  We analyze deep near-IR adaptive optics imaging as well as new proper motion
data of the nuclear star cluster of the Milky Way. The surface density
distribution of faint stars peaks within 0.2" of the black hole candidate
SgrA*. The radial density distribution of this stellar 'cusp' follows a power
law of exponent 1.3-1.4. The K-band luminosity function of the overall nuclear
stellar cluster (within 9" of SgrA*) resembles that of the large scale,
Galactic bulge, but shows an excess of stars at K<14.
  We find that most of the massive early type stars at distances 1-10" from
SgrA* are located in two rotating and geometrically thin disks. These disks are
inclined at large angles and counter-rotate with respect to each other. Their
stellar content is essentially the same, indicating that they formed at the
same time.
  The star closest to SgrA* in 2002, S2, exhibits a 3.8 micron excess. We
propose that the mid-IR emission either comes from the accretion flow around
the black hole itself, or from dust in the accretion flow that is heated by the
ultra-violet emission of S2.
