upgrade ast 8.7.1

1 files changed, 0 insertions, 264 deletions

diff --git a/ast/erfa/apco.c b/ast/erfa/apco.c
deleted file mode 100644
index 1b61ab8..0000000
--- a/ast/erfa/apco.c
+++ /dev/null
@@ -1,264 +0,0 @@
-#include "erfa.h"
-
-void eraApco(double date1, double date2,
-             double ebpv[2][3], double ehp[3],
-             double x, double y, double s, double theta,
-             double elong, double phi, double hm,
-             double xp, double yp, double sp,
-             double refa, double refb,
-             eraASTROM *astrom)
-/*
-**  - - - - - - - -
-**   e r a A p c o
-**  - - - - - - - -
-**
-**  For a terrestrial observer, prepare star-independent astrometry
-**  parameters for transformations between ICRS and observed
-**  coordinates.  The caller supplies the Earth ephemeris, the Earth
-**  rotation information and the refraction constants as well as the
-**  site coordinates.
-**
-**  Given:
-**     date1  double       TDB as a 2-part...
-**     date2  double       ...Julian Date (Note 1)
-**     ebpv   double[2][3] Earth barycentric PV (au, au/day, Note 2)
-**     ehp    double[3]    Earth heliocentric P (au, Note 2)
-**     x,y    double       CIP X,Y (components of unit vector)
-**     s      double       the CIO locator s (radians)
-**     theta  double       Earth rotation angle (radians)
-**     elong  double       longitude (radians, east +ve, Note 3)
-**     phi    double       latitude (geodetic, radians, Note 3)
-**     hm     double       height above ellipsoid (m, geodetic, Note 3)
-**     xp,yp  double       polar motion coordinates (radians, Note 4)
-**     sp     double       the TIO locator s' (radians, Note 4)
-**     refa   double       refraction constant A (radians, Note 5)
-**     refb   double       refraction constant B (radians, Note 5)
-**
-**  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)
-**
-**  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) The vectors eb, eh, and all the astrom vectors, are with respect
-**     to BCRS axes.
-**
-**  3) The geographical coordinates are with respect to the ERFA_WGS84
-**     reference ellipsoid.  TAKE CARE WITH THE LONGITUDE SIGN
-**     CONVENTION:  the longitude required by the present function is
-**     right-handed, i.e. east-positive, in accordance with geographical
-**     convention.
-**
-**  4) xp and yp are the coordinates (in radians) of the Celestial
-**     Intermediate Pole with respect to the International Terrestrial
-**     Reference System (see IERS Conventions), measured along the
-**     meridians 0 and 90 deg west respectively.  sp is the TIO locator
-**     s', in radians, which positions the Terrestrial Intermediate
-**     Origin on the equator.  For many applications, xp, yp and
-**     (especially) sp can be set to zero.
-**
-**     Internally, the polar motion is stored in a form rotated onto the
-**     local meridian.
-**
-**  5) The refraction constants refa and refb are for use in a
-**     dZ = A*tan(Z)+B*tan^3(Z) model, where Z is the observed
-**     (i.e. refracted) zenith distance and dZ is the amount of
-**     refraction.
-**
-**  6) 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.
-**
-**  7) In cases where the caller does not wish to provide the Earth
-**     Ephemeris, the Earth rotation information and refraction
-**     constants, the function eraApco13 can be used instead of the
-**     present function.  This starts from UTC and weather readings etc.
-**     and computes suitable values using other ERFA functions.
-**
-**  8) 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.
-**
-**  9) The context structure astrom produced by this function is used by
-**     eraAtioq, eraAtoiq, eraAtciq* and eraAticq*.
-**
-**  Called:
-**     eraAper      astrometry parameters: update ERA
-**     eraC2ixys    celestial-to-intermediate matrix, given X,Y and s
-**     eraPvtob     position/velocity of terrestrial station
-**     eraTrxpv     product of transpose of r-matrix and pv-vector
-**     eraApcs      astrometry parameters, ICRS-GCRS, space observer
-**     eraCr        copy r-matrix
-**
-**  Copyright (C) 2013-2016, NumFOCUS Foundation.
-**  Derived, with permission, from the SOFA library.  See notes at end of file.
-*/
-{
-   double sl, cl, r[3][3], pvc[2][3], pv[2][3];
-
-
-/* Longitude with adjustment for TIO locator s'. */
-   astrom->along = elong + sp;
-
-/* Polar motion, rotated onto the local meridian. */
-   sl = sin(astrom->along);
-   cl = cos(astrom->along);
-   astrom->xpl = xp*cl - yp*sl;
-   astrom->ypl = xp*sl + yp*cl;
-
-/* Functions of latitude. */
-   astrom->sphi = sin(phi);
-   astrom->cphi = cos(phi);
-
-/* Refraction constants. */
-   astrom->refa = refa;
-   astrom->refb = refb;
-
-/* Local Earth rotation angle. */
-   eraAper(theta, astrom);
-
-/* Disable the (redundant) diurnal aberration step. */
-   astrom->diurab = 0.0;
-
-/* CIO based BPN matrix. */
-   eraC2ixys(x, y, s, r);
-
-/* Observer's geocentric position and velocity (m, m/s, CIRS). */
-   eraPvtob(elong, phi, hm, xp, yp, sp, theta, pvc);
-
-/* Rotate into GCRS. */
-   eraTrxpv(r, pvc, pv);
-
-/* ICRS <-> GCRS parameters. */
-   eraApcs(date1, date2, pv, ebpv, ehp, astrom);
-
-/* Store the CIO based BPN matrix. */
-   eraCr(r, astrom->bpn );
-
-/* 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.
-**  
-*/