Journal
NUCLEAR PHYSICS B
Volume 831, Issue 1-2, Pages 178-203Publisher
ELSEVIER
DOI: 10.1016/j.nuclphysb.2010.01.012
Keywords
Dark Matter; PAMELA; FERMI
Categories
Funding
- Direct For Mathematical & Physical Scien
- Division Of Physics [0653354] Funding Source: National Science Foundation
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The cosmic-ray excess observed by PAMELA in the positron fraction and by FERMI and HESS in e(-) + e(+) can be interpreted in terms of DM annihilations or decays into leptonic final states. Final states into tau's or 4 mu give the best-fit to the excess. However, in the annihilation scenario, they are incompatible with photon and neutrino constraints, unless DM has a quasi-constant density profile. Final states involving e's are less constrained but poorly fit the excess, unless hidden sector radiation makes their energy spectrum smoother, allowing a fit to all the data with a combination of leptonic modes. In general, DM lighter than about a TeV cannot fit the excesses, so PAMELA should find a greater positron fraction at higher energies. The DM interpretation can be tested by FERMI gamma observations above 10 GeV: if the e(+/-) excess is everywhere in the DM halo, Inverse Compton scattering on ambient light produces a well-predicted gamma excess that FERMI should soon detect. (C) 2010 Elsevier B.V. All rights reserved.
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