original_string: public static function Apcg($date1, $date2, array $ebpv, array $ehp,
            iauASTROM &$astrom) {
  
      /* Geocentric observer */
      $pv = [ [ 0.0, 0.0, 0.0],
          [ 0.0, 0.0, 0.0]];
  
      /* Compute the star-independent astrometry parameters. */
      IAU::Apcs($date1, $date2, $pv, $ebpv, $ehp, $astrom);
  
      /* Finished. */
    }
code: public static function Apcg($date1, $date2, array $ebpv, array $ehp,
            iauASTROM &$astrom) {
  
      /* Geocentric observer */
      $pv = [ [ 0.0, 0.0, 0.0],
          [ 0.0, 0.0, 0.0]];
  
      /* Compute the star-independent astrometry parameters. */
      IAU::Apcs($date1, $date2, $pv, $ebpv, $ehp, $astrom);
  
      /* Finished. */
    }
code_tokens: public static function Apcg ( $ date1 , $ date2 , array $ ebpv , array $ ehp , iauASTROM & $ astrom ) { /* Geocentric observer */ $ pv = [ [ 0.0 , 0.0 , 0.0 ] , [ 0.0 , 0.0 , 0.0 ] ] ; /* Compute the star-independent astrometry parameters. */ IAU :: Apcs ( $ date1 , $ date2 , $ pv , $ ebpv , $ ehp , $ astrom ) ; /* Finished. */ }
docstring: - - - - - - - -
  i a u A p c g
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  For a geocentric observer, prepare star-independent astrometry
  parameters for transformations between ICRS and GCRS coordinates.
  The Earth ephemeris is supplied by the caller.
  
  The parameters produced by this function are required in the
  parallax, light deflection and aberration parts of the astrometric
  transformation chain.
  
  This function is part of the International Astronomical Union's
  SOFA (Standards of Fundamental Astronomy) software collection.
  
  Status:  support function.
  
  Given:
  date1  double       TDB as a 2-part...
  date2  double       ...Julian Date (Note 1)
  ebpv   double[2][3] Earth barycentric pos/vel (au, au/day)
  ehp    double[3]    Earth heliocentric position (au)
  
  Returned:
  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       unchanged
  xpl    double       unchanged
  ypl    double       unchanged
  sphi   double       unchanged
  cphi   double       unchanged
  diurab double       unchanged
  eral   double       unchanged
  refa   double       unchanged
  refb   double       unchanged
  
  Notes:
  
  1) The TDB date date1+date2 is a Julian Date, apportioned in any
  convenient way between the two arguments.  For example,
  JD(TDB)=2450123.7 could be expressed in any of these ways, among
  others:
  
  date1          date2
  
  2450123.7           0.0       (JD method)
  2451545.0       -1421.3       (J2000 method)
  2400000.5       50123.2       (MJD method)
  2450123.5           0.2       (date & time method)
  
  The JD method is the most natural and convenient to use in cases
  where the loss of several decimal digits of resolution is
  acceptable.  The J2000 method is best matched to the way the
  argument is handled internally and will deliver the optimum
  resolution.  The MJD method and the date & time methods are both
  good compromises between resolution and convenience.  For most
  applications of this function the choice will not be at all
  critical.
  
  TT can be used instead of TDB without any significant impact on
  accuracy.
  
  2) All the vectors are with respect to BCRS axes.
  
  3) 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.
  
  4) The context structure astrom produced by this function is used by
  iauAtciq* and iauAticq*.
  
  Called:
  iauApcs      astrometry parameters, ICRS-GCRS, space observer
  
  This revision:   2013 October 9
  
  SOFA release 2015-02-09
  
  Copyright (C) 2015 IAU SOFA Board.  See notes at end.
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