The Density of Dark Matter in the Galactic Bulge and Implications for
  Indirect Detection
  A recent study, making use of the number of horizontal branch stars observed
in infrared photometric surveys and kinematic measurements of M-giant stars
from the BRAVA survey, combined with N-body simulations of stellar populations,
has presented a new determination of the dark matter mass within the bulge-bar
region of the Milky Way. That study constrains the total mass within the $\pm
2.2 \times \pm 1.4 \times \pm 1.2$ kpc volume of the bulge-bar region to be
($1.84 \pm 0.07) \times 10^{10} \, M_{\odot}$, of which 9-30% is made up of
dark matter. Here, we use this result to constrain the the Milky Way's dark
matter density profile, and discuss the implications for indirect dark matter
searches. Although uncertainties remain significant, these results favor dark
matter distributions with a cusped density profile. For example, for a scale
radius of 20 kpc and a local dark matter density of 0.4 GeV/cm$^3$, density
profiles with an inner slope of 0.69 to 1.40 are favored, approximately
centered around the standard NFW value. In contrast, profiles with large
flat-density cores are disfavored by this information.
