The dust-to-stellar mass ratio as a valuable tool to probe the evolution of local and distant star forming galaxies

TL;DR

This paper investigates how the dust-to-stellar mass ratio evolves in star-forming galaxies across different redshifts, using observational data and chemical evolution models to understand dust survival and galaxy evolution.

Contribution

It introduces a comprehensive analysis of the dust-to-stellar mass ratio's evolution with redshift, combining data and models to interpret dust survival in different galaxy types.

Findings

Spiral galaxies maintain a nearly constant DTS over time.

Proto-spheroid starburst galaxies show an early steep increase in DTS.

DTS decreases at higher redshifts, indicating less dust survival in early universe galaxies.

Abstract

The survival of dust grains in galaxies depends on various processes. Dust can be produced in stars, it can grow in the interstellar medium and be destroyed by astration and interstellar shocks. In this paper, we assemble a few data samples of local and distant star-forming galaxies to analyse various dust-related quantities in low and high redshift galaxies, to study how the relations linking the dust mass to the stellar mass and star formation rate evolve with redshift. We interpret the available data by means of chemical evolution models for discs and proto-spheroid (PSPH) starburst galaxies. In particular, we focus on the dust-to-stellar mass (DTS) ratio, as this quantity represents a true measure of how much dust per unit stellar mass survives the various destruction processes in galaxies and is observable. The theoretical models outline the strong dependence of this quantity on the underlying star formation history. Spiral galaxies are characterised by a nearly constant DTS as a function of the stellar mass and cosmic time, whereas PSPHs present an early steep increase of the DTS, which stops at a maximal value and decreases in the latest stages. In their late starburst phase, these models show a decrease of the DTS with their mass, which allows us to explain the observed anti-correlation between the DTS and the stellar mass. The observed redshift evolution of the DTS ratio shows an increase from z~0 to z~1, followed by a roughly constant behaviour at 1<z<2.5. Our models indicate a steep decrease of the global DTS at early times, which implies an expected decrease of the DTS at larger redshift.