Subjects: Astronomy >> Astrophysical processes submitted time 2023-02-19
Jaeyeon Kim
Mélanie Chevance
J. M. Diederik Kruijssen
Adam K. Leroy
Andreas Schruba
Ashley T. Barnes
Frank Bigiel
Guillermo A. Blanc
Yixian Cao
Enrico Congiu
Daniel A. Dale
Christopher M. Faesi
Simon C. O. Glover
Kathryn Grasha
Brent Groves
Annie Hughes
Ralf S. Klessen
Kathryn Kreckel
Rebecca McElroy
Hsi-An Pan
Abstract： The processes of star formation and feedback, regulating the cycle of matter between gas and stars on the scales of giant molecular clouds (GMCs; $\sim$100pc), play a major role in governing galaxy evolution. Measuring the time-scales of GMC evolution is important to identify and characterise the specific physical mechanisms that drive this transition. By applying a robust statistical method to high-resolution CO and narrow-band H$\alpha$ imaging from the PHANGS survey, we systematically measure the evolutionary timeline from molecular clouds to exposed young stellar regions on GMC scales, across the discs of an unprecedented sample of 54 star-forming main-sequence galaxies (excluding their unresolved centres). We find that clouds live for about $1{-}3$ GMC turbulence crossing times ($5{-}30$Myr) and are efficiently dispersed by stellar feedback within $1{-}5$Myr once the star-forming region becomes partially exposed, resulting in integrated star formation efficiencies of $1{-}8$%. These ranges reflect physical galaxy-to-galaxy variation. In order to evaluate whether galactic environment influences GMC evolution, we correlate our measurements with average properties of the GMCs and their local galactic environment. We find several strong correlations that can be physically understood, revealing a quantitative link between galactic-scale environmental properties and the small-scale GMC evolution. Notably, the measured CO-visible cloud lifetimes become shorter with decreasing galaxy mass, mostly due to the increasing presence of CO-dark molecular gas in such environment. Our results represent a first step towards a comprehensive picture of cloud assembly and dispersal, which requires further extension and refinement with tracers of the atomic gas, dust, and deeply-embedded stars.
Peer Review Status:
Awaiting Review
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