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/* |
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*+ |
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* Name: |
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* palMapqk |
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* Purpose: |
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* Quick mean to apparent place |
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* Language: |
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* Starlink ANSI C |
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* Type of Module: |
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* Library routine |
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* Invocation: |
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* void palMapqk ( double rm, double dm, double pr, double pd, |
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* double px, double rv, double amprms[21], |
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* double *ra, double *da ); |
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* Arguments: |
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* rm = double (Given) |
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* Mean RA (radians) |
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* dm = double (Given) |
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* Mean declination (radians) |
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* pr = double (Given) |
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* RA proper motion, changes per Julian year (radians) |
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* pd = double (Given) |
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* Dec proper motion, changes per Julian year (radians) |
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* px = double (Given) |
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* Parallax (arcsec) |
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* rv = double (Given) |
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* Radial velocity (km/s, +ve if receding) |
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* amprms = double [21] (Given) |
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* Star-independent mean-to-apparent parameters (see palMappa). |
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* ra = double * (Returned) |
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* Apparent RA (radians) |
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* dec = double * (Returned) |
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* Apparent dec (radians) |
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* Description: |
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* Quick mean to apparent place: transform a star RA,Dec from |
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* mean place to geocentric apparent place, given the |
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* star-independent parameters. |
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* |
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* Use of this routine is appropriate when efficiency is important |
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* and where many star positions, all referred to the same equator |
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* and equinox, are to be transformed for one epoch. The |
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* star-independent parameters can be obtained by calling the |
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* palMappa routine. |
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* |
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* If the parallax and proper motions are zero the palMapqkz |
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* routine can be used instead. |
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* Notes: |
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* - The reference frames and timescales used are post IAU 2006. |
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* - The mean place rm, dm and the vectors amprms[1-3] and amprms[4-6] |
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* are referred to the mean equinox and equator of the epoch |
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* specified when generating the precession/nutation matrix |
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* amprms[12-20]. In the call to palMappa (q.v.) normally used |
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* to populate amprms, this epoch is the first argument (eq). |
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* - Strictly speaking, the routine is not valid for solar-system |
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* sources, though the error will usually be extremely small. |
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* However, to prevent gross errors in the case where the |
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* position of the Sun is specified, the gravitational |
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* deflection term is restrained within about 920 arcsec of the |
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* centre of the Sun's disc. The term has a maximum value of |
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* about 1.85 arcsec at this radius, and decreases to zero as |
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* the centre of the disc is approached. |
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* Authors: |
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* PTW: Patrick T. Wallace |
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* TIMJ: Tim Jenness (JAC, Hawaii) |
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* {enter_new_authors_here} |
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* History: |
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* 2012-03-01 (TIMJ): |
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* Initial version with documentation from SLA/F |
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* Adapted with permission from the Fortran SLALIB library. |
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* {enter_further_changes_here} |
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* Copyright: |
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* Copyright (C) 2000 Rutherford Appleton Laboratory |
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* Copyright (C) 2012 Science and Technology Facilities Council. |
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* All Rights Reserved. |
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* Licence: |
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* This program is free software; you can redistribute it and/or |
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* modify it under the terms of the GNU General Public License as |
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* published by the Free Software Foundation; either version 3 of |
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* the License, or (at your option) any later version. |
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* |
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* This program is distributed in the hope that it will be |
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* useful, but WITHOUT ANY WARRANTY; without even the implied |
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* warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR |
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* PURPOSE. See the GNU General Public License for more details. |
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* |
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* You should have received a copy of the GNU General Public License |
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* along with this program; if not, write to the Free Software |
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* Foundation, Inc., 51 Franklin Street, Fifth Floor, Boston, |
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* MA 02110-1301, USA. |
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* Bugs: |
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* {note_any_bugs_here} |
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*- |
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*/ |
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#include "pal.h" |
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#include "palmac.h" |
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#include "pal1sofa.h" |
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1
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void palMapqk ( double rm, double dm, double pr, double pd, |
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double px, double rv, double amprms[21], |
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double *ra, double *da ) { |
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/* local constants */ |
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const double VF = 0.210945028; /* Km/s to AU/year */ |
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/* Local Variables: */ |
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int i; |
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double ab1, abv[3], p[3], w, p1dv, p2[3], p3[3]; |
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double pmt, gr2e, eb[3], q[3], pxr, em[3]; |
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double pde, pdep1, p1[3], ehn[3], pn[3]; |
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/* Unpack scalar and vector parameters. */ |
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1
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pmt = amprms[0]; |
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1
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gr2e = amprms[7]; |
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1
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ab1 = amprms[11]; |
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4
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for( i = 0; i < 3; i++ ) { |
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eb[i] = amprms[i+1]; |
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3
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ehn[i] = amprms[i+4]; |
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3
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abv[i] = amprms[i+8]; |
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} |
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/* Spherical to x,y,z. */ |
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1
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eraS2c( rm, dm, q); |
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/* Space motion (radians per year) */ |
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1
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pxr = px * PAL__DAS2R; |
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1
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w = VF * rv * pxr; |
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em[0] = -pr * q[1] - pd * cos(rm) * sin(dm) + w * q[0]; |
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1
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em[1] = pr * q[0] - pd * sin(rm) * sin(dm) + w * q[1]; |
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em[2] = pd * cos(dm) + w * q[2]; |
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/* Geocentric direction of star (normalised) */ |
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4
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for( i = 0; i < 3; i++ ) { |
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3
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p[i] = q[i] + pmt * em[i] - pxr * eb[i]; |
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} |
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eraPn( p, &w, pn ); |
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150
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/* Light deflection (restrained within the Sun's disc) */ |
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pde = eraPdp( pn, ehn ); |
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1
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pdep1 = pde + 1.0; |
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1
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w = gr2e / ( pdep1 > 1.0e-5 ? pdep1 : 1.0e-5 ); |
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4
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for( i = 0; i < 3; i++) { |
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3
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p1[i] = pn[i] + w * ( ehn[i] - pde * pn[i] ); |
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} |
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/* Aberration (normalisation omitted). */ |
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p1dv = eraPdp( p, abv ); |
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w = 1.0 + p1dv / ( ab1 + 1.0 ); |
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4
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for( i = 0; i < 3; i++ ) { |
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3
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p2[i] = ( ab1 * p1[i] ) + ( w * abv[i] ); |
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} |
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165
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/* Precession and nutation. */ |
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1
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eraRxp( (double(*)[3]) &rms[12], p2, p3 ); |
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168
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/* Geocentric apparent RA,dec. */ |
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1
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eraC2s( p3, ra, da ); |
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*ra = eraAnp( *ra ); |
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1
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} |