  The late-type stellar population in the Galactic Center was first predicted
to reside in a dynamically relaxed cusp (power law slope ranging from 3/2 to
7/4). However, observations - which rely on models to correct for projection
effects - have suggested a flat distribution instead. The need for this
correction is due to the lack of information regarding the line-of-sight
distances. With a two decade long baseline in astrometric measurements, we are
now able to measure significant projected radial accelerations, six of which
are newly reported here, that directly constrain line-of-sight distances. Here
we present a statistical approach to take advantage of this information and
more accurately constrain the shape of the radial density profile of the
late-type stellar population in the Galactic Center.
