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The Cold Interstellar Medium of Galaxies in the Local Universe
- Amélie Saintonge1, and Barbara Catinella2,3
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View Affiliations Hide AffiliationsAffiliations: 1Department of Physics and Astronomy, University College London, London, United Kingdom; email: [email protected] 2International Centre for Radio Astronomy Research, The University of Western Australia, Crawley, Western Australia, Australia 3ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australian Capital Territory, Australia
- Vol. 60:319-361 (Volume publication date September 2022) https://doi.org/10.1146/annurev-astro-021022-043545
- First published as a Review in Advance on June 01, 2022
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Copyright © 2022 by Annual Reviews. All rights reserved
Abstract
The cold interstellar medium (ISM) plays a central role in the galaxy evolution process. It is the reservoir that fuels galaxy growth via star formation, the repository of material formed by these stars, and a sensitive tracer of internal and external processes that affect entire galaxies. Consequently, significant efforts have gone into systematic surveys of the cold ISM of the galaxies in the local Universe. This review discusses the resulting network of scaling relations connecting the atomic and molecular gas masses of galaxies with their other global properties (stellar masses, morphologies, metallicities, star-formation activity…) and their implications for our understanding of galaxy evolution. Key take-home messages are as follows:
- ▪ From a gas perspective, there are three main factors that determine the star-formation rate of a galaxy: the total mass of its cold ISM, how much of that gas is molecular, and the rate at which any molecular gas is converted into stars. All three of these factors vary systematically across the local galaxy population.
- ▪ The shape and scatter of both the star-formation main sequence and the mass–metallicity relation are deeply linked to the availability of atomic and molecular gas.
- ▪ Future progress will come from expanding our exploration of scaling relations into new parameter space (in particular, the regime of dwarf galaxies), better connecting the cold ISM of large samples of galaxies with the environment that feeds them (the circumgalactic medium, in particular), and understanding the impact of these large scales on the efficiency of the star-formation process on molecular cloud scales.
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