The effect of non-equilibrium metal cooling on the interstellar medium

TL;DR

This study uses advanced galaxy simulations with non-equilibrium metal cooling to explore how chemical and physical parameters influence galaxy evolution, revealing significant effects on gas thermodynamics and molecular content.

Contribution

It introduces a novel self-consistent approach combining GASOLINE2 and KROME, including non-equilibrium metal cooling and metal injection, to improve galaxy evolution modeling.

Findings

Non-equilibrium metal cooling significantly affects gas temperature and molecular content.

Higher initial metallicity leads to colder gas and more molecular hydrogen.

Simulations match observed star formation and metal emission line relations.

Abstract

By using a novel interface between the modern smoothed particle hydrodynamics code GASOLINE2 and the chemistry package KROME, we follow the hydrodynamical and chemical evolution of an isolated galaxy. In order to assess the relevance of different physical parameters and prescriptions, we constructed a suite of ten simulations, in which we vary the chemical network (primordial and metal species), how metal cooling is modelled (non-equilibrium versus equilibrium; optically thin versus thick approximation), the initial gas metallicity (from ten to hundred per cent solar), and how molecular hydrogen forms on dust. This is the first work in which metal injection from supernovae, turbulent metal diffusion, and a metal network with non-equilibrium metal cooling are self-consistently included in a galaxy simulation. We find that properly modelling the chemical evolution of several metal species and the corresponding non-equilibrium metal cooling has important effects on the thermodynamics of the gas, the chemical abundances, and the appearance of the galaxy: the gas is typically warmer, has a larger molecular gas mass fraction, and has a smoother disc. We also conclude that, at relatively high metallicity, the choice of molecular-hydrogen formation rates on dust is not crucial. Moreover, we confirm that a higher initial metallicity produces a colder gas and a larger fraction of molecular gas, with the low-metallicity simulation best matching the observed molecular Kennicutt-Schmidt relation. Finally, our simulations agree quite well with observations which link star formation rate to metal emission lines.