Dark Matter Profile in the Galactic Center

TL;DR

A quasiequilibrium profile of dark matter particles in the inner parsec of the Galaxy, rhodm proportional to r(-3/2), caused by scattering with the dense stellar cluster around the supermassive black hole in Sgr A* and is independent of the initial conditions.

Abstract

We describe a quasi-equilibrium profile of dark matter particles in the inner parsec of the Galaxy, rho ~ r^-3/2. This "mini-cusp" profile is caused by scattering with the dense stellar cluster around the supermassive black hole in Sgr A* and is independent of the initial conditions. The implications for detection of gamma rays from WIMP dark matter annihilation in the Galactic center are a mild enhancement of the flux, and a characteristic central feature in the angular distribution which could be detectable by high-resolution Atmospheric Cherenkov Telescopes.

Figures (1)

• Figure 1: Minimum detectable annihilation cross section times velocity as a function of WIMP mass. The filled circles correspond to SUSY model WIMPs with $\Omega_\chi h^2 = 0.11 \pm 0.01$Spergel:03 and the open circles correspond to SUSY models with $\Omega_\chi h^2$ between 1$\sigma$ and 2$\sigma$ away from the central value.