2023/07/29 by Saqib Hussain, Hussain, Saqib, G. Pagliaroli +3
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Dark Matter and Cosmic Phenomena #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Neutrino Physics Research
paper · pdf · doi:10.48550/arxiv.2307.15851
openalex publication_date 2023/07/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We compute the contribution from clusters of galaxies to the diffuse neutrino and γ-ray background. Due to their unique magnetic-field configuration, cosmic rays (CRs) with energy ≤1017 eV can be confined within these structures over cosmological time scales, and generate secondary particles, including neutrinos and γ-rays, through interactions with the background gas and photons. We employ three-dimensional (3D) cosmological magnetohydrodynamical (MHD) simulations of structure formation to model the turbulent intergalactic and intracluster media. We propagate CRs in these environments using multi-dimensional Monte Carlo simulations across different redshifts (from z ∼ 5 to z = 0), considering all relevant photohadronic, photonuclear, and hadronuclear interactions. We also include the cosmological evolution of the CR sources. We find that for CRs injected with a spectral index 1.5 - 2.7 and cutoff energy Emax = 1016 - 1017~eV, clusters contribute to a substantial fraction to the diffuse fluxes observed by the IceCube and Fermi-LAT, and most of the contribution comes from clusters with M > 1014 M\odot and redshift z < 0.3. We also estimated the multimessenger contributions from the local galaxy cluster.