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

John H Bieging, W. L. Peters, B. Vila Vilaro, K. Schlottman, C. Kulesa

Research output: Contribution to journalArticle

Abstract

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 0.75 o 1 o, 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.

Original languageEnglish (US)
Pages (from-to)396
Number of pages1
JournalProceedings of the International Astronomical Union
Volume2
Issue numberS237
DOIs
StatePublished - Aug 2006

Fingerprint

H II regions
molecular clouds
Telescopes
Stars
star formation
Compaction
telescopes
Heating
Molecules
molecular gases
Gases
compression
heating
stars
gas
molecules

Keywords

  • ISM: clouds
  • ISM: molecules
  • Submillimeter

ASJC Scopus subject areas

  • Physics and Astronomy (miscellaneous)
  • Aerospace Engineering

Cite this

Sequential star formation in the Sh 254-258 molecular cloud : HHT maps of CO J=3-2 and 2-1 emission. / Bieging, John H; Peters, W. L.; Vilaro, B. Vila; Schlottman, K.; Kulesa, C.

In: Proceedings of the International Astronomical Union, Vol. 2, No. S237, 08.2006, p. 396.

Research output: Contribution to journalArticle

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