**ACTION:**- Quick mean to apparent place: transform a star from
mean place to geocentric apparent place, given the
star-independent parameters. The reference frames and
timescales used are post IAU 1976.
**CALL:**`CALL sla_MAPQK (RM, DM, PR, PD, PX, RV, AMPRMS, RA, DA)`

**GIVEN:**-

*RM,DM***D**mean (radians) *PR,PD***D**proper motions: changes per Julian year *PX***D**parallax (arcsec) *RV***D**radial velocity (km s ^{-1}, +ve if receding)*AMPRMS***D(21)**star-independent mean-to-apparent parameters: (1) time interval for proper motion (Julian years) (2-4) barycentric position of the Earth (AU) (5-7) heliocentric direction of the Earth (unit vector) (8) (gravitational radius of Sun)(Sun-Earth distance) (9-11) **v**: barycentric Earth velocity in units of c(12) (13-21) precession/nutation matrix

**RETURNED:**-

*RA,DA***D**apparent (radians)

**NOTES:**- 1.
- Use of this routine is appropriate when efficiency is important and where many star positions, all referred to the same equator and equinox, are to be transformed for one epoch. The star-independent parameters can be obtained by calling the sla_MAPPA routine.
- 2.
- If the parallax and proper motions are zero the sla_MAPQKZ routine can be used instead.
- 3.
- The vectors AMPRMS(2-4) and AMPRMS(5-7) are referred to the mean equinox and equator of epoch EQ.
- 4.
- Strictly speaking, the routine is not valid for solar-system sources, though the error will usually be extremely small. However, to prevent gross errors in the case where the position of the Sun is specified, the gravitational deflection term is restrained within about of the centre of the Sun's disc. The term has a maximum value of about at this radius, and decreases to zero as the centre of the disc is approached.

**REFERENCES:**- 1.
- 1984
*Astronomical Almanac*, pp B39-B41. - 2.
- Lederle & Schwan, 1984.
*Astr.Astrophys.***134**, 1-6.

Starlink User Note 67

P. T. Wallace

12 October 1999

E-mail:ptw@star.rl.ac.uk