IDM2008 - Identification of Dark Matter 2008 18-22 August 2008 AlbaNova
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Dark Matter Annihilations in the WMAP Sky (15'+5')

 The WMAP experiment has revealed an excess of microwave emission from the region around the center of our Galaxy. This signal, known as the "WMAP Haze'', has the properties expected of synchrotron emission from relativistic electrons and positrons generated in dark matter annihilations. In particular, 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.

Id: 414
Place: AlbaNova
Room: Oskar Klein auditorium
Starting date:
 20-Aug-2008 17:35
Duration: 20'
Contribution type: Talk
Primary Authors: Prof. HOOPER, Dan (Fermilab/University of Chicago)
Presenters: Prof. HOOPER, Dan
Material: Slides

Included in session: Multi messenger searches and the galactic centre
Included in track: Multi messenger searches