Observational predictions for the survival of atomic hydrogen in simulated Fornax-like galaxy clusters

TL;DR

This study uses high-resolution cosmological simulations to predict the distribution and survival of neutral hydrogen in galaxy clusters similar to Fornax, providing insights into cold gas persistence in hot cluster environments.

Contribution

It offers the first detailed predictions of HI distribution in Fornax-like clusters using TNG50 simulations, aligning with upcoming MeerKAT observations.

Findings

Fornax-like halos have an extended HI distribution detectable by MeerKAT.

Approximately 12% of the area within the virial radius contains HI at certain sensitivities.

Most HI outside galaxies is associated with satellite galaxies.

Abstract

The presence of dense, neutral hydrogen clouds in the hot, diffuse intra-group and intra-cluster medium is an important clue to the physical processes controlling the survival of cold gas and sheds light on cosmological baryon flows in massive halos. Advances in numerical modeling and observational surveys means that theory and observational comparisons are now possible. In this paper, we use the high-resolution TNG50 cosmological simulation to study the HI distribution in seven halos with masses similar to the Fornax galaxy cluster. Adopting observational sensitivities similar to the MeerKAT Fornax Survey (MFS), an ongoing HI survey that will probe to column densities of $10^{18}$ cm$^{-2}$, we find that Fornax-like TNG50 halos have an extended distribution of neutral hydrogen clouds. Within one virial radius, we predict the MFS will observe a total HI covering fraction around $\sim$ 12\% (mean value) for 10 kpc pixels and 6\% for 2 kpc pixels. If we restrict this to gas more than 10 half-mass radii from galaxies, the mean values only decrease mildly, to 10\% (4\%) for 10 (2) kpc pixels (albeit with significant halo-to-halo spread). Although there are large amounts of HI outside of galaxies, the gas seems to be associated with satellites, judging both by the visual inspection of projections and by comparison of the line of sight velocities of galaxies and intracluster HI.