region by the Atmospheric Cerenkov Telescopes HESS [@hess], MAGIC [@magic], WHIPPLE [@whipple] and CANGAROO-II [@cangaroo] has made efforts to identify gamma rays from dark matter annihilations more difficult. This source appears to be coincident with the dynamical center of the Milky Way (Sgr A$^*$) and has no detectable angular extension (less than 1.2 arcminutes). Its spectrum is well described by a power-law, $dN_{\gamma}/dE_{\gamma} \propto E_{\gamma}^{-\alpha}$, where $\alpha=2.25 \pm
0.04 (\rm{stat}) \pm 0.10 (\rm{syst})$ over the range of 160 GeV to 20 TeV. Although speculations were initially made that this source could be the product of annihilations of very heavy ($\gsim 10$ TeV) dark matter particles [@actdark], the spectral shape appears inconsistent with a dark matter interpretation. The source of these gamma rays is more likely an astrophysical accelerator associated with our Galaxy’s central supermassive black hole [@hessastro]. Although this gamma ray source represents a formidable background for GLAST and other experiments searching for dark matter annihilation radiation [@gabi], it may be possible to reduce the impact of this and other backgrounds by studying the angular distribution of gamma rays from this region of the sky [@Dodelson:2007gd].

The prospects for identifying dark matter annihilation radiation from the Galactic Center depends critically 