Star Formation Around Supergiant Shells in the LMC

Abstract

We examine the recent star formation associated with four supergiant shells (SGSs) in the Large Magellanic Cloud (LMC): LMC 1, 4, 5, and 6, which have been shown to have simple expanding-shell structures. H II regions and OB associations are used to infer star formation in the last few Myr, while massive young stellar objects (YSOs) reveal the current ongoing star formation. Distributions of ionized, H I, and molecular components of the interstellar gas are compared with the sites of recent and current star formation to determine whether triggering has taken place. We find that a great majority of the current star formation has occurred in gravitationally unstable regions, and that evidence of triggered star formation is prevalent at both large and local scales.

12 pages, 4 figures, accepted for publication in the Astronomical Journal, improved image quality of figures

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• Supernova Remnants and Star Formation in the Large Magellanic Cloud
• Spitzer Observations of the HII Region NGC 2467: An Analysis of Triggered Star Formation
• The Supershell-Molecular Cloud Connection: Large-Scale Stellar Feedback and the Formation of the Molecular ISM
• Dense Molecular Clumps associated with the LMC Supergiant Shells LMC 4 \& LMC 5
• ASTE observations in the 345 GHz window towards the HII region N113 of the Large Magellanic Cloud
• Young Stellar Clusters with a Schuster Mass Distribution - I: Stationary Winds
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• Internal Structures of Molecular Clouds in the LMC Revealed by ALMA
• The VMC Survey - XXXII. Pre-main sequence populations in the Large Magellanic Cloud
• Pre-main Sequence stars in LH91
• Properties of star formation of the Large Magellanic Cloud as probed by young stellar objects