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SUMMARY:VLA 3 GHz Radio Continuum Mapping of Nearby PHANGS Galaxies: Traci
 ng the Life Cycle of Star Formation
DTSTART;VALUE=DATE-TIME:20261028T174500Z
DTEND;VALUE=DATE-TIME:20261028T175500Z
DTSTAMP;VALUE=DATE-TIME:20261025T223016Z
UID:indico-contribution-3634@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Hamid Hassani (University of Alberta)\nMassive stars
  strongly reshape their surroundings through radiation\, stellar winds\, a
 nd eventually supernova explosions\, but when these different feedback mec
 hanisms begin to dominate remains uncertain. We present VLA 3 GHz radio co
 ntinuum observations of 13 nearby PHANGS galaxies to trace the evolution o
 f star-forming regions during their first ~10 Myr. Combining these data wi
 th HST\, JWST\, VLT/MUSE\, and AstroSat observations\, we separate the rad
 io emission into thermal free–free and non-thermal synchrotron component
 s and connect their evolution to stellar age and other tracers of recent s
 tar formation. The radio observations also reveal a small population of 36
  embedded\, PAH- and dust-continuum-bright but optically faint star-formin
 g regions\, representing less than 10% of the radio sources and demonstrat
 ing the ability of radio emission to probe the earliest obscured phases of
  star formation. We find a clear evolution in radio properties with stella
 r age: from 1–3 to 6–10 Myr\, the median thermal fraction decreases fr
 om ~61% to ~33%\, while the median radio spectral index steepens from −0
 .05 to −0.51. The youngest regions already exhibit a non-thermal fractio
 n of ~28% before the expected onset of core-collapse supernovae\, suggesti
 ng that massive-star winds and associated shocks may contribute to early c
 osmic-ray acceleration. These results provide a resolved view of how radio
  emission evolves from the embedded phase through the emergence of synchro
 tron emission during the first ~10 Myr of stellar feedback.\n\nhttps://nyx
 .physics.mcgill.ca/event/587/contributions/3634/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3634/
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