update ast 8.6.2

1 files changed, 287 insertions, 0 deletions

diff --git a/ast/erfa/apco13.c b/ast/erfa/apco13.c
new file mode 100644
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+++ b/ast/erfa/apco13.c
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+#include "erfa.h"
+
+int eraApco13(double utc1, double utc2, double dut1,
+              double elong, double phi, double hm, double xp, double yp,
+              double phpa, double tc, double rh, double wl,
+              eraASTROM *astrom, double *eo)
+/*
+**  - - - - - - - - - -
+**   e r a A p c o 1 3
+**  - - - - - - - - - -
+**
+**  For a terrestrial observer, prepare star-independent astrometry
+**  parameters for transformations between ICRS and observed
+**  coordinates.  The caller supplies UTC, site coordinates, ambient air
+**  conditions and observing wavelength, and ERFA models are used to
+**  obtain the Earth ephemeris, CIP/CIO and refraction constants.
+**
+**  The parameters produced by this function are required in the
+**  parallax, light deflection, aberration, and bias-precession-nutation
+**  parts of the ICRS/CIRS transformations.
+**
+**  Given:
+**     utc1   double     UTC as a 2-part...
+**     utc2   double     ...quasi Julian Date (Notes 1,2)
+**     dut1   double     UT1-UTC (seconds, Note 3)
+**     elong  double     longitude (radians, east +ve, Note 4)
+**     phi    double     latitude (geodetic, radians, Note 4)
+**     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 eraASTROM* 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)
+**     eo     double*    equation of the origins (ERA-GST)
+**
+**  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 eraDtf2d 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 eraDat 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 ERFA_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
+**      ephemeris, Earth rotation information and refraction constants,
+**      the function eraApco 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
+**
+**       eraApcg eraApcg13    geocentric      ICRS <-> GCRS
+**       eraApci eraApci13    terrestrial     ICRS <-> CIRS
+**       eraApco eraApco13    terrestrial     ICRS <-> observed
+**       eraApcs eraApcs13    space           ICRS <-> GCRS
+**       eraAper eraAper13    terrestrial     update Earth rotation
+**       eraApio eraApio13    terrestrial     CIRS <-> observed
+**
+**      Those with names ending in "13" use contemporary ERFA 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 eraAtioq, eraAtoiq, eraAtciq* and eraAticq*.
+**
+**  Called:
+**     eraUtctai    UTC to TAI
+**     eraTaitt     TAI to TT
+**     eraUtcut1    UTC to UT1
+**     eraEpv00     Earth position and velocity
+**     eraPnm06a    classical NPB matrix, IAU 2006/2000A
+**     eraBpn2xy    extract CIP X,Y coordinates from NPB matrix
+**     eraS06       the CIO locator s, given X,Y, IAU 2006
+**     eraEra00     Earth rotation angle, IAU 2000
+**     eraSp00      the TIO locator s', IERS 2000
+**     eraRefco     refraction constants for given ambient conditions
+**     eraApco      astrometry parameters, ICRS-observed
+**     eraEors      equation of the origins, given NPB matrix and s
+**
+**  Copyright (C) 2013-2016, NumFOCUS Foundation.
+**  Derived, with permission, from the SOFA library.  See notes at end of file.
+*/
+{
+   int j;
+   double tai1, tai2, tt1, tt2, ut11, ut12, ehpv[2][3], ebpv[2][3],
+          r[3][3], x, y, s, theta, sp, refa, refb;
+
+
+/* UTC to other time scales. */
+   j = eraUtctai(utc1, utc2, &tai1, &tai2);
+   if ( j < 0 ) return -1;
+   j = eraTaitt(tai1, tai2, &tt1, &tt2);
+   j = eraUtcut1(utc1, utc2, dut1, &ut11, &ut12);
+   if ( j < 0 ) return -1;
+
+/* Earth barycentric & heliocentric position/velocity (au, au/d). */
+   (void) eraEpv00(tt1, tt2, ehpv, ebpv);
+
+/* Form the equinox based BPN matrix, IAU 2006/2000A. */
+   eraPnm06a(tt1, tt2, r);
+
+/* Extract CIP X,Y. */
+   eraBpn2xy(r, &x, &y);
+
+/* Obtain CIO locator s. */
+   s = eraS06(tt1, tt2, x, y);
+
+/* Earth rotation angle. */
+   theta = eraEra00(ut11, ut12);
+
+/* TIO locator s'. */
+   sp = eraSp00(tt1, tt2);
+
+/* Refraction constants A and B. */
+   eraRefco(phpa, tc, rh, wl, &refa, &refb);
+
+/* Compute the star-independent astrometry parameters. */
+   eraApco(tt1, tt2, ebpv, ehpv[0], x, y, s, theta,
+           elong, phi, hm, xp, yp, sp, refa, refb, astrom);
+
+/* Equation of the origins. */
+   *eo = eraEors(r, s);
+
+/* Return any warning status. */
+   return j;
+
+/* Finished. */
+
+}
+/*----------------------------------------------------------------------
+**  
+**  
+**  Copyright (C) 2013-2016, NumFOCUS Foundation.
+**  All rights reserved.
+**  
+**  This library is derived, with permission, from the International
+**  Astronomical Union's "Standards of Fundamental Astronomy" library,
+**  available from http://www.iausofa.org.
+**  
+**  The ERFA version is intended to retain identical functionality to
+**  the SOFA library, but made distinct through different function and
+**  file names, as set out in the SOFA license conditions.  The SOFA
+**  original has a role as a reference standard for the IAU and IERS,
+**  and consequently redistribution is permitted only in its unaltered
+**  state.  The ERFA version is not subject to this restriction and
+**  therefore can be included in distributions which do not support the
+**  concept of "read only" software.
+**  
+**  Although the intent is to replicate the SOFA API (other than
+**  replacement of prefix names) and results (with the exception of
+**  bugs;  any that are discovered will be fixed), SOFA is not
+**  responsible for any errors found in this version of the library.
+**  
+**  If you wish to acknowledge the SOFA heritage, please acknowledge
+**  that you are using a library derived from SOFA, rather than SOFA
+**  itself.
+**  
+**  
+**  TERMS AND CONDITIONS
+**  
+**  Redistribution and use in source and binary forms, with or without
+**  modification, are permitted provided that the following conditions
+**  are met:
+**  
+**  1 Redistributions of source code must retain the above copyright
+**    notice, this list of conditions and the following disclaimer.
+**  
+**  2 Redistributions in binary form must reproduce the above copyright
+**    notice, this list of conditions and the following disclaimer in
+**    the documentation and/or other materials provided with the
+**    distribution.
+**  
+**  3 Neither the name of the Standards Of Fundamental Astronomy Board,
+**    the International Astronomical Union nor the names of its
+**    contributors may be used to endorse or promote products derived
+**    from this software without specific prior written permission.
+**  
+**  THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS
+**  "AS IS" AND ANY EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT
+**  LIMITED TO, THE IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS
+**  FOR A PARTICULAR PURPOSE ARE DISCLAIMED.  IN NO EVENT SHALL THE
+**  COPYRIGHT HOLDER OR CONTRIBUTORS BE LIABLE FOR ANY DIRECT, INDIRECT,
+**  INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING,
+**  BUT NOT LIMITED TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES;
+**  LOSS OF USE, DATA, OR PROFITS; OR BUSINESS INTERRUPTION) HOWEVER
+**  CAUSED AND ON ANY THEORY OF LIABILITY, WHETHER IN CONTRACT, STRICT
+**  LIABILITY, OR TORT (INCLUDING NEGLIGENCE OR OTHERWISE) ARISING IN
+**  ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE
+**  POSSIBILITY OF SUCH DAMAGE.
+**  
+*/