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Diffstat (limited to 'ast/erfa/apco13.c')
| -rw-r--r-- | ast/erfa/apco13.c | 287 |
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diff --git a/ast/erfa/apco13.c b/ast/erfa/apco13.c deleted file mode 100644 index cdd4d4f..0000000 --- a/ast/erfa/apco13.c +++ /dev/null @@ -1,287 +0,0 @@ -#include "erfa.h" - -int eraApco13(double utc1, double utc2, double dut1, - double elong, double phi, double hm, double xp, double yp, - double phpa, double tc, double rh, double wl, - eraASTROM *astrom, double *eo) -/* -** - - - - - - - - - - -** e r a A p c o 1 3 -** - - - - - - - - - - -** -** For a terrestrial observer, prepare star-independent astrometry -** parameters for transformations between ICRS and observed -** coordinates. The caller supplies UTC, site coordinates, ambient air -** conditions and observing wavelength, and ERFA models are used to -** obtain the Earth ephemeris, CIP/CIO and refraction constants. -** -** The parameters produced by this function are required in the -** parallax, light deflection, aberration, and bias-precession-nutation -** parts of the ICRS/CIRS transformations. -** -** Given: -** utc1 double UTC as a 2-part... -** utc2 double ...quasi Julian Date (Notes 1,2) -** dut1 double UT1-UTC (seconds, Note 3) -** elong double longitude (radians, east +ve, Note 4) -** phi double latitude (geodetic, radians, Note 4) -** hm double height above ellipsoid (m, geodetic, Notes 4,6) -** xp,yp double polar motion coordinates (radians, Note 5) -** phpa double pressure at the observer (hPa = mB, Note 6) -** tc double ambient temperature at the observer (deg C) -** rh double relative humidity at the observer (range 0-1) -** wl double wavelength (micrometers, Note 7) -** -** Returned: -** 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) -** eo double* equation of the origins (ERA-GST) -** -** Returned (function value): -** int status: +1 = dubious year (Note 2) -** 0 = OK -** -1 = unacceptable date -** -** Notes: -** -** 1) utc1+utc2 is quasi Julian Date (see Note 2), apportioned in any -** convenient way between the two arguments, for example where utc1 -** is the Julian Day Number and utc2 is the fraction of a day. -** -** However, JD cannot unambiguously represent UTC during a leap -** second unless special measures are taken. The convention in the -** present function is that the JD day represents UTC days whether -** the length is 86399, 86400 or 86401 SI seconds. -** -** Applications should use the function eraDtf2d to convert from -** calendar date and time of day into 2-part quasi Julian Date, as -** it implements the leap-second-ambiguity convention just -** described. -** -** 2) The warning status "dubious year" flags UTCs that predate the -** introduction of the time scale or that are too far in the -** future to be trusted. See eraDat for further details. -** -** 3) UT1-UTC is tabulated in IERS bulletins. It increases by exactly -** one second at the end of each positive UTC leap second, -** introduced in order to keep UT1-UTC within +/- 0.9s. n.b. This -** practice is under review, and in the future UT1-UTC may grow -** essentially without limit. -** -** 4) The geographical coordinates are with respect to the ERFA_WGS84 -** reference ellipsoid. TAKE CARE WITH THE LONGITUDE SIGN: the -** longitude required by the present function is east-positive -** (i.e. right-handed), in accordance with geographical convention. -** -** 5) The polar motion xp,yp can be obtained from IERS bulletins. The -** values are the coordinates (in radians) of the Celestial -** Intermediate Pole with respect to the International Terrestrial -** Reference System (see IERS Conventions 2003), measured along the -** meridians 0 and 90 deg west respectively. For many -** applications, xp and yp can be set to zero. -** -** Internally, the polar motion is stored in a form rotated onto -** the local meridian. -** -** 6) If hm, the height above the ellipsoid of the observing station -** in meters, is not known but phpa, the pressure in hPa (=mB), is -** available, an adequate estimate of hm can be obtained from the -** expression -** -** hm = -29.3 * tsl * log ( phpa / 1013.25 ); -** -** where tsl is the approximate sea-level air temperature in K -** (See Astrophysical Quantities, C.W.Allen, 3rd edition, section -** 52). Similarly, if the pressure phpa is not known, it can be -** estimated from the height of the observing station, hm, as -** follows: -** -** phpa = 1013.25 * exp ( -hm / ( 29.3 * tsl ) ); -** -** Note, however, that the refraction is nearly proportional to -** the pressure and that an accurate phpa value is important for -** precise work. -** -** 7) The argument wl specifies the observing wavelength in -** micrometers. The transition from optical to radio is assumed to -** occur at 100 micrometers (about 3000 GHz). -** -** 8) It is advisable to take great care with units, as even unlikely -** values of the input parameters are accepted and processed in -** accordance with the models used. -** -** 9) In cases where the caller wishes to supply his own Earth -** ephemeris, Earth rotation information and refraction constants, -** the function eraApco can be used instead of the present function. -** -** 10) This is one of several functions that inserts into the astrom -** structure star-independent parameters needed for the chain of -** astrometric transformations ICRS <-> GCRS <-> CIRS <-> observed. -** -** The various functions support different classes of observer and -** portions of the transformation chain: -** -** functions observer transformation -** -** eraApcg eraApcg13 geocentric ICRS <-> GCRS -** eraApci eraApci13 terrestrial ICRS <-> CIRS -** eraApco eraApco13 terrestrial ICRS <-> observed -** eraApcs eraApcs13 space ICRS <-> GCRS -** eraAper eraAper13 terrestrial update Earth rotation -** eraApio eraApio13 terrestrial CIRS <-> observed -** -** Those with names ending in "13" use contemporary ERFA models to -** compute the various ephemerides. The others accept ephemerides -** supplied by the caller. -** -** The transformation from ICRS to GCRS covers space motion, -** parallax, light deflection, and aberration. From GCRS to CIRS -** comprises frame bias and precession-nutation. From CIRS to -** observed takes account of Earth rotation, polar motion, diurnal -** aberration and parallax (unless subsumed into the ICRS <-> GCRS -** transformation), and atmospheric refraction. -** -** 11) The context structure astrom produced by this function is used -** by eraAtioq, eraAtoiq, eraAtciq* and eraAticq*. -** -** Called: -** eraUtctai UTC to TAI -** eraTaitt TAI to TT -** eraUtcut1 UTC to UT1 -** eraEpv00 Earth position and velocity -** eraPnm06a classical NPB matrix, IAU 2006/2000A -** eraBpn2xy extract CIP X,Y coordinates from NPB matrix -** eraS06 the CIO locator s, given X,Y, IAU 2006 -** eraEra00 Earth rotation angle, IAU 2000 -** eraSp00 the TIO locator s', IERS 2000 -** eraRefco refraction constants for given ambient conditions -** eraApco astrometry parameters, ICRS-observed -** eraEors equation of the origins, given NPB matrix and s -** -** Copyright (C) 2013-2016, NumFOCUS Foundation. -** Derived, with permission, from the SOFA library. See notes at end of file. -*/ -{ - int j; - double tai1, tai2, tt1, tt2, ut11, ut12, ehpv[2][3], ebpv[2][3], - r[3][3], x, y, s, theta, sp, refa, refb; - - -/* UTC to other time scales. */ - j = eraUtctai(utc1, utc2, &tai1, &tai2); - if ( j < 0 ) return -1; - j = eraTaitt(tai1, tai2, &tt1, &tt2); - j = eraUtcut1(utc1, utc2, dut1, &ut11, &ut12); - if ( j < 0 ) return -1; - -/* Earth barycentric & heliocentric position/velocity (au, au/d). */ - (void) eraEpv00(tt1, tt2, ehpv, ebpv); - -/* Form the equinox based BPN matrix, IAU 2006/2000A. */ - eraPnm06a(tt1, tt2, r); - -/* Extract CIP X,Y. */ - eraBpn2xy(r, &x, &y); - -/* Obtain CIO locator s. */ - s = eraS06(tt1, tt2, x, y); - -/* Earth rotation angle. */ - theta = eraEra00(ut11, ut12); - -/* TIO locator s'. */ - sp = eraSp00(tt1, tt2); - -/* Refraction constants A and B. */ - eraRefco(phpa, tc, rh, wl, &refa, &refb); - -/* Compute the star-independent astrometry parameters. */ - eraApco(tt1, tt2, ebpv, ehpv[0], x, y, s, theta, - elong, phi, hm, xp, yp, sp, refa, refb, astrom); - -/* Equation of the origins. */ - *eo = eraEors(r, s); - -/* Return any warning status. */ - return j; - -/* 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. -** -*/ |