Relation between halo spin and cosmic web filaments at z=3

Abstract

We investigate the spin evolution of dark matter haloes and their dependence on the number of connected filaments from the cosmic web at high redshift (spin-filament relation hereafter). To this purpose, we have simulated $5000$ haloes in the mass range $5\times 10^9{h}^{-1}{M}_{\odot }$ to $5\times 10^{11}{h}^{-1}{M}_{\odot }$ at $z=3$ in cosmological N-body simulations. We confirm the relation found by Prieto et al. 2015 where haloes with fewer filaments have larger spin. We also found that this relation is more significant for higher halo masses, and for haloes with a passive (no major mergers) assembly history. Another finding is that haloes with larger spin or with fewer filaments have their filaments more perpendicularly aligned with the spin vector. Our results point to a picture in which the initial spin of haloes is well described by tidal torque theory and then gets subsequently modified in a predictable way because of the topology of the cosmic web, which in turn is given by the currently favoured LCDM model. Our spin-filament relation is a prediction from LCDM that could be tested with observations.

arXiv comment8 pages, 9 figures. Accepted for publication in MNRAS

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• Formation and Morphology of the First Galaxies in the Cosmic Morning
• Wobbling galaxy spin axes in dense environments
• Assessing the reliability of the Bisous filament finder
• Living with Neighbors. V. Better-aligned Spiral+Spiral Galaxy Pairs Show Stronger Star Formation