Using the Horizon-AGN simulation we find a mass dependent spin orientation trend for galaxies: the spin of low-mass, rotation-dominated, blue, star-forming galaxies are preferentially aligned with their closest filament, whereas high-mass, velocity dispersion- supported, red quiescent galaxies tend to possess a spin perpendicular to these filaments. We explore the physical mechanisms driving galactic spin swings and quantify how much mergers and smooth accretion re-orient them relative to their host filaments and impact their shape. In particular, we analyze the effect of dispersion and morphology of galaxies and discuss potential tracers for prospective surveys.
@article{arxiv.1410.4111,
title = {How do galaxies build up their spin in the cosmic web?},
author = {charlotte Welker and Yohan Dubois and Julien Devriendt and Christophe Pichon and Sebastien Peirani},
journal= {arXiv preprint arXiv:1410.4111},
year = {2017}
}
Comments
proceedings of IAU 308 Conference, Tallinn, june 2014