update ast

1 files changed, 0 insertions, 116 deletions

diff --git a/ast/pal/palRvlsrk.c b/ast/pal/palRvlsrk.c
deleted file mode 100644
index 968188a..0000000
--- a/ast/pal/palRvlsrk.c
+++ /dev/null
@@ -1,116 +0,0 @@
-/*
-*+
-*  Name:
-*     palRvlsrk
-
-*  Purpose:
-*     Velocity component in a given direction due to the Sun's motion
-*     with respect to an adopted kinematic Local Standard of Rest.
-
-*  Language:
-*     Starlink ANSI C
-
-*  Type of Module:
-*     Library routine
-
-*  Invocation:
-*     double palRvlsrk( double r2000, double d2000 )
-
-*  Arguments:
-*     r2000 = double (Given)
-*        J2000.0 mean RA (radians)
-*     d2000 = double (Given)
-*        J2000.0 mean Dec (radians)
-
-*  Returned Value:
-*     Component of "standard" solar motion in direction R2000,D2000 (km/s).
-
-*  Description:
-*     This function returns the velocity component in a given direction
-*     due to the Sun's motion with respect to an adopted kinematic
-*     Local Standard of Rest. The result is +ve when the Sun is receding
-*     from the given point on the sky.
-
-*  Notes:
-*     - The Local Standard of Rest used here is one of several
-*     "kinematical" LSRs in common use.  A kinematical LSR is the mean
-*     standard of rest of specified star catalogues or stellar
-*     populations.  The Sun's motion with respect to a kinematical LSR
-*     is known as the "standard" solar motion.
-*     - There is another sort of LSR, the "dynamical" LSR, which is a
-*     point in the vicinity of the Sun which is in a circular orbit
-*     around the Galactic centre.  The Sun's motion with respect to
-*     the dynamical LSR is called the "peculiar" solar motion.  To
-*     obtain a radial velocity correction with respect to the
-*     dynamical LSR use the routine palRvlsrd.
-
-*  Reference:
-*     - Delhaye (1965), in "Stars and Stellar Systems", vol 5, p73.
-
-*  Authors:
-*     PTW: Pat Wallace (STFC)
-*     DSB: David Berry (JAC, Hawaii)
-*     {enter_new_authors_here}
-
-*  History:
-*     2012-02-16 (DSB):
-*        Initial version.
-*        Adapted with permission from the Fortran SLALIB library.
-*     {enter_further_changes_here}
-
-*  Copyright:
-*     Copyright (C) 1995 Rutherford Appleton Laboratory
-*     Copyright (C) 2012 Science and Technology Facilities Council.
-*     All Rights Reserved.
-
-*  Licence:
-*     This program is free software: you can redistribute it and/or
-*     modify it under the terms of the GNU Lesser General Public
-*     License as published by the Free Software Foundation, either
-*     version 3 of the License, or (at your option) any later
-*     version.
-*
-*     This program is distributed in the hope that it will be useful,
-*     but WITHOUT ANY WARRANTY; without even the implied warranty of
-*     MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE.  See the
-*     GNU Lesser General Public License for more details.
-*
-*     You should have received a copy of the GNU Lesser General
-*     License along with this program.  If not, see
-*     <http://www.gnu.org/licenses/>.
-
-*  Bugs:
-*     {note_any_bugs_here}
-*-
-*/
-
-#include "pal.h"
-#include "pal1sofa.h"
-
-double palRvlsrk( double r2000, double d2000 ){
-
-/* Local Variables: */
-   double vb[ 3 ];
-
-/*
-*  Standard solar motion (from Methods of Experimental Physics, ed Meeks,
-*  vol 12, part C, sec 6.1.5.2, p281):
-*
-*  20 km/s towards RA 18h Dec +30d (1900).
-*
-*  The solar motion is expressed here in the form of a J2000.0
-*  equatorial Cartesian vector:
-*
-*      VA(1) = X = -SPEED*COS(RA)*COS(DEC)
-*      VA(2) = Y = -SPEED*SIN(RA)*COS(DEC)
-*      VA(3) = Z = -SPEED*SIN(DEC)
-*/
-
-   double va[ 3 ] = { -0.29000, +17.31726, -10.00141 };
-
-/* Convert given J2000 RA,Dec to x,y,z. */
-   eraS2c( r2000, d2000, vb );
-
-/* Compute dot product with Solar motion vector. */
-   return eraPdp( va, vb );
-}