The WMAP experiment has revealed an excess of microwave emission from the region around the center of our Galaxy .
It has been suggested that this signal , known as the “ WMAP Haze ” , could be synchrotron emission from relativistic electrons and positrons generated in dark matter annihilations .
In this letter , we revisit this possibility .
We find that the angular distribution of the WMAP Haze matches the prediction for dark matter annihilations with a cusped density profile , \rho ( r ) \propto r ^ { -1.2 } in the inner kiloparsecs .
Comparing the intensity in different WMAP frequency bands , we find that a wide range of possible WIMP annihilation modes are consistent with the spectrum of the haze for a WIMP with a mass in the 100 GeV to multi-TeV range .
Most interestingly , we find that to generate the observed intensity of the haze , the dark matter annihilation cross section is required to be approximately equal to the value needed for a thermal relic , \sigma v \sim 3 \times 10 ^ { -26 } cm ^ { 3 } /s .
No boost factors are required .
If dark matter annihilations are in fact responsible for the WMAP Haze , and the slope of the halo profile continues into the inner Galaxy , GLAST is expected to detect gamma rays from the dark matter annihilations in the Galactic Center if the WIMP mass is less than several hundred GeV .