On the nature of variations in the measured star formation efficiency of molecular clouds

Michael Y. Grudic*, Philip F. Hopkins, Eve J. Lee, Norman Murray, Claude André Faucher-Giguère, L. Clifton Johnson

*Corresponding author for this work

Research output: Contribution to journalArticle

4 Scopus citations

Abstract

Measurements of the star formation efficiency (SFE) of giant molecular clouds (GMCs) in the Milky Way generally show a large scatter, which could be intrinsic or observational. We use magnetohydrodynamic simulations of GMCs (including feedback) to forward-model the relationship between the true GMC SFE and observational proxies. We show that individual GMCs trace broad ranges of observed SFE throughout collapse, star formation, and disruption. Low measured SFEs (${\ll} 1\hbox{ per cent}$) are 'real' but correspond to early stages; the true 'per-freefall' SFE where most stars actually form can be much larger. Very high (${\gg} 10\hbox{ per cent}$) values are often artificially enhanced by rapid gas dispersal. Simulations including stellar feedback reproduce observed GMC-scale SFEs, but simulations without feedback produce 20× larger SFEs. Radiative feedback dominates among mechanisms simulated. An anticorrelation of SFE with cloud mass is shown to be an observational artefact. We also explore individual dense 'clumps' within GMCs and show that (with feedback) their bulk properties agree well with observations. Predicted SFEs within the dense clumps are ∼2× larger than observed, possibly indicating physics other than feedback from massive (main-sequence) stars is needed to regulate their collapse.

Original languageEnglish (US)
Pages (from-to)1501-1518
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Volume488
Issue number2
DOIs
StatePublished - Jun 26 2019

Keywords

  • H II regions
  • ISM: clouds
  • galaxies: star formation
  • stars: formation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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