The W3 molecular cloud

Details The W3 molecular cloud The W3 molecular cloud

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297..662t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 15, 1985, p. 662-676. Research supported by the University of Ari

Astronomy and Astrophysics

Astrophysics

49

Astronomical Photometry, Molecular Clouds, Pre-Main Sequence Stars, Stellar Evolution, Absorption Spectra, Carbon, Interstellar Gas, Interstellar Matter, Line Spectra, Oxygen

Scientific paper

Extensive J = 1→0 12C16O and 13C16O observations of the W3 molecular cloud are presented and discussed. Four luminous star-forming regions, W3A, W3(OH), W3 North, and AFGL 333 are investigated. The molecular gas velocities are best explained as the result of material being swept up via the expansion of the neighboring giant W4 H II region. The analysis of the motions within the W3A and W3(OH) clouds shows that, as predicted by the theory of externally induced star formation, the young embedded stars are moving with the swept-up material, not with the undisturbed gas. The mass structure of the core of the W3 cloud is discussed in detail.

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