High-energy neutrinos and gamma rays from galaxy clusters

Abstract

Galaxy clusters are rich astrophysical environments. Their properties are linked to the complex processes that take place in their interiors, many of which involve cosmic rays (CRs) and charged leptons. These particles can be accelerated by shocks in the intracluster medium (ICM), or injected in the ICM by the astrophysical objects embedded therein. Hadronic and/or leptonic interactions can produce high-energy secondaries. Here I briefly review the mechanisms responsible for this emission. Then, I compare theoretical predictions for the total emission of gamma rays and neutrinos by the whole population of galaxy clusters with observations. Finally, I discuss the prospects for detecting high-energy emission from galaxy clusters with the current and next generation of gamma-ray and neutrino telescopes.