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Star formation in galaxies is regulated by turbulence, outflows, gas heatingand cloud dispersal -- processes which depend sensitively on the properties ofthe interstellar medium (ISM) into which supernovae (SNe) explode.Unfortunately, direct measurements of ISM environments around SNe remainscarce, as SNe are rare and often distant. Here we demonstrate a new approach:mapping the ISM around the massive stars that are soon to explode. Thisprovides a much larger census of explosion sites than possible with only SNe,and allows comparison with sensitive, high-resolution maps of the atomic andmolecular gas from the Jansky VLA and ALMA. In the well-resolved Local Groupspiral M33, we specifically observe the environments of red supergiants (RSGs,progenitors of Type II SNe), Wolf-Rayet stars (WRs, tracing stars $>$30M$_{\odot}$, and possibly future stripped-envelope SNe), and supernova remnants(SNRs, locations where SNe have exploded). We find that massive stars evolvenot only in dense, molecular-dominated gas (with younger stars in denser gas),but also a substantial fraction ($\sim$45\% of WRs; higher for RSGs) evolve inlower-density, atomic-gas-dominated, inter-cloud media. We show that thesemeasurements are consistent with expectations from different stellar-age tracermaps, and can be useful for validating SN feedback models in numericalsimulations of galaxies. Along with the discovery of a 20-pc diameter moleculargas cavity around a WR, these findings re-emphasize the importance ofpre-SN/correlated-SN feedback evacuating the dense gas around massive starsbefore explosion, and the need for high-resolution (down to pc-scale) surveysof the multi-phase ISM in nearby galaxies.

Where do stars explode in the ISM? -- The distribution of dense gas around massive stars and supernova remnants in M33