### SYNOPSYS

void slaAmpqk(ra, da, amprms, rm, dm)

double ra
double da
double *amprms
double *rm
double *dm

### DESCRIPTION

```
Convert star RA,Dec from geocentric apparent to mean place.

The mean coordinate system is the post IAU 1976 system,
loosely called FK5.

Use of this routine is appropriate when efficiency is important
and where many star positions are all to be transformed for
one epoch and equinox.  The star-independent parameters can be
obtained by calling the slaMappa routine.

```

#### Given

```     ra       double      apparent RA (radians)
da       double      apparent Dec (radians)

```
amprms double star-independent mean-to-apparent parameters
```
(0)      time interval for proper motion (Julian years)
(1-3)    barycentric position of the Earth (AU)
(4-6)    heliocentric direction of the Earth (unit vector)
(7)      (grav rad Sun)*2/(Sun-Earth distance)
(8-10)   abv: barycentric Earth velocity in units of c
(11)     sqrt(1-v*v) where v=modulus(abv)
(12-20)  precession/nutation (3,3) matrix

```

#### Returned

```     *rm      double      mean RA (radians)
*dm      double      mean Dec (radians)

```

#### References

```     1984 Astronomical Almanac, pp B39-B41.
(also Lederle & Schwan, Astron. Astrophys. 134, 1-6, 1984)

```

#### Notes

```
1)  The accuracy is limited by the routine slaEvp, called
by slaMappa, which computes the Earth position and
velocity using the methods of Stumpff.  The maximum
error is about 0.3 milliarcsecond.

2)  Iterative techniques are used for the aberration and
light deflection corrections so that the routines
slaAmp (or slaAmpqk) and slaMap (or slaMapqk) are
accurate inverses;  even at the edge of the Sun's disc
the discrepancy is only about 1 nanoarcsecond.

```

### Called

``` slaDcs2c, slaDimxv, slaDvdv, slaDvn, slaDcc2s,