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One of the fundamental factors regulating the evolution of galaxies isstellar feedback. However, we still do not have strong observationalconstraints on the relative importance of the different feedback mechanisms(e.g. radiation, ionised gas pressure, stellar winds) in driving HII regionevolution and molecular cloud disruption. In this letter, we constrain therelative importance of the various feedback mechanisms from young massive starpopulations by resolving HII regions across the disk of the nearby star-forminggalaxy NGC 1672. We combine measurements of ionised gas nebular lines obtainedby PHANGS-MUSE, with high-resolution imaging from the HST in both thenarrow-band H{\alpha} and broad-band filters. We identify a sample of 40isolated, compact HII regions in the HST H{\alpha} image, for which we measurethe sizes that were previously unresolved in seeing-limited ground-basedobservations. Additionally, we identify the ionisation source(s) for each HIIregion from catalogues produced as part of the PHANGS-HST survey. We find thatthe HII regions investigated are mildly dominated by thermal or wind pressure,yet their elevation above the radiation pressure is within the expecteduncertainty range. We see that radiation pressure provides a substantiallyhigher contribution to the total pressure than previously found in theliterature over similar size scales. In general, we find higher pressureswithin more compact HII regions, which is driven by the inherent size scalingrelations of each pressure term, albeit with significant scatter introduced bythe variation in the stellar population properties (e.g. luminosity, mass, age,metallicity). For nearby galaxies, here we provide a promising approach thatcould yield the statistics required to map out how the importance of differentstellar feedback mechanisms evolve over the lifetime of an HII region.

Linking stellar populations to HII regions across nearby galaxies: I. Constraining pre-supernova feedback from young clusters in NGC1672