upgrade AST

1 files changed, 0 insertions, 273 deletions

diff --git a/ast/erfa/starpv.c b/ast/erfa/starpv.c
deleted file mode 100644
index 77173ed..0000000
--- a/ast/erfa/starpv.c
+++ /dev/null
@@ -1,273 +0,0 @@
-#include "erfa.h"
-
-int eraStarpv(double ra, double dec,
-              double pmr, double pmd, double px, double rv,
-              double pv[2][3])
-/*
-**  - - - - - - - - - -
-**   e r a S t a r p v
-**  - - - - - - - - - -
-**
-**  Convert star catalog coordinates to position+velocity vector.
-**
-**  Given (Note 1):
-**     ra     double        right ascension (radians)
-**     dec    double        declination (radians)
-**     pmr    double        RA proper motion (radians/year)
-**     pmd    double        Dec proper motion (radians/year)
-**     px     double        parallax (arcseconds)
-**     rv     double        radial velocity (km/s, positive = receding)
-**
-**  Returned (Note 2):
-**     pv     double[2][3]  pv-vector (AU, AU/day)
-**
-**  Returned (function value):
-**            int           status:
-**                              0 = no warnings
-**                              1 = distance overridden (Note 6)
-**                              2 = excessive speed (Note 7)
-**                              4 = solution didn't converge (Note 8)
-**                           else = binary logical OR of the above
-**
-**  Notes:
-**
-**  1) The star data accepted by this function are "observables" for an
-**     imaginary observer at the solar-system barycenter.  Proper motion
-**     and radial velocity are, strictly, in terms of barycentric
-**     coordinate time, TCB.  For most practical applications, it is
-**     permissible to neglect the distinction between TCB and ordinary
-**     "proper" time on Earth (TT/TAI).  The result will, as a rule, be
-**     limited by the intrinsic accuracy of the proper-motion and
-**     radial-velocity data;  moreover, the pv-vector is likely to be
-**     merely an intermediate result, so that a change of time unit
-**     would cancel out overall.
-**
-**     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.
-**
-**  2) The resulting position and velocity pv-vector is with respect to
-**     the same frame and, like the catalog coordinates, is freed from
-**     the effects of secular aberration.  Should the "coordinate
-**     direction", where the object was located at the catalog epoch, be
-**     required, it may be obtained by calculating the magnitude of the
-**     position vector pv[0][0-2] dividing by the speed of light in
-**     AU/day to give the light-time, and then multiplying the space
-**     velocity pv[1][0-2] by this light-time and adding the result to
-**     pv[0][0-2].
-**
-**     Summarizing, the pv-vector returned is for most stars almost
-**     identical to the result of applying the standard geometrical
-**     "space motion" transformation.  The differences, which are the
-**     subject of the Stumpff paper referenced below, are:
-**
-**     (i) In stars with significant radial velocity and proper motion,
-**     the constantly changing light-time distorts the apparent proper
-**     motion.  Note that this is a classical, not a relativistic,
-**     effect.
-**
-**     (ii) The transformation complies with special relativity.
-**
-**  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; the radial velocity is in km/s, but
-**     the pv-vector result is in AU and AU/day.
-**
-**  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 constant PXMIN).
-**     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), it is arbitrarily set to zero.  When this action
-**     occurs, 2 is added to the status.
-**
-**  8) The relativistic adjustment involves an iterative calculation.
-**     If the process fails to converge within a set number (IMAX) of
-**     iterations, 4 is added to the status.
-**
-**  9) The inverse transformation is performed by the function
-**     eraPvstar.
-**
-**  Called:
-**     eraS2pv      spherical coordinates to pv-vector
-**     eraPm        modulus of p-vector
-**     eraZp        zero p-vector
-**     eraPn        decompose p-vector into modulus and direction
-**     eraPdp       scalar product of two p-vectors
-**     eraSxp       multiply p-vector by scalar
-**     eraPmp       p-vector minus p-vector
-**     eraPpp       p-vector plus p-vector
-**
-**  Reference:
-**
-**     Stumpff, P., 1985, Astron.Astrophys. 144, 232-240.
-**
-**  Copyright (C) 2013-2016, NumFOCUS Foundation.
-**  Derived, with permission, from the SOFA library.  See notes at end of file.
-*/
-{
-/* Smallest allowed parallax */
-   static const double PXMIN = 1e-7;
-
-/* Largest allowed speed (fraction of c) */
-   static const double VMAX = 0.5;
-
-/* Maximum number of iterations for relativistic solution */
-   static const int IMAX = 100;
-
-   int i, iwarn;
-   double w, r, rd, rad, decd, v, x[3], usr[3], ust[3],
-          vsr, vst, betst, betsr, bett, betr,
-          dd, ddel, ur[3], ut[3],
-          d = 0.0, del = 0.0,       /* to prevent */
-          odd = 0.0, oddel = 0.0,   /* compiler   */
-          od = 0.0, odel = 0.0;     /* warnings   */
-
-
-/* Distance (AU). */
-   if (px >= PXMIN) {
-      w = px;
-      iwarn = 0;
-   } else {
-      w = PXMIN;
-      iwarn = 1;
-   }
-   r = ERFA_DR2AS / w;
-
-/* Radial velocity (AU/day). */
-   rd = ERFA_DAYSEC * rv * 1e3 / ERFA_DAU;
-
-/* Proper motion (radian/day). */
-   rad = pmr / ERFA_DJY;
-   decd = pmd / ERFA_DJY;
-
-/* To pv-vector (AU,AU/day). */
-   eraS2pv(ra, dec, r, rad, decd, rd, pv);
-
-/* If excessive velocity, arbitrarily set it to zero. */
-   v = eraPm(pv[1]);
-   if (v / ERFA_DC > VMAX) {
-      eraZp(pv[1]);
-      iwarn += 2;
-   }
-
-/* Isolate the radial component of the velocity (AU/day). */
-   eraPn(pv[0], &w, x);
-   vsr = eraPdp(x, pv[1]);
-   eraSxp(vsr, x, usr);
-
-/* Isolate the transverse component of the velocity (AU/day). */
-   eraPmp(pv[1], usr, ust);
-   vst = eraPm(ust);
-
-/* Special-relativity dimensionless parameters. */
-   betsr = vsr / ERFA_DC;
-   betst = vst / ERFA_DC;
-
-/* Determine the inertial-to-observed relativistic correction terms. */
-   bett = betst;
-   betr = betsr;
-   for (i = 0; i < IMAX; i++) {
-      d = 1.0 + betr;
-      del = sqrt(1.0 - betr*betr - bett*bett) - 1.0;
-      betr = d * betsr + del;
-      bett = d * betst;
-      if (i > 0) {
-         dd = fabs(d - od);
-         ddel = fabs(del - odel);
-         if ((i > 1) && (dd >= odd) && (ddel >= oddel)) break;
-         odd = dd;
-         oddel = ddel;
-      }
-      od = d;
-      odel = del;
-   }
-   if (i >= IMAX) iwarn += 4;
-
-/* Replace observed radial velocity with inertial value. */
-   w = (betsr != 0.0) ? d + del / betsr : 1.0;
-   eraSxp(w, usr, ur);
-
-/* Replace observed tangential velocity with inertial value. */
-   eraSxp(d, ust, ut);
-
-/* Combine the two to obtain the inertial space velocity. */
-   eraPpp(ur, ut, pv[1]);
-
-/* Return the status. */
-   return iwarn;
-
-}
-/*----------------------------------------------------------------------
-**  
-**  
-**  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.
-**  
-*/