update ast 8.6.2

1 files changed, 264 insertions, 0 deletions

diff --git a/ast/erfa/apco.c b/ast/erfa/apco.c
new file mode 100644
index 0000000..1b61ab8
--- /dev/null
+++ b/ast/erfa/apco.c
@@ -0,0 +1,264 @@
+#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.
+**  
+*/