Cosmic Ballet III: Halo spin evolution in the cosmic web

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