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The late-type stellar population in the Galactic Center was first predictedto reside in a dynamically relaxed cusp (power law slope ranging from 3/2 to7/4). However, observations - which rely on models to correct for projectioneffects - have suggested a flat distribution instead. The need for thiscorrection is due to the lack of information regarding the line-of-sightdistances. With a two decade long baseline in astrometric measurements, we arenow able to measure significant projected radial accelerations, six of whichare newly reported here, that directly constrain line-of-sight distances. Herewe present a statistical approach to take advantage of this information andmore accurately constrain the shape of the radial density profile of thelate-type stellar population in the Galactic Center.

The late-type stellar density profile in the Galactic Center: A statistical approach