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Sequential star formation in the Sh 254-258 molecular cloud: HHT maps of CO J=3-2 and 2-1 emission

Published online by Cambridge University Press:  01 August 2006

J. H. Bieging ,
W. L. Peters ,
B. Vila Vilaro ,
K. Schlottman  and
C. Kulesa
J. H. Bieging
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA email: jbieging@as.arizona.edu
W. L. Peters
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA email: jbieging@as.arizona.edu
B. Vila Vilaro
Affiliation:
National Astronomical Observatory of Japan, Tokyo
K. Schlottman
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA email: jbieging@as.arizona.edu
C. Kulesa
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA email: jbieging@as.arizona.edu
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Abstract

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The molecular cloud associated with the Sh 254-258 group of 5 small H II regions appears to be forming a (late)-OB association. We have mapped the associated molecular cloud in the J=2-1 line of the CO molecule over 0.75o × 1o, and the CO J=3-2 line toward the 2 main peaks, with the University of Arizona Heinrich Hertz Submm Telescope (HHT). We propose a scenario for sequential formation of the stars exciting the H II regions, triggered by the compression/heating of the molecular gas.

Keywords

ISM: cloudsISM: moleculessubmillimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 396
Copyright
Copyright © International Astronomical Union 2007