Speaker
Description
Galaxy clusters are the largest gravitationally-bounded systems in the Universe. In these objects, the dark matter (DM) represents almost 85% of their content, while ~5% are galaxies and the rest corresponds to hot gas filling the Intra Cluster Medium (ICM). If the DM is a heavy particle like the Weakly Interactive Massive Particles (WIMPs), galaxy clusters are exceptional targets to constraint DM particle properties by searching for diffuse gamma-ray emission obtained as final stable products of annihilation or decay to heavy quarks and leptons. In this work, we investigate an additional component to the diffuse emission in galaxy clusters, that results from the propagation of electrons and positrons originated from DM annihilation or decay. Indeed, for nearby clusters, we expect to have a significant boost in the expected emission from this e-e+ channel in the GeV-TeV energy regime. As an example, we simulate a Perseus-like cluster using CRpropa to obtain the expected emission at Earth, and compare to the sensitivity of both Fermi- LAT and LHAASO.