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Diffstat (limited to 'ast/pal/palMapqkz.c')
| -rw-r--r-- | ast/pal/palMapqkz.c | 150 |
1 files changed, 0 insertions, 150 deletions
diff --git a/ast/pal/palMapqkz.c b/ast/pal/palMapqkz.c deleted file mode 100644 index 44a2c79..0000000 --- a/ast/pal/palMapqkz.c +++ /dev/null @@ -1,150 +0,0 @@ -/* -*+ -* Name: -* palMapqkz - -* Purpose: -* Quick mean to apparent place (no proper motion or parallax). - -* Language: -* Starlink ANSI C - -* Type of Module: -* Library routine - -* Invocation: -* void palMapqkz( double rm, double dm, double amprms[21], -* double *ra, double *da ) - -* Arguments: -* rm = double (Given) -* Mean RA (radians). -* dm = double (Given) -* Mean Dec (radians). -* amprms = double[21] (Given) -* Star-independent mean-to-apparent parameters (see palMappa): -* (0-3) not used -* (4-6) heliocentric direction of the Earth (unit vector) -* (7) not used -* (8-10) abv: barycentric Earth velocity in units of c -* (11) sqrt(1-v^2) where v=modulus(abv) -* (12-20) precession/nutation (3,3) matrix -* ra = double * (Returned) -* Apparent RA (radians). -* da = double * (Returned) -* Apparent Dec (radians). - -* Description: -* Quick mean to apparent place: transform a star RA,dec from -* mean place to geocentric apparent place, given the -* star-independent parameters, and assuming zero parallax -* and proper motion. -* -* Use of this function is appropriate when efficiency is important -* and where many star positions, all with parallax and proper -* motion either zero or already allowed for, and all referred to -* the same equator and equinox, are to be transformed for one -* epoch. The star-independent parameters can be obtained by -* calling the palMappa function. -* -* The corresponding function for the case of non-zero parallax -* and proper motion is palMapqk. - -* Notes: -* - The reference systems and timescales used are IAU 2006. -* - The mean place rm, dm and the vectors amprms[1-3] and amprms[4-6] -* are referred to the mean equinox and equator of the epoch -* specified when generating the precession/nutation matrix -* amprms[12-20]. In the call to palMappa (q.v.) normally used -* to populate amprms, this epoch is the first argument (eq). -* - The vector amprms(4-6) is referred to the mean equinox and -* equator of epoch eq. -* - Strictly speaking, the routine is not valid for solar-system -* sources, though the error will usually be extremely small. -* However, to prevent gross errors in the case where the -* position of the Sun is specified, the gravitational -* deflection term is restrained within about 920 arcsec of the -* centre of the Sun's disc. The term has a maximum value of -* about 1.85 arcsec at this radius, and decreases to zero as -* the centre of the disc is approached. - -* Authors: -* PTW: Pat Wallace (STFC) -* {enter_new_authors_here} - -* History: -* 2012-02-13 (PTW): -* Initial version. -* Adapted with permission from the Fortran SLALIB library. -* {enter_further_changes_here} - -* Copyright: -* Copyright (C) 1999 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" - -void palMapqkz ( double rm, double dm, double amprms[21], double *ra, - double *da ){ - -/* Local Variables: */ - int i; - double ab1, abv[3], p[3], w, p1dv, p2[3], p3[3]; - double gr2e, pde, pdep1, ehn[3], p1[3]; - -/* Unpack scalar and vector parameters. */ - ab1 = amprms[11]; - gr2e = amprms[7]; - for( i = 0; i < 3; i++ ) { - abv[i] = amprms[i+8]; - ehn[i] = amprms[i+4]; - } - -/* Spherical to x,y,z. */ - eraS2c( rm, dm, p ); - -/* Light deflection (restrained within the Sun's disc) */ - pde = eraPdp( p, ehn ); - pdep1 = pde + 1.0; - w = gr2e / ( pdep1 > 1.0e-5 ? pdep1 : 1.0e-5 ); - for( i = 0; i < 3; i++) { - p1[i] = p[i] + w * ( ehn[i] - pde * p[i] ); - } - -/* Aberration. */ - p1dv = eraPdp( p1, abv ); - w = 1.0 + p1dv / ( ab1 + 1.0 ); - for( i = 0; i < 3; i++ ) { - p2[i] = ( ( ab1 * p1[i] ) + ( w * abv[i] ) ); - } - -/* Precession and nutation. */ - eraRxp( (double(*)[3]) &rms[12], p2, p3 ); - -/* Geocentric apparent RA,dec. */ - eraC2s( p3, ra, da ); - *ra = eraAnp( *ra ); -} |