void mexFunction(int nlhs, mxArray *plhs[], int nrhs, const mxArray *prhs[]) { double TT1, TT2, dX, dY, *xVec; size_t numRow, numVec; mxArray *retMat; double *retData; double GCRS2CIRS[3][3]; if(nrhs<3||nrhs>4){ mexErrMsgTxt("Wrong number of inputs"); } if(nlhs>2) { mexErrMsgTxt("Wrong number of outputs."); } checkRealDoubleArray(prhs[0]); numRow = mxGetM(prhs[0]); numVec = mxGetN(prhs[0]); if(!(numRow==3||numRow==6)) { mexErrMsgTxt("The input vector has a bad dimensionality."); } xVec=(double*)mxGetData(prhs[0]); TT1=getDoubleFromMatlab(prhs[1]); TT2=getDoubleFromMatlab(prhs[2]); //If some values from the function getEOP will be needed. if(nrhs<4||mxGetM(prhs[3])==0) { mxArray *retVals[2]; double *dXdY; mxArray *JulUTCMATLAB[2]; double JulUTC[2]; int retVal; //Get the time in UTC to look up the parameters by going to TAI and //then UTC. retVal=iauTttai(TT1, TT2, &JulUTC[0], &JulUTC[1]); if(retVal!=0) { mexErrMsgTxt("An error occurred computing TAI."); } retVal=iauTaiutc(JulUTC[0], JulUTC[1], &JulUTC[0], &JulUTC[1]); switch(retVal){ case 1: mexWarnMsgTxt("Dubious Date entered."); break; case -1: mexErrMsgTxt("Unacceptable date entered"); break; default: break; } JulUTCMATLAB[0]=doubleMat2Matlab(&JulUTC[0],1,1); JulUTCMATLAB[1]=doubleMat2Matlab(&JulUTC[1],1,1); //Get the Earth orientation parameters for the given date. mexCallMATLAB(2,retVals,2,JulUTCMATLAB,"getEOP"); mxDestroyArray(JulUTCMATLAB[0]); mxDestroyArray(JulUTCMATLAB[1]); //%We do not need the polar motion coordinates. mxDestroyArray(retVals[0]); checkRealDoubleArray(retVals[1]); if(mxGetM(retVals[1])!=2||mxGetN(retVals[1])!=1) { mxDestroyArray(retVals[1]); mexErrMsgTxt("Error using the getEOP function."); return; } dXdY=(double*)mxGetData(retVals[1]); dX=dXdY[0]; dY=dXdY[1]; //Free the returned arrays. mxDestroyArray(retVals[1]); } else {//Get the celestial pole offsets size_t dim1, dim2; checkRealDoubleArray(prhs[4]); dim1 = mxGetM(prhs[4]); dim2 = mxGetN(prhs[4]); if((dim1==2&&dim2==1)||(dim1==1&&dim2==2)) { double *dXdY=(double*)mxGetData(prhs[4]); dX=dXdY[0]; dY=dXdY[1]; } else { mexErrMsgTxt("The celestial pole offsets have the wrong dimensionality."); return; } } { double x, y, s; double omega; //Get the X,Y coordinates of the Celestial Intermediate Pole (CIP) and //the Celestial Intermediate Origin (CIO) locator s, using the IAU 2006 //precession and IAU 2000A nutation models. iauXys06a(TT1, TT2, &x, &y, &s); //Add the CIP offsets. x += dX; y += dY; //Get the GCRS-to-CIRS matrix iauC2ixys(x, y, s, GCRS2CIRS); } //Allocate space for the return vectors. retMat=mxCreateDoubleMatrix(numRow,numVec,mxREAL); retData=(double*)mxGetData(retMat); { size_t curVec; for(curVec=0;curVec<numVec;curVec++) { //Multiply the position vector with the rotation matrix. iauRxp(GCRS2CIRS, xVec+numRow*curVec, retData+numRow*curVec); //If a velocity vector was given. if(numRow>3) { double *velGCRS=xVec+numRow*curVec+3;//Velocity in GCRS double *retDataVel=retData+numRow*curVec+3; //Convert velocity from GCRS to CIRS. iauRxp(GCRS2CIRS, velGCRS, retDataVel); } } } plhs[0]=retMat; //If the rotation matrix is desired on the output. if(nlhs>1) { double *elPtr; size_t i,j; plhs[1]=mxCreateDoubleMatrix(3,3,mxREAL); elPtr=(double*)mxGetData(plhs[1]); for (i=0;i<3;i++) { for(j=0;j<3;j++) { elPtr[i+3*j]=GCRS2CIRS[i][j]; } } } }
void iauApco(double date1, double date2, double ebpv[2][3], double ehp[3], double x, double y, double s, double theta, double elong, double phi, double hm, double xp, double yp, double sp, double refa, double refb, iauASTROM *astrom) /* ** - - - - - - - - ** i a u A p c o ** - - - - - - - - ** ** For a terrestrial observer, prepare star-independent astrometry ** parameters for transformations between ICRS and observed ** coordinates. The caller supplies the Earth ephemeris, the Earth ** rotation information and the refraction constants as well as the ** site coordinates. ** ** This function is part of the International Astronomical Union's ** SOFA (Standards of Fundamental Astronomy) software collection. ** ** Status: support function. ** ** Given: ** date1 double TDB as a 2-part... ** date2 double ...Julian Date (Note 1) ** ebpv double[2][3] Earth barycentric PV (au, au/day, Note 2) ** ehp double[3] Earth heliocentric P (au, Note 2) ** x,y double CIP X,Y (components of unit vector) ** s double the CIO locator s (radians) ** theta double Earth rotation angle (radians) ** elong double longitude (radians, east +ve, Note 3) ** phi double latitude (geodetic, radians, Note 3) ** hm double height above ellipsoid (m, geodetic, Note 3) ** xp,yp double polar motion coordinates (radians, Note 4) ** sp double the TIO locator s' (radians, Note 4) ** refa double refraction constant A (radians, Note 5) ** refb double refraction constant B (radians, Note 5) ** ** Returned: ** astrom iauASTROM* 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) ** ** Notes: ** ** 1) The TDB date date1+date2 is a Julian Date, apportioned in any ** convenient way between the two arguments. For example, ** JD(TDB)=2450123.7 could be expressed in any of these ways, among ** others: ** ** date1 date2 ** ** 2450123.7 0.0 (JD method) ** 2451545.0 -1421.3 (J2000 method) ** 2400000.5 50123.2 (MJD method) ** 2450123.5 0.2 (date & time method) ** ** The JD method is the most natural and convenient to use in cases ** where the loss of several decimal digits of resolution is ** acceptable. The J2000 method is best matched to the way the ** argument is handled internally and will deliver the optimum ** resolution. The MJD method and the date & time methods are both ** good compromises between resolution and convenience. For most ** applications of this function the choice will not be at all ** critical. ** ** TT can be used instead of TDB without any significant impact on ** accuracy. ** ** 2) The vectors eb, eh, and all the astrom vectors, are with respect ** to BCRS axes. ** ** 3) The geographical coordinates are with respect to the WGS84 ** reference ellipsoid. TAKE CARE WITH THE LONGITUDE SIGN ** CONVENTION: the longitude required by the present function is ** right-handed, i.e. east-positive, in accordance with geographical ** convention. ** ** 4) xp and yp are the coordinates (in radians) of the Celestial ** Intermediate Pole with respect to the International Terrestrial ** Reference System (see IERS Conventions), measured along the ** meridians 0 and 90 deg west respectively. sp is the TIO locator ** s', in radians, which positions the Terrestrial Intermediate ** Origin on the equator. For many applications, xp, yp and ** (especially) sp can be set to zero. ** ** Internally, the polar motion is stored in a form rotated onto the ** local meridian. ** ** 5) The refraction constants refa and refb are for use in a ** dZ = A*tan(Z)+B*tan^3(Z) model, where Z is the observed ** (i.e. refracted) zenith distance and dZ is the amount of ** refraction. ** ** 6) 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. ** ** 7) In cases where the caller does not wish to provide the Earth ** Ephemeris, the Earth rotation information and refraction ** constants, the function iauApco13 can be used instead of the ** present function. This starts from UTC and weather readings etc. ** and computes suitable values using other SOFA functions. ** ** 8) 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 ** ** iauApcg iauApcg13 geocentric ICRS <-> GCRS ** iauApci iauApci13 terrestrial ICRS <-> CIRS ** iauApco iauApco13 terrestrial ICRS <-> observed ** iauApcs iauApcs13 space ICRS <-> GCRS ** iauAper iauAper13 terrestrial update Earth rotation ** iauApio iauApio13 terrestrial CIRS <-> observed ** ** Those with names ending in "13" use contemporary SOFA 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. ** ** 9) The context structure astrom produced by this function is used by ** iauAtioq, iauAtoiq, iauAtciq* and iauAticq*. ** ** Called: ** iauAper astrometry parameters: update ERA ** iauC2ixys celestial-to-intermediate matrix, given X,Y and s ** iauPvtob position/velocity of terrestrial station ** iauTrxpv product of transpose of r-matrix and pv-vector ** iauApcs astrometry parameters, ICRS-GCRS, space observer ** iauCr copy r-matrix ** ** This revision: 2013 October 9 ** ** SOFA release 2013-12-02 ** ** Copyright (C) 2013 IAU SOFA Board. See notes at end. */ { double sl, cl, r[3][3], pvc[2][3], pv[2][3]; /* Longitude with adjustment for TIO locator s'. */ astrom->along = elong + sp; /* Polar motion, rotated onto the local meridian. */ sl = sin(astrom->along); cl = cos(astrom->along); astrom->xpl = xp*cl - yp*sl; astrom->ypl = xp*sl + yp*cl; /* Functions of latitude. */ astrom->sphi = sin(phi); astrom->cphi = cos(phi); /* Refraction constants. */ astrom->refa = refa; astrom->refb = refb; /* Local Earth rotation angle. */ iauAper(theta, astrom); /* Disable the (redundant) diurnal aberration step. */ astrom->diurab = 0.0; /* CIO based BPN matrix. */ iauC2ixys(x, y, s, r); /* Observer's geocentric position and velocity (m, m/s, CIRS). */ iauPvtob(elong, phi, hm, xp, yp, sp, theta, pvc); /* Rotate into GCRS. */ iauTrxpv(r, pvc, pv); /* ICRS <-> GCRS parameters. */ iauApcs(date1, date2, pv, ebpv, ehp, astrom); /* Store the CIO based BPN matrix. */ iauCr(r, astrom->bpn ); /* Finished. */ /*---------------------------------------------------------------------- ** ** Copyright (C) 2013 ** Standards Of Fundamental Astronomy Board ** of the International Astronomical Union. ** ** ===================== ** SOFA Software License ** ===================== ** ** NOTICE TO USER: ** ** BY USING THIS SOFTWARE YOU ACCEPT THE FOLLOWING SIX TERMS AND ** CONDITIONS WHICH APPLY TO ITS USE. ** ** 1. The Software is owned by the IAU SOFA Board ("SOFA"). ** ** 2. Permission is granted to anyone to use the SOFA software for any ** purpose, including commercial applications, free of charge and ** without payment of royalties, subject to the conditions and ** restrictions listed below. ** ** 3. You (the user) may copy and distribute SOFA source code to others, ** and use and adapt its code and algorithms in your own software, ** on a world-wide, royalty-free basis. That portion of your ** distribution that does not consist of intact and unchanged copies ** of SOFA source code files is a "derived work" that must comply ** with the following requirements: ** ** a) Your work shall be marked or carry a statement that it ** (i) uses routines and computations derived by you from ** software provided by SOFA under license to you; and ** (ii) does not itself constitute software provided by and/or ** endorsed by SOFA. ** ** b) The source code of your derived work must contain descriptions ** of how the derived work is based upon, contains and/or differs ** from the original SOFA software. ** ** c) The names of all routines in your derived work shall not ** include the prefix "iau" or "sofa" or trivial modifications ** thereof such as changes of case. ** ** d) The origin of the SOFA components of your derived work must ** not be misrepresented; you must not claim that you wrote the ** original software, nor file a patent application for SOFA ** software or algorithms embedded in the SOFA software. ** ** e) These requirements must be reproduced intact in any source ** distribution and shall apply to anyone to whom you have ** granted a further right to modify the source code of your ** derived work. ** ** Note that, as originally distributed, the SOFA software is ** intended to be a definitive implementation of the IAU standards, ** and consequently third-party modifications are discouraged. All ** variations, no matter how minor, must be explicitly marked as ** such, as explained above. ** ** 4. You shall not cause the SOFA software to be brought into ** disrepute, either by misuse, or use for inappropriate tasks, or ** by inappropriate modification. ** ** 5. The SOFA software is provided "as is" and SOFA makes no warranty ** as to its use or performance. SOFA does not and cannot warrant ** the performance or results which the user may obtain by using the ** SOFA software. SOFA makes no warranties, express or implied, as ** to non-infringement of third party rights, merchantability, or ** fitness for any particular purpose. In no event will SOFA be ** liable to the user for any consequential, incidental, or special ** damages, including any lost profits or lost savings, even if a ** SOFA representative has been advised of such damages, or for any ** claim by any third party. ** ** 6. The provision of any version of the SOFA software under the terms ** and conditions specified herein does not imply that future ** versions will also be made available under the same terms and ** conditions. * ** In any published work or commercial product which uses the SOFA ** software directly, acknowledgement (see www.iausofa.org) is ** appreciated. ** ** Correspondence concerning SOFA software should be addressed as ** follows: ** ** By email: [email protected] ** By post: IAU SOFA Center ** HM Nautical Almanac Office ** UK Hydrographic Office ** Admiralty Way, Taunton ** Somerset, TA1 2DN ** United Kingdom ** **--------------------------------------------------------------------*/ }
void iauApci(double date1, double date2, double ebpv[2][3], double ehp[3], double x, double y, double s, iauASTROM *astrom) /* ** - - - - - - - - ** i a u A p c i ** - - - - - - - - ** ** For a terrestrial observer, prepare star-independent astrometry ** parameters for transformations between ICRS and geocentric CIRS ** coordinates. The Earth ephemeris and CIP/CIO are supplied by the ** caller. ** ** The parameters produced by this function are required in the ** parallax, light deflection, aberration, and bias-precession-nutation ** parts of the astrometric transformation chain. ** ** This function is part of the International Astronomical Union's ** SOFA (Standards of Fundamental Astronomy) software collection. ** ** Status: support function. ** ** Given: ** date1 double TDB as a 2-part... ** date2 double ...Julian Date (Note 1) ** ebpv double[2][3] Earth barycentric position/velocity (au, au/day) ** ehp double[3] Earth heliocentric position (au) ** x,y double CIP X,Y (components of unit vector) ** s double the CIO locator s (radians) ** ** Returned: ** astrom iauASTROM* 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 unchanged ** xpl double unchanged ** ypl double unchanged ** sphi double unchanged ** cphi double unchanged ** diurab double unchanged ** eral double unchanged ** refa double unchanged ** refb double unchanged ** ** Notes: ** ** 1) The TDB date date1+date2 is a Julian Date, apportioned in any ** convenient way between the two arguments. For example, ** JD(TDB)=2450123.7 could be expressed in any of these ways, among ** others: ** ** date1 date2 ** ** 2450123.7 0.0 (JD method) ** 2451545.0 -1421.3 (J2000 method) ** 2400000.5 50123.2 (MJD method) ** 2450123.5 0.2 (date & time method) ** ** The JD method is the most natural and convenient to use in cases ** where the loss of several decimal digits of resolution is ** acceptable. The J2000 method is best matched to the way the ** argument is handled internally and will deliver the optimum ** resolution. The MJD method and the date & time methods are both ** good compromises between resolution and convenience. For most ** applications of this function the choice will not be at all ** critical. ** ** TT can be used instead of TDB without any significant impact on ** accuracy. ** ** 2) All the vectors are with respect to BCRS axes. ** ** 3) In cases where the caller does not wish to provide the Earth ** ephemeris and CIP/CIO, the function iauApci13 can be used instead ** of the present function. This computes the required quantities ** using other SOFA functions. ** ** 4) 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 ** ** iauApcg iauApcg13 geocentric ICRS <-> GCRS ** iauApci iauApci13 terrestrial ICRS <-> CIRS ** iauApco iauApco13 terrestrial ICRS <-> observed ** iauApcs iauApcs13 space ICRS <-> GCRS ** iauAper iauAper13 terrestrial update Earth rotation ** iauApio iauApio13 terrestrial CIRS <-> observed ** ** Those with names ending in "13" use contemporary SOFA 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. ** ** 5) The context structure astrom produced by this function is used by ** iauAtciq* and iauAticq*. ** ** Called: ** iauApcg astrometry parameters, ICRS-GCRS, geocenter ** iauC2ixys celestial-to-intermediate matrix, given X,Y and s ** ** This revision: 2013 September 25 ** ** SOFA release 2015-02-09 ** ** Copyright (C) 2015 IAU SOFA Board. See notes at end. */ { /* Star-independent astrometry parameters for geocenter. */ iauApcg(date1, date2, ebpv, ehp, astrom); /* CIO based BPN matrix. */ iauC2ixys(x, y, s, astrom->bpn); /* Finished. */ /*---------------------------------------------------------------------- ** ** Copyright (C) 2015 ** Standards Of Fundamental Astronomy Board ** of the International Astronomical Union. ** ** ===================== ** SOFA Software License ** ===================== ** ** NOTICE TO USER: ** ** BY USING THIS SOFTWARE YOU ACCEPT THE FOLLOWING SIX TERMS AND ** CONDITIONS WHICH APPLY TO ITS USE. ** ** 1. The Software is owned by the IAU SOFA Board ("SOFA"). ** ** 2. Permission is granted to anyone to use the SOFA software for any ** purpose, including commercial applications, free of charge and ** without payment of royalties, subject to the conditions and ** restrictions listed below. ** ** 3. You (the user) may copy and distribute SOFA source code to others, ** and use and adapt its code and algorithms in your own software, ** on a world-wide, royalty-free basis. That portion of your ** distribution that does not consist of intact and unchanged copies ** of SOFA source code files is a "derived work" that must comply ** with the following requirements: ** ** a) Your work shall be marked or carry a statement that it ** (i) uses routines and computations derived by you from ** software provided by SOFA under license to you; and ** (ii) does not itself constitute software provided by and/or ** endorsed by SOFA. ** ** b) The source code of your derived work must contain descriptions ** of how the derived work is based upon, contains and/or differs ** from the original SOFA software. ** ** c) The names of all routines in your derived work shall not ** include the prefix "iau" or "sofa" or trivial modifications ** thereof such as changes of case. ** ** d) The origin of the SOFA components of your derived work must ** not be misrepresented; you must not claim that you wrote the ** original software, nor file a patent application for SOFA ** software or algorithms embedded in the SOFA software. ** ** e) These requirements must be reproduced intact in any source ** distribution and shall apply to anyone to whom you have ** granted a further right to modify the source code of your ** derived work. ** ** Note that, as originally distributed, the SOFA software is ** intended to be a definitive implementation of the IAU standards, ** and consequently third-party modifications are discouraged. All ** variations, no matter how minor, must be explicitly marked as ** such, as explained above. ** ** 4. You shall not cause the SOFA software to be brought into ** disrepute, either by misuse, or use for inappropriate tasks, or ** by inappropriate modification. ** ** 5. The SOFA software is provided "as is" and SOFA makes no warranty ** as to its use or performance. SOFA does not and cannot warrant ** the performance or results which the user may obtain by using the ** SOFA software. SOFA makes no warranties, express or implied, as ** to non-infringement of third party rights, merchantability, or ** fitness for any particular purpose. In no event will SOFA be ** liable to the user for any consequential, incidental, or special ** damages, including any lost profits or lost savings, even if a ** SOFA representative has been advised of such damages, or for any ** claim by any third party. ** ** 6. The provision of any version of the SOFA software under the terms ** and conditions specified herein does not imply that future ** versions will also be made available under the same terms and ** conditions. * ** In any published work or commercial product which uses the SOFA ** software directly, acknowledgement (see www.iausofa.org) is ** appreciated. ** ** Correspondence concerning SOFA software should be addressed as ** follows: ** ** By email: [email protected] ** By post: IAU SOFA Center ** HM Nautical Almanac Office ** UK Hydrographic Office ** Admiralty Way, Taunton ** Somerset, TA1 2DN ** United Kingdom ** **--------------------------------------------------------------------*/ }
void mexFunction(int nlhs, mxArray *plhs[], int nrhs, const mxArray *prhs[]) { size_t numRow,numVec; mxArray *retMat; double *xVec, *retData; double TT1, TT2, UT11, UT12; //The if-statements below should properly initialize all of the EOP. //The following initializations to zero are to suppress warnings when //compiling with -Wconditional-uninitialized. double dX=0; double dY=0; double deltaT=0; double LOD=0; double GCRS2TIRS[3][3]; //Polar motion matrix. ITRS=POM*TIRS. We will just be setting it to the //identity matrix as polar motion is not taken into account when going //to the TIRS. double rident[3][3]={{1,0,0},{0,1,0},{0,0,1}}; double Omega[3];//The rotation vector in the TIRS if(nrhs<3||nrhs>6){ mexErrMsgTxt("Wrong number of inputs"); } if(nlhs>2) { mexErrMsgTxt("Wrong number of outputs."); } checkRealDoubleArray(prhs[0]); numRow = mxGetM(prhs[0]); numVec = mxGetN(prhs[0]); if(!(numRow==3||numRow==6)) { mexErrMsgTxt("The input vector has a bad dimensionality."); } xVec=(double*)mxGetData(prhs[0]); TT1=getDoubleFromMatlab(prhs[1]); TT2=getDoubleFromMatlab(prhs[2]); //If some values from the function getEOP will be needed if(nrhs<=5||mxIsEmpty(prhs[3])||mxIsEmpty(prhs[4])||mxIsEmpty(prhs[5])) { mxArray *retVals[5]; double *dXdY; mxArray *JulUTCMATLAB[2]; double JulUTC[2]; int retVal; //Get the time in UTC to look up the parameters by going to TAI and //then UTC. retVal=iauTttai(TT1, TT2, &JulUTC[0], &JulUTC[1]); if(retVal!=0) { mexErrMsgTxt("An error occurred computing TAI."); } retVal=iauTaiutc(JulUTC[0], JulUTC[1], &JulUTC[0], &JulUTC[1]); switch(retVal){ case 1: mexWarnMsgTxt("Dubious Date entered."); break; case -1: mexErrMsgTxt("Unacceptable date entered"); break; default: break; } JulUTCMATLAB[0]=doubleMat2Matlab(&JulUTC[0],1,1); JulUTCMATLAB[1]=doubleMat2Matlab(&JulUTC[1],1,1); //Get the Earth orientation parameters for the given date. mexCallMATLAB(5,retVals,2,JulUTCMATLAB,"getEOP"); mxDestroyArray(JulUTCMATLAB[0]); mxDestroyArray(JulUTCMATLAB[1]); //%We do not need the polar motion coordinates. mxDestroyArray(retVals[0]); checkRealDoubleArray(retVals[1]); if(mxGetM(retVals[1])!=2||mxGetN(retVals[1])!=1) { mxDestroyArray(retVals[1]); mxDestroyArray(retVals[2]); mxDestroyArray(retVals[3]); mxDestroyArray(retVals[4]); mexErrMsgTxt("Error using the getEOP function."); return; } dXdY=(double*)mxGetData(retVals[1]); dX=dXdY[0]; dY=dXdY[1]; //This is TT-UT1 deltaT=getDoubleFromMatlab(retVals[3]); LOD=getDoubleFromMatlab(retVals[4]); //Free the returned arrays. mxDestroyArray(retVals[1]); mxDestroyArray(retVals[2]); mxDestroyArray(retVals[3]); mxDestroyArray(retVals[4]); } //If deltaT=TT-UT1 is given if(nrhs>3&&!mxIsEmpty(prhs[3])) { deltaT=getDoubleFromMatlab(prhs[3]); } //Obtain UT1 from terestrial time and deltaT. iauTtut1(TT1, TT2, deltaT, &UT11, &UT12); //Get celestial pole offsets, if given. if(nrhs>4&&!mxIsEmpty(prhs[4])) { size_t dim1, dim2; checkRealDoubleArray(prhs[4]); dim1 = mxGetM(prhs[4]); dim2 = mxGetN(prhs[4]); if((dim1==2&&dim2==1)||(dim1==1&&dim2==2)) { double *dXdY=(double*)mxGetData(prhs[4]); dX=dXdY[0]; dY=dXdY[1]; } else { mexErrMsgTxt("The celestial pole offsets have the wrong dimensionality."); return; } } //If LOD is given if(nrhs>5&&mxIsEmpty(prhs[5])) { LOD=getDoubleFromMatlab(prhs[5]); } //Compute the rotation matrix for going from GCRS to ITRS as well as //the instantaneous vector angular momentum due to the Earth's rotation //in TIRS coordinates. { double x, y, s, era; double rc2i[3][3]; double omega; //Get the X,Y coordinates of the Celestial Intermediate Pole (CIP) and //the Celestial Intermediate Origin (CIO) locator s, using the IAU 2006 //precession and IAU 2000A nutation models. iauXys06a(TT1, TT2, &x, &y, &s); //Add the CIP offsets. x += dX; y += dY; //Get the GCRS-to-CIRS matrix iauC2ixys(x, y, s, rc2i); //Find the Earth rotation angle for the given UT1 time. era = iauEra00(UT11, UT12); //Set the polar motion matrix to the identity matrix so that the //conversion stops at the TIRS instead of the ITRS. //Combine the GCRS-to-CIRS matrix, the Earth rotation angle, and use //the identity matrix instead of the polar motion matrix to get a //to get the rotation matrix to go from GCRS to TIRS. iauC2tcio(rc2i, era, rident,GCRS2TIRS); //Next, to be able to transform the velocity, the rotation of the Earth //has to be taken into account. //The angular velocity vector of the Earth in the TIRS in radians. omega=getScalarMatlabClassConst("Constants","IERSMeanEarthRotationRate"); //Adjust for LOD omega=omega*(1-LOD/86400.0);//86400.0 is the number of seconds in a TT //day. Omega[0]=0; Omega[1]=0; Omega[2]=omega; } //Allocate space for the return vectors. retMat=mxCreateDoubleMatrix(numRow,numVec,mxREAL); retData=(double*)mxGetData(retMat); { size_t curVec; for(curVec=0;curVec<numVec;curVec++) { //Multiply the position vector with the rotation matrix. iauRxp(GCRS2TIRS, xVec+numRow*curVec, retData+numRow*curVec); //If a velocity vector was given. if(numRow>3) { double *posGCRS=xVec+numRow*curVec; double posTIRS[3]; double *velGCRS=xVec+numRow*curVec+3;//Velocity in GCRS double velTIRS[3]; double *retDataVel=retData+numRow*curVec+3; double rotVel[3]; //If a velocity was provided with the position, first //convert to TIRS coordinates, then account for the //rotation of the Earth. //Convert velocity from GCRS to TIRS. iauRxp(GCRS2TIRS, velGCRS, velTIRS); //Convert position from GCRS to TIRS iauRxp(GCRS2TIRS, posGCRS, posTIRS); //Evaluate the cross product for the angular velocity due //to the Earth's rotation. iauPxp(Omega, posTIRS, rotVel); //Subtract out the instantaneous velocity due to rotation. iauPmp(velTIRS, rotVel, retDataVel); } } } plhs[0]=retMat; //If the rotation matrix is desired on the output. if(nlhs>1) { double *elPtr; size_t i,j; plhs[1]=mxCreateDoubleMatrix(3,3,mxREAL); elPtr=(double*)mxGetData(plhs[1]); for (i=0;i<3;i++) { for(j=0;j<3;j++) { elPtr[i+3*j]=GCRS2TIRS[i][j]; } } } }
void iauC2ixy(double date1, double date2, double x, double y, double rc2i[3][3]) /* ** - - - - - - - - - ** i a u C 2 i x y ** - - - - - - - - - ** ** Form the celestial to intermediate-frame-of-date matrix for a given ** date when the CIP X,Y coordinates are known. IAU 2000. ** ** This function is part of the International Astronomical Union's ** SOFA (Standards Of Fundamental Astronomy) software collection. ** ** Status: support function. ** ** Given: ** date1,date2 double TT as a 2-part Julian Date (Note 1) ** x,y double Celestial Intermediate Pole (Note 2) ** ** Returned: ** rc2i double[3][3] celestial-to-intermediate matrix (Note 3) ** ** Notes: ** ** 1) The TT date date1+date2 is a Julian Date, apportioned in any ** convenient way between the two arguments. For example, ** JD(TT)=2450123.7 could be expressed in any of these ways, ** among others: ** ** date1 date2 ** ** 2450123.7 0.0 (JD method) ** 2451545.0 -1421.3 (J2000 method) ** 2400000.5 50123.2 (MJD method) ** 2450123.5 0.2 (date & time method) ** ** The JD method is the most natural and convenient to use in ** cases where the loss of several decimal digits of resolution ** is acceptable. The J2000 method is best matched to the way ** the argument is handled internally and will deliver the ** optimum resolution. The MJD method and the date & time methods ** are both good compromises between resolution and convenience. ** ** 2) The Celestial Intermediate Pole coordinates are the x,y components ** of the unit vector in the Geocentric Celestial Reference System. ** ** 3) The matrix rc2i is the first stage in the transformation from ** celestial to terrestrial coordinates: ** ** [TRS] = RPOM * R_3(ERA) * rc2i * [CRS] ** ** = RC2T * [CRS] ** ** where [CRS] is a vector in the Geocentric Celestial Reference ** System and [TRS] is a vector in the International Terrestrial ** Reference System (see IERS Conventions 2003), ERA is the Earth ** Rotation Angle and RPOM is the polar motion matrix. ** ** 4) Although its name does not include "00", This function is in fact ** specific to the IAU 2000 models. ** ** Called: ** iauC2ixys celestial-to-intermediate matrix, given X,Y and s ** iauS00 the CIO locator s, given X,Y, IAU 2000A ** ** Reference: ** ** McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003), ** IERS Technical Note No. 32, BKG (2004) ** ** This revision: 2013 June 18 ** ** SOFA release 2016-05-03 ** ** Copyright (C) 2016 IAU SOFA Board. See notes at end. */ { /* Compute s and then the matrix. */ iauC2ixys(x, y, iauS00(date1, date2, x, y), rc2i); return; /*---------------------------------------------------------------------- ** ** Copyright (C) 2016 ** Standards Of Fundamental Astronomy Board ** of the International Astronomical Union. ** ** ===================== ** SOFA Software License ** ===================== ** ** NOTICE TO USER: ** ** BY USING THIS SOFTWARE YOU ACCEPT THE FOLLOWING SIX TERMS AND ** CONDITIONS WHICH APPLY TO ITS USE. ** ** 1. The Software is owned by the IAU SOFA Board ("SOFA"). ** ** 2. Permission is granted to anyone to use the SOFA software for any ** purpose, including commercial applications, free of charge and ** without payment of royalties, subject to the conditions and ** restrictions listed below. ** ** 3. 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The provision of any version of the SOFA software under the terms ** and conditions specified herein does not imply that future ** versions will also be made available under the same terms and ** conditions. * ** In any published work or commercial product which uses the SOFA ** software directly, acknowledgement (see www.iausofa.org) is ** appreciated. ** ** Correspondence concerning SOFA software should be addressed as ** follows: ** ** By email: [email protected] ** By post: IAU SOFA Center ** HM Nautical Almanac Office ** UK Hydrographic Office ** Admiralty Way, Taunton ** Somerset, TA1 2DN ** United Kingdom ** **--------------------------------------------------------------------*/ }