text:
\section{Luminosity -- Linewidth Correlations}

There is a strong correlation between the total luminosities of galaxies
and the global rotation velocities (Tully \& Fisher 1977). \markcite{tfi}
The correlation can
be applied to give distances to galaxies.  The
rotation parameter gives an expectation luminosity and the apparent
luminosity falls off from this value as the square of the distance.
Aaronson, Huchra, \& Mould \markcite{aa} (1979) noted the
advantages of {\it infrared} luminosities: obscuration
is minimized and the light comes from old stars
which have less stochastic variability than the young stars. There is a
substantial correlation between color and luminosity for spirals so the
detailed
correlations between luminosity and the rotation rate parameter depend
on wavelength (Tully, Mould, \& Aaronson \markcite{tm} 1982), steepening toward the
infrared.

The original demonstration of the correlation used photographic or $B$ band
data while the Aaronson et al. collaboration pioneered work at aperture
$H$ band ($1.6 \mu$m).  In recent years, there has been a great deal of
work at intermediate bands; either in the red where the contrast against
the sky background is optimal (Pierce \& Tully 1988, \markcite{pt1} 1992;
\markcite{pt2} Willick 1991; \markcite{wi}
Courteau 1996 \markcite{co}) or at $I$ band where obscuration effects are the most
diminished within the spectral domain accessible to CCD cameras
(Pierce \& Tully 1988, 1992; Han 1992; \markcite{ha} Mathewson, Ford, \&
Buchhorn 1992; \markcite{mat}
Giovanelli et al 1997). \markcite{gio}

Since the seminal aperture photometry work by Aaronson et al., there has
been only limited work at longer wavelengths (eg, Peletier \& Willner
1991, \markcite{pe1} 1993) \markcite{pe2} although electronic imagers have
become available with
reasonably large formats.  The primary disadvantage at wavelengths
greater than 1~micron is the strong and variable atmospheric emission.
All but the very centers of the highest surface brightness galaxies
emit below the flux levels of the sky.  Our experience is at $K^{\prime}$,
($2.1 \mu$m) a shift of the $K$ band to avoid thermal emission (Wainscoat
\& Cowie 1992). \markcite{wa}  One observes several scalelengths
farther out in a galaxy at $R$ or $I$ than at $K^{\prime}$\ with a fixed integration
at the same telescope focus (Tully et al. 1996). \markcite{tv2}  On the other hand,
there is the considerable advantage that obscuration problems are almost
eliminated by $K^{\prime}$\ (25\% of the $I$ extinction according to Tully et al.
1998). \markcite{tp2}  If
extinction can be largely negated then one can restrict to samples that
are highly inclined which minimizes the corrections required for
projection effects in the kinematic parameter.  Arguably the most
dangerous
potential systematic effects arise out of uncertain inclination and
extinction corrections.  Hence, although the correlations at $K^{\prime}$\ are
no better than at $I$ and are a lot more work to acquire, they do eliminate
some systematic problems.  The first order of business is to see if one
gets the same results across the spectrum from blue to infrared bands.

\section{$K^{\prime}$\ Photometry of the Separate Samples}

Our strategy parallels the optical band procedures described by
Tully \& Pierce (1999; hereafter TP). \markcite{tp}  Template luminosity -- HI
profile linewidth
correlations are produced for magnitude-limited cluster samples.
In the present case, data are available for two clusters.  We vary
the assumed differential distance modulus between clusters until an rms
minimization is achieved with a linear regression slope to the common
data set.  The regression takes errors to be in linewidths, the
prescription described by TP to avoid the Malmquist (1920) bias
caused by a magnitude limit.
The absolute scale of the correlation is set by least squares fit of
the template relation to the luminosity--linewidth properties of a
small number of galaxies with accurate independent distances.

\subsection{The Ursa Major Cluster}

The Ursa Major Cluster is as close to home as the Virgo or Fornax
clusters but
it is much more irregular, with no defined center, and a dynamical
collapse
time not much less than the age of the universe.  The 79 known members
are predominantly HI-rich disk systems, similar to those found in low
density environments.  The sample was discussed by Tully et al. (1996)
and the data used in the current paper are presented in that earlier
publication.  There are 38 galaxies with $I<13.4$ (after corrections),
inclination
$i\ge45^{\circ}$ and type S$a$ or later.  The same sample is used to
study optical band luminosity--linewidth correlations by TP and we use
the same HI profile and inclination information.
The small corrections for extinction as a function of galaxy inclination
are those described by Tully et al.
(1998).  The tiny corrections for Galactic extinction are derived from
the selected reddening given by Schlegel, Finkbeiner, \& Davis (1998);
\markcite{scl}
we take $A_{K^{\prime}}^b=0.37E(B-V)$.
The relevant data are gathered together in Table~1.

\subsection{The Pisces Cluster}

The sample to be considered is a spatially restricted subset of the
material discussed by TP.  The Perseus-Pisces
filament is a prominent structure at roughly 5,000~\ifmmode{\hbox{km~s}^{-1}}\else{km~s$^{-1}$}\fi\ that includes
several Abell and other clusters.  The study of optical correlations
by TP drew galaxies from a $20^{\circ}$ length of the filament.
Here we consider 27 galaxies drawn from the restricted range
$0^h49^m < R.A. < 1^h32^m$.  There are several sub-condensations of
galaxies in this so-called Pisces Cluster but the structure is
irregular and probably dynamically young overall.  Sakai, Giovanelli,
\& Wegner \markcite{sak} (1994) identify separate NGC~383 and NGC~507 groups within
this region.  TP failed to find any differential in distances
between separate components.

The $K^{\prime}$\ photometry to be used is published here for the first time
although it was involved in the analysis by Tully et al. (1998).
The observations were made on 10 November, 1995, with the University of
Hawaii 2.2m telescope on Mauna Kea.  A 1024x1024 HgCdTe detector provided
a field of 193 arcsec with 0.19 arcsec pixels.  Five dithered 60 sec
exposures were combined.  The observing sequence would run
sky - object 1 - object 2 - sky - object3 - object4 - sky ...
Hence object observations were always either immediately preceded or
followed by sky observations so there could be proper subtraction of the
sky background.  Pixel to pixel variations are eliminated using a
combination of dome and sky flats.
Dithered images were registered and median filtered to
eliminate defects.

Reductions were carried out with IRAF routines.  Once contaminating
sources were masked, elliptical isophotes were fit progressively with
radius, exponential disks were fit, and fluxes were extrapolated to
infinity to give total magnitudes.

The small reddening corrections follow the same prescriptions mentioned
in the previous sub-section.
The HI profile information and inclinations are again the same as those
used in the optical study of TP.  The relevant material is
presented in Table~1.

\subsection{Zero-Point Calibrators}

A special set-up provides a very wide field for $K^{\prime}$\ observations.
The University of Hawaii 0.61m telescope is used to piggyback an 0.25m
telescope that feeds the 1024x1024 HgCdTe detector.  The set-up gives a
29 arcmin field with 1.69 arcsec pixels.  This field of view is greater
than the dimensions of all
galaxies in the northern sky with the exceptions of M31 and M33.

Observations of many of the largest galaxies were undertaken
6-11 February, 1997.  Among the galaxies successfully observed, there are
four that have accurate independent distances.  Cepheid
variables have been observed in NGC~3031 (Freedman et al. 1994: \markcite{fr}
$(m-M)_0=27.80$),
NGC~3198 (Kelson et al. 1999: \markcite{ke} $(m-M)_0=30.80$), NGC~3627
(Saha et al. 1999; \markcite{sah} Gibson et al. 1999: \markcite{gib}
$(m-M)_0=30.06$), and NGC~4258 (Maoz et al. 1999: \markcite{mao}
$(m-M)_0=29.54$).  HI line profile
information is available for each of these galaxies.  The 4 galaxies are
among the expanded
set of calibrators used in the TP optical band study.

The observing strategy with the small telescope is similar to that used
with the 2.2m telescope except the exposures extend over an hour per
object so more frequent excursions are needed between object and sky.
We observe in the pattern
object - sky north - object - sky south - object - sky east - object -
sky west (5 object, 4 sky).  Exposures were 120 seconds and the pattern
was repeated twice per object, resulting in a cumulative on-target
exposure of 20 minutes.

Reduction procedures are similar between the observations taken with
the large and small telescopes except for a caveat about flat fielding.
Dome flats are not possible with the 0.25m telescope because the dome
is not sufficiently out of focus.  The observations with the small
telescope were obtained remotely and we were not successful with
twilight flats during the run in question.  Hence flats were exclusively
generated by median filtering all the off-object frames.

Adjustments for inclination and extinction within our galaxy follow the
same recipes previously mentioned.  Again, inclination and HI linewidth
information is taken from TP.  This material is gathered in Table~1.

\section{Tabulated Data}

The data is accumulated in Table~1 and provides information comparable
to that in a table in TP.  The following information is provided
in each column. (1) Principal Galaxies Catalogue (PGC) number from the
Lyon Extragalactic Database. (2) Alternative
names; by preference, NGC (N), UGC (U), Zwicky (Z).
(3) Morphological types (T:1,3,5,7,9=Sa,Sb,Sc,Sd,Sm). (4) Systemic
velocity in the rest frame of the cosmic microwave background.
(5) Galactic foreground extinction coefficient, $E(B-V)$.
(6) Axial ratio of minor axis to major axis, $q$. (7) Inclination, $i$.
(8) Total magnitudes, $K^{\prime}$$_T$.
(9) Total magnitudes adjusted for galactic extinction ($b$),
inclination-dependent extinction ($i$), and $k$-correction ($k$),
$K^{\prime}$$_T^{bik}$.
(10) Absolute magnitudes at the accepted distance modulus,
$M_{K^{\prime}}^{bik}$.
(11) HI linewidth, $W_{20}$. (12) Linewidth uncertainty.
(13) Logarithm of adjusted linewidth, ${\rm log} W_R^i$.
(14) References for HI linewidths.

HI linewidth references are given by a 3 figure code.  If the code is less
than 600 then the reference is provided by Huchtmeier \&  Richter
\markcite{hu} (1989)
for that code.  We have been maintaining a database that follows on from
Huchtmeier \&  Richter and the additional references of concern are given
here: 601 $=$ Begeman \markcite{be} (1989),
619 $=$ Magri \markcite{mag} (1990),
630 $=$ Haynes \& Giovanelli \markcite{hg1} (1991$a$), 631 $=$ Haynes \&
Giovanelli \markcite{hg2} (1991$b$), 637 $=$ Roth et al. (1991),
\markcite{ro}
655 $=$ Schneider et al. \markcite{scn} (1992),
660 $=$ Broeils \markcite{br} (1992),
700 $=$ Wegner et al. \markcite{we} (1993),
701 $=$ Haynes et al. \markcite{hg3} (1997), 702 $=$ Haynes, private communication,
706 $=$ Giovanelli et al. (1997),
707 $=$ Tully \& Verheijen \markcite{tv} (1997).

\section{The $K^{\prime}$\ Luminosity--Linewidth Template Relation}

In the two panels of Figure~1, one sees apparent magnitudes plotted
against a logarithmic linewidth parameter for the two separate clusters.
The linewidth parameter is derived from the 21~cm HI profile width and
approximates $2 V_{max}$, where $V_{max}$ is the rotation curve maximum
velocity (Tully \& Fouqu\'e 1985). \markcite{tfo}  Within type and inclination limits,
the Ursa Major sample is complete to $I_T^{bik}=13.4^m$ and the Pisces
sample is almost complete to $I_T^{bik}=13.8^m$ (where $I_T$ magnitudes
are extrapolated to infinity and the superscripts indicate corrections
have been made for Galactic and internal extinction and the redshift
effect).

In Figure~2, the Pisces sample has been shifted $2.55^m$ to achieve a
best fit with the Ursa Major data.  The fitting procedure is described
in TP.  Here is a brief review.  Least squares fits are made with
errors taken in linewidths, the procedure that nulls the Malmquist bias
that arises with magnitude-limited samples.  (Naive application of the
regression with errors in magnitude to give distances would result in biased
distances $\sim10\%$ low.)
A fit is made to the Ursa
Major data alone, and the slope is force fit to the Pisces data to obtain a
preliminary offset.  Once this offset is applied, a fit is made to the
combined data sets, then the new fit is applied separately to the two
clusters to determine a residual difference.  The Pisces offset is
corrected by the residual, the process is repeated, and convergence is
rapidly achieved.  The best fit is illustrated by the dashed line in
Fig.~2.  The rms scatter of the 65 points is $\pm 0.44^m$.

\section{The Zero--Point Calibration}

Accurate distances are known for 4 galaxies with $K^{\prime}$\ apparent magnitude
and HI linewidth information: NGC~3031, NGC~3198, NGC~3627, and
NGC~4258.  The intrinsic luminosity--linewidth relation for the four
systems is shown in Figure~3.  The dashed line has the slope derived from
the Ursa Major + Pisces template and a zero-point that minimizes the sum
of the deviations squared.  This line is described by the formula:
\begin{equation}
M_{K^{\prime}}^{bik} = -23.13(\pm0.12) - 8.78(\pm0.33) ({\rm log}W_R^i - 2.5)
\end{equation}
The $1\sigma$ error on the slope is derived from the 2 cluster fit.
The error on the zero-point is derived from the constraint from the 4
galaxies with Cepheid distances.
The rms scatter of the four points is $\pm 0.22^m$.

The fit of the template data to the absolute calibration is seen in
Figure~4.  This fit requires a distance modulus for the Ursa Major
Cluster of 31.31 and a modulus for Pisces of 33.86.

\section{Distances to Additional Galaxies}

Ten additional galaxies were observed at $K^{\prime}$\ with the 0.25m aperture
wide field arrangement.  The absolute calibration of the $K^{\prime}$\
luminosity--linewidth correlation given by Eq.~(1) can be used to
establish the distances of these galaxies.  Information about these
systems is provided in Table~2.  The format of this table resembles
that of Table~1 with small differences.  The systemic velocities
are the $V_{GSR}$ values of the Third Reference Catalogue (de Vaucouleurs
et al. 1991) \markcite{de} rather than velocities in the frame of the microwave
background
and the absolute magnitudes are calculated from Eq.~(1).
There are two additional HI profile references: 613 $=$ Cayatte et al.
\markcite{ca} (1990) and 638 $=$ Rupen \markcite{ru} (1991).

From the scatter in the luminosity--linewidth plots,
the rms uncertainty for an individual modulus is judged to be
$\pm 0.4^m$.
The corrected linewidth for NGC~2841 is larger than the value for any
of the calibrator or template systems.  Hence application to this
galaxy involves an extrapolation of the luminosity--linewidth
correlation.

\section{The Hubble Constant}

The constraints on the Hubble Constant provided by TP are more
restrictive but this first determination with the $K^{\prime}$\ correlation
is worth noting.  The Ursa Major Cluster is strongly disturbed from
Hubble expansion by its proximity to the Virgo Cluster but the Pisces
Cluster is distant enough that its velocity may predominantly reflect
the Hubble flow.  The velocity of this cluster in the microwave
background frame is 4771~\ifmmode{\hbox{km~s}^{-1}}\else{km~s$^{-1}$}\fi\ (Han \& Mould 1992) \markcite{hm} and the distance
from the $K^{\prime}$\ calibration is 59~Mpc, whence
H$_0 = 81$~\ifmmode{\hbox{km~s}^{-1}}\else{km~s$^{-1}$}\fi Mpc$^{-1}$.

The statistical errors in this determination of H$_0$ are
dominated by the small number of zero-point calibrators.  A reduced
$\chi^2$ goodness of fit is presented in Figure~5.  The 95\%
probability limits on the Hubble Constant {\it from this uncertainty
alone} are $\pm 9$.

There is limited value in exploring all the potential uncertainties
in the current analysis because the same issues are addressed in TP,
but in that paper we use many more template galaxies, more
calibrators, and more
clusters extending to larger velocities.  The present $K^{\prime}$\ sample is
a subset of the optical sample and we use the same HI profile and
inclination information.  With so many factors held the same, we are
able to see if there are any significant systematics due only to the
photometry.  In particular, the $K^{\prime}$\ version has little sensitivity
to extinction.  The scale difference is a remarkably small
$0.03^m$, a 1\% distance effect (the $1\sigma$ uncertainty with the
use of only
4 calibrators is 5\%).  The analysis at $B,R,I$ bands by TP gives
H$_0=77$
with essentially the entire difference a result of extending the
analysis to include twelve clusters.

\section{In Memorium}

Our colleague Peter Witchalls carried out the photometric reductions
of the Pisces sample.  Sadly, he died before he saw the results of his
effort.

\clearpage

\begin{deluxetable}{llcrccrrrrrrcl}
\scriptsize
\tablewidth{6.9in}
\tablenum{1}
\tablecaption{Data for 4 Calibrators and 2 Clusters\label{b}}
\tablecolumns{14}
\tablehead{
\colhead{PGC}&
\colhead{Name}&
\colhead{Ty}&
\multicolumn{1}{c}{$V_{\rm 3K}$}&
\multicolumn{1}{c}{$E(B-V)$}&
\multicolumn{1}{c}{b/a}&
\multicolumn{1}{c}{Inc}&
\colhead{$K^{\prime}_{T}$}&
\colhead{$K^{\prime{\rm bik}}_{T}$}&
\colhead{$M_{K^\prime}^{\rm bik}$}&
\colhead{$W_{20}$}&
\colhead{e$_{20}$}&
\colhead{$\log W^i_R$}&
\multicolumn{1}{c}{H{\sc I} References}
}
\startdata
\multicolumn{14}{c}{Zero-Point Calibrators: 4 galaxies with independent
distances} \\ \tablevspace{4pt}
\tablevspace{-1pt}
\tableline
\tablevspace{13pt}
28630& N~3031& 2&   48& 0.080& 0.54& 59.& 3.55&  3.44& $-$24.36&  444&  7&
2.676& 80 102 185 296\\
30197& N~3198& 5&  880& 0.013& 0.42& 68.& 7.79&  7.71& $-$23.09&  321&  5&
2.484& 80 183 373 480 523 601\\
34695& N~3627& 3& 1066& 0.032& 0.61& 54.& 5.87&  5.80& $-$24.26&  381&  5&
2.626& 80 113 183 373 473 515\\
39600& N~4258& 4&  657& 0.016& 0.36& 72.& 5.23&  5.10& $-$24.44&  442&  5&
2.628& 183 373 387 442 473 480\\
\cutinhead{Ursa Major: 38 galaxies, distance modulus = 31.31}\\
34971& U~6399&   9&  1002& 0.015& 0.28& 78.& 11.09& 11.04& $-$20.27&  173&
20& 2.153&  373\\
35202& U~6446&   7&   826& 0.016& 0.62& 53.& 11.50& 11.47& $-$19.84&  156&
9& 2.193&  157 373 706\\
35616& N~3718&   1&  1174& 0.014& 0.42& 68.&  7.47&  7.36& $-$23.95&  481&
5& 2.678& 80 372 373 417 441 442\\
35676& N~3726&   5&  1079& 0.017& 0.62& 53.&  7.96&  7.91& $-$23.40&  294&
6& 2.504& 80 203 373 387 429 480\\
35711& N~3729&   2&  1249& 0.011& 0.66& 50.&  8.60&  8.56& $-$22.75&  279&
15& 2.496&  441\\
35999& N~3769&   3&   947& 0.023& 0.33& 75.&  9.10&  9.01& $-$22.30&  263&
8& 2.366&  387 417 631\\
36343& U~6667&   6&  1170& 0.017& 0.15& 90.& 10.81& 10.72& $-$20.59&  199&
11& 2.212&  373 387 706\\
36699& N~3877&   5&  1114& 0.023& 0.22& 84.&  7.75&  7.60& $-$23.71&  359&
7& 2.507&  373 387 429 660
706\\
36825& U~6773&   9&  1124& 0.017& 0.50& 62.& 11.23& 11.21& $-$20.10&  119&
7& 2.026&  630 655\\
36875& N~3893&   5&  1176& 0.021& 0.65& 51.&  7.84&  7.79& $-$23.52&  312&
5& 2.546& 80 203 373 387 417
660\\
37036& N~3917&   6&  1158& 0.022& 0.23& 83.&  9.08&  8.95& $-$22.36&  295&
6& 2.412&  201 373 387 660
702\\
37037& U~6816&   9&  1055& 0.014& 0.69& 47.& 11.91& 11.89& $-$19.42&  141&
7& 2.184&  373 515\\
37038& U~6818&   7&  1033& 0.022& 0.28& 78.& 11.70& 11.65& $-$19.66&  176&
12& 2.161&  373 387\\
37290& N~3949&   4&  1009& 0.021& 0.63& 52.&  8.43&  8.38& $-$22.93&  286&
6& 2.495&  373 387 442 706\\
37306& N~3953&   4&  1241& 0.030& 0.50& 62.&  7.03&  6.94& $-$24.37&  426&
5& 2.641&  183 373 387 416
660 706\\
37466& N~3972&   4&  1014& 0.014& 0.28& 78.&  9.39&  9.29& $-$22.02&  266&
11& 2.367&  373 387\\
37525& U~6917&   7&  1113& 0.027& 0.58& 57.& 10.30& 10.26& $-$21.05&  202&
8& 2.295&  373 387\\
37542& N~3985&   9&  1157& 0.026& 0.70& 53.& 10.19& 10.16& $-$21.15&  179&
10& 2.257&  377 417 619\\
37553& U~6923&   8&  1248& 0.028& 0.40& 69.& 11.04& 10.99& $-$20.32&  174&
6& 2.176&  373 387 436 515\\
37617& N~3992&   4&  1230& 0.029& 0.50& 62.&  7.23&  7.13& $-$24.18&  479&
5& 2.697& 80 183 203 373 387
436\\
37691& N~4013&   3&  1064& 0.017& 0.22& 84.&  7.68&  7.51& $-$23.80&  409&
7& 2.570&  373 473 701\\
37697& N~4010&   7&  1116& 0.025& 0.16& 90.&  9.22&  9.08& $-$22.23&  276&
7& 2.375&  373 387 706\\
37719& U~6973&   2&   947& 0.021& 0.39& 70.&  8.23&  8.13& $-$23.18&  346&
10& 2.514&  707\\
37735& U~6983&   6&  1263& 0.027& 0.64& 52.& 10.52& 10.48& $-$20.83&  197&
7& 2.310&  157 373 387 706\\
38068& N~4051&   4&   928& 0.013& 0.75& 50.&  7.86&  7.83& $-$23.48&  267&
8& 2.475& 80 116 373\\
38283& N~4085&   5&   945& 0.018& 0.26& 80.&  9.20&  9.08& $-$22.23&  304&
7& 2.430&  373 387 407 442
619 706\\
38302& N~4088&   4&   952& 0.020& 0.38& 71.&  7.46&  7.35& $-$23.96&  373&
5& 2.548&  373 387 407 442
619\\
38356& U~7089&   8&  1007& 0.015& 0.20& 87.& 11.11& 11.06& $-$20.25&  159&
7& 2.104&  373 459\\
38370& N~4100&   4&  1272& 0.023& 0.30& 77.&  8.02&  7.88& $-$23.43&  404&
9& 2.573&  373 387 442 706\\
38375& U~7094&   8&  1011& 0.013& 0.36& 72.& 11.58& 11.57& $-$19.74&  112&
20& 1.967&  655\\
38392& N~4102&   2&  1021& 0.020& 0.57& 57.&  7.86&  7.80& $-$23.51&  328&
11& 2.537&  373 387 637\\
38643& N~4138&   1&  1105& 0.014& 0.63& 52.&  8.19&  8.14& $-$23.17&  329&
10& 2.566&  140 241 619\\
38795& N~4157&   3&   963& 0.021& 0.19& 90.&  7.52&  7.33& $-$23.98&  425&
7& 2.586&  373 387 706\\
38988& N~4183&   6&  1158& 0.015& 0.16& 90.&  9.76&  9.63& $-$21.68&  256&
7& 2.338&  201 373 706\\
39237& N~4218&   9&   923& 0.016& 0.60& 55.& 10.83& 10.80& $-$20.51&  156&
8& 2.182&  158 293 347 619\\
39241& N~4217&   3&  1234& 0.017& 0.27& 79.&  7.61&  7.46& $-$23.85&  421&
13& 2.589&  158 373 387 512 706\\
39285& N~4220&   1&  1136& 0.018& 0.31& 76.&  8.36&  8.23& $-$23.08&  372&
15& 2.535&  619\\
40537& N~4389&   4&   925& 0.015& 0.68& 49.&  9.12&  9.09& $-$22.22&  192&
8& 2.317&  346 373 387 619\\
\cutinhead{ Pisces filament: 27 galaxies, distance modulus = 33.86}
 2865& U~501&  5& 4769& 0.061& 0.14& 90.& 10.31& 10.08& $-$23.78&  404&  8&
2.557& 452 543\\
 2899& U~509&  5& 4825& 0.061& 0.42& 68.& 12.41& 12.33& $-$21.53&  236& 10&
2.324& 452\\
 2928& U~511&  5& 4287& 0.060& 0.22& 85.& 12.25& 12.10& $-$21.76&  310&  9&
2.430& 384 452\\
2964& Z501-024& 5& 4686& 0.066& 0.22& 85.& 12.56& 12.43& $-$21.43&  257&
15& 2.336& 565\\
 3020& U~525&  3& 4621& 0.060& 0.59& 56.& 11.52& 11.46& $-$22.40&  242&  7&
2.386& 452 543\\
 3108& U~540&  3& 4661& 0.053& 0.57& 57.& 11.13& 11.06& $-$22.80&  289&  7&
2.470& 452 543\\
 3133& U~542&  5& 4205& 0.056& 0.20& 90.& 10.00&  9.81& $-$24.05&  397&  7&
2.549& 452 543\\
 3222& U~557&  3& 4192& 0.060& 0.42& 68.& 11.90& 11.80& $-$22.06&  295&  8&
2.437& 452 543\\
 3235& U~556&  3& 4318& 0.057& 0.20& 90.& 10.28& 10.09& $-$23.77&  414&  8&
2.569& 452 543\\
 3260& N~295&  3& 5163& 0.062& 0.40& 69.&  9.05&  8.91& $-$24.95&  475& 15&
2.663& 543\\
 3274& N~296&  5& 5340& 0.064& 0.28& 78.& 11.72& 11.61& $-$22.25&  257&  9&
2.343& 452 543\\
 3336& U~575&  4& 4346& 0.061& 0.16& 90.& 11.51& 11.33& $-$22.53&  323& 17&
2.449& 452 543\\
 \tablebreak
 3606& U~623&  1& 4529& 0.059& 0.41& 69.& 10.66& 10.54& $-$23.32&  395& 15&
2.576& 452 543\\
 3611& N~338&  2& 4479& 0.055& 0.35& 73.&  9.04&  8.88& $-$24.98&  564&  8&
2.734& 452 543\\
 3664& U~633&  3& 5272& 0.064& 0.25& 82.& 10.76& 10.58& $-$23.28&  422&  7&
2.581& 452 543\\
 3866& U~669&  5& 5556& 0.070& 0.22& 85.& 10.95& 10.81& $-$23.05&  281& 15&
2.380& 452 543\\
 4110& U~714&  5& 4345& 0.064& 0.72& 45.& 10.86& 10.81& $-$23.05&  258& 15&
2.487& 452\\
 4561& N~444&  5& 4544& 0.064& 0.26& 80.& 11.52& 11.39& $-$22.47&  293&  8&
2.407& 452 543\\
 4563& U~809&  5& 3920& 0.059& 0.18& 90.& 11.37& 11.19& $-$22.67&  346& 14&
2.483& 543 700\\
 4596& N~452&  2& 4670& 0.066& 0.29& 78.&  9.40&  9.22& $-$24.64&  528& 12&
2.693& 452 543\\
 4735& U~841&  4& 5287& 0.062& 0.22& 84.& 11.48& 11.33& $-$22.53&  312&  8&
2.433& 452 543\\
 5035& N~494&  2& 5168& 0.061& 0.35& 73.&  9.35&  9.19& $-$24.67&  527& 15&
2.701& 452\\
 5061& N~496&  4& 5722& 0.072& 0.55& 59.& 10.53& 10.44& $-$23.42&  340& 20&
2.539& 452\\
 5284& U~987&  1& 4373& 0.060& 0.32& 75.&  9.72&  9.57& $-$24.29&  416&  8&
2.586& 452 543\\
 5344& N~536&  3& 4911& 0.052& 0.33& 74.&  8.80&  8.63& $-$25.23&  549& 10&
2.719& 543 700\\
 5440& U~1033& 5& 3757& 0.051& 0.18& 90.& 10.75& 10.56& $-$23.30&  367&  7&
2.512& 452 543\\
 5702& N~582&  3& 4070& 0.053& 0.24& 82.&  9.62&  9.43& $-$24.43&  474&  7&
2.638& 452 543\\
\enddata
\end{deluxetable}

\begin{deluxetable}{lccccccccccccl}
\scriptsize
\tablewidth{6.9in}
\tablenum{2}
\tablecaption{Distance Derivations for 10 Galaxies\label{t}}
\tablecolumns{14}
\tablehead{
\colhead{PGC}&
\colhead{Name}&
\colhead{Modulus}&
\colhead{Ty}&
\colhead{$E(B-V)$}&
\colhead{b/a}&
\colhead{Inc}&
\colhead{$K^\prime_T$}&
\colhead{$K^{\prime\rm bik}_T$}&
\colhead{$M_{K^\prime}^{\rm bik}$}&
\colhead{$W_{20}$}&
\colhead{e$_{20}$}&
\colhead{$\log W^i_R$}&
\multicolumn{1}{c}{H{\sc I} References}\nl
}
\startdata
24930& N~2683&  30.09&  3&    0.033&  0.25&   81.&
        6.16&   5.99&   $-$24.09&       440& 5&      2.609&  183     373
        377     473     660\\
26512& N~2841&  31.85&  3&    0.015&  0.45&   66.&
        6.19&   6.07&   $-$25.77&       614& 4&      2.801&  183
        373     442     473     522\\
33550& N~3521&  30.31&  4&    0.058&  0.50&   62.&
        5.64&   5.53&   $-$24.77&       468& 5&      2.687&  183     373
        393     473     515\\
39028& N~4192&  31.08&  2&    0.035&  0.21&   86.&
        6.94&   6.74&   $-$24.33&       470& 5&      2.636&  151     373
        375     509     613\\
39422& N~4244&  28.67&  6&    0.021&  0.20&   90.&
        7.69&   7.59&   $-$21.07&       221& 7&      2.265&  373
        442\\
42002& N~4559&  29.03&  6&    0.018&  0.40&   69.&
        7.12&   7.05&   $-$21.97&       256& 5&      2.368&  201     373
        442     660\\
42038& N~4565&  30.42&   3&   0.015&  0.22&   85.&
        5.79&   5.59&   $-$24.82&       528& 5&      2.692&  183     373
        473     638\\
42637& N~4631&  28.79&  7&    0.017&  0.22&   85.&
        6.18&   6.04&   $-$22.74&       322& 6&      2.455&  183     222
        373\\
45948& N~5033&  31.07&  5&    0.012&  0.47&   64.&
        6.62&   6.52&   $-$24.54&       450& 4&      2.660&  183
        390     515     523     562\\
46153& N~5055&  29.54&  4&    0.017&  0.52&   61.&
        5.44&   5.36&   $-$24.17&       400& 5&      2.618&  183
        373     374     473     480\\
\enddata
\end{deluxetable}

\clearpage

redpajama_set_name: RedPajamaArXiv


text:
Rocky Point Bird Observatory Migration Monitoring: Who, what, when, where and WHY
Posted on August 4, 2022 in Environment, Hosted Organizations
Why do we band birds? It's simple: conservation.
Rocky Point Bird Observatory is part of an international effort to monitor landbird migration and has been a member of the Canadian Migration Monitoring Network (CMMN) since 2001. Members of the CMMN track the migration of Canada's birds in the spring and fall each year, adding to our knowledge of population trends, demographics, phenology, and other essential information about the species that pass through each location.
RPBO's bird monitoring projects are comprised of three types of monitoring: bird banding, general observation, and audio-visual census. Bird banding permits assessment of age, gender and condition of individual birds – information that cannot otherwise be obtained.
Red-breasted Sapsuckers (Sphyrapicus ruber) were caught in record numbers in 2021 Photo Credit: David Bell
As well, recapture of individual banded birds gives us information on survival rates. Census and general observation information provide complementary data on abundance. All data collected in the course of our research are widely shared with the Canadian Wildlife Service, Bird Studies Canada, the Institute for Bird Populations and the US Geological Survey, where they are used to help establish population trends at the regional, national, and international levels.
The more we learn, the more we can understand about the needs of birds. And the better equipped we are to protect birds and the places they need to survive.
One of the ways that our donors support us is through endowment funds, such as the one held at the Victoria Foundation. RPBO has been in operation for 28 years, and the consistency of our data is extremely important. Our donors are creating a legacy that ensures we can continue to achieve our mission in the years to come. Thank you!
In 2021, 263,111 individual birds of 198 species were recorded over the course of the 2021 season
Migration Monitoring – July 21 to October 18, 2022
On October 18, 2022, RPBO will complete its 28th 90-day sampling period of autumnal landbird migration monitoring on Department of National Defense (DND) lands at Rocky Point.
In 2012 we began operating a second site at Pedder Bay Marina. This property is open to the public (unlike Rocky Point) and thus provides us with the opportunity for public education. On October 18, 2022, RPBO will complete its 11th season at this location.
Objectives of the fall sampling effort include the collection of data that will allow:
The estimation of annual abundance and productivity indices,
The study of migration ecology of landbirds using Rocky Point and Pedder Bay, and
RPBO to contribute these data to national efforts to monitor landbird populations (CMMN).
These objectives are met through mist netting and observer surveys during the 90-day survey season. RPBO meets a fourth objective – raising public awareness about conservation issues facing migrant landbirds through public education and outreach. Public (volunteer) involvement has been a key component of RPBO's data collection efforts over the past 28 years.
Banders-in-charge reports can be viewed on our Reports and Publications page.
In 2021, an incredible 115 volunteers donated 5504 hours of their time and experience between the stations throughout the season
RPBO's first Orchard Oriole (left, David Bell) and Common Grackle (centre bottom, David Bell), Pedder Bays first Tennessee Warbler (centre top, David Bell), and an "Eastern" Willow Flycatcher (right, Liam Singh).
Rocky Point Bird Observatory wishes to thank the Willard and Elva Dawson Fund, administered by the Victoria Foundation, for their support of this project. Combined with the generosity of our regular contributors, the grant we received means that RPBO can continue to gather data, which is used to monitor bird population trends, investigate declines, and recommend actions to protect the health of ecosystems on which we all depend.
Tags: birds, conservation, landbird migration monitoring, migration, Rocky Point Bird Observatory

redpajama_set_name: RedPajamaCommonCrawl


text:
Nicomachus (Oud-Grieks: ) was een populaire naam in Hellas:
 Nicomachus (Dulichum), een vrijer van Penelope
 Nicomachus (zoon van Machaon)
 Nicomachus (vader van Aristoteles)
 Nicomachus (grammateus van Athene)
 Nicomachus (zoon van Aristoteles), een zoon van Aristoteles bij de slavin Herpyllis
 Nicomachus (treurdichter uit Alexandrië)
 Nicomachus (komisch dichter)
 Nicomachus (dichter van de nieuwe komedie)
 Nicomachus Gerasenus, een pythagoreër uit Gerasa in Arabië
 Nicomachus (schilder)
 Nicomachus (beeldhouwer)
 Nicomachus (edelsteensnijder)

Het was tevens een cognomen in het Imperium Romanum:
 Metius Falconius Nicomachus, een senator;
 Virius Nicomachus Flavianus, een laatantiek schrijver en politicus

redpajama_set_name: RedPajamaWikipedia


text:
.. module:: emcee

.. _upgrade:

Upgrading From Pre-3.0 Versions
===============================

The version 3 release of emcee is the biggest update in years.
That being said, we've made every attempt to maintain backwards compatibility
while still offering new features.
The main new features include:

1. A :ref:`moves` interface that allows the use of a variety of ensemble
   proposals,

2. A more self consistent and user-friendly :ref:`blobs` interface,

3. A :ref:`backends` interface that simplifies the process of serializing the
   sampling results, and

4. The long requested progress bar (implemented using `tqdm
   <https://github.com/tqdm/tqdm>`_) so that users can watch the grass grow
   while the sampler does its thing (this is as simple as installing tqdm and
   setting ``progress=True`` in :class:`EnsembleSampler`).

To improve the stability and supportability of emcee, we also removed some
features.
The main removals are as follows:

1. The ``threads`` keyword argument has been removed in favor of the ``pool``
   interface (see the :ref:`parallel` tutorial for more information).
   The old interface had issues with memory consumption and hanging processes
   when the sampler object wasn't explicitly deleted.
   The ``pool`` interface has been supported since the first release of emcee
   and existing code should be easy to update following the :ref:`parallel`
   tutorial.

2. The ``MPIPool`` has been removed and forked to the `schwimmbad
   <https://github.com/adrn/schwimmbad>`_ project.
   There was a longstanding issue with memory leaks and random crashes of the
   emcee implementation of the ``MPIPool`` that have been fixed in schwimmbad.
   schwimmbad also supports several other ``pool`` interfaces that can be used
   for parallel sampling.
   See the :ref:`parallel` tutorial for more details.

3. The ``PTSampler`` has been removed and forked to the `ptemcee
   <https://github.com/willvousden/ptemcee>`_ project.
   The existing implementation had been gathering dust and there aren't enough
   resources to maintain the sampler within the emcee project.

redpajama_set_name: RedPajamaGithub


A compressed index of collections of genomes of the same species. MuGI reports all occurrences of a given pattern, in exact and approximate matching model, against a collection of thousand(s) genomes. Its unique feature is the small index size, which is customizable.
Indexes of large genome collections on a PC.
The work was supported by the Polish Ministry of Science and Higher Education under the project DEC-2013/09/B/ST6/03117 and European Social Fund project UDA-POKL.04.01.01-00-106/09. The work was performed using the infrastructure supported by POIG.02.03.01-24-099/13 grant: ''GeCONiI---Upper Silesian Center for Computational Science and Engineering''.


No one can ever be too careful. Accidents happen all the time. The trick is learning how to prevent these accidents from happening. Having safety mats is a great way to reduce the extent of injury from a fall.
Mattek identifies the three areas or places that require safety mats.
An accident may occur in case anyone gets too close to the industrial machinery. With industrial safety mats, people do not need to worry much. These mats are made of durable materials that contain pressure sensors. The machines are placed on the mats, or the mats are placed around the machines.
The pressure sensors are then wired to the switch of the machines. Once anyone crosses over to the dangerous side of the machine, the sensors detect the shift in pressure and stop the machine to avoid fatal accidents.
It is common for children to fall in playgrounds with swings, climbing frames and bouncing castles. These accidents often cause injuries. Playground safety mats made of thick absorbent rubber are often used to prevent injuries. The rubber absorbs shock from the impact of a fall; hence, protecting the victim.
Martial artists are always practicing new moves. Their training requires them to fight and throw each other to the ground. Some of the moves that they practice might be deadly, and the mats protect them. Safety mats are thick and act as shock absorbers.
A safety mat is ideal for Judo and karate studios, as well as yoga facilities. Using this product minimises injury from a fall, as some of the yoga styles can render you unable to remain standing.
Safety is imperative for any environment. Preventing an injury is always cheaper than facing its repercussions. Safety mats go a long way in promoting safety in residential, commercial and industrial properties.


Published 04/20/2019 08:28:11 pm at 04/20/2019 08:28:11 pm in Minwax Pro Series Wiping Stain.
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text:
Essay Example on Sexual Assault, Domestic and Family Violence in Australia
Categories: Family Domestic violence Sexual assault
In Australia, sexual assault, family and domestic violence occurs across all ages, socio-economic groups and cultures. Most of the victims are women. Somehow, the countrys education system has failed to sufficiently explain even the basic concepts of these issues. Considering that most of the perpetrators are young people, education on domestic and sexual violence should be directed towards them. This essay educates young people in Australia on the consequences of sexual assault, domestic and family violence.
Often, it is taken for granted that family violence and sexual assault is something that will outgrow the society. It is seen as a throwback from a past era of unequal times. In Australia, gender based violence does not show any signs of becoming extinct, even within the much-hyped 21st century. Sexist attitudes towards gender roles are still quite persistent, something that is rather surprising.
It seems that very many young people, especially women, are quite ignorant on matters to do with sexual assault, domestic and family violence. For instance, many young women undergo encounters that can be described as sexual assault, often in the hands of their partners or boyfriends. Yet, that is not how they viewed the situations. Such women may feel that being pressurized by someone into having sex is wrong. However, when describing the incidences, many of them did not use the terms sexual assault or rape. As a matter of fact, some of them thought that a certain degree of coercion or pressure was fairly normal, even if it was unpleasant to them. Also, some of them are not aware that rape in marriage is against the law.
Due to lack of education, basic concepts such as sexual assault, consent and domestic violence have not been adequately explained to many young people in Australia. The message that abusive behavior and violence is unacceptable is not being passed through. Rather, individuals, particularly young women who are victims of violence continue to be stigmatized and blamed not only by their peers but also by society at large. To make matters worse, women who have undergone either physical or sexual assault in the hands of their partners and spouses report higher rates of several serious or life-threatening health problems.
Some surveys have been conducted with the aim of finding out what needs to be done in order to minimize or altogether do away with sexual assault, domestic and family violence in Australia. Results from these surveys have always given the same answer: education. The Australian government should embed anti-violence education program into the education program in a way that reaches pupils and students of all ages.
The aim of such education programs would be to develop the skills needed by young people to treat their future partners with respect. They will give young people access to the language and the concepts they require to deal with what makes a majority of them uncomfortable: to name violence for what it actually is. Implementing these educational programs may have its own challenges as it would take time for them to reach every school in the country. Also, given that they are resource-intensive, it can be difficult to obtain long-term funding.
Bottoms, B. L., Peter-Hagene, L. C., Epstein, M. A., Wiley, T. R., Reynolds, C. E., & Rudnicki, A. G. (2016). Abuse characteristics and individual differences related to disclosing childhood sexual, physical, and emotional abuse and witnessed domestic violence. Journal of interpersonal violence,31(7), 1308-1339.
Chappell, L., & Curtin, J. (2013). Does federalism matter? Evaluating state architecture and family and domestic violence policy in Australia and New Zealand. Publius: The Journal of Federalism, 43(1), 24-43.
Fisher, C. (2013). Changed and changing gender and family roles and domestic violence in African refugee background communities post-settlement in Perth, Australia. Violence against women, 19(7), 833-847.
OBrien, K. L., Cohen, L., Pooley, J. A., & Taylor, M. F. (2013). Lifting the domestic violence cloak of silence: Resilient Australian womens reflected memories of their childhood experiences of witnessing domestic violence.Journal of Family Violence, 28(1), 95-108.
Pain, R. (2014). Everyday terrorism Connecting domestic violence and global terrorism. Progress in Human Geography, 38(4), 531-550.
Purcell, R., Baksheev, G. N., & Mullen, P. E. (2014). A descriptive study of juvenile family violence: Data from intervention order applications in a Childrens Court. International journal of law and psychiatry, 37(6), 558-563.
Roberts, D., Chamberlain, P., & Delfabbro, P. (2015). Women's experiences of the processes associated with the Family Court of Australia in the context of domestic violence: a thematic analysis. Psychiatry, Psychology and Law,22(4), 599-615.
Essay Example on Sexual Assault, Domestic and Family Violence in Australia. (2019, Nov 18). Retrieved from https://speedypaper.com/essays/sexual-assault-domestic-and-family-violence-in-australia
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Maternity Parenting Childhood Racism Bullying Child abuse Domestic violence Substance abuse Sexual assault Sexual abuse Drug abuse


text:
TN PSQ
2022 Caduceus Retreat Examines "Personality and Recovery"
2022 Caduceus Retreat
Franklin Marriott Cool Springs
e-tmf.org/2022-caduceus-retreat
Registration is now open for the 2022 Caduceus Retreat — open only to current and former participants of the TMF Physician's Health Program. This year's sessions are titled, "Personality and Recovery: How Did 'I' Get Here?" led by Sky Kershner, MSW, DMin (see course description below). The retreat will close Sunday with a recovery message from retired U.S. Airline Captain Lyle Prouse.
TMF's 35th retreat is scheduled for Friday, June 10-Sunday, June 12, at the Franklin Marriott Cool Springs in Franklin, TN. Details and sign-up information are on the TMF Caduceus Retreat web page at e-tmf.org/2022-caduceus-retreat.
Sky Kershner
Sky Kershner, MSW, DMin, is an emotionally focused pastoral counselor and has a deep interest in the mysteries of personality, relationships, addiction, and recovery. As an Assistant Professor at West Virginia University School of Medicine, Charleston Division, he teaches Affect Phobia Therapy and Psychodynamics. He is a member of the Motivational Interviewing Network of Trainers and is a MINT Certified Trainer (one of 80 worldwide).
As a person in recovery, Dr. Kershner states that he comes from a long line of men with drinking problems, having wrestled with his own drinking when he was in his psychotherapy residency in New York City, where, he says, if you are anxious enough, you can do 90 meetings in seven days!
Dr. Kershner has received several awards for his professional work, including the West Virginia Civil Rights Award and West Virginia Counselor of the Year. His biggest "15 minutes of fame" moment was appearing as a guest therapist on the Discovery Studios television show "Hoarders."
Learn more about Dr. Kershner.
Lyle Prouse
Retired Airline Captain Lyle Prouse is the first person arrested and convicted under a federal law for flying under the influence. A decorated U.S. Marine Corps pilot in Vietnam, Prouse made headlines for his 1990 arrest; he was fired from his airline, stripped of all flying certifications, and served 16 months in federal prison. Despite seemingly impossible obstacles, Prouse got sober, returned to Northwest Airlines, and retired as a 747 captain. In January 2001 he received a full pardon from then President Bill Clinton.
Mr. Prouse will share his story during the Spiritual session of the Caduceus Retreat on Sunday morning.
Learn more about Mr. Prouse.
Register & Book Your Room by May 20
Registration for the meeting is $110.00 per person, due by May 20. Attendees can register and pay online or download a PDF form and mail registration in with payment. To register, visit the Caduceus Retreat web page.
Rooms at the Franklin Marriott Cool Springs are available at a special TMF rate of $159.00 per person, per night, plus tax; the deadline to access the TMF rate is May 20 and the room block is limited, so early reservations are encouraged.
Reservations can be made via the Caduceus Retreat web page or by calling the Franklin Marriott Cool Springs directly at 615-261-6100; to receive the special rate please mention you are with the TMF Caduceus Retreat.
Attendance Required for PHP Participants
The Caduceus Retreat is required attendance for current participants in the TMF Physician's Health Program; graduates are encouraged to attend to continue learning and growing in recovery, and to connect with and support colleagues who are just beginning their recovery journey.
For more information, contact Jennifer Rainwater at 615-467-6411 or jenniferr@e-tmf.org.
Personality and Recovery: How Did 'I' Get Here?
Why are we attracted to some things and to some people, and not others? How do we get addicted to some substances or behaviors and have no trouble at all with others? Why do we have trouble with some feelings and not others?
And what does all of this say about how we do our recovery?
This interactive and experiential retreat will look at how we do our personalities, what we like and don't like, through three lenses: the lens of our personalities (the Enneagram), the lens of our brain structures, and the lens of our feelings, anxieties, and defenses.
Learn More About the TMF & How to Support Our Mission
The TMF operates solely on contributions from individuals, hospitals and grants.
You can help support the TMF through donations, annual gifts and special events.
Please contact us and find out how
you can get involved in helping your
fellow health professionals heal.
© 2023 Tennessee Medical Foundation
5141 Virginia Way


text:
NMC directs Enquirer Editor to apologise to judge, Judicial Service
The National Media Commission (NMC) has directed the Editor of the Enquirer, Mr Raymond Archer to apologise to Mrs Justice Henrietta Abban, an Appeals Court Judge, and the Judicial Service for a front-page story in the newspaper last June with the caption "The 'Beauty Queen' who jailed Tsatsu'"
It has also directed that the apology should be published three consecutive times in the newspaper's editions, according to a statement signed by Mr Paul Adi-Gyamfi, Chairman of the NMC.
The statement said the directive followed the determination of a complaint lodged against the newspaper and its editor by the Judicial Service.
It said Mr Justice Alex P. Opoku-Acheampong, Judicial Secretary, who filed the complaint on behalf of the Judicial Service, considered the publication as a scurrilous attack on Mrs Justice Abban and gross disrespect and an affront to the court over which she presided.
The statement said the NMC after examining the evidence presented by both parties and after hearing the parties came to the conclusion that the publication was provocative, unwarranted and in bad taste.
The NMC appealed to the media to refrain from unfair and unwarranted comments on members of the judiciary as such comments eroded the confidence people had in the judiciary, which was the bedrock of the country's young democracy.
Justice Abban jailed Tsatsu Tsikata, Former Chief Executive of the Ghana National Petroleum Corporation, for five years for wilfully causing financial loss of more than 230,000 Ghana cedis to the State.


text:
Q: Ahlfors' proof of Cauchy's theorem in a disk I'm stuck in two parts of Ahlfors' proof of Cauchy's theorem in a disk (page 113), that is, if $f$ is holomorphic in an open disc $D$ then $\int_\gamma f(z)dz=0$ over every closed curve $\gamma$ in $D$.
First part:
Fix $z_0\in D$. We define $F(z)=\int_\sigma f(\zeta)d\zeta$ where $\sigma$ is the path joining $z_0$ with $z$ by taking an horizontal line from $z_0$ and getting to $z$ with a vertical line (hope it is clear).
"It is immediately seen that $\frac{\partial F}{\partial y}(z)=if(z)$". Not for me. I mean, I'm geometrically and intuitively inclined to understand that when we derive vertically, since it is a constant path what we should get is the value of $f$. I don't see how the $i$ appears, though, and I formally don't understand what's going on.
First of all, what does $\frac{\partial F}{\partial y}$ mean? This is what I understand by that: if $F=u+iv$ then $\frac{\partial F}{\partial y}=\frac{\partial u}{\partial y} + i \frac{\partial v}{\partial y}$. Right?
I also found the following formula scribbled on my notebook:
$\int_\gamma f(z)dz = \int_\gamma f(z) dx + i \int_\gamma f(z) dy$. Is this correct? I don't see how it makes sense to integrate with respect to $x$ a complex-valued function: what am I supposed to do with the $y$'s in the integrand? I'm guessing some abuse of notation is going on here.
Anyway, I'm guessing this is something easy and I'm just confused by notation.
Second part: we get that $\frac{\partial F}{\partial y}(z)=if(z)$ and $\frac{\partial F}{\partial x}(z)=f(z)$. "Hence $F$ is holomorphic with derivative $f$". How is that? I mean, we have $\frac{\partial F}{\partial x}= -i \frac{\partial F}{\partial y}$, which does not seem like Cauchy-Riemann to me. I'm guessing this is the same confusion as above.
Hope I was not overly verbose.

A: Why is $
\frac{\partial F}{\partial x} = -i \frac{\partial F}{\partial y}
$ called the Cauchy–Riemann equation for $F(z)$?
A function of the complex variable $z = x + iy$ is also sometimes considered as a function of the pair of real variables $(x, y)$. Thus, if $F(z) = u(x, y) + i v(x, y)$, then
$$
\frac{\partial F}{\partial x} = \frac{\partial u}{\partial x} + i \frac{\partial v}{\partial x}\quad \text{and} \quad
\frac{\partial F}{\partial y} = \frac{\partial u}{\partial y} + i \frac{\partial v}{\partial y}.
$$
Now, the Cauchy–Riemann equations for $F(z)$ are
$$
\frac{\partial u}{\partial x} = \frac{\partial v}{\partial y}\quad \text{and} \quad
\frac{\partial u}{\partial y} = -\frac{\partial v}{\partial x}.
$$
On the other hand,
$$
\frac{\partial F}{\partial x} = -i \frac{\partial F}{\partial y}\ \iff \ \frac{\partial u}{\partial x} + i \frac{\partial v}{\partial x} = \frac{\partial v}{\partial y} -i\frac{\partial u}{\partial y}.
$$
Comparing the real and imaginary parts, we see that the two Cauchy–Riemann equations for $F(z)$ can also be concisely stated as
$$
\bbox[5px,border:2px solid black]
{
\frac{\partial F}{\partial x} = -i \frac{\partial F}{\partial y}.
}
$$
Does it make sense to write $\int_\gamma f(z)\, dz = \int_\gamma f(z)\, dx + i \int_\gamma f(z)\, dy$?
Ahlfors defines the complex line integral of the continuous function $f(z)$ over a piecewise differentiable arc $\gamma$ as
$$
\int_\gamma f(z)\, dz = \int_a^b f(z(t)) z'(t)\, dt\label{defn}\tag{1}
$$
where $z = z(t)$, $a \leq t \leq b$, is a parametrization of the arc $\gamma$. This is given in $\S$4.1.1 on page 102.
On the next page, Ahlfors defines line integrals with respect to $\bar{z}$ as
$$
\int_\gamma f\, \overline{dz} = \overline{\int_\gamma \bar{f}\, dz}.
$$
Finally, line integrals with respect to $x$ and $y$ are defined as
\begin{align}
\int_\gamma f\, dx &= \frac{1}{2} \left( \int_\gamma f\, dz + \int_\gamma f\, \overline{dz} \right), \\
\int_\gamma f\, dy &= \frac{1}{2i} \left( \int_\gamma f\, dz - \int_\gamma f\, \overline{dz} \right).
\end{align}
Then, one sees that we indeed have
$$
\bbox[5px,border:2px solid black]
{
\int_\gamma f\, dz = \int_\gamma f\, dx + i \int_\gamma f\, dy.
}\label{zxy}\tag{2}
$$
Furthermore, using \eqref{defn} one can show the analogous formulas
\begin{align}
\int_\gamma f\, dx &= \int_a^b f(z(t)) x'(t)\, dt, \label{xt}\tag{3} \\
\int_\gamma f\, dy &= \int_a^b f(z(t)) y'(t)\, dt, \label{yt}\tag{4}
\end{align}
where $z(t) = (x(t),y(t))$, $a \leq t \leq b$, is a parametrization of the arc $\gamma$.
How is it immediate that $\partial F / \partial y = i f(z)$?
Here, $F(z)$ is defined as
$$
F(z) = \int_\sigma f\, dz
$$
where $\sigma$ is the horizontal line segment from $(x_0, y_0)$ to $(x, y_0)$ followed by the vertical line segment from $(x, y_0)$ to $(x, y)$.
Now, write $F(z)$ as
$$
F(z) = \int_{\sigma_1} f\, dz + \int_{\sigma_2} f\, dz,
$$
where $\sigma_1$ is the horizontal line segment from $(x_0, y_0)$ to $(x, y_0)$, and $\sigma_2$ is the vertical line segment from $(x,y_0)$ to $(x,y)$.
Then, further expanding each integral on the right using \eqref{zxy}, we get
$$
F(z) = \int_{\sigma_1} f\, dx + i\int_{\sigma_2} f\, dy,
$$
since $\int_{\sigma_1} f\, dy = 0 = \int_{\sigma_2} f\, dx$ (use \eqref{xt} and \eqref{yt} to convince yourself that this is indeed so).
So, consider the values $F(z(k))$ where $z(k) = x + i(y + k)$. Note that $z(0) = z$. By the definition of partial derivative, we have
$$
\frac{\partial F}{\partial y}(z) = \lim_{k \to 0} \frac{F(z(k)) - F(z)}{k} = i \lim_{k \to 0} \frac{1}{k} \int_{z}^{z(k)} f\, dy,
$$
where the last integral is along the straight line segment from $z = (x,y)$ to $z(k) = (x, y+k)$. Using \eqref{yt}, we have
$$
\int_{z}^{z(k)} f\, dy = \int_{y}^{y+k} f(x,t) \cdot 1\, dt,
$$
so by the first fundamental theorem of calculus, the limit is precisely $f(z)$. Thus,
$$
\bbox[5px,border:2px solid black]
{
\frac{\partial F}{\partial y}(z) = i f(z).
}
$$

A: Second part: The Cauchy-Riemann equations are equivalent to $\frac{\partial F}{\partial y}(z) = if(z)$. This form dictates when a function is conformal. In particular, look at the matrix $$ \begin{bmatrix} u_x & -v_x \\ v_x & \ \ \ u_x \end{bmatrix}$$
This is precisely the matrix representation of a complex number.

redpajama_set_name: RedPajamaStackExchange


text:
Seventh Son Trailer
Follow Jeff Bridges
Director: Sergey Bodrov
Genre(s): Sci-fi, Fantasy
John Gregory is a Spook charged with ridding the country of witches, beasts and malevolent forces. But, as the years tick by, he realises that he must enlist another to keep evil at bay in the form of Thomas Ward, the seventh son of the seventh son who possesses the power to see things others cannot. When the powerful witch Mother Malkin makes her return, after Gregory thought he'd defeated her years ago, Thomas is forced to confront her and slay her once and for all. But things aren't as easy they seem when he befriends a witch girl who convinces him that not all witches are bad. Will Thomas succeed in sending Malkin back to the grave? Or will he find himself putting his trust in the wrong people?
'Seventh Son' is the dark fantasy adventure based on the first book of the 'The Wardstone Chronicles' novel series, 'The Spook's Apprenticeby' by Joseph Delaney. It has been directed by Sergey Bodrov ('Mongol: The Rise to Power of Genghis Khan', 'The Quickie') and written by Max Borenstein ('Swordswallowers and Thin Men'), Matt Greenberg ('Reign of Fire') and Charles Leavitt ('Blood Diamond'). It is set currently set for release on January 17th 2014.
Starring: Jeff Bridges, Ben Barnes, Julianne Moore, Antje Traue, Kit Harington, Olivia Williams, Djimon Hounsou, Alicia Vikander, Jason Scott Lee, Gerard Plunkett, Zahf Paroo, Faustino Di Bauda, Billy Wickman, Timothy Webber, Fraser Aitcheson, Sean Carey, Candice-May Langlois, Loyd Catlett, Carmel Amit, Taya Clyne


January 10, 2018 Delaware O-line coach to take over at Belhaven Blaine McCorkle, offensive line coach at traditional Division I FCS contender Delaware, will take over after the Air Raid left town at Belhaven.
November 28, 2017 Mumme resigns from Belhaven After four seasons and eight wins as head coach at Belhaven, Air Raid guru Hal Mumme is moving on.
September 6, 2016 ETBU out to prove it's no one-hit wonder ETBU linebacker CJ Johnson is expected to play a pivotal role all season for the Tigers, who have high hopes of repeating atop the ASC, but this time come away with a playoff bid.


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text:
Villarreal v Arsenal Preview
Arsenal striker Robin van Persie has been ruled out of Tuesday's Champions League quarter-final first leg against Villarreal with a groin injury. The 25-year-old picked up the problem on international duty with the Netherlands and missed Arsenal's 2-0 win over Manchester City on Saturday.
Samir Nasri (virus) and Theo Walcott (knee) have been passed fit. But Eduardo (groin), Abou Diaby (thigh) and Tomas Rosicky remain sidelined and Andrey Arshavin is ineligible.
Van Persie is Arsenal's top scorer this season with 16 goals and helped the Gunners reach the last eight with the only goal in their last 16 first leg against Roma and a spot kick during the penalty shoot-out in the second leg.
Villarreal have injury problems on their own, with Spain winger Santi Cazorla set to miss the remainder of the season. The influential 24-year-old fractured his fibula during his side's 3-0 defeat at Almeria.
This tie is a repeat of the 2005/06 semi-final, won 1-0 by Arsenal thanks to Kolo Touré's first-leg goal in the last European match played at Highbury – although the London club needed a last-minute penalty save by Jens Lehmann from Juan Román Riquelme in the second leg to escape El Madrigal with a goalless draw.
Villarreal's record against English clubs is: P9 W3 D5 L1. At home their record is: P5 W2 D3 L0. In those five past meetings with English opposition at El Madrigal, they conceded just one goal scored, curiously, by a Spaniard – Everton FC's Mikel Arteta.
• Arsenal have lost three European finals to Spanish opposition. They lost 5-4 on penalties to Valencia CF following a goalless draw in the 1979/80 UEFA Cup Winners' Cup final and succumbed 2-1 to Real Zaragoza in the final of the same competition in 1994/95 before a 2-1 defeat by FC Barcelona in the 2005/06 UEFA Champions League final in Paris.
• That defeat by Barcelona was Robert Pirès' final appearance for Arsenal after six seasons with the club, during which he won two Premier League titles and two FA Cups. Voted the English Football Writers' Player of the Year in 2002, he made 284 appearances, scoring 84 goals, before moving to Villarreal in summer 2006.
• Villarreal have kept only four clean sheets in their last 30 matches in all competitions having managed six in their opening nine games this season. In contrast, Arsenal have kept clean sheets in six of their last eight Premier League games, and have conceded only four league goals in 2009 – all away from home – fewer than any other side.
It hurts me to say that Arsenal are my dark horse for the Champions League this year as I am not a big Wenger fan. But he is getting players back and healthy at the right time of the season and I would be not be surprised to see Arsenal do a cup double this year.


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Nothing is set to embark on their "Tired of Tourism" tour next week, which includes a July 8th stop at Union Transfer for their record release show with Citizen, Culture Abuse, and Marry Lattimore & Jeff Zeigler. Get tickets and information for the gig at the XPN Concert Calendar, and watch the video for "A.C.D. (Abcessive Compulsive Disorder)" below.


Named after Julia Mancuso, who grew up in Squaw Vally and has 4 Olympic skiing medals, the most for any American woman.
This run used to be called Exhibition and parallels the Exhibition Chair.
Turn left off the top of Exhibition and follow the run to the base area.
Watch for the cat track transition (Easy Street) part way down.
The run gets significantly steeper after the cat track and is frequently used for competitions.
It is an easier blue above the cat track and a hard blue below.
The Men's Olympic Slalom in 1960 was run on this hill.


When planning work on a hard to reach site, trackway can prove to be incredibly helpful. However, when looking to hire temporary roads, how can you know that you're choosing the right company?
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Every site is different – from how even/uneven the ground is, to the sheer amount of space you have. This means that one of the first things you should look out for when speaking with a trackway hire company is if they offer to conduct a survey of your site.
Having an expert visit your site and walk the distance that you will be laying temporary roadways won't just help them get an idea of how many panels you require (and enable them to give you an accurate estimate). They will also be able to identify any potential issues with a particular route (e.g. overheard lines, trees, fences, awkward angles) that you may overlook.
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Whether you're looking for further information into your hire, you need to discuss your quote, or the timeline of your job changes, having one dedicated point of contact can make things significantly easier.
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When choosing your trackway provider, you may also want to consider the industries and sectors that they have experience working with.
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It's no secret that we love our radiologists here at Bay Imaging Consultants and we don't need special holidays to thank them. Let's face it, we are just not above taking the time to gush about how amazing our bright, caring, and talented board-certified radiologists are on a daily basis. But just in case you needed a few more reasons for why we think our BICARD radiologists are the best, we've highlighted four of our favorite below!
All of the radiologists at BICRAD are board certified, meaning they are deemed qualified and experienced to operate within an elevated level of care and excellence as determined by the American Board of Radiologists. To become a board certified radiologist, the American Board of Radiologists conducts exams to measure the qualification of those who have completed their training in the radiology profession. Board certification must be maintained and is an essential part of ensuring quality care. You can verify board certification status on the ABR website.
When it comes to radiology, it's important to stay with the changing technological times. Our radiologists are abreast of the latest technology and work to improve innovation in the tools and methods they use as well as the types of care they provide because they know that new technology has the power to save lives. The machines we use at our offices are checked regularly and up to the standards of excellence you should expect from your radiologists.
When looking for an imaging facility, it's most important to find a radiologist that cares. Our radiologists want to deliver the best care possible to their patients, not just with cutting-edge technology, years of experience, and the safest machines in the industry, but they also seek to connect with you as a person. Our radiologists will show you they understand and are willing to address your concerns, answer any questions you might have, and work with you to deliver a diagnostic or treatment plan tailored to your unique needs. Our radiologists know that you're not just a patient, you're a person.
The board-certified BICRAD radiologists are some of the best in the profession and seek to provide a level of care and excellence that ultimately saves lives. Today and every day, we want to thank them for being the best!


text:
Das Dorf İzbırak (auch Zaz) aramäisch: ܙܰܐܙ, ist ein Dorf in der Provinz Mardin im Südosten der Türkei. Es befindet sich im Bezirk Midyat und in der historischen Region Tur Abdin.

Im Dorf befinden sich zahlreiche Kirchen, Mor Dimet, Mort Shmuni und Ruinen der Kirche von Mor Gabriel.

Geschichte

Von der Antike bis in die frühe Neuzeit

Zaz wird als Siedlung von Zazabukha bezeichnet, in der der assyrische König Ashurnasirpal II während seines Feldzugs gegen Nairi lagerte und 879 v. Chr. von Chabkhi Tribut erhielt. Bögen an der Nordseite der Kirche von Mor Dimet deuten darauf hin, dass ursprünglich vorchristliche Gebäude auf dem Gelände standen. Die Kirche von Mor Dimet wurde 932 erbaut, aus welchem Jahr eine Grabinschrift erhalten ist. Eine Kopie der aramäischen Diptychen (aramäisch: Sphar Ḥaye, "Buch des Lebens"), die im frühen 16. Jahrhundert im Dorf geschrieben wurde, wurde 1909 gefunden, ging aber beim Aramäischen Völkermord verloren.

20. Jahrhundert
Bis 1915 wurde Zaz ausschließlich von Angehörigen der syrisch-orthodoxen Kirche in 200 Familien bewohnt. Während der Massaker an den syrischen Christen während des Ersten Weltkriegs wurde das Dorf im August 1915 von Kurden angegriffen, und die Dorfbewohner flüchteten in die Kirche von Mor Dimet und in zwei große Häuser. Nachdem sie die Zusicherung erhalten hatten, dass die Dorfbewohner nicht verletzt würden, verließ ein Teil der Dorfbewohner die Gebäude, wurde aber von den Kurden auf einen Hügel namens Ferburne gebracht und dort getötet. Zwei Überlebende des Massakers in Ferburne konnten entkommen und kehrten nach Zaz zurück und warnten die Dorfbewohner, die sich darauf in der Kirche verbarrikadierten und einem dreitägigen Sturm auf die Kirche standhielten. Nach dem Rückzug der Kurden blieben die Christen von Zaz zwei weitere Wochen in der Kirche. Inzwischen hatten die Kurden die Behörden in Mardin alarmiert, dass die Bewohner von Zaz mit ausländischer Hilfe einen Aufstand unternommen hätten. Eine schwerbewaffnete und mit Artillerie ausgerüstete Abteilung der regulären osmanischen Armee rückte daraufhin nach Zaz vor und nahm zunächst die Kirche unter Kanonenbeschuss. Nachdem die Belagerten das Feuer nicht erwiderten, stellte der befehlshabende Major das Feuer ein und inspizierte die Lage. Nachdem er festgestellt hatte, dass die Angaben über Bewaffnung und ausländische Unterstützung, die die militärische Intervention ausgelöst hatten, falsch waren, brachte er mit militärischer Eskorte die Einwohner nach Kfar Boran, wo sie sich anschließend unter dem Schutz des Militärs einen Monat lang aufhielten. Dann wurden sie in das inzwischen von seinen christlichen Bewohnern entblößte Midyat in die Kirche Mart Schmuni gebracht. Dort litten sie unter Hunger, Durst und Krankheiten bis zum Ende der Massaker. Lediglich 100 Personen überlebten. Sie zerstreuten sich über die muslimischen Dörfer des Tur Abdin und arbeiteten dort. Ein Teil der Überlebenden wurde 1920 von Çelebi, Agha des Heverkan-Clans, bei der Rückkehr nach Zaz unterstützt.

1924 wurde der Kirche von Mor Dimet eine Portikus hinzugefügt.

In den frühen neunziger Jahren des 20. Jahrhunderts kam es im Rahmen des kurdisch-türkischen Konflikts in der Nähe des Dorfes zu Scharmützeln zwischen Dorfwächtern, dem türkischen Militär und Milizen der kurdischen Arbeiterpartei (PKK). Dorfwächter und ihre Verwandten erpressten am 18. Februar 1992 20 Millionen türkische Lira von den Dorfbewohnern, indem sie drohten, den Muhtar Gevriye Akyol zu töten. Die aramäischen Dorfbewohner mussten im April 1993 nach Midyat fliehen, nachdem sie Morddrohungen von Dorfwächtern erhalten hatten. Sie blieben dort in der Hoffnung, dass sich die Situation verbessern würde, erhielten jedoch erneut Morddrohungen, als sie im Sommer nach Zaz zurückkehrten. Die vier kurdischen Familien durften bleiben, während die Aramäer nach Europa auswanderten, insbesondere nach Deutschland und Schweden.

Einzelnachweise

Ort in der Provinz Mardin


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That the cosmological, ontological, and teleological arguments can rightly be considered arguments for the existence of God must be called into question in light of the considerations I have mentioned in my most recent posts.
I have tried to show that a genuine experience of the divine entails (at least for the major religions) both a sense that one is subject to external moral requirements and a sense that one's own nature is in harmony with ultimate reality. But even if we could establish that the universe was designed by a supernatural intelligence (and, just to be clear, I don't think this it is possible to establish this) this would not entail that the nature of this intelligence is in harmony with our own. Nor would it entail that we are subject objectively valid moral requirements. Prometheus' defiance of Zeus is an excellent illustration of this point. For all that can be established via the teleological argument, the intelligent designer may be as capricious and amoral as Zeus. Prometheus most emphatically did not experience a fundamental harmony with Zeus.
So, if we understand God as an intelligent being who is the ultimate ground of all reality, who places moral demands on us, and whose nature is in fundamental harmony with our own, then I don't think that it is correct to say that the teleological argument or the cosmological argument are arguments for the existence of God (the ontological argument presents a slightly more complex issue, one that I will put off for now). Furthermore, the current very public debate between the so-called new atheists (such as Harris, Dawkins, Hitchens) and traditional theists almost completely misses the point. Rather than arguing that science does not need the notion of an intelligent designer to explain the existence of complex life in the universe, and rather than debating whether Big Bang cosmology implies that the universe had a beginning and thus requires an external cause, atheists' time would be better spent demanding that theists prove that there is an all-loving, intelligent being who is the source of all reality and whose nature is in fundamental accord with human nature.
As an example of the sort of mistake I have in mind, I offer the following quote from Keith Ward's response to Dawkins, Why There Almost Certainly is a God. Ward says, "The question of God is the question of whether conscious mind can exist without any physical body, and whether that mind could account for the origin of the universe." (p. 19) While that is an interesting question it is misleading to say that this is the question of God because a positive answer would not necessarily imply that this consciousness is all-loving, worthy of worship or even gives a damn about us. Ward also approvingly quotes Dawkins statement of the God Hypothesis: "There exists a superhuman, supernatural intelligence who deliberately designed and created the universe and everything in it, including us." I don't think that atheists (or theists for that matter) should let such definitions go unquestioned. Obviously the above hypothesis leaves some very central aspects of religious belief out. In fact, I would argue that it leaves out everything that is essential and valuable about religious belief since the religious experience is fundamentally about feeling a kinship with ultimate reality and understanding that one must work to improve oneself. This is what God is supposed to account for. When a skeptic says "Show me God," this is what should be demanded.
One aspect of religion that I think should be somewhat surprising is the conjunction of two seemingly unrelated aspects: that of wonder or awe at the power, beauty, and mystery of the universe and the feeling of being morally compelled to engage in certain behaviors (and to avoid others). Why should reverence be tied to morality?
Dawkins wants to simultaneously endorse the "pantheistic reverence" of Einstein and insist that such reverence does not entail a belief in anything supernatural. Dawkins is certainly right about this; the feelings of awe and wonder so well-articulated by Dawkins, Carl Sagan and other scientists do not have any obvious theistic implications. And I agree that a naturalist can be religious in this sense and not believe in anything supernatural.
What is conspicuously absent in Dawkins analysis, however, is any recognition of the other side of religious feeling; the sense that what we stand in awe of has some kind of legitimate authority over how we live our lives; that we are compelled by some source of authority outside of ourselves to change for the better–to bring our activities, thoughts, and emotions in line with the objective standard of Goodness, Righteousness, and Justice.
Perhaps because it is easier for conscious beings to understand other conscious beings, it is natural for humans to understand both of these aspects (awe and duty) in an anthropomorphic way. Theism is the view that the ultimate source of beauty, power, and creation is a person (a special kind of very powerful person, but a person nonetheless); and this view is coupled to the understanding of morality as the dictate of Divine Will. This deep connection between the feelings of awe and obligation would naturally lead a theist to be very suspicious of Dawkins and Einsteins religious sensitivities. The natural question to ask Dawkins would be whether that which he reveres in nature holds any ethical power over us. Does the feeling of transcendent wonder at the glory of the universe generate, as a matter of necessity, any sense of obligation in oneself toward the universe and its parts (or the transcendent glory)? There is no doubt that Dawkins does feel the compulsion of objective morality; he rightly points out that an atheist can recognize the power of objective moral values. The question is whether this appreciation of morality is connected to his feelings of wonder, awe, and reverence for the natural world.
Of course I believe that the Divine Command Theory is a failed understanding of the source of moral authority; the idea that moral obligation can be tied to divine will is as deeply flawed as the parallel view that the source of logical entailment could be found in the will of God. Nonetheless it remains that case that genuine religious feeling seems to involve not just awe and reverence but also an understanding that proper reverence requires us to examine ourselves and improve ourselves, to bring our behavior, thoughts, and values in line with an ultimate and external standard. This is why one of the tests of genuine religious experience is whether that experience brings about a change in attitude and behavior.
However, that these two feelings should be connected remains somewhat of a mystery to me: Why should an appreciation of ultimate reality entail a change in myself? I'll leave that question for next time.