High-Energy Neutrino Production in Clusters of Galaxies
  In this work, we compute the contribution from clusters of galaxies to the
diffuse neutrino background. Clusters of galaxies can potentially produce
cosmic rays (CRs) up to very-high energies via large-scale shocks and turbulent
acceleration. Due to their unique magnetic-field configuration, CRs with energy
$\leq 10^{17}$ eV can be trapped within these structures over cosmological time
scales, and generate secondary particles, including neutrinos and gamma rays,
through interactions with the background gas and photons. We employ
three-dimensional cosmological magnetohydrodynamical simulations of structure
formation to model the turbulent intergalactic medium. We use the distribution
of clusters within this cosmological volume to extract the properties of this
population. We propagate CRs in this environment using multi-dimensional Monte
Carlo simulations across different redshifts (from $z \sim 5 \; \text{to} \; z
=0$), 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
$E_{max} = 10^{16} - 10^{17}$ eV, clusters contribute to a substantial fraction
to the diffuse flux observed by the IceCube Neutrino Observatory, and most of
the contribution comes from clusters with $M > 10^{14} \; M_{\odot}$ and
redshift $z < 0.3$.
