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.
Highlights
One of the major open issues in our understanding of the Universe is the existence of an extremelyweakly 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 resulting from the primordial nucleosynthesis
The experimental information available on the Cosmic Ray Electron (CRE) spectrum has been dramatically expanded with a high precision measurement of the electron spectrum from 7 GeV to 1 TeV by the Fermi LAT [3,4,5]
No positive detection of Cosmic Ray Electron (CRE) anisotropy was reported by the Fermi-LAT collaboration, but some stringent upper limits were published [12] and the pulsar scenario is still compatible with these upper limits
Summary
One of the major open issues in our understanding of the Universe is the existence of an extremelyweakly 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 resulting from the primordial nucleosynthesis. The AMS-02 collaboration presented the measurement of the positron fraction [13] that confim the positron ratio rise observed by PAMELA and Fermi Large Area Telescope (Fermi-LAT ) and extend it up to 350 GeV (see figure 2).
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