src/Marando/IAU/iauApio13.php
public static function Apio13($utc1, $utc2, $dut1, $elong, $phi, $hm, $xp,
          $yp, $phpa, $tc, $rh, $wl, iauASTROM &$astrom) {

    $j;
    $tai1;
    $tai2;
    $tt1;
    $tt2;
    $ut11;
    $ut12;
    $sp;
    $theta;
    $refa;
    $refb;

    /* UTC to other time scales. */
    $j = IAU::Utctai($utc1, $utc2, $tai1, $tai2);
    if ($j < 0)
      return -1;
    $j = IAU::Taitt($tai1, $tai2, $tt1, $tt2);
    $j = IAU::Utcut1($utc1, $utc2, $dut1, $ut11, $ut12);
    if ($j < 0)
      return -1;

    /* TIO locator s'. */
    $sp = IAU::Sp00($tt1, $tt2);

    /* Earth rotation angle. */
    $theta = IAU::Era00($ut11, $ut12);

    /* Refraction constants A and B. */
    IAU::Refco($phpa, $tc, $rh, $wl, $refa, $refb);

    /* CIRS <-> observed astrometry parameters. */
    IAU::Apio($sp, $theta, $elong, $phi, $hm, $xp, $yp, $refa, $refb, $astrom);

    /* Return any warning status. */
    return $j;

    /* Finished. */
  }
public static function Apio13($utc1, $utc2, $dut1, $elong, $phi, $hm, $xp,
          $yp, $phpa, $tc, $rh, $wl, iauASTROM &$astrom) {

    $j;
    $tai1;
    $tai2;
    $tt1;
    $tt2;
    $ut11;
    $ut12;
    $sp;
    $theta;
    $refa;
    $refb;

    /* UTC to other time scales. */
    $j = IAU::Utctai($utc1, $utc2, $tai1, $tai2);
    if ($j < 0)
      return -1;
    $j = IAU::Taitt($tai1, $tai2, $tt1, $tt2);
    $j = IAU::Utcut1($utc1, $utc2, $dut1, $ut11, $ut12);
    if ($j < 0)
      return -1;

    /* TIO locator s'. */
    $sp = IAU::Sp00($tt1, $tt2);

    /* Earth rotation angle. */
    $theta = IAU::Era00($ut11, $ut12);

    /* Refraction constants A and B. */
    IAU::Refco($phpa, $tc, $rh, $wl, $refa, $refb);

    /* CIRS <-> observed astrometry parameters. */
    IAU::Apio($sp, $theta, $elong, $phi, $hm, $xp, $yp, $refa, $refb, $astrom);

    /* Return any warning status. */
    return $j;

    /* Finished. */
  }
public static function Apio13 ( $ utc1 , $ utc2 , $ dut1 , $ elong , $ phi , $ hm , $ xp , $ yp , $ phpa , $ tc , $ rh , $ wl , iauASTROM & $ astrom ) { $ j ; $ tai1 ; $ tai2 ; $ tt1 ; $ tt2 ; $ ut11 ; $ ut12 ; $ sp ; $ theta ; $ refa ; $ refb ; /* UTC to other time scales. */ $ j = IAU :: Utctai ( $ utc1 , $ utc2 , $ tai1 , $ tai2 ) ; if ( $ j < 0 ) return - 1 ; $ j = IAU :: Taitt ( $ tai1 , $ tai2 , $ tt1 , $ tt2 ) ; $ j = IAU :: Utcut1 ( $ utc1 , $ utc2 , $ dut1 , $ ut11 , $ ut12 ) ; if ( $ j < 0 ) return - 1 ; /* TIO locator s'. */ $ sp = IAU :: Sp00 ( $ tt1 , $ tt2 ) ; /* Earth rotation angle. */ $ theta = IAU :: Era00 ( $ ut11 , $ ut12 ) ; /* Refraction constants A and B. */ IAU :: Refco ( $ phpa , $ tc , $ rh , $ wl , $ refa , $ refb ) ; /* CIRS <-> observed astrometry parameters. */ IAU :: Apio ( $ sp , $ theta , $ elong , $ phi , $ hm , $ xp , $ yp , $ refa , $ refb , $ astrom ) ; /* Return any warning status. */ return $ j ; /* Finished. */ }
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For a terrestrial observer, prepare star-independent astrometry
parameters for transformations between CIRS and observed
coordinates.  The caller supplies UTC, site coordinates, ambient air
conditions and observing wavelength.

This function is part of the International Astronomical Union's
SOFA (Standards of Fundamental Astronomy) software collection.

Status:  support function.

Given:
utc1   double      UTC as a 2-part...
utc2   double      ...quasi Julian Date (Notes 1,2)
dut1   double      UT1-UTC (seconds)
elong  double      longitude (radians, east +ve, Note 3)
phi    double      geodetic latitude (radians, Note 3)
hm     double      height above ellipsoid (m, geodetic Notes 4,6)
xp,yp  double      polar motion coordinates (radians, Note 5)
phpa   double      pressure at the observer (hPa = mB, Note 6)
tc     double      ambient temperature at the observer (deg C)
rh     double      relative humidity at the observer (range 0-1)
wl     double      wavelength (micrometers, Note 7)

Returned:
astrom iauASTROM*  star-independent astrometry parameters:
pmt    double       unchanged
eb     double[3]    unchanged
eh     double[3]    unchanged
em     double       unchanged
v      double[3]    unchanged
bm1    double       unchanged
bpn    double[3][3] unchanged
along  double       longitude + s' (radians)
xpl    double       polar motion xp wrt local meridian (radians)
ypl    double       polar motion yp wrt local meridian (radians)
sphi   double       sine of geodetic latitude
cphi   double       cosine of geodetic latitude
diurab double       magnitude of diurnal aberration vector
eral   double       "local" Earth rotation angle (radians)
refa   double       refraction constant A (radians)
refb   double       refraction constant B (radians)

Returned (function value):
int         status: +1 = dubious year (Note 2)
0 = OK
-1 = unacceptable date

Notes:

1)  utc1+utc2 is quasi Julian Date (see Note 2), apportioned in any
convenient way between the two arguments, for example where utc1
is the Julian Day Number and utc2 is the fraction of a day.

However, JD cannot unambiguously represent UTC during a leap
second unless special measures are taken.  The convention in the
present function is that the JD day represents UTC days whether
the length is 86399, 86400 or 86401 SI seconds.

Applications should use the function iauDtf2d to convert from
calendar date and time of day into 2-part quasi Julian Date, as
it implements the leap-second-ambiguity convention just
described.

2)  The warning status "dubious year" flags UTCs that predate the
introduction of the time scale or that are too far in the future
to be trusted.  See iauDat for further details.

3)  UT1-UTC is tabulated in IERS bulletins.  It increases by exactly
one second at the end of each positive UTC leap second,
introduced in order to keep UT1-UTC within +/- 0.9s.  n.b. This
practice is under review, and in the future UT1-UTC may grow
essentially without limit.

4)  The geographical coordinates are with respect to the WGS84
reference ellipsoid.  TAKE CARE WITH THE LONGITUDE SIGN:  the
longitude required by the present function is east-positive
(i.e. right-handed), in accordance with geographical convention.

5)  The polar motion xp,yp can be obtained from IERS bulletins.  The
values are the coordinates (in radians) of the Celestial
Intermediate Pole with respect to the International Terrestrial
Reference System (see IERS Conventions 2003), measured along the
meridians 0 and 90 deg west respectively.  For many applications,
xp and yp can be set to zero.

Internally, the polar motion is stored in a form rotated onto
the local meridian.

6)  If hm, the height above the ellipsoid of the observing station
in meters, is not known but phpa, the pressure in hPa (=mB), is
available, an adequate estimate of hm can be obtained from the
expression

hm = -29.3 * tsl * log ( phpa / 1013.25 );

where tsl is the approximate sea-level air temperature in K
(See Astrophysical Quantities, C.W.Allen, 3rd edition, section
52).  Similarly, if the pressure phpa is not known, it can be
estimated from the height of the observing station, hm, as
follows:

phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) );

Note, however, that the refraction is nearly proportional to the
pressure and that an accurate phpa value is important for
precise work.

7)  The argument wl specifies the observing wavelength in
micrometers.  The transition from optical to radio is assumed to
occur at 100 micrometers (about 3000 GHz).

8)  It is advisable to take great care with units, as even unlikely
values of the input parameters are accepted and processed in
accordance with the models used.

9)  In cases where the caller wishes to supply his own Earth
rotation information and refraction constants, the function
iauApc can be used instead of the present function.

10) This is one of several functions that inserts into the astrom
structure star-independent parameters needed for the chain of
astrometric transformations ICRS <-> GCRS <-> CIRS <-> observed.

The various functions support different classes of observer and
portions of the transformation chain:

functions         observer        transformation

iauApcg iauApcg13    geocentric      ICRS <-> GCRS
iauApci iauApci13    terrestrial     ICRS <-> CIRS
iauApco iauApco13    terrestrial     ICRS <-> observed
iauApcs iauApcs13    space           ICRS <-> GCRS
iauAper iauAper13    terrestrial     update Earth rotation
iauApio iauApio13    terrestrial     CIRS <-> observed

Those with names ending in "13" use contemporary SOFA models to
compute the various ephemerides.  The others accept ephemerides
supplied by the caller.

The transformation from ICRS to GCRS covers space motion,
parallax, light deflection, and aberration.  From GCRS to CIRS
comprises frame bias and precession-nutation.  From CIRS to
observed takes account of Earth rotation, polar motion, diurnal
aberration and parallax (unless subsumed into the ICRS <-> GCRS
transformation), and atmospheric refraction.

11) The context structure astrom produced by this function is used
by iauAtioq and iauAtoiq.

Called:
iauUtctai    UTC to TAI
iauTaitt     TAI to TT
iauUtcut1    UTC to UT1
iauSp00      the TIO locator s', IERS 2000
iauEra00     Earth rotation angle, IAU 2000
iauRefco     refraction constants for given ambient conditions
iauApio      astrometry parameters, CIRS-observed

This revision:   2013 October 9

SOFA release 2015-02-09

Copyright (C) 2015 IAU SOFA Board.  See notes at end.
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