update ast 8.6.3

1 files changed, 214 insertions, 0 deletions

diff --git a/ast/erfa/starpm.c b/ast/erfa/starpm.c
new file mode 100644
index 0000000..69b7708
--- /dev/null
+++ b/ast/erfa/starpm.c
@@ -0,0 +1,214 @@
+#include "erfa.h"
+
+int eraStarpm(double ra1, double dec1,
+              double pmr1, double pmd1, double px1, double rv1,
+              double ep1a, double ep1b, double ep2a, double ep2b,
+              double *ra2, double *dec2,
+              double *pmr2, double *pmd2, double *px2, double *rv2)
+/*
+**  - - - - - - - - - -
+**   e r a S t a r p m
+**  - - - - - - - - - -
+**
+**  Star proper motion:  update star catalog data for space motion.
+**
+**  Given:
+**     ra1    double     right ascension (radians), before
+**     dec1   double     declination (radians), before
+**     pmr1   double     RA proper motion (radians/year), before
+**     pmd1   double     Dec proper motion (radians/year), before
+**     px1    double     parallax (arcseconds), before
+**     rv1    double     radial velocity (km/s, +ve = receding), before
+**     ep1a   double     "before" epoch, part A (Note 1)
+**     ep1b   double     "before" epoch, part B (Note 1)
+**     ep2a   double     "after" epoch, part A (Note 1)
+**     ep2b   double     "after" epoch, part B (Note 1)
+**
+**  Returned:
+**     ra2    double     right ascension (radians), after
+**     dec2   double     declination (radians), after
+**     pmr2   double     RA proper motion (radians/year), after
+**     pmd2   double     Dec proper motion (radians/year), after
+**     px2    double     parallax (arcseconds), after
+**     rv2    double     radial velocity (km/s, +ve = receding), after
+**
+**  Returned (function value):
+**            int        status:
+**                          -1 = system error (should not occur)
+**                           0 = no warnings or errors
+**                           1 = distance overridden (Note 6)
+**                           2 = excessive velocity (Note 7)
+**                           4 = solution didn't converge (Note 8)
+**                        else = binary logical OR of the above warnings
+**
+**  Notes:
+**
+**  1) The starting and ending TDB dates ep1a+ep1b and ep2a+ep2b are
+**     Julian Dates, apportioned in any convenient way between the two
+**     parts (A and B).  For example, JD(TDB)=2450123.7 could be
+**     expressed in any of these ways, among others:
+**
+**             epna          epnb
+**
+**         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.
+**
+**  2) In accordance with normal star-catalog conventions, the object's
+**     right ascension and declination are freed from the effects of
+**     secular aberration.  The frame, which is aligned to the catalog
+**     equator and equinox, is Lorentzian and centered on the SSB.
+**
+**     The proper motions are the rate of change of the right ascension
+**     and declination at the catalog epoch and are in radians per TDB
+**     Julian year.
+**
+**     The parallax and radial velocity are in the same frame.
+**
+**  3) Care is needed with units.  The star coordinates are in radians
+**     and the proper motions in radians per Julian year, but the
+**     parallax is in arcseconds.
+**
+**  4) The RA proper motion is in terms of coordinate angle, not true
+**     angle.  If the catalog uses arcseconds for both RA and Dec proper
+**     motions, the RA proper motion will need to be divided by cos(Dec)
+**     before use.
+**
+**  5) Straight-line motion at constant speed, in the inertial frame,
+**     is assumed.
+**
+**  6) An extremely small (or zero or negative) parallax is interpreted
+**     to mean that the object is on the "celestial sphere", the radius
+**     of which is an arbitrary (large) value (see the eraStarpv
+**     function for the value used).  When the distance is overridden in
+**     this way, the status, initially zero, has 1 added to it.
+**
+**  7) If the space velocity is a significant fraction of c (see the
+**     constant VMAX in the function eraStarpv), it is arbitrarily set
+**     to zero.  When this action occurs, 2 is added to the status.
+**
+**  8) The relativistic adjustment carried out in the eraStarpv function
+**     involves an iterative calculation.  If the process fails to
+**     converge within a set number of iterations, 4 is added to the
+**     status.
+**
+**  Called:
+**     eraStarpv    star catalog data to space motion pv-vector
+**     eraPvu       update a pv-vector
+**     eraPdp       scalar product of two p-vectors
+**     eraPvstar    space motion pv-vector to star catalog data
+**
+**  Copyright (C) 2013-2016, NumFOCUS Foundation.
+**  Derived, with permission, from the SOFA library.  See notes at end of file.
+*/
+{
+   double pv1[2][3], tl1, dt, pv[2][3], r2, rdv, v2, c2mv2, tl2,
+          pv2[2][3];
+   int j1, j2, j;
+
+
+/* RA,Dec etc. at the "before" epoch to space motion pv-vector. */
+   j1 = eraStarpv(ra1, dec1, pmr1, pmd1, px1, rv1, pv1);
+
+/* Light time when observed (days). */
+   tl1 = eraPm(pv1[0]) / ERFA_DC;
+
+/* Time interval, "before" to "after" (days). */
+   dt = (ep2a - ep1a) + (ep2b - ep1b);
+
+/* Move star along track from the "before" observed position to the */
+/* "after" geometric position. */
+   eraPvu(dt + tl1, pv1, pv);
+
+/* From this geometric position, deduce the observed light time (days) */
+/* at the "after" epoch (with theoretically unneccessary error check). */
+   r2 = eraPdp(pv[0], pv[0]);
+   rdv = eraPdp(pv[0], pv[1]);
+   v2 = eraPdp(pv[1], pv[1]);
+   c2mv2 = ERFA_DC*ERFA_DC - v2;
+   if (c2mv2 <=  0) return -1;
+   tl2 = (-rdv + sqrt(rdv*rdv + c2mv2*r2)) / c2mv2;
+
+/* Move the position along track from the observed place at the */
+/* "before" epoch to the observed place at the "after" epoch. */
+   eraPvu(dt + (tl1 - tl2), pv1, pv2);
+
+/* Space motion pv-vector to RA,Dec etc. at the "after" epoch. */
+   j2 = eraPvstar(pv2, ra2, dec2, pmr2, pmd2, px2, rv2);
+
+/* Final status. */
+   j = (j2 == 0) ? j1 : -1;
+
+   return j;
+
+}
+/*----------------------------------------------------------------------
+**  
+**  
+**  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.
+**  
+*/