# The fate of the gaseous disks of galaxies that fall into clusters

## TL;DR

This study uses simulations to examine how galaxy gas content is affected by cluster environment, showing that cool-core clusters can strip all gas from infalling galaxies, while non-cool-core clusters do not.

## Contribution

It provides new insights into the gas loss mechanisms of galaxies in clusters, highlighting the impact of cluster core properties on galaxy evolution.

## Key findings

- Galaxies lose all gas in cool-core clusters after a single crossing.
- Galaxies in non-cool-core clusters retain some gas after crossing.
- Star formation rate is temporarily enhanced during cluster crossing.

## Abstract

Galaxy clusters are known to induce gas loss in infalling galaxies due to the ram pressure exerted by the intracluster medium over their gas content. In this paper, we investigate this process through a set of simulations of Milky Way like galaxies falling inside idealised clusters of 10$^{14}$ M$_\odot$ and 10$^{15}$ M$_\odot$, containing a cool-core or not, using the adaptive mesh refinement code RAMSES. We use these simulations to constrain how much of the initial mass contained in the gaseous disk of the galaxy will be converted into stars and how much of it will be lost, after a single crossing of the entire cluster. We find that, if the galaxy reaches the central region of a cool-core cluster, it is expected to lose all its gas, independently of its entry conditions and of the cluster's mass. On the other hand, it is expected to never lose all its gas after crossing a cluster without a cool-core just once. Before reaching the centre of the cluster, the SFR of the galaxy is always enhanced, by a factor of 1.5 to 3. If the galaxy crosses the cluster without being completely stripped, its final amount of gas is on average two times smaller after crossing the 10$^{15}$ M$_\odot$ cluster, relative to the 10$^{14}$ M$_\odot$ cluster. This is reflected in the final SFR of the galaxy, which is also two times smaller in the former, ranging from 0.5 $-$ 1 M$_\odot$ yr$^{-1}$, compared to 1 $-$ 2 M$_\odot$ yr$^{-1}$ for the latter.