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IDM2008 - Identification of Dark Matter 2008
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: slide Slides
Included in session: Multi messenger searches and the galactic centre
Included in track: Multi messenger searches

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