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Gravitational potentials of the Milky Way and extragalactic structures caninfluence the propagation of the cosmic neutrino background (CNB). Ofparticular interest to future CNB observatories, such as PTOLEMY, is the CNBnumber density on Earth. In this study, we have developed a simulationframework that maps the trajectories of relic neutrinos as they move throughthe local gravitational environment. The potentials are based on the darkmatter halos found in state-of-the-art cosmological N-body simulations,resulting in a more nuanced and realistic input than the previously employedanalytical models. We find that the complex dark matter distributions, alongwith their dynamic evolution, influence the abundance and anisotropies of theCNB in ways unaccounted for by earlier analytical methods. Importantly, thesecosmological simulations contain multiple instances of Milky Way-like halosthat we employ to model a variety of gravitational landscapes. Consequently, wenotice a variation in the CNB number densities that can be primarily attributedto the differences in the masses of these individual halos. For neutrino massesbetween $0.01$ and $0.3$ eV, we note clustering factors within the range of$1+\mathcal{O}(10^{-3})$ to $1+\mathcal{O}(1)$. Furthermore, the asymmetricnature of the underlying dark matter distributions within the halos results innot only overdense, but intriguingly, underdense regions within the full-skyanisotropy maps. Gravitational clustering appears to have a significant impacton the angular power spectra of these maps, leading to orders of magnitude morepower on smaller scales beyond multipoles of $\ell = 3$ when juxtaposed againstpredictions by primordial fluctuations. We discuss how our results reshape ourunderstanding of relic neutrino clustering and how this might affectobservability of future CNB observatories such as PTOLEMY.

Influence of local structure on relic neutrino abundances and anisotropies