  We report a new analysis of stellar dynamics in the Galactic centre, based on
improved sky and LOS velocities for >100 stars within a few arcsec of SgrA*.
Overall the motions do not deviate strongly from isotropy. For 32 stars with
all 3 components determined the absolute, LOS and sky velocities agree well, as
for a spherical cluster. The projected radial and tangential motions of all 104
pm stars are also consistent with overall isotropy. However, the projected
velocities of the young, early type stars have a strong radial dependence. Most
of the bright HeI stars 1-10" from SgrA* are on tangential orbits. This
anisotropy of the HeI stars and most of the brighter IRS16 complex members is
largely caused by a CW and counter-rotating, coherent rotation pattern. The
overall rotation of the young star cluster probably is a remnant of the angular
momentum in the cloud these stars formed from. The fainter, fast stars within
\~1" of SgrA* appear to be largely moving on radial or very elliptical orbits.
We have not detected nonlinear motion for any of them. Most of the SgrA*
cluster members also are on CW orbits. Spectroscopy shows them to be early type
stars. We propose that the SgrA* cluster stars are those members of the early
type cluster with small angular momentum which can plunge to the vicinity of
SgrA*. Our anisotropy-independent estimate of the Sun-GC distance is 7.8-8.2
kpc (+/- 0.9 kpc). We include velocity anisotropy in estimating the central
mass distribution. We confirm previous conclusions that a compact central mass
concentration is present and dominates the potential from 0.01-1 pc. The
central mass ranges from 2.6-3.3E6 M_sun. (abridged)
