2 micron spectroscopy within 0 ''.13 of Sagittarius A

We present moderate- (R approximate to 2700) and high-resolution (R approxi mate to 22,400) 2.0-2.4 mu m spectroscopy of the central 0.1 arcsec(2) of t he Galaxy obtained with the facility near-infrared spectrometer (NIRSPEC) f or the Keek II telescope. The composite spectra do not have any features at tributable to the brightest stars in the central cluster; i.e., after backg round subtraction, W12CO(2-0) < 2 Angstrom. This Stringent limit leads us t o conclude that the majority, if not all, of the stars are hotter than typi cal red giants. Coupled with previously reported photometry, we conclude th at the sources are likely OB main-sequence stars. In addition, the continuu m slope in the composite spectrum is bluer than that of a red giant and is similar to that of the nearby hot star IRS 16NW. It is unlikely that they a re late-type giants stripped of their outer envelopes because such sources would be much fainter than those observed. Given their inferred youth (tau( age) < 20 Myr), we suggest the possibility that the stars have formed withi n 0.1 pc of the supermassive black hole. We find a newly identified broad-l ine component (V-FWHM approximate to 1000 km s(-1)) toward the 2.2178 mu m [Fe III] line located within a few arcseconds of Sagittarius AX. A similar component is not seen in the Br gamma emission.