A varying mass-to-light ratio in the galactic center cluster?

We reanalyze published kinematic and photometric data for the cool star population in the central 10 pc (240 '') of the Galaxy, while (1) isolating the photometric data appropriate to this population, and (2) properly allowing for projection effects. Under the assumptions that the system is spherical and isotropic, we find that M/L(K) varies from less than or equal to 1 outside a radius of 0.8 pc to >2 at 0.35 pc. This behavior cannot be due to the presence of a central massive black hole. We suggest that such a varying M/L(K) may be due to an increasing concentration of stellar remnants toward the Galactic center. Our derived mass-radius curve confirms the existence of similar to 3 x 10(6) M(.) within 0.35 pc of the Galactic center, and similar to 1.5 x 10(6) M(.) within 0.2 pc. However, the latter estimate is subject to the uncertain distribution of cool stars in this region. We also consider the dynamics of the hot star population close to the Galactic center and show that the velocity dispersion of the He I stars and the surface brightness distribution of the hot stars are consistent with the mass distribution inferred from the cool stars.