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#include "erfa.h" |
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int eraStarpm(double ra1, double dec1, |
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double pmr1, double pmd1, double px1, double rv1, |
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double ep1a, double ep1b, double ep2a, double ep2b, |
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double *ra2, double *dec2, |
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double *pmr2, double *pmd2, double *px2, double *rv2) |
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/* |
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** - - - - - - - - - - |
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** e r a S t a r p m |
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** - - - - - - - - - - |
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** |
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** Star proper motion: update star catalog data for space motion. |
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** |
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** Given: |
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** ra1 double right ascension (radians), before |
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** dec1 double declination (radians), before |
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** pmr1 double RA proper motion (radians/year), before |
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** pmd1 double Dec proper motion (radians/year), before |
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** px1 double parallax (arcseconds), before |
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** rv1 double radial velocity (km/s, +ve = receding), before |
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** ep1a double "before" epoch, part A (Note 1) |
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** ep1b double "before" epoch, part B (Note 1) |
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** ep2a double "after" epoch, part A (Note 1) |
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** ep2b double "after" epoch, part B (Note 1) |
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** |
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** Returned: |
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** ra2 double right ascension (radians), after |
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** dec2 double declination (radians), after |
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** pmr2 double RA proper motion (radians/year), after |
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** pmd2 double Dec proper motion (radians/year), after |
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** px2 double parallax (arcseconds), after |
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** rv2 double radial velocity (km/s, +ve = receding), after |
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** |
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** Returned (function value): |
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** int status: |
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** -1 = system error (should not occur) |
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** 0 = no warnings or errors |
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** 1 = distance overridden (Note 6) |
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** 2 = excessive velocity (Note 7) |
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** 4 = solution didn't converge (Note 8) |
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** else = binary logical OR of the above warnings |
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** |
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** Notes: |
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** |
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** 1) The starting and ending TDB dates ep1a+ep1b and ep2a+ep2b are |
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** Julian Dates, apportioned in any convenient way between the two |
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** parts (A and B). For example, JD(TDB)=2450123.7 could be |
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** expressed in any of these ways, among others: |
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** |
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** epna epnb |
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** |
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** 2450123.7 0.0 (JD method) |
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** 2451545.0 -1421.3 (J2000 method) |
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** 2400000.5 50123.2 (MJD method) |
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** 2450123.5 0.2 (date & time method) |
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** |
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** The JD method is the most natural and convenient to use in |
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** cases where the loss of several decimal digits of resolution |
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** is acceptable. The J2000 method is best matched to the way |
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** the argument is handled internally and will deliver the |
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** optimum resolution. The MJD method and the date & time methods |
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** are both good compromises between resolution and convenience. |
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** |
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** 2) In accordance with normal star-catalog conventions, the object's |
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** right ascension and declination are freed from the effects of |
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** secular aberration. The frame, which is aligned to the catalog |
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** equator and equinox, is Lorentzian and centered on the SSB. |
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** |
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** The proper motions are the rate of change of the right ascension |
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** and declination at the catalog epoch and are in radians per TDB |
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** Julian year. |
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** |
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** The parallax and radial velocity are in the same frame. |
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** |
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** 3) Care is needed with units. The star coordinates are in radians |
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** and the proper motions in radians per Julian year, but the |
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** parallax is in arcseconds. |
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** |
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** 4) The RA proper motion is in terms of coordinate angle, not true |
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** angle. If the catalog uses arcseconds for both RA and Dec proper |
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** motions, the RA proper motion will need to be divided by cos(Dec) |
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** before use. |
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** |
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** 5) Straight-line motion at constant speed, in the inertial frame, |
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** is assumed. |
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** |
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** 6) An extremely small (or zero or negative) parallax is interpreted |
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** to mean that the object is on the "celestial sphere", the radius |
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** of which is an arbitrary (large) value (see the eraStarpv |
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** function for the value used). When the distance is overridden in |
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** this way, the status, initially zero, has 1 added to it. |
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** |
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** 7) If the space velocity is a significant fraction of c (see the |
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** constant VMAX in the function eraStarpv), it is arbitrarily set |
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** to zero. When this action occurs, 2 is added to the status. |
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** |
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** 8) The relativistic adjustment carried out in the eraStarpv function |
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** involves an iterative calculation. If the process fails to |
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** converge within a set number of iterations, 4 is added to the |
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** status. |
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** |
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** Called: |
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** eraStarpv star catalog data to space motion pv-vector |
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** eraPvu update a pv-vector |
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** eraPdp scalar product of two p-vectors |
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** eraPvstar space motion pv-vector to star catalog data |
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** |
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** Copyright (C) 2013-2020, NumFOCUS Foundation. |
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** Derived, with permission, from the SOFA library. See notes at end of file. |
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*/ |
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{ |
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double pv1[2][3], tl1, dt, pv[2][3], r2, rdv, v2, c2mv2, tl2, |
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pv2[2][3]; |
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int j1, j2, j; |
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/* RA,Dec etc. at the "before" epoch to space motion pv-vector. */ |
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j1 = eraStarpv(ra1, dec1, pmr1, pmd1, px1, rv1, pv1); |
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/* Light time when observed (days). */ |
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tl1 = eraPm(pv1[0]) / ERFA_DC; |
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/* Time interval, "before" to "after" (days). */ |
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dt = (ep2a - ep1a) + (ep2b - ep1b); |
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/* Move star along track from the "before" observed position to the */ |
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/* "after" geometric position. */ |
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eraPvu(dt + tl1, pv1, pv); |
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/* From this geometric position, deduce the observed light time (days) */ |
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/* at the "after" epoch (with theoretically unneccessary error check). */ |
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r2 = eraPdp(pv[0], pv[0]); |
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rdv = eraPdp(pv[0], pv[1]); |
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v2 = eraPdp(pv[1], pv[1]); |
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c2mv2 = ERFA_DC*ERFA_DC - v2; |
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if (c2mv2 <= 0) return -1; |
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tl2 = (-rdv + sqrt(rdv*rdv + c2mv2*r2)) / c2mv2; |
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/* Move the position along track from the observed place at the */ |
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/* "before" epoch to the observed place at the "after" epoch. */ |
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eraPvu(dt + (tl1 - tl2), pv1, pv2); |
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/* Space motion pv-vector to RA,Dec etc. at the "after" epoch. */ |
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j2 = eraPvstar(pv2, ra2, dec2, pmr2, pmd2, px2, rv2); |
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/* Final status. */ |
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j = (j2 == 0) ? j1 : -1; |
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return j; |
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} |
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/*---------------------------------------------------------------------- |
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** |
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** |
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** Copyright (C) 2013-2020, NumFOCUS Foundation. |
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** All rights reserved. |
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** |
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** This library is derived, with permission, from the International |
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** Astronomical Union's "Standards of Fundamental Astronomy" library, |
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** available from http://www.iausofa.org. |
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** |
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** The ERFA version is intended to retain identical functionality to |
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** the SOFA library, but made distinct through different function and |
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** file names, as set out in the SOFA license conditions. The SOFA |
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** original has a role as a reference standard for the IAU and IERS, |
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** and consequently redistribution is permitted only in its unaltered |
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** state. The ERFA version is not subject to this restriction and |
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** therefore can be included in distributions which do not support the |
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** concept of "read only" software. |
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** |
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** Although the intent is to replicate the SOFA API (other than |
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** replacement of prefix names) and results (with the exception of |
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** bugs; any that are discovered will be fixed), SOFA is not |
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** responsible for any errors found in this version of the library. |
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** |
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** If you wish to acknowledge the SOFA heritage, please acknowledge |
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** that you are using a library derived from SOFA, rather than SOFA |
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** itself. |
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** |
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** |
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** TERMS AND CONDITIONS |
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** |
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** Redistribution and use in source and binary forms, with or without |
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** modification, are permitted provided that the following conditions |
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** are met: |
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** |
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** 1 Redistributions of source code must retain the above copyright |
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** notice, this list of conditions and the following disclaimer. |
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** |
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** 2 Redistributions in binary form must reproduce the above copyright |
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** notice, this list of conditions and the following disclaimer in |
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** the documentation and/or other materials provided with the |
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** distribution. |
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** |
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** 3 Neither the name of the Standards Of Fundamental Astronomy Board, |
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** the International Astronomical Union nor the names of its |
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** contributors may be used to endorse or promote products derived |
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** from this software without specific prior written permission. |
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** |
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** THIS SOFTWARE IS PROVIDED BY THE COPYRIGHT HOLDERS AND CONTRIBUTORS |
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** "AS IS" AND ANY EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT |
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** LIMITED TO, THE IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS |
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** FOR A PARTICULAR PURPOSE ARE DISCLAIMED. IN NO EVENT SHALL THE |
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** COPYRIGHT HOLDER OR CONTRIBUTORS BE LIABLE FOR ANY DIRECT, INDIRECT, |
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** INCIDENTAL, SPECIAL, EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING, |
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** BUT NOT LIMITED TO, PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES; |
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** LOSS OF USE, DATA, OR PROFITS; OR BUSINESS INTERRUPTION) HOWEVER |
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** CAUSED AND ON ANY THEORY OF LIABILITY, WHETHER IN CONTRACT, STRICT |
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** LIABILITY, OR TORT (INCLUDING NEGLIGENCE OR OTHERWISE) ARISING IN |
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** ANY WAY OUT OF THE USE OF THIS SOFTWARE, EVEN IF ADVISED OF THE |
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** POSSIBILITY OF SUCH DAMAGE. |
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** |
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*/ |