The W3 molecular cloud

Extensive J = 1 to 0 (C-12)(O-16) and (C-13)(O-16) observations of the W3 molecular cloud and the surrounding region are presented and discussed. The velocity structure in the region is strongly suggestive of a model of large-scale, externally induced star formation. It is shown that star formation...

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Published inThe Astrophysical journal Vol. 297; no. 2; pp. 662 - 676
Main Authors Thronson, H. A., Jr, Lada, C. J., Hewagama, T.
Format Journal Article
LanguageEnglish
Published Legacy CDMS University of Chicago Press 01.10.1985
Subjects
Astronomy
Astrophysics
Earth, ocean, space
Exact sciences and technology
Interstellar medium (ism) and nebulae in milky way
Molecular clouds, h2 clouds, dense clouds, and dark clouds
Stellar systems. Galactic and extragalactic objects and systems. The universe
Carbon monoxide
Structure
Molecular cloud
Stellar formation region
Interstellar molecule
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Summary:Extensive J = 1 to 0 (C-12)(O-16) and (C-13)(O-16) observations of the W3 molecular cloud and the surrounding region are presented and discussed. The velocity structure in the region is strongly suggestive of a model of large-scale, externally induced star formation. It is shown that star formation occurred in W3 and the nearby star-forming region W3(OH) after the gas within which they lie was swept up by the expanding W4 ionization front. Two condensations dominate the mass structure of the core of W3, one associated with IRS 4 and the other with IRS 5 and 1. A velocity difference between the two condensations is interpreted as indicating the two sources actually are discrete knots.
Bibliography:CDMS
Legacy CDMS
ISSN:0004-637X
1538-4357
DOI:10.1086/163565