New composition dependent cooling and heating curves for galaxy evolution simulations

TL;DR

This paper introduces a new set of composition-dependent cooling and heating curves for low-density gas, optimized for galaxy evolution simulations, accounting for key elements, ionization processes, and self-shielding effects.

Contribution

It provides a comprehensive, easily interpolated table of cooling/heating curves based on five parameters, improving simulation accuracy for galaxy formation models.

Findings

Accurate ionization equilibrium for 14 key elements across wide temperature and density ranges.

Inclusion of self-shielding effects enhances modeling of cold, dense gas clouds.

Curves are computationally efficient for use in large-scale simulations.

Abstract

In this paper, we present a new calculation of composition-dependent radiative cooling and heating curves of low-density gas, intended primarily for use in numerical simulations of galaxy formation and evolution. These curves depend on only five parameters: temperature, density, redshift, [Fe/H], and [Mg/Fe]. They are easily tabulated and can be efficiently interpolated during a simulation. The ionization equilibrium of 14 key elements is determined for temperatures between 10K and 10^9K and densities up to 100 amu/cm^3 taking into account collisional and radiative ionization, by the cosmic UV background and an interstellar radiation field, and by charge-transfer reactions. These elements, ranging from H to Ni, are the ones most abundantly produced and/or released by SNIa, SNII, and intermediate-mass stars. Self-shielding of the gas at high densities by neutral Hydrogen is taken into account in an approximate way by exponentially suppressing the H-ionizing part of the cosmic UV background for HI densities above a threshold density of n_HI,crit=0.007 cm^-3. We discuss how the ionization equilibrium, and the cooling and heating curves depend on the physical properties of the gas. The main advantage of the work presented here is that, within the confines of a well-defined chemical evolution model and adopting the ionization equilibrium approximation, it provides accurate cooling and heating curves for a wide range of physical and chemical gas properties, including the effects of self-shielding. The latter is key to resolving the formation of cold, neutral, high-density clouds suitable for star formation in galaxy simulations.