(C-13)O observations of cool giant molecular clouds

Details (C-13)O observations of cool giant molecular clouds (C-13)O observations of cool giant molecular clouds

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...152..371p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 152, no. 2, Nov. 1985, p. 371-386.

Astronomy and Astrophysics

Astrophysics

71

Carbon Monoxide, Galactic Structure, Interstellar Matter, Molecular Clouds, Stellar Evolution, Astronomical Maps, Far Infrared Radiation, Gas Density, Line Of Sight, Milky Way Galaxy

Scientific paper

Extensive (C-13)O (J = 1-0) mapping of nearby molecular complexes selected, from their far infrared and radio continuum properties, as complexes forming stars, but not very massive stars (less than 15 solar masses), reveals a highly fragmented and dispersed structure. The bulk of the (C-13)O emission comes from condensations about 1 to 3 pc in size, the mass of which (a few hundred solar masses) lies in a subthermally excited turbulent envelope. The condensations, grouped at the 10 pc scale in larger structures, which often appear elongated, have a surface filling factor around unity, corresponding to a low volume filling factor inside the complexes. Within two condensations, where they have been looked for, one or several cores of size 0.2 pc or less, and mass a few solar masses, have been detected in high resolution (C-18)O maps. Radiative transfer calculations with a 1 pc centrally condensed structure proposed by Falgarone and Puget (1985) reproduces rather well the observations in various CO isotopes, with a low number of a priori assumptions.

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