Anisotropy of the cosmic gamma-ray background from dark matter annihilation

Abstract

High-energy photons from dark matter annihilation contribute to the cosmic gamma-ray background (CGB). Since dark matter particles are weakly interacting, annihilation can happen only in high density regions such as dark matter halos. The precise shape of the energy spectrum of CGB depends on the nature of dark matter particles, as well as the cosmological evolution of dark matter halos. In order to discriminate between the signals from dark matter annihilation and other astrophysical sources, however, the information from the energy spectrum may not be sufficient. We show that dark matter annihilation also produces a characteristic anisotropy of the CGB, which provides a powerful tool for testing the origin. We develop the formalism based on a halo model approach to calculate the three-dimensional power spectrum of dark matter clumping, which determines the power spectrum of annihilation signals. We show that the sensitivity of future gamma-ray detectors such as GLAST should allow us to measure the angular power spectrum of CGB anisotropy, if dark matter particles are supersymmetric neutralinos and they account for most of the observed mean intensity of CGB in GeV region. On the other hand, if dark matter has a relatively small mass, and accounts for most of the CGB in MeV region, then the future Advanced Compton Telescope should be able to measure the anisotropy in MeV region. As the intensity of photons from annihilation is proportional to the density squared, we show that the predicted shape of the angular power spectrum of gamma rays from dark matter annihilation is different from that due to other astrophysical sources such as blazars. Therefore, the angular power spectrum of the CGB provides a smoking-gun signature of dark matter annihilation.

15 pages, 12 figures; minor revision, added references; accepted to PRD

References in corpus (1)

• Can Dark Matter Annihilation Dominate the Extragalactic Gamma-Ray Background?

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