory  C.  G.  H.  and  Feldhausen. 

(435)  The  Observatory  barometer  with  which  mine  has  from  time  to  time  been  compared 
is  that  by  Jones,  fixed  to  the  pier  of  the  mural  circle.  The  height  of  its  cistern  above  the 
floor  is  2  feet  6  inches,  and  above  the  level  of  the  sea  about  32  feet. 

The  barometer  of  comparison  was  a  portable  one  by  Troughton,  the  same  which  has 
accompanied  me  in  all  my  expeditions,  and  which  was  sent  out  by  me  in  charge  of  the  late 
Professor  Henderson,  for  the  purpose  of  ascertaining  the  difference  of  zero  points  between 
the  standard  barometer  of  the  Royal  Society  (R)  and  the  mural  circle  barometer  (J)  above 
mentioned,  which  he  thus  ascertained  to  be  as  follows  : — 

1832.  By  first  comparison— Going  out  from  London  to  C.  G.  H.      .       .       •       J  =  R  +  0*009 

1833.  By  second    ditto    —Returning  from  C.  G.  H.  to  London     .       .       .       J  =  R  +  0.007 

Mean,  J  =  R  +  0.008 ;  the  portable  barometer  thus  appearing  to  have  preserved  a  very 
satisfactory  fixity  of  its  zero  point  during  the  interval,  including  both  voyages.  During  the 
voyage  homeward,  Mr.  Henderson  took  the  opportunity  of  comparing  this  barometer  with 
that  of  the  Observatory  at  St.  Helena,  then  under  the  direction  of  Lieut.  Johnson,  which  was 
thus  ascertained  to  read  0.026  higher  than  the  standard  of  the  Royal  Society. 

(436)  Previous  to  embarking  for  the  Cape,  I  procured  the  same  barometer  to  be  com- 
pared with  that  of  the  Royal  Society  above  mentioned  (the  standard  constructed  by  Professor 
Daniell),  the  result  of  which  comparison  was  R  =  H  +  0.050,  1833,  Oct.  10. ..23,  A.  Com- 
parison with  the  Observatory  barometer  made  soon  after  my  arrival  at  the  Cape,  viz.  from 

5  u 


442 


APPENDIX. 


March  26  to  April  4,  1834,  gave  J  =  H  +  0.055,  whence  J  =  R  +  0.005.  These  three 
determinations,  whose  mean  is  +  0.007,  satisfactorily  prove  the  fixity  of  zero  of  the  Cape 
barometer;  the  differences,  though  regularly  progressive,  being  too  minute  to  be  calculated 
upon  as  certain. 

(437)  The  observations  by  which  the  difference  of  level  between  the  Observatory  and 
Feldhausen  has  been  determined,  were  those  taken  at  both  stations  during  the  hourly 
meteorological  observations  at  the  equinoxes  and  solstices,  during  such  term  days  as  admit 
of  a  perfectly  satisfactory  comparison,  both  from  circumstances  of  weather  and  from  a  direct 
intercomparison  of  instruments  free  from  all  doubt  of  change  in  the  intervals — a  condition 
rendered  necessary  by  having  been  obliged,  on  more  than  one  occasion,  to  refill  the  portable 
barometer,  by  reason  of  accidents.  The  term  days  selected  are  those  of  the  21st  and  22nd 
Dec.  1834,  June  and  Dec.  1835;  March  and  June,  1836;  and  June  and  September,  1837; 
and  the  results  are  as  follows : — 


Dec. 
1834. 

June, 
1835. 

Dec. 
1835. 

March, 
1836. 

June, 
1830. 

June, 
1837. 

Sept. 
1837. 

Mean  difference  of  barom.  readings  reduced  to  32 

26 
69.6 
O.170 

37 
54.0 
0.188 

-0.059 

34 
68.6 
O.199 
—  O.078 

3+ 
65.1 
0.196 
— 0.062 

31 
53.8 
0.201 
—0.078 

35 
56.1 
0.263 
-0.149 

36 

55-4 
0.273 
-0.149 

O.I  I  I 

97.13 
+8.13 

0.129 
1 12.87 

+5-5* 

O.I2I 
IO5.87 
+  8.62 

O.134 
103.25 
+  7.60 

0.123 
107.62 
+  5.21 

O.I  12 

98.00 

+  S-2S 

0. 124 
108.50 
+  5.64 

105.26 

118.39 

1 14.49 

117.25 

112.83 

103.25 

1 14. 14 

The  mean  of  these  seven  results  gives  112.23  feet  for  tbe  difference  of  level  between 
the  cisterns  of  the  barometers  at  the  Observatory  and  at  Feldhausen,  the  latter  being  the 
higher. 


APPENDIX  C. 

On  the  Temperature  acquired  by  the  Surface  Soil  under  Exposure  to  clear  Sunshine,  and  some 
other  Effects  of  Accumulated  Solar  Radiation ;  and  on  the  Quantity  of  Heat  given  out 
by  the  Sun.      Suggestion  of  an  Improvement  on  the  Ice  Calorimeter. 

(438)  In  Art.  429,  the  temperature  acquired  by  the  surface  soil  of  the  sandy  region 
called  the  Cape  Flats,  intervening  between  table  and  false  bays,  is  stated  to  amount  frequently 
to  140°  or  150°  Fahr.  That  this  is  no  exaggeration,  the  following  experiments  on  thermo- 
meters variously  exposed  will  show  : — 

Oct.  30,  1837.    At  2h  51m  apparent  time,  p.m.,  the  sun's  rays  being  already  oblique,  the  following  tempe- 
ratures were  taken  : —  0 
Thermometer  just  immersed  in  a  heap  of  earth  cast  up  by  ants,  and  quite  dry    ....  125 


APPENDIX. 


443 


In  a  convex  heap  of  sandy  soil,  in  a  small  garden  enclosure  sheltered  from  wind,  and  moist  0 

at  three  or  four  inches  below  the  surface  143 

In  contact  with  a  stem  of  Albuca  viridifiora  in  flower,  at  half  an  inch  below  the  surface     .       .  120 
Nov.  7,  1837-    2h  23"'  p.m.  app.  time.    Temperature  of  a  heap  of  garden  mould  just  below  the  surface     .  155 

Under  the  still  green  leaf  of  Brunswickia  multiflora  96 

In  contact  with  the  stem  of  a  tuberous  Pelargonium  in  full  flower,  just  below  the  surface  .  .  131 
Inserted  an  inch  into  the  moist  and  decaying  crown  of  Hcemanthus  Tigrinus  losing  its  leaves    .  102 

Nov.  24,  1837.    lh  45m  p.m.  app.  time.    Temperature  of  a  heap  of  garden  mould  145-5 

Dec.  I,  1837.    0h  36"  p.m.     In  a  sand  heap  sheltered  from  wind,  in  the  small  garden  enclosure 

above  mentioned  162 

Dec.  3,  1837-    0h  21™  p.m.    Thermometer  in  the  sun,  supported  1\  inches  above  the  soil  of  a  hard 

trodden  sandy  path  A  =  117-5 

Buried  a  quarter  of  an  inch  deep,  in  contact  with  a  seedling  fir  of  this  year's  growth, 

quite  healthy  B  =  148.2 

Temperature  of  air  at  same  time  in  shade  C  =  88.5 

Wet  bulb  thermometer.    Same  exposure  D  =  64.6 

1"  30"  p.m.    Same  exposures    .       .       .  A  =  118.0,  B  =  149.8,  C  =  90.5,  D  =  63.5 

V  50-  p.m.  „  .    A=  121.0,  B  =  150.8,  C  =  90.5,  D  =  65.5 

2h  44m  p.m.  „  ....     A  =  114.8,  B  =  148.0,  C  =  90.0,  D  =  63.5 

4"  12m  p.m.  „   A  =  107.5,  C  =  84.5,  D  =  63.5 

Dec.  5,  1837.    lh  15m  p.m.    External  thermometer  in  shade  E  =  98 

Wet  bulb  thermometer  also  in  shade  F  =  68.5 

Thermometer  under  the  soil  of  the  garden   G  =  159 

1"  57"  p.m   E  =  95.5,  F  =  68.5,  G  =  159 

„  2"  57-  p.m  E  =  91.5,  F  =  68.5,  G  =  150 

4-  13"'  p.m  E  =  91.2,  F  =  70.5,  G  =  119 

„  5h  0"  p.m.    Temperature  of  soil  (long  since  shaded),  at  four  inches  below  the  surface,  102 

(439)  When,  however,  the  heat  communicated  from  the  sun  is  confined  and  prevented 
from  escape,  and  so  forced  to  accumulate,  very  high  temperatures  are  attained.  Thus,  in 
a  small  mahogany  box  blackened  inside,  covered  with  window-glass  fitted  to  the  size,  but 
without  putty,  and  simply  exposed  perpendicularly  to  the  sun's  rays,  an  enclosed  thermometer 
marked,  on  Nov.  23,  1837,  149° ;  on  Nov.  24,  146°,  150°,  152°,  &c.  &c.  When  sand  was 
heaped  round  the  box,  to  cut  off  the  contact  of  cold  air,  the  temperature  rose  on  Dec.  3,  1837, 
to  177°.  And  when  the  same  box,  with  its  enclosed  thermometer,  was  established  under  an 
external  frame  of  wood  well  sanded  up  at  the  sides,  and  protected  by  a  sheet  of  window-glass 
(in  addition  to  that  of  the  box  within),  the  temperatures  attained  on  Dec.  3,  1837,  were — 
at  lh  30m  p.m.  (Appar.  T.)  207°.0 ;  at  lh  50m,  217°.5  ;  and  at  2"  44m,  218°,  and  that  with  a 
steady  breeze  sweeping  over  the  spot  of  exposure.  Again  on  Dec.  5,  under  a  similar  form 
of  exposure,  temperatures  were  observed  at  0h  19m  of  224° ;  at  0h  29m,  230°;  at  lh  15m,  239°; 
at  lh  57m,  248°;  and  at  2h  57m,  240°.5.  As  those  temperatures  far  surpass  that  of  boiling 
water,  some  amusing  experiments  were  made  by  exposing  eggs,  fruit,  meat,  &c,  in  the  same 
manner  (Dec.  21,  1837,  et  seq.),  all  of  which,  after  a  moderate  length  of  exposure,  were 
found  perfectly  cooked — the  eggs  being  rendered  hard  and  powdery  to  the  centre  ;  and  on 
one  occasion  a  very  respectable  stew  of  meat  and  vegetables  was  prepared,  and  eaten  with 
no  small  relish  by  the  entertained  bystanders.  I  doubt  not,  that  by  multiplying  the  enclosing 
vessels,  constructing  them  of  copper  blackened  inside,  insulating  them  from  contact  with  each 


444 


APPENDIX. 


other  by  charcoal  supports,  surrounding  the  exterior  one  with  cotton,  and  burying  it  so 
surrounded  in  dry  sand,  a  temperature  approaching  to  ignition  might  readily  be  commanded 
without  the  use  of  lenses. 

(440)  Immediately  subsequent  to  the  December  solstice  of  1836,  some  experiments  were 
instituted  for  the  purpose  of  ascertaining  the  absolute  force  of  solar  radiation  by  its  direct 
unimpeded  effect  in  communicating  heat  to  a  given  quantity  of  water  in  a  given  time,  the 
rays  being  intromitted  through  an  aperture  of  given  area.  The  opportunities  taken  for 
experiment  being  when  the  zenith  distance  of  the  sun  was  under  12°,  the  uncertainty,  if  any, 
which  may  be  supposed  to  attach  to  the  law  of  reflection  of  light  and  heat  at  oblique  incidences 
will  have  no  perceptible  influence  on  the  result ;  and  the  quantity  of  heat  lost  by  reflection  at 
the  surface  of  the  water  will  be  almost  precisely  the  same  as  at  a  perpendicular  incidence, 
which  by  Fresnel's  formula  (presuming  light  and  heat  to  be  similarly  reflected)  is  0.0207 
of  the  incident  beam.  The  form  of  the  experiment  was  as  follows  : — A  light  cylindrical  vessel 
of  tinned  iron,  open  at  the  top  3|  inches  in  diameter,  and  2.4  in.  in  depth,  weighing  1069 
grains,  was  nearly  filled  with  water  moderately  darkened  by  a  slight  admixture  of  ink. 
This  vessel  was  placed  on  a  light  wooden  support,  covered  with  cotton  cloth,  and  touching 
it  only  in  a  narrow  ring  (to  avoid  the  communication  of  heat  by  conduction),  in  the  interior 
of  an  iron  cylinder  of  much  larger  diameter,  to  protect  it  from  wind  and  external  radiation, 
the  upper  part  of  which  was  covered  by  an  iron  plate  well  protected  from  sunshine  by  several 
separate  diaphragms  of  paper  laid  lightly  one  over  the  other  thereon.  This  plate  had  a 
circular  aperture  somewhat  wider  than  that  of  the  tin  cylinder,  and  vertically  over  it,  centre 
corresponding  to  centre.  The  mouth  of  the  tin  cylinder  was  covered  with  a  circle  of  stiff 
paper,  having  an  aperture  exactly  circular  and  concentric  with  the  cylinder,  so  as  to  admit 
a  vertical  or  nearly  vertical  sunbeam  somewhat  less  in  section  than  the  vessel,  and  wholly 
incident  on  the  surface  of  the  contained  liquid.  This  cover  also  projected  over  the  exterior 
of  the  cylinder  on  all  sides,  so  as  to  prevent  any  ray  from  striking  on  its  outside,  even  when 
the  upper  iron  plate  was  removed  from  the  exterior  vessel.  Lastly,  to  cut  off  effectually  all 
lateral  radiation  from  the  region  of  sky  near  the  sun,  a  paper  diaphragm  but  very  little 
more  in  aperture  than  the  mouth  of  the  tin  cylinder  was  laid  concentrically  on  the  upper 
iron  plate  and  its  diaphragms. 

(441)  Plunged  into  the  liquid,  and  resting  on  the  bottom  when  not  in  use,  was  a  circular 
plate  of  mica  3^  inches  in  diameter,  attached  to  a  light  rod  of  reed  0.1  inch  in  diameter,  for 
the  purpose  of  completely  stirring  and  mixing  the  strata  of  the  liquid  by  one  or  two  up 
and  down  movements.  When  thus  prepared,  the  whole  apparatus  was  placed  in  the  sun- 
shine at  noon,  or  somewhat  before,  and  so  adjusted  that  on  the  admission  of  sunlight  a 
narrow  ring  of  light  surrounded  concentrically  the  aperture  in  the  diaphragm  of  the  tin 
cylinder  beneath,  which  was  carefully  watched  during  the  progress  of  the  experiment,  and 
kept  unaltered.  These  arrangements  being  made,  the  sun  was  shaded  off — the  temperature 
of  the  liquid  (after  stirring  by  the  mica-plate)  taken  by  an  exceedingly  delicate  and  sensitive 
thermometer  by  Crichton,  and  again  after  a  certain  noted  number  of  minutes.  The  shade 
being  then  removed,  the  sun  was  allowed  to  shine  into  the  aperture  on  the  liquid,  for  ten 
minutes.  During  this  exposure,  the  liquid  was  three  times  stirred  by  the  mica-plate,  allowing 
five  seconds  for  each  stirring,  and  shading  the  aperture  during  that  operation  (which,  of  course, 


APPENDIX. 


445 


was  not  counted  as  part  of  the  ten  minutes'  exposure).  The  temperature  was  now  again  taken, 
and,  after  remaining  shaded  again  a  certain  noted  number  of  minutes,  finally  once  more. 
The  mean  of  the  minutely  change  of  temperature,  deduced  from  the  shade  observations,  being 
obtained,  was  applied  as  a  correction  (in  all  cases  a  very  small  one)  to  the  minutely  elevation 
of  temperature  in  the  sun  exposure ;  and  thus  the  true  effect  of  the  sun  was  concluded.  The 
following  detail  of  an  experiment  of  this  kind,  made  on  Dec.  31,  1836,  will  more  fully  explain 
the  nature  of  the  process  : — 

Quantity  of  inked  water  used  (supposed  to  have  the  same  capacity  for  heat  as  pure  water) 
=  4500  grains.  Tin  vessel  =  1069  grains,  equivalent  in  capacity  to  134  grains  of  water. 
Stirrer  =  20  grains,  equivalent  to  4  grains  of  water.  Total  quantity  heated  =  4638  grains  of 
water.  Diameter  of  aperture  =  3.024  inches,  area  =  7.1821  square  inches,  which,  multiplied 
by  cos.  10°  51',  the  sun's  zenith  distance,  gives  7.0538  for  the  area  of  the  section  of  the 
sunbeam. 

Apparent  Time, 
h.  m.  s. 

11  51    0 — Temperature  of  the  shaded  liquid   72.3  >  „  ...  „„  , 

1 1         r\    t  *     a           a.          rp          .  ™  A  Gained  in  4"\  +  0°.l 

11  55    0 — Liquid  exposed  to  ©.    Temperature  72.4  S 

0    5  15 — Liquid  shaded  (having  been  three  times  stirred).    Temperature        >„  .     ,  .    ,„       _  ' 
,                        8  mn  „  f  Gained  in  1<K  +  3°.9 

taken  .   76.3  S 

0  15    0— Temperature  finally  taken  76.4. .  Gained  in  10",  +  0°.l 

The  gain  of  heat  per  minute,  in  the  sun,  is  0.390  ;  and  in  the  shade,  by  a  mean  of 
both  observations,  +  0.017  ;  consequently,  0.373  is  the  effect  due  to  the  sun  alone,  per 
minute. 

(442)  If  we  define  the  actine  to  be  that  intensity  of  solar  radiation,  which,  if  entirely 
intromitted  and  absorbed,  would  suffice  to  melt  one-millionth  of  a  metre  in  thickness  per 
minute  off  the  surface  of  a  sheet  of  ice  co-extensive  in  area  with  the  sunbeam,  and  perpen- 
dicularly exposed  to  it ; — if,  moreover,  we  designate  by  A  the  minutely  increase  of  temperature 
operated  in  a  quantity  of  water  (or  equivalent  water)  Q  grains ;  by  S,  the  sectional  area  of 
the  sunbeam ;  by  A,  the  number  of  actines  expressing  the  intensity  of  the  beam ; — and  if, 
further,  we  denote  by  c  the  grains  (252.46)  in  a  cubic  inch  of  water ;  by  A,  the  latent  heat 
of  ice  (135°.5);  by  m,  the  inches  (39.37079)  in  one  metre;  and  by  I,  the  ratio  of  the  intro- 
mitted to  the  incident  heat  (=  0.9793,  very  nearly  constant  for  such  small  incidences); — we 
shall  have,  for  the  intensity  of  the  sunbeam  in  question, 

-  =  rr.-°.A  =  «•  v 

In  the  experiment  above  related,  we  have  Q  =  4638,  A  =  0.373,  S  =  7.0537 ; 
whence  A  =  185.96,  the  power  of  the  sun  on  this  occasion  expressed  in  actines,  as  above 
specified. 

(443)  The  following  are  the  particulars  and  results  of  six  experiments  of  this 
kind :  — 


446 


APPENDIX. 


Date. 

Sun's 
zenith 
distance. 

Area  of 
aperture  in 
square 
inches. 

Sectional 
area  of 
sunbeam, 
S. 

Water 
grains 
heated, 
Q. 

II  1' 
11  Cull ; ;  - 

effect  per 
minute, 
A. 

Sun's 
power  in 
actines. 

Remarks. 

1836 

0  / 

0 

Dec.  23. . . 

10  29 

6.9750 

6.8585 

4636 

0.320 

164.0 

Wind.    Apparatus  not  sufficiently  sheltered. 

Dec.  24. . . 

10  30 

7.1821 

7.0619 

4738 

0.432 

219.7 

All  circumstances  eminently  favourable,  but  ex- 
periment not  well  made. 

Dec.  27. 

10  36 

7.1821 

7-059S 

4638 

0.400 

199.2 

Cirrous  haze. 

Dec.  31. . . 

10  51 

7.1821 

7.0538 

4638 

0-373 

186.0 

Clear  sky.    Good  experiment. 

Jan.  1.  .. 

10  55 

7.1321 

7.0031 

4638 

0.387 

194.3 

Superb  Sky.   A  slight  shadow  of  the  stirring  rod 
allowed  for. 

Jan.  9.   . . 

II  50 

7.182I 

7.0294 

4638 

0.370 

185. 1 

Pure  water  used.    Sky  perfect. 

191.4 

(444)  From  these  experiments,  it  appears  that  at  midsummer,  at  noon,  and  at  140  feet 
above  the  mean  sea  level,  the  force  of  the  sun's  radiation  at  the  Cape  of  Good  Hope  is  such 
as  would  suffice  to  melt  191.4  millionths  of  a  metre  in  thickness  per  minute,  from  a  surface 
of  ice  perpendicularly  exposed  to  its  action  (if  wholly  intromitted  and  absorbed) ;  that 
is  to  say,  0.0075355  in.,  which  is  at  the  rate  of  an  inch  in  2  hours  12  min.  42  sec.  If  this 
fraction  (0.0075355)  be  multiplied  by  the  square  of  the  cosecant  of  16'  V.5,  the  sun's  apparent 
semi-diameter,  we  get  347.15  in.  or  28.93  feet,  for  the  thickness  of  ice  which  the  sun's 
ordinary  expenditure  of  heat  would  suffice  to  melt  per  minute,  at  its  own  surface,*  supposing 
it  partly  intercepted  by  an  atmosphere  similar  in  constitution  and  equal  in  thickness  to  that 
of  the  earth.  As  the  heat  absorbed  in  traversing  our  atmosphere  cannot  be  taken  at  less 
than  one-third  of  the  total  incident  heat,  this  would  give  43.39  feet  per  minute  for  the 
unimpeded  effect  of  the  solar  radiation  so  estimated.  M.  Pouillet  concludes  from  his  experi- 
ments (made  in  June  1837)  11.80  met.  or  38.71  feet  for  the  value  of  this  element.  Taking 
it  at  40  feet,  which,  as  intermediate  between  the  two  estimates,  cannot  be  far  from  the  truth, 
it  will  appear,  by  an  easy  calculation,  that  the  ordinary  expenditure  of  heat  by  the  sun,  per 
minute,  would  suffice  to  melt  a  cylinder  of  ice  184  feet  in  diameter,  and  in  length  extending 
from  that  luminary  to  a  Centauri.  Aliter,  that  a  cylindrical  rod  of  ice,  45.3  miles  in  diameter, 
and  of  indefinite  length,  continually  darted  into  the  sun  with  the  velocity  of  light,  would  barely 
suffice  to  employ  its  whole  radiant  heat  for  its  fusion,  without  at  all  reducing  the  temperature 
of  the  surface. 

(445)  The  weight  or  bulk  of  ice  at  the  glacial  temperature  (32),  which  a  certain  quantity 
of  heat  is  capable  of  melting,  is  the  most  definite,  perhaps  the  only  definite,  measure  of  that 
quantity  ;  being,  so  far  as  we  can  see,  strictly  proportional  to  it,  which  we  are  not  sure  to 
be  the  case  as  to  increase  of  temperature  in  solids  and  liquids,  in  all  parts  of  the  thermometric 
6cale;  and  which,  we  are  sure,  is  not  the  case  as  to  their  dilatation.    I  may,  therefore,  be 


*  This  mode  of  figuring  to  ourselves  the  temperature  of  the  solar  surface  is  due  to  M.  Pouillet,  and  is 
perhaps  the  best  and  most  illustrative  the  subject  admits  of. 


APPENDIX. 


447 


allowed  here  to  offer  a  suggestion  for  the  improvement  of  the  Ice  Calorimeter  of  Lavoisier 
and  Laplace,  which  may  rescue  it  from  the  disrepute  into  which  it  has  (it  appears  to  me 
undeservedly)  fallen,  in  consequence  of  the  experiments  of  Wedgwood  (Phil.  Trans.  1784), 
and  restore  it  to  the  place  it  ought  to  hold  as  an  exact  philosophical  instrument.  The 
objections  brought  against  it  in  the  paper  referred  to  are  twofold  :  1st,  That  the  drainage  of 
the  water  melted  off  from  the  pounded  ice  is  uncertain ;  and  2nd,  That  while  melting  in 
one  part  of  the  apparatus,  it  is  arrested  and  prevented  from  running  off  by  actually  freezing 
again  in  another.  The  former  of  these  objections  is  undoubtedly  valid,  especially  when  small 
quantities  are  concerned.  As  part  of  the  ice  is  melted,  its  capillary  communications  and 
cells  are  altered  in  dimension ;  and  they  are  also  otherwise  changed  by  the  collapse  of  the 
solid  ice.  The  simultaneous  thawing  and  freezing,  on  which  the  latter  objection  is  grounded, 
undoubtedly  took  place  in  the  experiments  described  by  Wedgwood,  and  is  attempted  to 
be  accounted  for  by  him  on  grounds  to  which  no  one  at  this  time  will  attribute  any  weight. 
It  is  impossible,  in  short,  but  that  that  ingenious  artist  must  have  been  deceived  as  to  the 
real  temperature  of  his  ice.  In  no  other  way  are  the  facts,  as  related  by  him,  explicable. 
Still,  that  he  should  have  been  so  deceived  is  enough  to  satisfy  us  that  nothing  short  of 
actual  immersion  of  the  pounded  ice  in  water  (the  use,  that  is  to  say,  of  a  mixture  of  ice 
or  snow  and  water)  can  satisfactorily  ensure  the  absence  of  an  undue  degree  of  cold  in  the 
interior  of  the  fragments  of  ice  used.  If  this,  however,  be  made  a  condition  of  the  experi- 
ment, it  is  evident  that  the  estimation  of  the  ice  melted,  by  drainage,  can  never  lead  to 
any  precise  results.  On  the  other  hand,  if  we  estimate  it  by  the  diminution  of  volume  of 
the  total  mass  of  mixed  ice  and  water  used,  produced  by  the  melting  of  part  of  the  ice,  there 
is  no  limit  to  the  precision  which  may  be  attained  other  than  the  mechanical  difficulty  of 
so  arranging  the  apparatus  as  to  afford  an  exact  measure  of  the  difference  of  volumes  before 
and  after  the  experiment.  For  this  purpose  it  is  necessary  that  the  mixed  mass  in  question 
shall  be  enclosed  in  a  vessel  which  it  exactly  fills,  terminating,  in  its  upper  part,  in  a  long 
graduated  open  tube,  to  a  certain  division  of  which,  as  a  zero  point,  the  water  can  be  driven 
by  an  adjusting  screw.  Into  an  insulated  and  water-tight  chamber  within  this,  communi- 
cating with  the  external  air  by  no  larger  adit  than  is  necessary,  and  which  must  be 
immediately  stopped  by  a  non-conducting  plug  or  stopper,  must  be  introduced  the  source 
of  heat  to  be  subjected  to  experiment.  The  whole  apparatus  must  then  be  plunged  into 
a  mixture  of  snow  and  water,  effectually  to  cut  off  all  communication  of  heat  from  without. 

(446)  The  construction  of  this  interior  chamber,  and  the  best  mode  of  introducing 
into  it  the  substances  operated  on,  will  necessarily  vary  according  to  the  nature  of  the 
experiment.  For  the  combustion  of  substances  in  oxygen,  no  communication  with  the 
external  air  is  needed,  as  their  ignition  may  be  effected  within  glass  or  copper  vessels 
completely  insulated,  by  the  voltaic  circuit.  For  inquiries  into  the  heat  given  off  by  the 
mixture  of  chemical  ingredients,  a  small  tubular  communication  with  the  external  air  will 
in  many  cases  suffice;  and  when  liquids  only  are  concerned,  it  will  often  be  practicable  to 
insure  their  mixture  within  a  perfectly  insulated  chamber,  by  the  breaking  of  thin  glass 
globes  containing  them,  by  agitation,  &c.  But  it  is  unnecessary  to  enumerate  cases,  for 
each  of  which  a  moderate  application  of  mechanical  ingenuity  will  readily  suggest  the 
appropriate  contrivance. 


448 


APPENDIX. 


APPENDIX  D. 


Approximate  Places  of  Seventy-Six  Ruby    Coloured,    or  very  intensely  Red,   Insulated  Stars, 
noticed  in  the  course  of  observation,  in  either  Hemisphere. 


R  A.  1830. 

N  P  D.  1830. 

Mag. 

Description. 

R  A. 

830. 

N  P  D. 

1830. 

Mag. 

Description. 

h. 

m.  s.d. 

0  / 

h. 

m. 

s.d. 

ti 

o 

0  38.0 

26  59 

49 

8' 

A  ruby  star. 

IO 

52 

10.4. 

107 

24 

40 

8 

Most  intense  and  curious 

o 

47  15-2 

23  13 

5° 

9 

Deep  orange  red. 

colour.    Scarlet,  almost 

0 

55  52-4 

37  28 

25 

10 

Full  garnet  colour. 

blood  colour.  Follows 

I 

19  8.7 

123  26 

1 

6 

Most  beautiful  orange  red. 
Two  observations. 

a  Hvdra>  421.  c,  and  is  1' 
south  of  it. 

I 

51  47-5 

35  35 

47 

8' 

Almost  ruby  red. 

1 1 

4 

27.'J 

170 

52 

12 

8 

Ruby,  almost  sanguine. 

I 

58  2.9 

89  22 

13 

7 

Very  red. 

1 1 

31 

j  /  j 

10  I 

37 

X  ? 

j  j 

8' 

Fine   ruby,    mclining  to 

2 

7  21.2 

45  35 

0 

Q 

Very  full  red  ;  almost  ruby. 

scarlet. 

2 

10  46.9 

93  45 

3 

8' 

Very  full  ruby  j  sanguine. 

12 

13 

28  <: 

IO4 

33 

<8 

8' 

Sombre  red. 

2 

26  8.5 

33  4° 

27 

Q 

Fine  ruby  red. 

12 

20 

OO 

45 

A.Q 
T7 

Q 

Peculiar  rich  ruby  purple. 

3 

8  15.8 

147  57 

44 

7 

High  orange  or  brick  red. 

Re  -  examined  —  no  re- 

3 

32  41.6 

75  45 

10 

Q 
J 

Very  red  ;  almost  ruby. 

markable  colour,  but  the 

3 

33  10.8 

36  38 

21 

q 

8 

Very  fiery  ;  almost  scarlet. 

star   probably  mistaken 

4 

34  12.6 

57  24 

3 

Remarkable  ruby  red. 

(in  another y). 

4 

37  4i-9 

38  4 

43 

q' 

Very  fiery  ;  almost  ruby. 

12 

37 

j  4 

I48 

45 

*T  1 

8' 

In  the  field  with  /3  Cruris. 

4  4°  52-7 

61  46 

21 

8 

A  very  extraordinary  ruby 

The  fullest  and  deepest 

coloured  star ;   a  most 

maroon  red ;   the  most 

intense     and  beautiful 

intense  blood  red  of  any 

.        xwu     UU3C1  Va* 

star  I  have  seen.    It  is 

tions. 

like  a   drop  of  blood, 

5 

9  35-5 

55  54  36 

8 

Very  remarkably  red. 
?  minute  of  R  A. 

when  contrasted  with  the 

whiteness  of  fi  Cruris. 

5  38  28.9 

136  32 

15 

8 

Vivid  sanguine  red,  like  a 

Several  observations. 

blood  drop.     A  superb 

12 

54 

33.I 

ISO 

31 

4 

9' 

Full  orange. 

specimen  of  its  class. 

13 

57 

8.0 

I48 

54 

45 

8 

Double,  equal.    Both  stars 

6 

2  51.8 

62  48 

1 

8' 

Ruby  coloured. 

brick  red. 

6 

15  46.5 

75  11 

35 

7 

Vivid  red. 

14 

4 

46.I 

149 

7 

4 

7' 

Ruby,  or  high  orange. 

6 

16  53.0 

116  57 

53 

8 

Very  intense  ruby  coloured. 

16 

32.4 

63 

31 

1 

7' 

Vivid  red  ;  almost  a  bright 

6 

24  48.0 

51  26 

47 

6' 

Superb  orange  red ;  very 

ruby  colour ;  fine. 
Ruby  coloured. 

rich  colour. 

14 

25 

O.O 

132 

37 

13 

9 

7 

15  59-5 

115  26 

23 

7 

Very  intense  fiery  red. 

14 

5* 

9-3 

»59 

25 

41 

6 

B.  5189.     Almost  scarlet. 

7 

40  1.4 

121  42 

54 

9 

Very  fine  ruby  colour. 

Two  observations. 

7 

52  25.1 

139  3i 

57 

8 

Rich  brick  red,  mclining  to 

15 

7 

10.7 

165 

18 

20 

7 

Very  high  red,  or  ruby. 

orange. 

15 

40 

45-8 

163 

59 

3 

9 
9' 

Sombre  red. 

8 

38  19.1 

117  35 

32 

8' 

Fiery  red,  very  high  colrd. 

15 

43 

27.9 

49 

54 

20 

Fine  deep  ruby  colour. 

8 

44  16.6 

137  45 

1 

9 
8' 

Ruby  coloured. 

15 

5* 

50.1 

53 

29 

17 

10 

Ruby  red. 

8 

45  46.8 

72  8 

10 

Very  fine  red,  between  ruby 

16 

5 

50.1 

135 

22 

30 

8' 

Ruby,  or  very  high  red. 

and  orange.    Brick  red. 

16 

17 

i7-5 

102 

1 

35 

8 

Dull  brick  red. 

8 

58  41.3 

143  *3 

34 

9 

Ruby  coloured. 

16 

29 

44.0 

122 

z 

0 

8 

Deep  red,  like  a  drop  of 

9 

27  56.0 

152  2 

48 

8 

Very  intense  sanguine  star, 

blood. 

between  scarlet  and  car- 

16 

48 

38.5 

144 

48 

34 

9 

Intense   ruby   red.  Two 

mine  red. 

observations.  (Double.) 

9 

48  31.0 

130  47 

12 

7' 

Scarlet  ;    remarkably  full 

17 

18 

48.3 

125 

29 

33 

Very  deep  red. 

rich  colour.    Three  ob- 

17 

19 

42.1 

109 

»9 

20 

\ 

A  ruby  star. 

servations. 

17 

28 

23.8 

131 

30 

58 

8 

Beautiful  ruby  red. 

9 

54  31-2 

149  24 

34 

8' 

Scarlet. 

17 

zS 

42.2 

147 

37 

41 

8 

Brilliant  scarlet,   or  very 

10 

4  27-i 

124  29 

10 

7 

B.  2874.    Scarlet.  Three 

high  orange. 

observations. 

17 

34 

57.6 

108 

34 

38 

8 

Remarkably  red. 

10 

8  39.3 

149  50 

30 

9 
6' 

Ruby  red. 

17 

45 

35-5 

88 

11 

35 

9 
7' 
8 

A  curious  ruby  coloured  st. 

10 

27  40.9 

128  41 

21 

B.  3085.    Extreme  orange, 
almost  scarlet.    Two  ob- 

17 
18 

49 
10 

31. 1 
46.4 

87 
89 

15 
12 

17 

32 

A  very  fine  orange  star. 
A  very  red  star. 

servations. 

18 

37 

33-9 

81 

25 

22 

9 

Plum  coloured   or  ruddy 

10 

37  4°'7 

147  10 

48 

9 

Ruby  coloured. 

purple. 

APPENDIX. 


449 


R  A.  1830. 

N  P  D. 

830. 

Mag. 

Description. 

R  A.  1830. 

N  P  D.  1830. 

Mag. 

Description. 

h. 

m.  s.d. 

0 

11 

h. 

m. 

s.d. 

0       /  // 

18 

41  5.6 

98 

5 

31 

9 

Most  remarkably  red. 

20 

17 

32.I 

118  48  37 

8 

Fine  ruby  coloured  star. 

'9 

24  35-7 

106 

+3 

15 

7 

Very  remarkably  red  ;  high 

21 

8 

42.8 

160  26  40 

6 

Ruby    red,    inclining  to 

scarlet,    or  good  ruby 

orange. 

colour.    Two  obs. 

21 

37 

19.7 

52  54  47 

8' 

Most  beautiful    and  ex- 

19 

56  30.9 

117 

42 

14 

7' 

Fine  ruby  coloured  star. 

tremely    intense  ruby 

Two  observations. 

colour.    Two  obs. 

19 

57  22-7 

150 

25 

21 

8' 

Very  red.    Ruby  star. 

21 

48 

53-5 

40  17  34 

9 

Fiery  red.    A  very  intense 

20 

3  46-3 

49 

0 

O 

10 

A  fine  dark  ruby  star. 

colour. 

20 

7  7-9 

in 

5° 

I  I 

6' 

A  fine  ruby  star.  Pure 

21 

56 

17.0 

62  28  0 

8' 

Very  ruddy  orange. 

ruby  colour.     This  is 

23 

40 

32.3 

45  45  4° 

10 

Ruby  coloured. 

perhaps  the  finest  of  my 
"  ruby  stars." 

APPENDIX  E. 

Geodesical  Determination  of  the  Site  of  the   Twenty-feet  Reflector  at  Feldhausen  with  respect 
to  the  Royal  Observatory  of  the  Cape  of  Good  Hope. 

(448)  The  connection  of  Feldhausen  with  the  Royal  Observatory,  and  its  relation  of 
situation  with  respect  to  that  building,  and  to  Lacaille's  station  in  Cape  Town,  is  made  out 
by  the  triangles  in  the  annexed  sketch  ;  in  which  O  is  the  station  on  the  western  wing  of 
the  Observatory,  33.71  feet  from  the  centre  of  the  western  dome,  from  which  Mr.  Maclear's 
angles  were  taken ;  M,  the  meridian  mark  of  the  Royal  Observatory  transit  instrument ; 

G,  a  gun  let  into  the  ground,  marking  the  western  extremity  of  the  base  measured  by  him 
in  1837,  for  the  verification  of  Lacaille's  triangulation ;  B,  a  signal  on  the  King's  blockhouse 
battery,  a  very  conspicuous  and  commanding  position  on  the  slope  of  the  Devil  Mountain ; 
C,  a  chimney  of  Mrs.  De  Witt's  house  in  Cape  Town,  124  feet  S.W.  of  Lacaille's  station ; 

H,  the  southern  boundary  stone  of  the  Feldhausen  grounds,  common  to  them  and  the  estate 
of  Mr.  Letterstedt,  of  Cape  Town ;  and  W,  a  conspicuous  and  very  remarkable  granite  block 
on  a  low  projecting  promontory  or  spur  of  the  Table  Mountain,  rising  high  enough  over  the 
protea  bushes  with  which  the  wastes  around  are  clothed,  to  command  from  its  summit  a 
superb  and  extensive  coup  ctceil  of  the  whole  surrounding  country  —  the  Cape  Flats,  the 
rugged  range  of  hills  extending  from  sea  to  sea  beyond  them,  on  the  east,  and  the  noble 
fagade  of  the  Table  Mountain  on  the  west. 

5  Y 


450 


APPENDIX. 


West. 


ir 


H 


North. 


South. 


East. 


M 


(449)  The  data  obligingly  furnished  me  by  Mr.  Maclear,  who  was  at  the  pains  to 
transport  a  repeating  circle,  by  Dollond,  to  tbe  point  H,  and  thereby  to  determine  the  angles 
OBH,  OHW,  so  as  to  complete  the  triangles  OBH  and  OHW,  are  as  follows  : — 


Distances  in  feet 


Whence  we  obtain 


Angles 


OM  =  2537.396 
OG  =  4241.88 
OC  =  17067.95 
IV OH  =  5°  9'  33"; 


OB  =  9864.60         BG  =  10363.82 
OH  =  21671.645      BC  =  13444.95 
MG  =  291 5.325       BH  =  1 5321 .025 
WHO  =  125°  41'  24". 


WH  =  2576.31  ;         OW  =  23269.30. 
Thus  the  positions  of  the  points  O  and  W  are  absolutely  determined. 

(450)  The  buildings  and  instruments  at  Feldhausen  being  so  completely  embosomed  in 
trees  as  to  admit  of  no  part  of  them  being  seen,  or  even  any  signal  sufficiently  high  to  be 
erected  so  as  to  become  visible  to  either  H  or  W,  a  pin  (a)  was  driven  into  the  ground 
in  the  centre  line  of  a  long  avenue  of  trees,  leading  in  front  of  the  house  and  alongside  of 
the  enclosure  in  which  the  telescopes  were  erected.  Over  this  pin  a  signal  was  erected, 
visible  from  both  H  and  W.  The  same  was  done  at  b,  another  pin  also  in  the  same  central 
line,  and  distant  from  a  by  very  exact  measurement  516.25  feet,  so  as  to  serve  as  a  small 
base  of  verification ;  the  rods  with  which  this  was  done  being  adjusted  by  the  standard  of 
the  Royal  Observatory.  The  following  angles  were  then  taken  from  H,  W,  a,  and  b, 
with   a  theodolite   by  Schenk    of  Berne,   on  the   Reichcnbach  construction,   a  delicate 


APPENDIX. 


451 


and  beautiful  instrument,  which  I  had  procured  in  Switzerland  some  years  before,  and 
brought  out  for  any  such  occasional  service  as  this,  which  might  require  its  use : — 

In  triangle  Hab,  angle 

a  =  136°  32'  15",  b  =  36°  11'  10",  H  =  7°  17'  0"; 

Sum  =  180°  0'  25";  Correction  of  each  angle  —  8".3; 

Corrected  angles,       a  =  136°  32'  6",        6  =  36°  11'  2",        H  =  7°  16'  52"; 

Whence  we  conclude 

Ha  =  2404.65;  Hb  =  2801.88. 

(451)  In  the  triangle  Wab,  the  measured  angles  were, — 

a  =  110  29  57-5,         b  =  63°  37'  27',         W  =  5°  52'  8"; 
Sum   179  59  32.5;  Correction  of  each  angle    =  +  9".2; 

Corrected  angles,    a  =  110°  30'  7",         b  =  63°  37'  36",  W  =  5°  52'  17". 

Whence 

Wa  =  4521.03,  Wb  =  4726.62 

These  distances  determine  a  and  b. 

(452)  As  a  verification,  the  distance  WH  may  be  computed  two  ways.  1st,  By  Mr. 
Maclear's  data  from  the  triangle  OWH,  in  which,  having 

OH  =  21671.645,         angle  O  =  5°  9'  33",         and  angle  II  =  125°  41'  24", 
we  find  by  computation 

WH  =  2576.31. 

And  2ndly,  By  the  triangle  WHb,  in  which  we  have 

Angle  WbH  =  Wba  —  Hba  =  63°  37'  36"  —  36°  11'  2"  =  27°  26'  34", 
by  the  former  triangles,  and  by  measurements  from  H  and  W, 

HWb  =  30°  4'  10",  WHb  =  122°  28'  23". 

The  sum  of  the  angles  is  170°  5£K  7",  and  the  deficiency  53",  which  must  in  this  case 
be  divided  between  the  two  angles  W  and  H,  the  angle  at  b  being  already  corrected.  This 
gives,  for  the  corrected  angles  in  WHb, 

W  =  30°  4'  36".5,         H  =  122°  28'  49".5,         b  =  27°  26'  34"; 
with  which,  and  the  side   Hb  =  2801.88,  we  find 

WH  =  2576.56; 

differing  only  by  0.25  of  a  foot,  or  3  inches,  from  the  other  result.  It  should  be  observed, 
that  the  deviations  of  the  angles  in  defect  of  180°  in  these  measurements  are  owing  by 
no  means  to  error  in  division  of  the  instrument,  but  to  the  irregular  form  and  awkward 
position  of  the  observer  and  instrument  on  the  crown  of  the  granite  crag  W,  which 
rendered  nice  observation  from  it  impracticable. 

(453)  The  site  of  the  reflector  (R)  was  now  easily  ascertained  by  prolonging  ab  to  a 
further  distance,  be  =  551.04  feet,  and  thence  erecting  a  perpendicular,  CR  =  56.69  feet, 
to  the  centre  of  its  foundation  ring.  The  geodesical  coordinates  of  this  point,  from  the 
centre  of  the  transit   instrument  at  the  Observatory,  were  finally  ascertained,  by  careful 


452 


APPENDIX. 


measurement  on  a  chart  laid  down  on  a  large  scale  from  these  data,  to  be  17,595  feet  in 
the  direction  of  the  meridian  to  the  south,  and  5190  feet  in  that  of  a  parallel  to  the  west  of 
that  centre.  Its  geographical  situation  was  therefore  in  lat.  2'  53".55  south,  and  in  long.  4s. 11 
to  the  west  of  the  Cape  Observatory.  The  record  of  its  site  is  preserved  on  the  spot  by 
a  granite  column  erected  after  our  departure  by  the  kindness  of  friends,  to  whom,  as  to 
the  locality  itself  and  to  the  colony,  every  member  of  my  family  had  become,  and  will 
remain,  attached  by  a  thousand  pleasing  and  grateful  recollections  of  years  spent  in  agreeable 
society,  cheerful  occupation,  and  unalloyed  happiness. 


FINIS. 


ERRATA,  ADDITIONS,  CORRECTIONS,  &c. 


Page. 

Line. 

Error. 

Correction. 

Page. 

Line. 

Error. 

Correction. 

xi 

15 

nowcv6i*j  this 

however  this 

299 

1  } 

radius  vestor 

radius  vector 

xii 

7 

as  on  one 

as  on  an 

text  K 

xiii 

26 

mit*i*Ai*  ■    in  ("hp 
111 11 1  <  1  ,   111  Lin 

mi t*i*("»»*  in  tli i» 
H  1  11  H  M    ill  LXIU 

12  1 

text  S 

3"-58 

4 

7 

search,  thereby  caused 

search  thereby  caused, 

299 

9".69 

it  to  become 

became 

300 

18 

has 

have 

7 

24 

argument 

arguments 

304 

15 

Lyra 

Lyra? 

18 

8 

n 

7T 

340 

24 

Sequel 

Sequence 

27 

19 

respecting 

respectively 

368 

10 

2.98  +  Log  M 

2.98  x  Log  M 

30 

13 

215.5 

215. 1 

14 

3-I5H 

2744.7 

19 

corraente 

corrente 

13  ) 

text  S 

course 

32 

14 

of  chart 

of  a  chart 

392 

cause 

34 

20 

7th,  13th 

7th  and  13th 

394 

25 

vened  sine 

versed  sine 

25 

Spira 

Spica 

395 

17 

nuclus 

nucleus 

35 

7 

Rigel,  were 

Rigel  were 

21 

0"  — 

comet 

'9 

April,  twelvemonths 

April  twelvemonths 

22 

perilielian 

perihelion 

135 

4 

Canis  Bootis 

Canes  Bootes 

397 

3 

as  give 

as  to  give 

141 

1 

in  thus 

and  in  thus 

406 

26 

time 

term 

H5 

22 

the  the  whole 

the  whole 

3  X 

(see  Art.  168) 

(on  further  and  better 

147 

33 

distinct 

distant 

4*7 

text  S 

consideration  of 

148 

29 

medium 

meridian 

what  is  sajd  on  this 

149 

'3 

nubecula 

nubecula? 

head  in  Art.  170) 

166 

8 

wire  secured 

wire  would  allow,  se- 

418 

4 

mean,  of  which 

mean  of  which 

6  * 

note  $ 

cured 

427 

24 

Jupiter 

Iapetus 

247 

valves 

values 

448 

10'' 52" 

a  Hydra? 

a  Hyd.  Crat. 

45i 
452 

25 
4 

170  59  7 
west 

J79  59  7 

west, 

In  the  table,  p.  391,  omitted  in  their  proper  places  between  Nos.  28,29  and  34,  35 — aih  o'",  1260. .  . .  129°, y  486  ; 
21*40"',  1260  1290;  7486.    Also  at  end  of  Art.  338,  add 

In  sweep  486  (N  P  D  1260. .  . .  1290)  at  2ih  om  the  commencement  of  the  sweep,  "  the  ground  of  the  heavens  was  most 
delicately  and  closely  stippled"— at  2ih  21"'  "  the  stippling  has  ceased  throughout  the  whole  breadth  of  the  sweep  though  the  sky 
continues  perfectly  bright"— at  2ih40m"the  stippling  of  the  sky  resumed  of  exquisite  closeness  and  delicacy.  The  left  eye 
shows  it  perfectly,  the  right  only  suggests  it.  It  is  like  the  first  aggregation  of  a  precipitate  in  a  liquid.  The  stippling  ceased  at 
42"  and  that  very  abruptly." 


CORRECTIONS  TO  BE  MADE  IN  THE  CATALOGUE  OF  NEBULAE. 


No. 

Obs. 

Col. 

In  the 

For 

Read 

No. 

Obs. 

Col. 

In  the 

For 

Read 

2309 

1 

/ 

735 

504 

3079 

R  A 

min. 

l6 

17 

2 

/ 

504 

735 

3  1 1 1 

4 

R  A 

sec. 

34.6 

32.6 

2342 

P  D 

min. 

31 

21 

3 126 

R  A 

sec. 

18.6 

14.6 

2349 

3 

P  D 

sec. 

37 

57 

3'52 

4 

R  A 

sec. 

42.4 

32.6 

2350 

/ 

448 

484 

3162 

/ 

556 

566 

2359 

3 

R  A 

sec. 

12. 1 

72.1 

3184 

P  D 

m,  s 

58  II 

25  31 

2392 

2 

R  A 

sec. 

30.1 

24.3 

3186 

R  A 

sec. 

37.2 

27.2 

2396 

R  A 

min. 

6 

5 

3197 

P  D 

min. 

33 

53 

2423 

/ 

822 

802 

3205 

P  D 

min. 

9 

7 

2445 

Desc. 

2441 

2440 

3224 

2 

R  A 

sec. 

74.6 

72.9 

2462 

2442 

2441 

3229 

P  D 

deg. 

158 

156 

P  D 

deg. 

126 

127 

3259 

R  A 

min. 

21 

22 

2501 

/ 

65, 

652 

3274 

P  D 

min. 

57 

27 

2529 

P  D 

deg. 

107 

127 

3292 

1 

R  A 

sec. 

17.3 

16.7 

2686 

3 

/ 

657 

658 

3346 

3 

P  D 

sec. 

9 

29 

2715 

R  A 

sec. 

14. 1 

41. 1 

35°9 

/ 

449 

45i 

2761 

1 

P  D 

sec. 

4 

54 

3533 

2 

P  D 

m,  s 

30  59 

2799 

1 

P  D 

min. 

16 

18 

36 1 1 

2 

P  D 

sec. 

17 

57 

2864 

/ 

573 

523 

3614 

R  A 

sec. 

10.8 

20.8 

2896 

R  A 

sec. 

3»-4 

48.4 

3679 

P  D 

deg. 

123 

119 

2905 

2 

P  D 

sec. 

3 

23 

37ii 

P  D 

min. 

16 

17 

2912 

R  A 

sec. 

38.8 

28.8 

3939 

f 

494 

495 

2441 

f 

513 

759 

3956 

P  D 

sec. 

45 

25 

2959 

R  A 

sec. 

32.4 

54.8 

3966 
3988 

P  D 

min. 

58 

28 

2961 

3 

P  D 

deg. 

158 

R  A 

sec. 

3 1.0 

41.0 

2972 

3 

P  D 

sec. 

39 

59 

4007 

R  A 

hour 

23 

0 

3009 

2 

P  D 

min. 

7 

9 

4008 

R  A 

hour 

23 

0 

3046 

P  D 

deg. 

113 

1 1 1 

4012 

R  A 

hour 

23 

0 

Notanda.  — 296 1,  obs.  3,  belongs  to  2959  ;  3229  is  a  third  obs.  of  323  1,  the  degree  being  wrong  ;  3259,  the  minute  ought 
to  be  22  in  both  the  observations. 


OMITTED   OBSERVATIONS  OF  NEBULJE,  &c,  AND  SUPPLEMENTARY  NEBULAE. 


No. 


Syn. 


R  A.  1880.0. 


2359 
4.016 
4017 

3170 

4018 
4019 
3358 

3369 
3660 

3689 
4020 

3726 

4021 


ii.609 


A.  456 


d.473 


h.   m.  s.d. 


5  18  38.9 

8  36  32.9 

9  23  59-1 

9  34  4-i 

10  18  2.5 

11  37  49.8 


16  48  32.1 

17  23  37.1 
17  28  28.1 


18  41  49.7 
54-5 


N  P  D.  1830.0. 


157  27  13 

122  2  41 

142  9  19 

II9  l6  35 

128  57  l8 

H5  26  54 


134  25  13 

122  27  15 

123  8  3 


H3  55  3i 
55  7 


Descriptive  Remarks,  &c. 


vL;  p  B  ;  between  3  st  8  m ;  seen  in  twilight  

F  ;  S  ;  R  ;  r  

CI  class  8  ;  not  m  comp  ;  not  v  rich ;  v  irreg  fig.  ;  5'  diam  ;  st 
12.13  m. 

CI  class  7  ;  of  irreg  sc  st ;  irreg  fig. ;  fills  field.  The  ^  taken  is 
one  of  2  chief  st,  the  1st  of  a  small  equilateral  triangle. 

e  F  ;  40"  ;  a  B  *  8  m  follows  

v  F  ;  above  a  s(!  11  m,  dist  ij'   

e  F ;  oval  orvlEj  vgvlbM;  j'l;  ij'br;  has  milky  way 
stars  in  it. 

Seen  beyond  meridian  in  sweeps  436,  437. 

A  v  L,  rich,  but  not  brilliant  cluster,  full  20'  diam  ;  not  m 

comp  M  ;  stars  12.13  m- 

A  B  :jc ,  chief  of  a  cl  3'  or  4'  in  extent   

A  p  rich,  L,  F,  cluster  ;  class  VII.  ;  nearly  fills  field;  composed 

of  concave  flakes;  not  m  comp  ;  st  13  or  15  m. 
See  a  remarkable  observation  of  this  nebula  by  Cacciatore,  in  the 

Astr.  Nachrichten,  No.  113. 

F  ;  S  ;  R  ;  15"  ;  the  following  of  a  group   

p  B  ;  R  ;  90"  ;  g  p  m  b  M  


CORRECTIONS  TO  BE  MADE  IN  THE  CATALOGUE  OF  DOUBLE  STARS. 


No. 

Obs. 

Col. 

In  the 

For 

Read 

No. 

Obs. 

Col. 

In  the 

For 

Read 

2306 

P  D 

deg. 

!°5 

106 

4196 

/ 

762 

763 

3248 

R  A 

min. 

21 

41 

4197 

P  D 

sec. 

9 

49 

3391 

2 

/ 

.. 

735 

4207 

/ 

762 

763 

3 

/ 

•  • 

.... 

502 

4256 

/ 

647 

697 

J429 

R  A 

hour 

0 

4278 

R  A 

sec. 

19.7 

14.9 

343 1 

R  A 

hour 

0 

4291 

R  A 

sec. 

39.0 

40.0 

344° 

R  A 

hour 

0 

43  !7 

/ 

694 

695 

3442 

R  A 

hour 

0 

4396 

R  A 

sec. 

31.4 

34.0 

3463 

2 

/ 

489 

4411 

R  A 

sec. 

58 

5-8 

3465 

1 

P  D 

sec. 

41 

21 

4420 

1 

/ 

476 

436 

3474 

/ 

624 

628 

443  6 

/ 

483 

438 

3511 

2 

/ 

642 

4439 

/ 

404 

444 

3607 

R  A 

sec. 

43.6 

42.6 

4510 

R  A 

min. 

7 

17 

3612 

1 

/ 

774 

747 

4535 

/ 

580 

58i 

3614 

P  D 

sec. 

31 

1 

4604 

3 

/ 

45  6 

45° 

3618 

1 

/ 

626 

526 

4683 

P  D 

deg. 

151 

152 

3643 

2 

/ 

804 

4738 

No. 

4638 

4738 

3681 

P  D 

min. 

30 

36 

4801 

R  A 

min. 

32 

34 

3701 

R  A 

hour 

4 

5 

4812 

2 

/ 

412 

462 

P  D 

deg. 

147 

i57 

4813 

f 

718 

717 

3706 

R  A 

sec. 

58.4 

50.2 

4829  ) 

3716 

2 

/ 

657 

658 

R  A 

min. 

35 

55 

3718 

P  D 

deg. 

126 

123 

4848 

1 

/ 

702 

792 

3723 

P  D 

sec. 

12 

52 

4860 

2 

/ 

573 

593 

3728 

1 

f 

628 

638 

4867 

2 

f 

454 

3763 

1 

P  D 

sec. 

25 

1  : 

3768 

1 

/ 

654 

658 

4875  | 

R  A 

sec. 

3-3 

2.3 

3829  | 

49 16 

/ 

466 

467 

P  D 

sec. 

25 

55 

4923 

/ 

698 

699 

3847  * 

4927 

/ 

598 

599 

—  s 

2 

/ 

639 

539 

4966 

R  A 

sec. 

55-i 

51. 1 

3884 

/ 

766 

767 

4973 

R  A 

sec. 

29.7 

25.7 

39°3 

/ 

666 

667 

4981 

/ 

466 

467 

39r3 

P  D 

min. 

47 

48 

5<=93 

P  D 

min. 

20 

30 

3948 

P  D 

min. 

33 

38 

5105 

I 

P  D 

sec. 

4 

44 

3954 

/ 

534 

535 

5!3° 

/ 

465 

466 

3961 

/ 

697 

679 

5294 

R  A 

min. 

35 

31 

4048 

1 

/ 

712 

772 

5296 

I 

R  A 

sec. 

44.6 

46.4 

4120 

2 

P  D 

min. 

58 

5326  ) 

165 

4132  } 

  S 

P  D 

deg. 

160 

—  s 

P  D 

sec. 

21 

41 

5333 

P  D 

m,  s 

25  54 

55  24 

4143 

/ 

555 

558 

5368 

2 

/ 

796 

797 

4155 

R  A 

min. 

5° 

49 

5409 

2 

/ 

5i3 

510 

Notes. — Nos.  2306,  3248,  belong  to  my  former  Catalogues. — In  No.  3941,  Remarks,  for  exclusively  read  excessively. 


No. 

R  A.  1830.0. 

N  P  D.  1830.0. 

Position. 

Dist. 

Magnitude. 

Remarks. 

Sweep. 

3350 

545° 
3852 

545 1 
5452 
4835 
4840 

4948 
5453 

h.  m.  s.  d. 
02  — 

148  26  ± 

0 

173.3 
90.0 
6.3 
12.6 

107.6 
81.8 

2i 

504 
520 
804 
532 
685 
696 
791 
588 
599 

5  J°  53-3 

6  15  .. 

7  15  4-i 
9  15  12.4 

15  59  59-5 

16  6  23.3 

17  14  8.8 

59  39 
134  43  .. 
113  53  30 
134  45  22 
143  47  2 
124  24  29 
112  37  33 
143  34  59 

.45 
3 
4 

9  10 
10=10 

9  12 
10=10 

3 
12 

9'  J3 

8  8' 

15 

3^ 
15 

296.6 
96.9 
268.3 

8  9 
8  11 

18    2  1 1.4 

12 

9  12 

+&0  +00  +40  +30  +2i0  +10 


Sou.  I A 


-2  0 


-410  -5o  -So 


3 

• 

«a 

* 

• 

• 

• 

• 

• 

■  jf 

•  • 

• 

• 

8 

t 

• 

2 

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+ 

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* 

I 

■ 

+ 

e 

- 

* 

*  a/  * 

*  ♦ 

« 

• 

• 

• 

-k 

• 

+ 

* 

.fc  *  *  +* 

• 

• 

• 

* 

■ 

"a 

* 

• 

4 

* 

- 

* 

* 

* 

i 

•fc 

+50  -hid  1  H 

J.F.WIfcrsi/uLdeiin,.  North, 


London  :  Sxaith.  f  Id 


-3C00\  -+40?" 


JSWfferscheL  dtiw, . 


London.:  Smith  .  Elder  &  C°  65.  CornhiU. 


Plat*  IV 


1 

• 

3 

4 

5 

« 

• 

6 

7 

9k- 

10 

31 

JFWHersrAel  deljjL 


London-  Smith.,  .Elder  Sc,  C°  65.  CornhiH 


London-  Smith .  ELder  &.  C?  65.  Corahill 


/ 


Plate  VL. 


1 

2 

s 

6 

•  • 

7 

• 

8 

• 

• 

10 

11 

12 

• 

13 

14 

is 

• 

16 

* 

17 

18 

19 

londcn.  Smith.  Elier  St  C  65.CorniulL 


Flats.  WL 


North, 

a.  H  vcbri 


B  ToZLGCLTUZ> 


r/  Hvdr 


7  Hydrv  ^ 

S oiuth. 


North, 


B  DoraAIis  • 


a  JZctsiculi 


7  Volcmtur 


•  yjfydri 

Souths 


T7uz-  two  .s'kfa^e^ila-nvn   Clouds  a*r  see/v  n'?jA,  t/ie  ??,<zA:esi 


dth  Elder  fc  C?  fo.Comhill. 


SoulA 


I'UUe  VUI. 


North. 

"  


Tk»  Grea-f,  AreitUa,  in,  foe.  Sword,  -  handle  of  OrioTt,  as   seen,   in,    foe.  Twenty -jee£  Ae/Zector-  at  Jeldha-usSn.  ■  G.  G  H . 

London:  Smith,  Elder  k  C5  6f>.  Oornhill . 


I 


Plate  XV 


Fife. 2. 


* 


JFWHerscJuL  cULt 


London;  Smit}i,Elder  &  C?  65  Comhill 


•H 


Plat/>  7M 


'  1  1  1  1  1  1    1  L  

XT.  W  Her  .Jul  id.  w  Wfst  t  en*/*! 


London:  Smith  .Elder  4  C?  ,15  Waterloo  JP.I 


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accurate  observation  of  their  habits  and  character.  Mr.  Angas's  volumes 
are  enriched  with  numerous  illustrations,  and  are  eminently  worthy  of 
the  confidence  of  readers.  They  bear  the  impress  of  truth,  are  the  pro- 
duction of  an  observant  and  intelligent  mind,  and  will  do  more  to 


familiarize  our  countrymen  with  the  scenery  and  natives  of  the  colonies 
described,  than  any  other  work  with  which  we  aie  acquainted."  — 
Eclectic  Review, 


"  After  a  careful  reading  of  these  two  volumes,  we  pronounce  them, 
without  any  hesitation,  to  afford,  on  the  whole,  the  most  faithful  pic- 
tures of  Savage  Life  and  Scenes  in  New  Zealand  yet  published. — 
Weekly  Chronicle. 

"  Mr.  Angas  writes  as  an  artist ;  and  he  does  not  write  the  worse  for 
that.  We  can  see  what  he  sees,  because  he  understands  the  art  of 
word-painting.  All  that  he  writes  is  eminently  objective.  There  is  an 
individuality  in  his  descriptions  which  brings  the  scene  or  the  person 
vividly  before  our  eyes.  Ii  is  nature— it  is  life— that  is  presented  to  us." 
— Atlas. 


MODERN    PAINTER  S." 


By  A  Graduate  of  Oxford. 


A  New  Edition,  revised  by  the  Author. 

Vol.  II.,  price  10s.  Gd.,  cloth. 


In  imperial  8vo.,  Vol.  I.  price  18s.  cloth ; 


"  We  are  prepared  emphatically  to  declare  that  this  work  is  the  most 
valuable  contribution  towards  a  proper  view  of  painting,  its  purpose 
and  means,  that  has  come  within  our  knowledge." — Foreign  Quarterly 
Review. 

"  This  is  the  production  of  a  highly  gifted  mind,  one  who  has  evidently 
bestowed  time  and  labour  to  obtain  a  practical  knowledge  of  the  fine 
arts,  and  who  writes  eloquently,  feelingly,  and  fearlessly."— Polytechnic 
Review. 

"  It  has  seldom  been  our  lot  to  take  up  a  work  more  admirably  con- 


ceived and  written  than  this  beautiful  and  elaborate  essay.  To  a  perfect 
idea  of  the  scope  of  the  inquiry,  and  a  mastery  of  all  the  technicalities 
required  tor  its  due  treatment,  the  Graduate  unites  considerable  metaphy- 
sical power,  extent  of  philosophical  and  scientific  knowledge,  a  clear  and 
manly  style  of  expression,  and  no  inconsiderable  command  of  humour 
and  satire." — Atlas. 

"  A  work  distinguished  by  an  enlightened  style  of  criticism— new  to 
English  readers,  and  by  the  profound  observation  of  nature  displayed  by 
the  author." — Dublin  University  Magazine. 


*%*  The  THIRD  VOLUME  is  preparing  for  Publication,  and  will  contain  numerous  Illustrations. 


WELLESLEY  COLLEGE  LIBRARY 


3  5002  03425  1814 


Science  fQB3.H52 

Results  of 
astronomical 
Herschel,  John  F. 


