src/Marando/IAU/iauAtciqz.php
public static function Atciqz($rc, $dc, iauASTROM &$astrom, &$ri, &$di) {
    $pco  = [];
    $pnat = [];
    $ppr  = [];
    $pi   = [];
    $w;

    /* BCRS coordinate direction (unit vector). */
    IAU::S2c($rc, $dc, $pco);

    /* Light deflection by the Sun, giving BCRS natural direction. */
    IAU::Ldsun($pco, $astrom->eh, $astrom->em, $pnat);

    /* Aberration, giving GCRS proper direction. */
    IAU::Ab($pnat, $astrom->v, $astrom->em, $astrom->bm1, $ppr);

    /* Bias-precession-nutation, giving CIRS proper direction. */
    IAU::Rxp($astrom->bpn, $ppr, $pi);

    /* CIRS RA,Dec. */
    IAU::C2s($pi, $w, $di);
    $ri = IAU::Anp($w);

    /* Finished. */
  }
public static function Atciqz($rc, $dc, iauASTROM &$astrom, &$ri, &$di) {
    $pco  = [];
    $pnat = [];
    $ppr  = [];
    $pi   = [];
    $w;

    /* BCRS coordinate direction (unit vector). */
    IAU::S2c($rc, $dc, $pco);

    /* Light deflection by the Sun, giving BCRS natural direction. */
    IAU::Ldsun($pco, $astrom->eh, $astrom->em, $pnat);

    /* Aberration, giving GCRS proper direction. */
    IAU::Ab($pnat, $astrom->v, $astrom->em, $astrom->bm1, $ppr);

    /* Bias-precession-nutation, giving CIRS proper direction. */
    IAU::Rxp($astrom->bpn, $ppr, $pi);

    /* CIRS RA,Dec. */
    IAU::C2s($pi, $w, $di);
    $ri = IAU::Anp($w);

    /* Finished. */
  }
public static function Atciqz ( $ rc , $ dc , iauASTROM & $ astrom , & $ ri , & $ di ) { $ pco = [ ] ; $ pnat = [ ] ; $ ppr = [ ] ; $ pi = [ ] ; $ w ; /* BCRS coordinate direction (unit vector). */ IAU :: S2c ( $ rc , $ dc , $ pco ) ; /* Light deflection by the Sun, giving BCRS natural direction. */ IAU :: Ldsun ( $ pco , $ astrom -> eh , $ astrom -> em , $ pnat ) ; /* Aberration, giving GCRS proper direction. */ IAU :: Ab ( $ pnat , $ astrom -> v , $ astrom -> em , $ astrom -> bm1 , $ ppr ) ; /* Bias-precession-nutation, giving CIRS proper direction. */ IAU :: Rxp ( $ astrom -> bpn , $ ppr , $ pi ) ; /* CIRS RA,Dec. */ IAU :: C2s ( $ pi , $ w , $ di ) ; $ ri = IAU :: Anp ( $ w ) ; /* Finished. */ }
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i a u A t c i q z
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Quick ICRS to CIRS transformation, given precomputed star-
independent astrometry parameters, and assuming zero parallax and
proper motion.

Use of this function is appropriate when efficiency is important and
where many star positions are to be transformed for one date.  The
star-independent parameters can be obtained by calling one of the
functions iauApci[13], iauApcg[13], iauApco[13] or iauApcs[13].

The corresponding function for the case of non-zero parallax and
proper motion is iauAtciq.

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

Status:  support function.

Given:
rc,dc  double     ICRS astrometric RA,Dec (radians)
astrom iauASTROM* star-independent astrometry parameters:
pmt    double       PM time interval (SSB, Julian years)
eb     double[3]    SSB to observer (vector, au)
eh     double[3]    Sun to observer (unit vector)
em     double       distance from Sun to observer (au)
v      double[3]    barycentric observer velocity (vector, c)
bm1    double       sqrt(1-|v|^2): reciprocal of Lorenz factor
bpn    double[3][3] bias-precession-nutation matrix
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:
ri,di  double     CIRS RA,Dec (radians)

Note:

All the vectors are with respect to BCRS axes.

References:

Urban, S. & Seidelmann, P. K. (eds), Explanatory Supplement to
the Astronomical Almanac, 3rd ed., University Science Books
(2013).

Klioner, Sergei A., "A practical relativistic model for micro-
arcsecond astrometry in space", Astr. J. 125, 1580-1597 (2003).

Called:
iauS2c       spherical coordinates to unit vector
iauLdsun     light deflection due to Sun
iauAb        stellar aberration
iauRxp       product of r-matrix and p-vector
iauC2s       p-vector to spherical
iauAnp       normalize angle into range +/- pi

This revision:   2013 October 9

SOFA release 2015-02-09

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