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Diffstat (limited to 'ast/erfa/aticqn.c')
| -rw-r--r-- | ast/erfa/aticqn.c | 237 |
1 files changed, 0 insertions, 237 deletions
diff --git a/ast/erfa/aticqn.c b/ast/erfa/aticqn.c deleted file mode 100644 index d69119e..0000000 --- a/ast/erfa/aticqn.c +++ /dev/null @@ -1,237 +0,0 @@ -#include "erfa.h" - -void eraAticqn(double ri, double di, eraASTROM *astrom, - int n, eraLDBODY b[], double *rc, double *dc) -/* -** - - - - - - - - - -** e r a A t i c q n -** - - - - - - - - - -** -** Quick CIRS to ICRS astrometric place transformation, given the star- -** independent astrometry parameters plus a list of light-deflecting -** bodies. -** -** Use of this function is appropriate when efficiency is important and -** where many star positions are all to be transformed for one date. -** The star-independent astrometry parameters can be obtained by -** calling one of the functions eraApci[13], eraApcg[13], eraApco[13] -** or eraApcs[13]. -* -* If the only light-deflecting body to be taken into account is the -* Sun, the eraAticq function can be used instead. -** -** Given: -** ri,di double CIRS RA,Dec (radians) -** astrom eraASTROM* star-independent astrometry parameters: -** pmt double PM time interval (SSB, Julian years) -** eb double[3] SSB to observer (vector, au) -** eh double[3] Sun to observer (unit vector) -** em double distance from Sun to observer (au) -** v double[3] barycentric observer velocity (vector, c) -** bm1 double sqrt(1-|v|^2): reciprocal of Lorenz factor -** bpn double[3][3] bias-precession-nutation matrix -** along double longitude + s' (radians) -** xpl double polar motion xp wrt local meridian (radians) -** ypl double polar motion yp wrt local meridian (radians) -** sphi double sine of geodetic latitude -** cphi double cosine of geodetic latitude -** diurab double magnitude of diurnal aberration vector -** eral double "local" Earth rotation angle (radians) -** refa double refraction constant A (radians) -** refb double refraction constant B (radians) -** n int number of bodies (Note 3) -** b eraLDBODY[n] data for each of the n bodies (Notes 3,4): -** bm double mass of the body (solar masses, Note 5) -** dl double deflection limiter (Note 6) -** pv [2][3] barycentric PV of the body (au, au/day) -** -** Returned: -** rc,dc double ICRS astrometric RA,Dec (radians) -** -** Notes: -** -** 1) Iterative techniques are used for the aberration and light -** deflection corrections so that the functions eraAticqn and -** eraAtciqn are accurate inverses; even at the edge of the Sun's -** disk the discrepancy is only about 1 nanoarcsecond. -** -** 2) If the only light-deflecting body to be taken into account is the -** Sun, the eraAticq function can be used instead. -** -** 3) The struct b contains n entries, one for each body to be -** considered. If n = 0, no gravitational light deflection will be -** applied, not even for the Sun. -** -** 4) The struct b should include an entry for the Sun as well as for -** any planet or other body to be taken into account. The entries -** should be in the order in which the light passes the body. -** -** 5) In the entry in the b struct for body i, the mass parameter -** b[i].bm can, as required, be adjusted in order to allow for such -** effects as quadrupole field. -** -** 6) The deflection limiter parameter b[i].dl is phi^2/2, where phi is -** the angular separation (in radians) between star and body at -** which limiting is applied. As phi shrinks below the chosen -** threshold, the deflection is artificially reduced, reaching zero -** for phi = 0. Example values suitable for a terrestrial -** observer, together with masses, are as follows: -** -** body i b[i].bm b[i].dl -** -** Sun 1.0 6e-6 -** Jupiter 0.00095435 3e-9 -** Saturn 0.00028574 3e-10 -** -** 7) For efficiency, validation of the contents of the b array is -** omitted. The supplied masses must be greater than zero, the -** position and velocity vectors must be right, and the deflection -** limiter greater than zero. -** -** Called: -** eraS2c spherical coordinates to unit vector -** eraTrxp product of transpose of r-matrix and p-vector -** eraZp zero p-vector -** eraAb stellar aberration -** eraLdn light deflection by n bodies -** eraC2s p-vector to spherical -** eraAnp normalize angle into range +/- pi -** -** Copyright (C) 2013-2016, NumFOCUS Foundation. -** Derived, with permission, from the SOFA library. See notes at end of file. -*/ -{ - int j, i; - double pi[3], ppr[3], pnat[3], pco[3], w, d[3], before[3], r2, r, - after[3]; - - -/* CIRS RA,Dec to Cartesian. */ - eraS2c(ri, di, pi); - -/* Bias-precession-nutation, giving GCRS proper direction. */ - eraTrxp(astrom->bpn, pi, ppr); - -/* Aberration, giving GCRS natural direction. */ - eraZp(d); - for (j = 0; j < 2; j++) { - r2 = 0.0; - for (i = 0; i < 3; i++) { - w = ppr[i] - d[i]; - before[i] = w; - r2 += w*w; - } - r = sqrt(r2); - for (i = 0; i < 3; i++) { - before[i] /= r; - } - eraAb(before, astrom->v, astrom->em, astrom->bm1, after); - r2 = 0.0; - for (i = 0; i < 3; i++) { - d[i] = after[i] - before[i]; - w = ppr[i] - d[i]; - pnat[i] = w; - r2 += w*w; - } - r = sqrt(r2); - for (i = 0; i < 3; i++) { - pnat[i] /= r; - } - } - -/* Light deflection, giving BCRS coordinate direction. */ - eraZp(d); - for (j = 0; j < 5; j++) { - r2 = 0.0; - for (i = 0; i < 3; i++) { - w = pnat[i] - d[i]; - before[i] = w; - r2 += w*w; - } - r = sqrt(r2); - for (i = 0; i < 3; i++) { - before[i] /= r; - } - eraLdn(n, b, astrom->eb, before, after); - r2 = 0.0; - for (i = 0; i < 3; i++) { - d[i] = after[i] - before[i]; - w = pnat[i] - d[i]; - pco[i] = w; - r2 += w*w; - } - r = sqrt(r2); - for (i = 0; i < 3; i++) { - pco[i] /= r; - } - } - -/* ICRS astrometric RA,Dec. */ - eraC2s(pco, &w, dc); - *rc = eraAnp(w); - -/* Finished. */ - -} -/*---------------------------------------------------------------------- -** -** -** Copyright (C) 2013-2016, NumFOCUS Foundation. -** All rights reserved. -** -** This library is derived, with permission, from the International -** Astronomical Union's "Standards of Fundamental Astronomy" library, -** available from http://www.iausofa.org. -** -** The ERFA version is intended to retain identical functionality to -** the SOFA library, but made distinct through different function and -** file names, as set out in the SOFA license conditions. The SOFA -** original has a role as a reference standard for the IAU and IERS, -** and consequently redistribution is permitted only in its unaltered -** state. The ERFA version is not subject to this restriction and -** therefore can be included in distributions which do not support the -** concept of "read only" software. -** -** Although the intent is to replicate the SOFA API (other than -** replacement of prefix names) and results (with the exception of -** bugs; any that are discovered will be fixed), SOFA is not -** responsible for any errors found in this version of the library. -** -** If you wish to acknowledge the SOFA heritage, please acknowledge -** that you are using a library derived from SOFA, rather than SOFA -** itself. -** -** -** TERMS AND CONDITIONS -** -** Redistribution and use in source and binary forms, with or without -** modification, are permitted provided that the following conditions -** are met: -** -** 1 Redistributions of source code must retain the above copyright -** notice, this list of conditions and the following disclaimer. -** -** 2 Redistributions in binary form must reproduce the above copyright -** notice, this list of conditions and the following disclaimer in -** the documentation and/or other materials provided with the -** distribution. -** -** 3 Neither the name of the Standards Of Fundamental Astronomy Board, -** the International Astronomical Union nor the names of its -** contributors may be used to endorse or promote products derived -** from this software without specific prior written permission. -** -** THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS -** "AS IS" AND ANY EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT -** LIMITED TO, THE IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS -** FOR A PARTICULAR PURPOSE ARE DISCLAIMED. IN NO EVENT SHALL THE -** COPYRIGHT HOLDER OR CONTRIBUTORS BE LIABLE FOR ANY DIRECT, INDIRECT, -** INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING, -** BUT NOT LIMITED TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES; -** LOSS OF USE, DATA, OR PROFITS; OR BUSINESS INTERRUPTION) HOWEVER -** CAUSED AND ON ANY THEORY OF LIABILITY, WHETHER IN CONTRACT, STRICT -** LIABILITY, OR TORT (INCLUDING NEGLIGENCE OR OTHERWISE) ARISING IN -** ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE -** POSSIBILITY OF SUCH DAMAGE. -** -*/ |