VERTICO IX: Signatures of environmental processing of the gas in Virgo cluster spiral galaxies through mapping of CO isotopologues

TL;DR

This study investigates how environmental effects in the Virgo cluster influence the molecular gas properties of spiral galaxies by mapping CO isotopologues, revealing changes in optical depth, abundances, and gas transparency related to galaxy interactions.

Contribution

It provides the first large-sample analysis of CO isotopologue emission in Virgo cluster spirals, linking environmental processing to variations in molecular gas conditions and abundances.

Findings

CO/13CO line ratio varies with galaxy properties

13CO/C18O ratios show significant radial and intergalactic variation

Molecular gas becomes more transparent as it is stripped from galaxies

Abstract

In this work we study CO isotopologue emission in the largest cluster galaxy sample to date: 48 VERTICO spiral galaxies in Virgo. We show for the first time in a significant sample that the physical conditions within the molecular gas appear to change as a galaxy's ISM is affected by environmental processes. 13CO is detected across the sample, both directly and via stacking, while C18O is detected in a smaller number of systems. We use these data to study trends with global and radial galaxy properties. We show that the CO/13CO line ratio changes systematically with a variety of galaxy properties, including mean gas surface density, HI-deficiency and galaxy morphology. 13CO/C18O line ratios vary significantly, both radially and between galaxies, suggesting real variations in abundances are present. Such abundance changes may be due to star formation history differences, or speculatively even stellar initial mass function variations. We present a model where the optical depth of the molecular gas appears to change as a galaxy's ISM is affected by environmental processes. The molecular gas appears to become more transparent as the molecular medium is stripped, and then more opaque as the tightly bound remnant gas settles deep in the galaxy core. This explains the variations we see, and also helps explain similar observations in cluster early-type galaxies. Next generation simulations and dedicated observations of additional isotopologues could thus provide a powerful tool to help us understand the impact of environment on the ISM, and thus the quenching of galaxies.