Cosmic Ballet III: halo spin evolution in the cosmic web

TL;DR

This study investigates how dark matter halo spins evolve within the cosmic web, revealing correlations with filament environment, thickness, and evolving alignment patterns across different halo masses and redshifts.

Contribution

It introduces a detailed analysis of halo spin evolution and alignment with the cosmic web, highlighting new correlations with filament properties and their redshift dependence.

Findings

Halo spin magnitude correlates with web environment and filament thickness.

Low-mass haloes align their spins along filament spines, high-mass haloes perpendicular.

Halo spins tend to become more perpendicular to filaments over time.

Abstract

We explore the evolution of halo spins in the cosmic web using a very large sample of dark matter haloes in the $\Lambda$CDM Planck-Millennium N-body simulation. We use the NEXUS+ multiscale formalism to identify the hierarchy of filaments and sheets of the cosmic web at several redshifts. We find that at all times the magnitude of halo spins correlates with the web environment, being largest in filaments, and, for the first time, we show that it also correlates with filament thickness as well as the angle between spin-orientation and the spine of the host filament. For example, massive haloes in thick filaments spin faster than their counterparts in thin filaments, while for low-mass haloes the reverse is true. We also have studied the evolution of alignment between halo spin orientations and the preferential axes of filaments and sheets. The alignment varies with halo mass, with the spins of low-mass haloes being predominantly along the filament spine, while those of high-mass haloes being predominantly perpendicular to the filament spine. On average, for all halo masses, halo spins become more perpendicular to the filament spine at later times. At all redshifts, the spin alignment shows a considerable variation with filament thickness, with the halo mass corresponding to the transition from parallel to perpendicular alignment varying by more than one order of magnitude. The environmental dependence of halo spin magnitude shows little evolution for $z\leq2$ and is likely a consequence of the correlations in the initial conditions or high redshift effects