Beyond halo mass: quenching galaxy mass assembly at the edge of filaments. (arXiv:2009.00013v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Song_H/0/1/0/all/0/1">Hyunmi Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laigle_C/0/1/0/all/0/1">Clotilde Laigle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hwang_H/0/1/0/all/0/1">Ho Seong Hwang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devriendt_J/0/1/0/all/0/1">Julien Devriendt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubois_Y/0/1/0/all/0/1">Yohan Dubois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraljic_K/0/1/0/all/0/1">Katarina Kraljic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pichon_C/0/1/0/all/0/1">Christophe Pichon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slyz_A/0/1/0/all/0/1">Adrianne Slyz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Rory Smith</a>
We examine how the mass assembly of central galaxies depends on their
location in the cosmic web. The HORIZON-AGN simulation is analysed at z~2 using
the DISPERSE code to extract multi-scale cosmic filaments. We find that the
dependency of galaxy properties on large-scale environment is mostly inherited
from the (large-scale) environmental dependency of their host halo mass. When
adopting a residual analysis that removes the host halo mass effect, we detect
a direct and non-negligible influence of cosmic filaments. Proximity to
filaments enhances the build-up of stellar mass, a result in agreement with
previous studies. However, our multi-scale analysis also reveals that, at the
edge of filaments, star formation is suppressed. In addition, we find clues for
compaction of the stellar distribution at close proximity to filaments. We
suggest that gas transfer from the outside to the inside of the haloes (where
galaxies reside) becomes less efficient closer to filaments, due to high
angular momentum supply at the vorticity-rich edge of filaments. This quenching
mechanism may partly explain the larger fraction of passive galaxies in
filaments, as inferred from observations at lower redshifts.
We examine how the mass assembly of central galaxies depends on their
location in the cosmic web. The HORIZON-AGN simulation is analysed at z~2 using
the DISPERSE code to extract multi-scale cosmic filaments. We find that the
dependency of galaxy properties on large-scale environment is mostly inherited
from the (large-scale) environmental dependency of their host halo mass. When
adopting a residual analysis that removes the host halo mass effect, we detect
a direct and non-negligible influence of cosmic filaments. Proximity to
filaments enhances the build-up of stellar mass, a result in agreement with
previous studies. However, our multi-scale analysis also reveals that, at the
edge of filaments, star formation is suppressed. In addition, we find clues for
compaction of the stellar distribution at close proximity to filaments. We
suggest that gas transfer from the outside to the inside of the haloes (where
galaxies reside) becomes less efficient closer to filaments, due to high
angular momentum supply at the vorticity-rich edge of filaments. This quenching
mechanism may partly explain the larger fraction of passive galaxies in
filaments, as inferred from observations at lower redshifts.
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