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authorWilliam Joye <wjoye@cfa.harvard.edu>2018-09-21 17:02:41 (GMT)
committerWilliam Joye <wjoye@cfa.harvard.edu>2018-09-21 17:02:41 (GMT)
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-/*
-*+
-* 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 );
-}