The Role of Galaxy Environment in Pressure-Regulated Star Formation and Gas Content in Galaxies

Pressure-regulated feedback-modulated (PRFM) models predict that star formation in galaxies is governed by the balance between interstellar medium (ISM) pressure and the energy output of massive stars. While multiple surveys have empirically confirmed the predictions of PRFM models at kiloparsec (kpc) scales, the influence of large-scale environment on these models remains uncertain. I will present new evidence demonstrating that environment plays a key role in the ISM pressure balance and star formation regulation of galaxies, based on 1.2 kpc-resolution gas and stellar data. Specifically, I compare the spatially resolved relationships between molecular-to-atomic gas ratios, star formation rates, and molecular gas depletion times as a function of dynamical equilibrium pressure in both field and cluster galaxies. My study focuses on galaxies in the Virgo Cluster, using data from the VERTICO (H_2) and VIVA (HI) surveys, and compares them to field galaxies from the HERACLES (H_2) and THINGS (HI) surveys. I find that at a given dynamical equilibrium pressure, cluster galaxies exhibit higher molecular-to-atomic gas ratios than field galaxies. Additionally, using atomic gas deficiency as a proxy for cluster-specific environmental processes, I will show how these mechanisms significantly reshape the relationships between gas content, star formation, and ISM pressure in these galaxies.