c2txy¶

erfa.c2txy(tta, ttb, uta, utb, x, y, xp, yp)[source]¶

Form the celestial to terrestrial matrix given the date, the UT1, the CIP coordinates and the polar motion.

Parameters:

ttadouble array
ttbdouble array
utadouble array
utbdouble array
xdouble array
ydouble array
xpdouble array
ypdouble array

Returns:

rc2tdouble array

Notes

Wraps ERFA function eraC2txy. The ERFA documentation is:

 - - - - - - - - -
  e r a C 2 t x y
 - - - - - - - - -

 Form the celestial to terrestrial matrix given the date, the UT1,
 the CIP coordinates and the polar motion.  IAU 2000.

 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)
    x,y      double         Celestial Intermediate Pole (Note 2)
    xp,yp    double         coordinates of the pole (radians, Note 3)

 Returned:
    rc2t     double[3][3]   celestial-to-terrestrial matrix (Note 4)

 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 o
    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 Celestial Intermediate Pole coordinates are the x,y
    components of the unit vector in the Geocentric Celestial
    Reference System.

 3) 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.

 4) 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), ERA is the Earth
    Rotation Angle and RPOM is the polar motion matrix.

 5) Although its name does not include "00", This function is in fact
    specific to the IAU 2000 models.

 Called:
    eraC2ixy     celestial-to-intermediate matrix, given X,Y
    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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