We present new observations of the nuclear star cluster in the central parsec of the Galaxy with the adaptive optics assisted , integral field spectrograph SINFONI on the ESO/VLT .
Our work allows the spectroscopic detection of early and late type stars to m _ { K } \geq 16 , more than 2 magnitudes deeper than our previous data sets .
Our observations result in a total sample of 177 bona fide early-type stars .
We find that most of these Wolf Rayet ( WR ) , O- and B- stars reside in two strongly warped disks between 0.8 ” and 12 ” from SgrA* , as well as a central compact concentration ( the S-star cluster ) centered on SgrA* .
The later type B stars ( m _ { K } > 15 ) in the radial interval between 0.8 ” and 12 ” seem to be in a more isotropic distribution outside the disks .
The observed dearth of late type stars in the central few arcseconds is puzzling , even when allowing for stellar collisions .
The stellar mass function of the disk stars is extremely top heavy with a best fit power law of \mathrm { d } N / \mathrm { d } m \propto m ^ { -0.45 \pm 0.3 } .Since at least the WR/O-stars were formed in situ in a single star formation event \sim 6 Myrs ago , this mass function probably reflects the initial mass function ( IMF ) .
The mass functions of the S-stars inside 0.8 ” and of the early-type stars at distances beyond 12 ” are compatible with a standard Salpeter/Kroupa IMF ( best fit power law of \mathrm { d } N / \mathrm { d } m \propto m ^ { -2.15 \pm 0.3 } ) .