upgrade AST

1 files changed, 0 insertions, 287 deletions

diff --git a/ast/erfa/apco13.c b/ast/erfa/apco13.c
deleted file mode 100644
index cdd4d4f..0000000
--- a/ast/erfa/apco13.c
+++ /dev/null
@@ -1,287 +0,0 @@
-#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.
-**  
-*/