The core of the W3 molecular cloud

Details The core of the W3 molecular cloud The core of the W3 molecular cloud

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...306..160t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 306, July 1, 1986, p. 160-165.

Astronomy and Astrophysics

Astrophysics

11

Density Distribution, Mass Distribution, Molecular Clouds, Star Formation, Stellar Evolution, Carbon Monoxide, Emission Spectra, Nebulae, Stellar Luminosity, Stellar Mass, Temperature Distribution, Velocity Distribution

Scientific paper

The center of the W3 molecular cloud was studied by using emission from the J = 2 - 1 transition of (C-12)(O-16) and (C-12)(O-18). In agreement with some earlier results, it is found that the velocity gradients, with the exception of small-scale high-velocity outflow, are quite modest. One part of the star-forming core appears to be moving independently of most of the source. Using emission from (C-12)(O-18) to estimate the mass distribution, it is found that the core of the W3 cloud is dominated by an east-west ridge of high column density. A core mass of 5000 solar masses is estimated, which compares with a stellar mass of about 3000 solar masses. The most luminous exciting stars are localized by mapping the (C-12)(O-16) excitation temperature. A simple formula is derived for estimating volume densities by using the observed dust temperature variation.

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