HI and H$_2$ gas evolution over cosmic times: ColdSIM

TL;DR

This paper uses advanced numerical simulations to study the evolution of cold cosmic gas, successfully reproducing observational data for HI and H$_2$, and highlighting the importance of non-equilibrium H$_2$ in understanding galaxy formation.

Contribution

It introduces a comprehensive non-equilibrium simulation framework for cold cosmic gas evolution, including detailed chemistry and feedback processes, aligning well with recent observations.

Findings

Neutral gas density increases with redshift.

H$_2$ fractions can reach 50% at high redshift.

H$_2$ depletion times are below the Hubble time.

Abstract

We present first results of the evolution of cold cosmic gas obtained through a set of state-of-the-art numerical simulations (ColdSIM). We model time-dependent atomic and molecular non-equilibrium chemistry coupled to HI and H$_2$ self-shielding, various UV backgrounds as suggested by the recent literature, H$_2$ dust grain catalysis, photoelectric heating, cosmic-ray heating, as well as hydrodynamics, star formation and feedback effects. By means of such non-equilibrium calculations we are finally able to reproduce the latest HI and H$_2$ observational data. The neutral-gas mass density parameter results around $\Omega_{\rm neutral} \!\sim\! 10^{-3}$ and increases from lower to higher redshift ($z$). The molecular-gas mass density parameter shows peak values of $ \Omega_{\rm H_2} \! \sim \! 10^{-4}$, while expected H$_2$ fractions can be as high as 50% of the cold gas mass at $ z\!\sim$4-8, in line with the latest high-$z$ measurements. Both observed HI and H$_2$ trends are well reproduced by our non-equilibrium H$_2$-based star formation modelling. H$_2$ depletion times remain below the Hubble time and comparable to the dynamical time at all epochs. These findings suggest that, besides HI, non-equilibrium H$_2$ analyses are key probes for assessing the cold gas and the role of UV background radiation. Abridged.