http://arxiv.org/abs/2212.12187
${\rm H}2$ detections are usually biased towards star-forming galaxies, whose low number statistics in clusters has led to contradictory results in the literature regarding the impact of environment on their ${\rm H}_2$ content, across redshifts. In this work, we employ the EAGLE simulation to investigate the relationship between the ${\rm H}_2$ content of star-forming galaxies and their environment for redshifts spanning $0\leq z\leq 1$. To do so, we divide the sample into those that are bound to clusters and those that are not. We find that, at any given redshift, the galaxies in clusters generally have lower ${\rm H}_2$content than their non-cluster counterparts with the same stellar mass (corresponding to an offset of $\lesssim 0.5$ dex), but this offset is virtually absent at $M\star\lesssim10^{9.3}~{\rm M}_\odot$. Tracking the galaxies back in time reveals that the deficit of ${\rm H}_2$ in cluster galaxies relative to non-cluster galaxies is not due to intrinsic differences in their stellar or active galactic nuclei feedback, but rather a result of a sharp drop in the ${\rm H}_2$ content of cluster galaxies after infall into their host halo; the longer the time since infall, the greater the deficit. Based on the histories of particles associated with our galaxies, the drop is attributed to lack of replenishment, depletion due to star formation, and gas escaping the galaxies in cluster environments. These results provide support and theoretical insights for existing molecular gas observations that show a deficit of ${\rm H}_2$ content for cluster galaxies, and provide predictions for future surveys.
A. Manuwal and A. Stevens
Mon, 26 Dec 22
22/39
Comments: Submitted to MNRAS
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