예제 #1
0
static double smpl(int nsub, double * momenta,int * err)
{
 //double q;
 double ans, ans0=0.0, ans1=0.0;
switch(nsub)
{
  case 1:
    *err=*err|d_1(momenta);
    sprod_(momenta);
    ans0=0;
    ans1=0+F1();
    break;
}
/*
  if(!strfun_calc)
  { strfun_calc=1;
    q=scale_();
    if(ans0) xstr0=strfun_(0,xbjo[0],xbjo[1],q);
    if(ans1) xstr1=strfun_(1,xbjo[0],xbjo[1],q);
  }
  */
  ans=ans0+ans1;
  if(!(*err) && 10000*Fmax*computer_eps>(ans>0 ? ans : -ans))*err=1;
//  return ans0*xstr0+ans1*xstr1;
  return ans0 + ans1;
}
예제 #2
0
파일: d34.c 프로젝트: miguelwon/MEtop_S4F
REAL S34_out(double GG, REAL * momenta,int * err)
{REAL  ans=0;
REAL DP[10];
REAL* V=va_out;
REAL mass[3],width[3];
char * Qtxt[3];
REAL Q0[3],Q1[3],Q2[3];
width[2]=V[7]; mass[2]=V[29];  Qtxt[2]="\3\4";
width[1]=V[13]; mass[1]=V[12];  Qtxt[1]="\1\2";
*err=*err|prepDen(2,nin_out,BWrange_out*
 BWrange_out,mass,width,Qtxt,momenta,Q0,Q1,Q2);
sprod_(5, momenta, DP);
{int i; for(i=0;i<1;i++) 
{ REAL r=Farr[i](GG,DP,Q0,Q1,Q2);
  if(r>Fmax) Fmax=r;
  ans+=r;
}}
return ans;
}
예제 #3
0
파일: d167.c 프로젝트: miguelwon/MEtop_S4F
REAL S167_out(double GG, REAL * momenta,int * err)
{REAL  ans=0;
REAL DP[15];
REAL* V=va_out;
REAL mass[4],width[4];
char * Qtxt[4];
REAL Q0[4],Q1[4],Q2[4];
width[2]=V[7]; mass[2]=V[53];  Qtxt[2]="\3\4";
width[1]=V[12]; mass[1]=V[11];  Qtxt[1]="\1\2\5";
width[3]=0.; mass[3]=V[53];  Qtxt[3]="\2\5";
*err=*err|prepDen(3,nin_out,BWrange_out*
 BWrange_out,mass,width,Qtxt,momenta,Q0,Q1,Q2);
sprod_(6, momenta, DP);
{int i; for(i=0;i<1;i++) 
{ REAL r=Farr[i](GG,DP,Q0,Q1,Q2);
  if(r>Fmax) Fmax=r;
  ans+=r;
}}
return ans;
}
예제 #4
0
파일: d7.c 프로젝트: miguelwon/MEtop_S4F
REAL S7_out(double GG, REAL * momenta,int * err)
{REAL  ans=0;
REAL DP[15];
REAL* V=va_out;
REAL mass[8],width[8];
char * Qtxt[8];
REAL Q0[8],Q1[8],Q2[8];
width[7]=0.; mass[7]=V[9];  Qtxt[7]="\2\3";
width[6]=0.; mass[6]=V[8];  Qtxt[6]="\2\3";
width[3]=V[10]; mass[3]=V[9];  Qtxt[3]="\1\2";
width[5]=0.; mass[5]=V[8];  Qtxt[5]="\1\2";
width[2]=V[6]; mass[2]=V[23];  Qtxt[2]="\4\5";
width[1]=V[10]; mass[1]=V[9];  Qtxt[1]="\1\2\3";
width[4]=0.; mass[4]=0;  Qtxt[4]="\1\3";
*err=*err|prepDen(7,nin_out,BWrange_out*
 BWrange_out,mass,width,Qtxt,momenta,Q0,Q1,Q2);
sprod_(6, momenta, DP);
{int i; for(i=0;i<21;i++) 
{ REAL r=Farr[i](GG,DP,Q0,Q1,Q2);
  if(r>Fmax) Fmax=r;
  ans+=r;
}}
return ans;
}
예제 #5
0
/* Subroutine */ int dehanttideinel_(doublereal *xsta, integer *yr, integer *
                                     month, integer *day, doublereal *fhr, doublereal *xsun, doublereal *
                                     xmon, doublereal *dxtide)
{
    /* Initialized data */

    static doublereal h20 = .6078;
    static doublereal l20 = .0847;
    static doublereal h3 = .292;
    static doublereal l3 = .015;

    /* System generated locals */
    doublereal d__1, d__2;

    /* Builtin functions */
    double sqrt(doublereal);

    /* Local variables */
    static doublereal mass_ratio_moon__;
    extern /* Subroutine */ int step2diu_(doublereal *, doublereal *,
                                          doublereal *, doublereal *), step2lon_(doublereal *, doublereal *,
                                                  doublereal *);
    static integer i__;
    extern /* Subroutine */ int zero_vec8__(doublereal *);
    static doublereal t, h2, l2, re;
    extern /* Subroutine */ int dat_(integer *, integer *, integer *,
                                     doublereal *, doublereal *, integer *);
    static doublereal scm, scs, dtt, jjm0, jjm1;
    extern /* Subroutine */ int st1l1_(doublereal *, doublereal *, doublereal
                                       *, doublereal *, doublereal *, doublereal *);
    static doublereal rsta, rmon, rsun, p2mon, p3mon, x2mon, x3mon, p2sun,
           p3sun, x2sun, x3sun, scmon;
    extern /* Subroutine */ int sprod_(doublereal *, doublereal *, doublereal
                                       *, doublereal *, doublereal *);
    static doublereal scsun;
    extern /* Subroutine */ int cal2jd_(integer *, integer *, integer *,
                                        doublereal *, doublereal *, integer *);
    static doublereal cosphi;
    static integer statut;
    static doublereal fac2mon, fac3mon, fac2sun, fac3sun;
    extern /* Subroutine */ int st1idiu_(doublereal *, doublereal *,
                                         doublereal *, doublereal *, doublereal *, doublereal *);
    static doublereal mass_ratio_sun__;
    extern /* Subroutine */ int st1isem_(doublereal *, doublereal *,
                                         doublereal *, doublereal *, doublereal *, doublereal *);
    static doublereal xcorsta[3];

    /* + */
    /*  - - - - - - - - - - - - - - - */
    /*   D E H A N T T I D E I N E L */
    /*  - - - - - - - - - - - - - - - */

    /*  This routine is part of the International Earth Rotation and */
    /*  Reference Systems Service (IERS) Conventions software collection. */

    /*  This subroutine computes the tidal corrections of station displacements */
    /*  caused by lunar and solar gravitational attraction (see References). */
    /*  The computations are calculated by the following steps: */

    /*  Step 1): General degree 2 and degree 3 corrections + CALL ST1IDIU */
    /*  + CALL ST1ISEM + CALL ST1L1. */

    /*  Step 2): CALL STEP2DIU + CALL STEP2LON */

    /*  It has been decided that the Step 3 non-correction for permanent tide */
    /*  would not be applied in order to avoid a jump in the reference frame. */
    /*  This Step 3 must be added in order to get the non-tidal station position */
    /*  and to conform with the IAG Resolution. */

    /*  In general, Class 1, 2, and 3 models represent physical effects that */
    /*  act on geodetic parameters while canonical models provide lower-level */
    /*  representations or basic computations that are used by Class 1, 2, or */
    /*  3 models. */

    /*  Status: Class 1 */

    /*     Class 1 models are those recommended to be used a priori in the */
    /*     reduction of raw space geodetic data in order to determine */
    /*     geodetic parameter estimates. */
    /*     Class 2 models are those that eliminate an observational */
    /*     singularity and are purely conventional in nature. */
    /*     Class 3 models are those that are not required as either Class */
    /*     1 or 2. */
    /*     Canonical models are accepted as is and cannot be classified as a */
    /*     Class 1, 2, or 3 model. */

    /*  Given: */
    /*     XSTA          d(3)   Geocentric position of the IGS station (Note 1) */
    /*     XSUN          d(3)   Geocentric position of the Sun (Note 2) */
    /*     XMON          d(3)   Geocentric position of the Moon (Note 2) */
    /*     YR            i      Year (Note 3) */
    /*     MONTH         i      Month (Note 3) */
    /*     DAY           i      Day of Month (Note 3) */
    /*     FHR           d      Hour in the day (Note 4) */

    /*  Returned: */
    /*     DXTIDE        d(3)   Displacement vector (Note 5) */

    /*  Notes: */

    /*  1) The IGS station is in ITRF co-rotating frame.  All coordinates, */
    /*     X, Y, and Z, are expressed in meters. */

    /*  2) The position is in Earth Centered Earth Fixed (ECEF) frame.  All */
    /*     coordinates are expressed in meters. */

    /*  3) The values are expressed in Coordinated Universal Time (UTC). */

    /*  4) The fractional hours in the day is computed as the hour + minutes/60.0 */
    /*     + sec/3600.0.  The unit is expressed in Universal Time (UT). */

    /*  5) The displacement vector is in the geocentric ITRF.  All components are */
    /*     expressed in meters. */

    /*  Called: */
    /*     SPROD             Finds the scalar product and unit vector of two vectors */
    /*     ZERO_VEC8         Returns the zero vector */
    /*     ST1IDIU           Corrects for the out-of-phase part of Love numbers */
    /*                       for the diurnal band */
    /*     ST1ISEM           Same as above for the semi-diurnal band */
    /*     ST1L1             Corrects for the latitude dependence of Love numbers */
    /*     CAL2JD            Computes Julian Date from Gregorian calendar date */
    /*     DAT               Computes the difference TAI-UTC */
    /*     STEP2DIU          Computes in-phase and out-of-phase corrections in */
    /*                       the diurnal band */
    /*     STEP2LON          Same as above for the long period band */

    /*  Test case: */
    /*     given input: XSTA(1) = 4075578.385D0 meters */
    /*                  XSTA(2) =  931852.890D0 meters */
    /*                  XSTA(3) = 4801570.154D0 meters */
    /*                  XSUN(1) = 137859926952.015D0 meters */
    /*                  XSUN(2) = 54228127881.4350D0 meters */
    /*                  XSUN(3) = 23509422341.6960D0 meters */
    /*                  XMON(1) = -179996231.920342D0 meters */
    /*                  XMON(2) = -312468450.131567D0 meters */
    /*                  XMON(3) = -169288918.592160D0 meters */
    /*                  YR      = 2009 */
    /*                  MONTH   = 4 */
    /*                  DAY     = 13 */
    /*                  FHR     = 0.00D0 seconds */

    /*     expected output:  DXTIDE(1) = 0.7700420357108125891D-01 meters */
    /*                       DXTIDE(2) = 0.6304056321824967613D-01 meters */
    /*                       DXTIDE(3) = 0.5516568152597246810D-01 meters */

    /*  References: */

    /*     Groten, E., 2000, Geodesists Handbook 2000, Part 4, */
    /*     http://www.gfy.ku.dk/~iag/HB2000/part4/groten.htm. See also */
    /*     ''Parameters of Common Relevance of Astronomy, Geodesy, and */
    /*     Geodynamics," J. Geod., 74, pp. 134-140 */

    /*     Mathews, P. M., Dehant, V., and Gipson, J. M., 1997, ''Tidal station */
    /*     displacements," J. Geophys. Res., 102(B9), pp. 20,469-20,477 */

    /*     Petit, G. and Luzum, B. (eds.), IERS Conventions (2010), */
    /*     IERS Technical Note No. 36, BKG (2010) */

    /*     Pitjeva, E. and Standish, E. M., 2009, ''Proposals for the masses */
    /*     of the three largest asteroids, the Moon-Earth mass ratio and the */
    /*     Astronomical Unit," Celest. Mech. Dyn. Astr., 103, pp. 365-372 */

    /*     Ries, J. C., Eanes, R. J., Shum, C. K. and Watkins, M. M., 1992, */
    /*     ''Progress in the Determination of the Gravitational Coefficient */
    /*     of the Earth," Geophys. Res. Lett., 19(6), pp. 529-531 */

    /*  Revisions: */
    /*  1996 March    23 V. Dehant      Original code */
    /*                   P. M. Mathews */
    /*                   J. Gipson */
    /*  2000 May      17 V. Dehant      Last modifications */
    /*                   P. M. Mathews */
    /*  2006 February 06 J. Ray         Header comments modified to clarify */
    /*                                  input/output units and systems */
    /*  2006 February 06 J. Ray         Subroutine DUTC modified for leap */
    /*                                  second on 2006.0 and to correct */
    /*                                  do 5 i=1,87 from 84 to 87 */
    /*  2006 August   31 G. Petit       Correct DUTC for dates after 2007 */
    /*  2007 June     20 H. Manche      Modified DUTC to correct past mistake */
    /*                                  and corrected DE line in subroutine */
    /*                                  STEP2DIU */
    /*  2007 October  23 H. Manche      Replace subroutines DUTC and FJLDY with */
    /*                   G. Petit       SOFA subroutines iau_CAL2JD and iau_DAT */
    /*                                  and correct time arguments of subroutine */
    /*                                  STEP2DIU */
    /*  2009 February 19 G. Petit       Update routine iau_DAT for 2009.0 leap */
    /*                                  second */
    /*  2009 August   06 B.E. Stetzler  Initial standardization of code */
    /*  2009 August   07 B.E. Stetzler  Updated MASS_RATIO_SUN, */
    /*                                  MASS_RATIO_MOON and RE to CBEs and */
    /*                                  provided a test case */
    /*  2009 August  07  B.E. Stetzler  Capitalized all variables for Fortran */
    /*                                  77 compatibility */
    /*  2009 September 01 B.E. Stetzler Removed 'iau_' from redistributed SOFA */
    /*                                  subroutines */
    /* ----------------------------------------------------------------------- */
    /* ---------------------------------------------------------------------- */
    /* NOMINAL SECOND DEGREE AND THIRD DEGREE LOVE NUMBERS AND SHIDA NUMBERS */
    /* ---------------------------------------------------------------------- */
    /* Parameter adjustments */
    --dxtide;
    --xmon;
    --xsun;
    --xsta;

    /* Function Body */
    /* ---------------------------------------------------------------------- */
    /* SCALAR PRODUCT OF STATION VECTOR WITH SUN/MOON VECTOR */
    /* ---------------------------------------------------------------------- */
    sprod_(&xsta[1], &xsun[1], &scs, &rsta, &rsun);
    sprod_(&xsta[1], &xmon[1], &scm, &rsta, &rmon);
    scsun = scs / rsta / rsun;
    scmon = scm / rsta / rmon;
    /* ---------------------------------------------------------------------- */
    /* COMPUTATION OF NEW H2 AND L2 */
    /* ---------------------------------------------------------------------- */
    /* Computing 2nd power */
    d__1 = xsta[1];
    /* Computing 2nd power */
    d__2 = xsta[2];
    cosphi = sqrt(d__1 * d__1 + d__2 * d__2) / rsta;
    /* Computing 2nd power */
    d__1 = cosphi;
    h2 = h20 - (1. - d__1 * d__1 * 1.5) * 6e-4;
    /* Computing 2nd power */
    d__1 = cosphi;
    l2 = l20 + (1. - d__1 * d__1 * 1.5) * 2e-4;
    /* P2 term */
    /* Computing 2nd power */
    d__1 = scsun;
    p2sun = (h2 / 2. - l2) * 3. * (d__1 * d__1) - h2 / 2.;
    /* Computing 2nd power */
    d__1 = scmon;
    p2mon = (h2 / 2. - l2) * 3. * (d__1 * d__1) - h2 / 2.;
    /* P3 term */
    /* Computing 3rd power */
    d__1 = scsun;
    p3sun = (h3 - l3 * 3.) * 2.5 * (d__1 * (d__1 * d__1)) + (l3 - h3) * 1.5 *
            scsun;
    /* Computing 3rd power */
    d__1 = scmon;
    p3mon = (h3 - l3 * 3.) * 2.5 * (d__1 * (d__1 * d__1)) + (l3 - h3) * 1.5 *
            scmon;
    /* ---------------------------------------------------------------------- */
    /* TERM IN DIRECTION OF SUN/MOON VECTOR */
    /* ---------------------------------------------------------------------- */
    x2sun = l2 * 3. * scsun;
    x2mon = l2 * 3. * scmon;
    /* Computing 2nd power */
    d__1 = scsun;
    x3sun = l3 * 3. / 2. * (d__1 * d__1 * 5. - 1.);
    /* Computing 2nd power */
    d__1 = scmon;
    x3mon = l3 * 3. / 2. * (d__1 * d__1 * 5. - 1.);
    /* ---------------------------------------------------------------------- */
    /* FACTORS FOR SUN/MOON USING IAU CURRENT BEST ESTIMATES (SEE REFERENCES) */
    /* ---------------------------------------------------------------------- */
    mass_ratio_sun__ = 332946.0482;
    mass_ratio_moon__ = .0123000371;
    re = 6378136.6;
    /* Computing 3rd power */
    d__1 = re / rsun;
    fac2sun = mass_ratio_sun__ * re * (d__1 * (d__1 * d__1));
    /* Computing 3rd power */
    d__1 = re / rmon;
    fac2mon = mass_ratio_moon__ * re * (d__1 * (d__1 * d__1));
    fac3sun = fac2sun * (re / rsun);
    fac3mon = fac2mon * (re / rmon);
    /* TOTAL DISPLACEMENT */
    for (i__ = 1; i__ <= 3; ++i__) {
        dxtide[i__] = fac2sun * (x2sun * xsun[i__] / rsun + p2sun * xsta[i__]
                                 / rsta) + fac2mon * (x2mon * xmon[i__] / rmon + p2mon * xsta[
                                             i__] / rsta) + fac3sun * (x3sun * xsun[i__] / rsun + p3sun *
                                                     xsta[i__] / rsta) + fac3mon * (x3mon * xmon[i__] / rmon +
                                                             p3mon * xsta[i__] / rsta);
        /* L10: */
    }
    zero_vec8__(xcorsta);
    /* +--------------------------------------------------------------------- */
    /* CORRECTIONS FOR THE OUT-OF-PHASE PART OF LOVE NUMBERS (PART H_2^(0)I */
    /* AND L_2^(0)I ) */
    /* ---------------------------------------------------------------------- */
    /* FIRST, FOR THE DIURNAL BAND */
    st1idiu_(&xsta[1], &xsun[1], &xmon[1], &fac2sun, &fac2mon, xcorsta);
    for (i__ = 1; i__ <= 3; ++i__) {
        dxtide[i__] += xcorsta[i__ - 1];
        /* L11: */
    }
    /* SECOND, FOR THE SEMI-DIURNAL BAND */
    st1isem_(&xsta[1], &xsun[1], &xmon[1], &fac2sun, &fac2mon, xcorsta);
    for (i__ = 1; i__ <= 3; ++i__) {
        dxtide[i__] += xcorsta[i__ - 1];
        /* L12: */
    }
    /* +--------------------------------------------------------------------- */
    /* CORRECTIONS FOR THE LATITUDE DEPENDENCE OF LOVE NUMBERS (PART L^(1) ) */
    /* ---------------------------------------------------------------------- */
    st1l1_(&xsta[1], &xsun[1], &xmon[1], &fac2sun, &fac2mon, xcorsta);
    for (i__ = 1; i__ <= 3; ++i__) {
        dxtide[i__] += xcorsta[i__ - 1];
        /* L13: */
    }
    /* CONSIDER CORRECTIONS FOR STEP 2 */
    /* +--------------------------------------------------------------------- */
    /* CORRECTIONS FOR THE DIURNAL BAND: */

    /*  FIRST, WE NEED TO KNOW THE DATE CONVERTED IN JULIAN CENTURIES */

    /*   1) CALL THE SUBROUTINE COMPUTING THE JULIAN DATE */
    /* ++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ */
    cal2jd_(yr, month, day, &jjm0, &jjm1, &statut);
    t = (jjm0 - 2451545. + jjm1 + *fhr / 24.) / 36525.;
    /* ++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ */
    /*   2) CALL THE SUBROUTINE COMPUTING THE CORRECTION OF UTC TIME */
    /* ++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ */
    dat_(yr, month, day, fhr, &dtt, &statut);
    /* ++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ */
    dtt += 32.184;
    /*     CONVERSION OF T IN TT TIME */
    t += dtt / 3.15576e9;
    /*  SECOND, WE CAN CALL THE SUBROUTINE STEP2DIU, FOR THE DIURNAL BAND */
    /*  CORRECTIONS, (in-phase and out-of-phase frequency dependence): */
    step2diu_(&xsta[1], fhr, &t, xcorsta);
    for (i__ = 1; i__ <= 3; ++i__) {
        dxtide[i__] += xcorsta[i__ - 1];
        /* L14: */
    }
    /*  CORRECTIONS FOR THE LONG-PERIOD BAND, */
    /*  (in-phase and out-of-phase frequency dependence): */
    step2lon_(&xsta[1], &t, xcorsta);
    for (i__ = 1; i__ <= 3; ++i__) {
        dxtide[i__] += xcorsta[i__ - 1];
        /* L15: */
    }
    /* CONSIDER CORRECTIONS FOR STEP 3 */
    /* ---------------------------------------------------------------------- */
    /* UNCORRECT FOR THE PERMANENT TIDE */

    /*      SINPHI=XSTA(3)/RSTA */
    /*      COSPHI=DSQRT(XSTA(1)**2+XSTA(2)**2)/RSTA */
    /*      COSLA=XSTA(1)/COSPHI/RSTA */
    /*      SINLA=XSTA(2)/COSPHI/RSTA */
    /*      DR=-DSQRT(5D0/4D0/PI)*H2*0.31460D0*(3D0/2D0*SINPHI**2-0.5D0) */
    /*      DN=-DSQRT(5D0/4D0/PI)*L2*0.31460D0*3D0*COSPHI*SINPHI */
    /*      DXTIDE(1)=DXTIDE(1)-DR*COSLA*COSPHI+DN*COSLA*SINPHI */
    /*      DXTIDE(2)=DXTIDE(2)-DR*SINLA*COSPHI+DN*SINLA*SINPHI */
    /*      DXTIDE(3)=DXTIDE(3)-DR*SINPHI      -DN*COSPHI */
    /* ----------------------------------------------------------------------- */
    return 0;
    /*  Finished. */
    /* +---------------------------------------------------------------------- */

    /*  Copyright (C) 2008 */
    /*  IERS Conventions Center */

    /*  ================================== */
    /*  IERS Conventions Software License */
    /*  ================================== */

    /*  NOTICE TO USER: */

    /*  BY USING THIS SOFTWARE YOU ACCEPT THE FOLLOWING TERMS AND CONDITIONS */
    /*  WHICH APPLY TO ITS USE. */

    /*  1. The Software is provided by the IERS Conventions Center ("the */
    /*     Center"). */

    /*  2. Permission is granted to anyone to use the Software for any */
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    /*     subject to the conditions and restrictions listed below. */

    /*  3. You (the user) may adapt the Software and its algorithms for your */
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    /*        shall be changed. */

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    /*     e) The source code must be included for all routine(s) that you */
    /*        distribute.  This notice must be reproduced intact in any */
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    /*  4. In any published work produced by the user and which includes */
    /*     results achieved by using the Software, you shall acknowledge */
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    /*  5. The Software is provided to the user "as is" and the Center makes */
    /*     no warranty as to its use or performance.   The Center does not */
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    /*  Correspondence concerning IERS Conventions software should be */
    /*  addressed as follows: */

    /*                     Gerard Petit */
    /*     Internet email: gpetit[at]bipm.org */
    /*     Postal address: IERS Conventions Center */
    /*                     Time, frequency and gravimetry section, BIPM */
    /*                     Pavillon de Breteuil */
    /*                     92312 Sevres  FRANCE */

    /*     or */

    /*                     Brian Luzum */
    /*     Internet email: brian.luzum[at]usno.navy.mil */
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    /*                     Earth Orientation Department */
    /*                     3450 Massachusetts Ave, NW */
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    /* ----------------------------------------------------------------------- */
} /* dehanttideinel_ */