update ast 8.6.3

1 files changed, 176 insertions, 0 deletions

diff --git a/ast/erfa/c2tpe.c b/ast/erfa/c2tpe.c
new file mode 100644
index 0000000..c6e4bda
--- /dev/null
+++ b/ast/erfa/c2tpe.c
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+#include "erfa.h"
+
+void eraC2tpe(double tta, double ttb, double uta, double utb,
+              double dpsi, double deps, double xp, double yp,
+              double rc2t[3][3])
+/*
+**  - - - - - - - - -
+**   e r a C 2 t p e
+**  - - - - - - - - -
+**
+**  Form the celestial to terrestrial matrix given the date, the UT1,
+**  the nutation and the polar motion.  IAU 2000.
+**
+**  Given:
+**     tta,ttb    double        TT as a 2-part Julian Date (Note 1)
+**     uta,utb    double        UT1 as a 2-part Julian Date (Note 1)
+**     dpsi,deps  double        nutation (Note 2)
+**     xp,yp      double        coordinates of the pole (radians, Note 3)
+**
+**  Returned:
+**     rc2t       double[3][3]  celestial-to-terrestrial matrix (Note 4)
+**
+**  Notes:
+**
+**  1) The TT and UT1 dates tta+ttb and uta+utb are Julian Dates,
+**     apportioned in any convenient way between the arguments uta and
+**     utb.  For example, JD(UT1)=2450123.7 could be expressed in any of
+**     these ways, among others:
+**
+**             uta            utb
+**
+**         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 and MJD methods are good compromises
+**     between resolution and convenience.  In the case of uta,utb, the
+**     date & time method is best matched to the Earth rotation angle
+**     algorithm used:  maximum precision is delivered when the uta
+**     argument is for 0hrs UT1 on the day in question and the utb
+**     argument lies in the range 0 to 1, or vice versa.
+**
+**  2) The caller is responsible for providing the nutation components;
+**     they are in longitude and obliquity, in radians and are with
+**     respect to the equinox and ecliptic of date.  For high-accuracy
+**     applications, free core nutation should be included as well as
+**     any other relevant corrections to the position of the CIP.
+**
+**  3) The arguments xp and yp 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 to 0 and 90 deg west respectively.
+**
+**  4) The matrix rc2t transforms from celestial to terrestrial
+**     coordinates:
+**
+**        [TRS] = RPOM * R_3(GST) * RBPN * [CRS]
+**
+**              = rc2t * [CRS]
+**
+**     where [CRS] is a vector in the Geocentric Celestial Reference
+**     System and [TRS] is a vector in the International Terrestrial
+**     Reference System (see IERS Conventions 2003), RBPN is the
+**     bias-precession-nutation matrix, GST is the Greenwich (apparent)
+**     Sidereal Time and RPOM is the polar motion matrix.
+**
+**  5) Although its name does not include "00", This function is in fact
+**     specific to the IAU 2000 models.
+**
+**  Called:
+**     eraPn00      bias/precession/nutation results, IAU 2000
+**     eraGmst00    Greenwich mean sidereal time, IAU 2000
+**     eraSp00      the TIO locator s', IERS 2000
+**     eraEe00      equation of the equinoxes, IAU 2000
+**     eraPom00     polar motion matrix
+**     eraC2teqx    form equinox-based celestial-to-terrestrial matrix
+**
+**  Reference:
+**
+**     McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003),
+**     IERS Technical Note No. 32, BKG (2004)
+**
+**  Copyright (C) 2013-2016, NumFOCUS Foundation.
+**  Derived, with permission, from the SOFA library.  See notes at end of file.
+*/
+{
+   double epsa, rb[3][3], rp[3][3], rbp[3][3], rn[3][3],
+          rbpn[3][3], gmst, ee, sp, rpom[3][3];
+
+
+/* Form the celestial-to-true matrix for this TT. */
+   eraPn00(tta, ttb, dpsi, deps, &epsa, rb, rp, rbp, rn, rbpn);
+
+/* Predict the Greenwich Mean Sidereal Time for this UT1 and TT. */
+   gmst = eraGmst00(uta, utb, tta, ttb);
+
+/* Predict the equation of the equinoxes given TT and nutation. */
+   ee = eraEe00(tta, ttb, epsa, dpsi);
+
+/* Estimate s'. */
+   sp = eraSp00(tta, ttb);
+
+/* Form the polar motion matrix. */
+   eraPom00(xp, yp, sp, rpom);
+
+/* Combine to form the celestial-to-terrestrial matrix. */
+   eraC2teqx(rbpn, gmst + ee, rpom, rc2t);
+
+   return;
+
+}
+/*----------------------------------------------------------------------
+**  
+**  
+**  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.
+**  
+*/