  High spatial resolution, near-infrared imaging and spectroscopy of the
nuclear star cluster have given key new insights about the dynamics, evolution
and mass distribution in the Milky Way Center. The central parsec is powered by
a cluster of hot, massive stars which must have formed a few million years ago.
Either star formation was triggered in the central parsec by the infall of a
very dense cloud, or a dense, young star cluster formed outside of the central
parsec sank rapidly into the nuclear region through dynamical friction. The
presence of luminous asymptotic giant branch (AGB) stars suggests that there
were earlier such star formation episodes. Measurements of radial and proper
motions for more than 200 stars delineate the stellar dynamics to a scale of a
few light days from the dynamic center which is coincident with the compact
radio source (SgrA*) within ~0.1" (800 AU). The stellar velocities increase
toward SgrA* with a Kepler law (to >1000 km/s for the innermost stars),
implying the presence of a three million solar mass central (dark) mass. The
observations make a compelling case that this mass concentration is a black
hole which is currently accreting at a low rate or radiating at low efficiency.
With the exception of the young, massive stars the velocity field of the
central stellar cluster is close to isotropic. The young stars are
characterized by a turbulent rotation pattern that still carries the imprint of
the angular momentum distribution in the original cloud or star cluster.
