On the origin of gas-poor galaxies in galaxy clusters using cosmological hydrodynamic simulations

TL;DR

This study uses cosmological hydrodynamic simulations to identify three main mechanisms of gas depletion in cluster galaxies, highlighting the roles of pre-processing, fast, and slow cluster processing, with their importance varying by cluster mass.

Contribution

It categorizes the mechanisms of gas depletion into three channels and quantifies their relative importance using simulations, emphasizing the role of pre-processing and orbital dynamics.

Findings

34% of galaxies are gas poor before cluster entry due to pre-processing.

43% of galaxies become gas deficient rapidly within clusters.

24% of galaxies retain gas after first pericentric pass, especially in less massive clusters.

Abstract

The environmental effect is commonly used to explain the excess of gas-poor galaxies in galaxy clusters. Meanwhile, the presence of gas-poor galaxies at cluster outskirts, where galaxies have not spent enough time to feel the cluster environmental effect, hints for the presence of pre-processing. Using cosmological hydrodynamic simulations on 16 clusters, we investigate the mechanisms of gas depletion of galaxies found inside clusters. The gas depletion mechanisms can be categorized into three channels based on where and when they took place. First, 34$\%$ of our galaxies are gas poor before entering clusters (`pre-processing'). They are mainly satellites that have undergone the environmental effect inside group halos. Second, 43$\%$ of the sample became quickly gas deficient in clusters before the first pericentric pass (`fast cluster processing'). Some of them were group satellites that are low in gas at the time of cluster entry compared to the galaxies directly coming from the field. Even the galaxies with large gas fractions take this channel if they fall into massive clusters ($> 10^{14.5}\, \rm M_{\odot}$) or approach cluster centers through radial orbits. Third, 24$\%$ of our sample retain gas even after their first pericentric pass (`slow cluster processing') as they fall into the less massive clusters and/or have circular orbits. The relative importance of each channel varies with a cluster's mass, while the exact degree of significance is subject to large uncertainties. Group pre-processing accounts for a third of the total gas depletion; but it also determines the gas fraction of galaxies at their cluster entry which in turn determines whether a galaxy should take the fast or the slow cluster processing.