fk45z¶
- erfa.fk45z(r1950, d1950, bepoch)[source]¶
Convert a B1950.0 FK4 star position to J2000.0 FK5, assuming zero proper motion in the FK5 system.
- Parameters:
- r1950double array
- d1950double array
- bepochdouble array
- Returns:
- r2000double array
- d2000double array
Notes
Wraps ERFA function
eraFk45z
. The ERFA documentation is:- - - - - - - - - e r a F k 4 5 z - - - - - - - - - Convert a B1950.0 FK4 star position to J2000.0 FK5, assuming zero proper motion in the FK5 system. This function converts a star's catalog data from the old FK4 (Bessel-Newcomb) system to the later IAU 1976 FK5 (Fricke) system, in such a way that the FK5 proper motion is zero. Because such a star has, in general, a non-zero proper motion in the FK4 system, the function requires the epoch at which the position in the FK4 system was determined. Given: r1950,d1950 double B1950.0 FK4 RA,Dec at epoch (rad) bepoch double Besselian epoch (e.g. 1979.3) Returned: r2000,d2000 double J2000.0 FK5 RA,Dec (rad) Notes: 1) The epoch bepoch is strictly speaking Besselian, but if a Julian epoch is supplied the result will be affected only to a negligible extent. 2) The method is from Appendix 2 of Aoki et al. (1983), but using the constants of Seidelmann (1992). See the function eraFk425 for a general introduction to the FK4 to FK5 conversion. 3) Conversion from equinox B1950.0 FK4 to equinox J2000.0 FK5 only is provided for. Conversions for different starting and/or ending epochs would require additional treatment for precession, proper motion and E-terms. 4) In the FK4 catalog the proper motions of stars within 10 degrees of the poles do not embody differential E-terms effects and should, strictly speaking, be handled in a different manner from stars outside these regions. However, given the general lack of homogeneity of the star data available for routine astrometry, the difficulties of handling positions that may have been determined from astrometric fields spanning the polar and non- polar regions, the likelihood that the differential E-terms effect was not taken into account when allowing for proper motion in past astrometry, and the undesirability of a discontinuity in the algorithm, the decision has been made in this ERFA algorithm to include the effects of differential E-terms on the proper motions for all stars, whether polar or not. At epoch J2000.0, and measuring "on the sky" rather than in terms of RA change, the errors resulting from this simplification are less than 1 milliarcsecond in position and 1 milliarcsecond per century in proper motion. References: Aoki, S. et al., 1983, "Conversion matrix of epoch B1950.0 FK4-based positions of stars to epoch J2000.0 positions in accordance with the new IAU resolutions". Astron.Astrophys. 128, 263-267. Seidelmann, P.K. (ed), 1992, "Explanatory Supplement to the Astronomical Almanac", ISBN 0-935702-68-7. Called: eraAnp normalize angle into range 0 to 2pi eraC2s p-vector to spherical eraEpb2jd Besselian epoch to Julian date eraEpj Julian date to Julian epoch eraPdp scalar product of two p-vectors eraPmp p-vector minus p-vector eraPpsp p-vector plus scaled p-vector eraPvu update a pv-vector eraS2c spherical to p-vector This revision: 2023 March 4 Copyright (C) 2013-2023, NumFOCUS Foundation. Derived, with permission, from the SOFA library. See notes at end of file.