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CO, HI, recent Spitzer SAGE results in the Large Magellanic Cloud

Published online by Cambridge University Press:  01 August 2006

Yasuo Fukui
Yasuo Fukui*
Affiliation:
Department of Physics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan email: fukui@a.phys.nagoya-u.ac.jp
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Abstract

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Formation of GMCs is one of the most crucial issues in galaxy evolution. I will compare CO and HI in the LMC in 3 dimensional space for the first time aiming at revealing the physical connection between GMCs and associated HI gas at a ~40 pc scale. The present major findings are 1) [total CO intensity] ∝ [total HI intensity]0.8 for the 110 GMCs, and 2) the HI intensity tends to increase with the evolution of GMCs. I argue that these findings are consistent with the growth of GMCs via HI accretion over a time scale of a few × 10 Myrs. I will also discuss the role of the background stellar gravity and the dynamical compression by supershells in formation of GMCs.

Keywords

stars: formationISM: atomsevolutionmoleculesMagellanic Cloudsgalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 31 - 39
Copyright
Copyright © International Astronomical Union 2007

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