c2t00a¶

erfa.c2t00a(tta, ttb, uta, utb, xp, yp)[source]¶

Form the celestial to terrestrial matrix given the date, the UT1 and the polar motion, using the IAU 2000A precession-nutation model.

Parameters:

ttadouble array
ttbdouble array
utadouble array
utbdouble array
xpdouble array
ypdouble array

Returns:

rc2tdouble array

Notes

Wraps ERFA function eraC2t00a. The ERFA documentation is:

- - - - - - - - - -
 e r a C 2 t 0 0 a
- - - - - - - - - -

Form the celestial to terrestrial matrix given the date, the UT1 and
the polar motion, using the IAU 2000A precession-nutation model.

Given:
   tta,ttb  double         TT as a 2-part Julian Date (Note 1)
   uta,utb  double         UT1 as a 2-part Julian Date (Note 1)
   xp,yp    double         CIP coordinates (radians, Note 2)

Returned:
   rc2t     double[3][3]   celestial-to-terrestrial matrix (Note 3)

Notes:

1) The TT and UT1 dates tta+ttb and uta+utb are Julian Dates,
   apportioned in any convenient way between the arguments uta and
   utb.  For example, JD(UT1)=2450123.7 could be expressed in any of
   these ways, among others:

           uta            utb

       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 and MJD methods are good compromises
   between resolution and convenience.  In the case of uta,utb, the
   date & time method is best matched to the Earth rotation angle
   algorithm used:  maximum precision is delivered when the uta
   argument is for 0hrs UT1 on the day in question and the utb
   argument lies in the range 0 to 1, or vice versa.

2) The arguments xp and yp 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.

3) The matrix rc2t transforms 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), RC2I is the
   celestial-to-intermediate matrix, ERA is the Earth rotation
   angle and RPOM is the polar motion matrix.

4) A faster, but slightly less accurate, result (about 1 mas) can
   be obtained by using instead the eraC2t00b function.

Called:
   eraC2i00a    celestial-to-intermediate matrix, IAU 2000A
   eraEra00     Earth rotation angle, IAU 2000
   eraSp00      the TIO locator s', IERS 2000
   eraPom00     polar motion matrix
   eraC2tcio    form CIO-based celestial-to-terrestrial matrix

Reference:

   McCarthy, D. D., Petit, G. (eds.), IERS Conventions (2003),
   IERS Technical Note No. 32, BKG (2004)

This revision:  2021 May 11

Copyright (C) 2013-2023, NumFOCUS Foundation.
Derived, with permission, from the SOFA library.  See notes at end of file.

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