A MUSE-ALMA view of the physics of star formation and feedback at high angular resolution in nearby galaxies

Using a revolutionary combination of high spatial resolution MUSE and ALMA data we examine, in unprecedented detail, how stars are formed in different galaxy environments using a statistical sample. The PHANGs collaboration has mosaicked across the disks of 19 nearby galaxies (distance <25Mpc) at high angular resolution (1"=50pc). By combining this matched resolution MUSE and ALMA data, we trace the relative distribution and evolution of the gas properties of these galaxies across multiple phases. This allows us to spatially map thousands of resolved molecular clouds and HII regions across the disks of galaxies. I will use this to show how star formation fuelling is connected to specific galactic environments, and address the energetics of star formation feedback. Additionally, we derive the ionisation properties of the circumnuclear gas in galaxies within our sample that host low-luminosity AGN or LINER-like centres. This allows us to show that they preferentially have extended ionised gas surrounding their nuclei as compared to quiescent galaxies. By connecting these ionised gas properties to those of the molecular gas we show evidence of outflowing gas implying that even low-level activity in their centres can drive feedback on large scales.