Dark Matter Signals in the gamma-ray sky

Abstract. Detection of gamma rays and cosmic rays from the annihilation or decay of dark matter particles is a promising method for identifying dark matter, understanding its intrinsic properties, and mapping its distribution in the universe. I will review recent results from the Fermi Gamma-ray Space Telescope and other space-based experiments, and highlight the constraints these currently place on particle dark matter models. I will also discuss the prospects for indirect searches to robustly identify or exclude a dark matter signal using upcoming data. One of the major open issues in our understanding of the Universe is the existence of an extremely-weakly interacting form of matter, the Dark Matter (DM), supported by a wide range of observations including large scale structures, the cosmic microwave background and the isotopic abundances re-sulting from the primordial nucleosynthesis. The DM might be detected indirectly through anomalous cosmic rays (CRs) produced by their annihilations in the galactic center, galactic halo or extragalactic structures such as dwarf spheroidal galaxies and clusters. These annihilations will produce γ-rays or antimatter, and fluxes of these particles can be measured in space-based detectors such as Fermi-LAT (γ-rays) and PAMELA or AMS (antimatter). γ-rays can also be measured in Cherenkov telescope