High resolution J = 2 - 1 and J = 1 - 0 carbon monoxide self-reversed line profiles toward molecular clouds

Details High resolution J = 2 - 1 and J = 1 - 0 carbon monoxide self-reversed line profiles toward molecular clouds High resolution J = 2 - 1 and J = 1 - 0 carbon monoxide self-reversed line profiles toward molecular clouds

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...245..495l&link_type=abstract

Astrophysical Journal, Part 1, vol. 245, Apr. 15, 1981, p. 495-511.

Astronomy and Astrophysics

Astrophysics

61

Astronomical Spectroscopy, Carbon Monoxide, High Resolution, Interstellar Gas, Molecular Clouds, Carbon 12, Carbon 13, Line Spectra, Optical Thickness, Spectral Line Width

Scientific paper

High resolution spectra of the J =2-1 and J=1-0 transitions of 12CO and 13CO have been obtained toward eight molecular clouds which have self-reversed 12CO line profiles. Accurate comparison of these two transitions is used to infer some of the physical conditions in the cloud cores and the absorbing envelopes.
The 2-1 12CO line profiles typically have deeper self-reversals but stronger line wings than the corresponding 1-0 line profiles. The CO excitation temperature of the absorbing layer is typically 10 to 18 K and no more than ∼5 K for AFGL 961. The velocity dispersion of the absorbing layer is 1.5-3.0 km s-1, about half that of the hotter cloud core. For five clouds, the velocity of this layer indicates collapse of the cloud envelope on a time scale ∼106 years.
The enhancement of the 2-1 line wings compared to the 1-0 line wings indicates that this emission arises in a region with a kinetic temperature TK ≲ TPK (CO) and that the line does not become optically thin except in the extreme line wings. A greater enhancement of the low-velocity 2-1 wing indicates that a systematic collapse occurs near the cores of W3, Mon R2, ρ Oph, and Cep A.

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