  We report preliminary results based on new near-infrared observations of the
central stellar cluster of our Galaxy conducted with the infrared spectrometer
ISAAC at the ESO VLT UT1 and the MPE speckle camera SHARP at the ESO NTT. We
obtained lambda / dlambda >= 3000 K-band spectroscopy of the 2.058 um He I,
2.165 um Br gamma emission lines, and 2.29 um CO bandhead absorption line.
These data demonstrate clearly that there is no strong CO bandhead absorption
originating in the northern part (S1/S2 area) of the central stellar cluster at
the position of Sgr A*. This makes it likely that these K~14.5 stars are O9 -
B0.5 stars with masses of 15 to 20 M(sun). Weaker CO bandhead absorption in the
southern part of the cluster (S10/S11 area) could be due to contributions from
neighbouring stars. We also report the detection of Br gamma line emission at
the position of the central stellar cluster which could be associated with the
'mini-spiral' rather than with the Sgr A* cluster itself. At the NTT we
obtained another epoch epoch of proper motion measurments. The changes of
source positions are consistent with the proper motion velocities derived from
earlier epochs.
