Discovering dark matter is one of today's biggest challenges of particle physics and cosmology. In particular, indirect dark matter detection aims to discriminate the flux of final stable particles —gamma rays, charged cosmic rays and neutrinos — produced by particle dark matter annihilation or decay from the dominant background induced by astrophysical processes. One of the key elements is the interplay between the theoretically expected dark matter signal (flux and angular signatures) and astrophysical backgrounds. I will present the state of the art of searches for dark matter with gamma rays from Mev to TeV energies, focusing in particular towards the center of the Galaxy, where the dark matter signal is expected to be the brightest. I will also discuss future perspectives and avenues for indirect dark matter detection.
Oct 2018 - Sep 2019
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