diff options
Diffstat (limited to 'ast/pal/palRvlsrd.c')
-rw-r--r-- | ast/pal/palRvlsrd.c | 116 |
1 files changed, 0 insertions, 116 deletions
diff --git a/ast/pal/palRvlsrd.c b/ast/pal/palRvlsrd.c deleted file mode 100644 index 4c93426..0000000 --- a/ast/pal/palRvlsrd.c +++ /dev/null @@ -1,116 +0,0 @@ -/* -*+ -* Name: -* palRvlsrd - -* Purpose: -* Velocity component in a given direction due to the Sun's motion -* with respect to the dynamical Local Standard of Rest. - -* Language: -* Starlink ANSI C - -* Type of Module: -* Library routine - -* Invocation: -* double palRvlsrd( 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 "peculiar" 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 the dynamical 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 the "dynamical" LSR, -* 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. -* - There is another type of LSR, called a "kinematical" LSR. A -* kinematical LSR is the mean standard of rest of specified star -* catalogues or stellar populations, and several slightly different -* kinematical LSRs are in use. The Sun's motion with respect to an -* agreed kinematical LSR is known as the "standard" solar motion. -* To obtain a radial velocity correction with respect to an adopted -* kinematical LSR use the routine sla_RVLSRK. - -* 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 palRvlsrd( double r2000, double d2000 ){ - -/* Local Variables: */ - double vb[ 3 ]; - -/* -* Peculiar solar motion from Delhaye 1965: in Galactic Cartesian -* coordinates (+9,+12,+7) km/s. This corresponds to about 16.6 km/s -* towards Galactic coordinates L2 = 53 deg, B2 = +25 deg, or RA,Dec -* 17 49 58.7 +28 07 04 J2000. -* -* 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 ] = { +0.63823, +14.58542, -7.80116 }; - -/* Convert given J2000 RA,Dec to x,y,z. */ - eraS2c( r2000, d2000, vb ); - -/* Compute dot product with Solar motion vector. */ - return eraPdp( va, vb ); -} |