The Detection of [C i] in Molecular Outflows Associated with Young Stellar Objects

Details The Detection of [C i] in Molecular Outflows Associated with Young Stellar Objects The Detection of [C i] in Molecular Outflows Associated with Young Stellar Objects

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...415..672w&link_type=abstract

Astrophysical Journal v.415, p.672

Astronomy and Astrophysics

Astronomy

14

Ism: Abundances, Ism: Jets And Outflows, Ism: Molecules

Scientific paper

The first observations of atomic carbon in molecular outflows are presented. Most of the outflow regions show similar [C I] and 13CO line profiles suggesting the [C I] emission from outflow sources traces the same volume of gas as the CO emission, as previous studies have suggested for molecular clouds in general. The [C I] and CO column densities for the 11 sources surveyed are computed over wing and line center velocities. If the [C I] column densities derived from line center velocities are probing conditions in the ambient cloud in the vicinity of the infrared source, then a comparison of these values indicates the carbon abundance in the low-velocity component of the outflows is essentially the same as in the ambient cloud; there is no evidence for shock enhancement of [C 1] in the swept-up material.
A map of the [C I] emission from the central arcminute of the luminous DR 21 outflow is presented. The [C I] emission is detected from the two CO outflow lobes; [C I] emission from the southwest lobe appears as a limb-brightened, conical shell. Outflow parameters derived from [C I] are consistent with those derived from CO, suggesting the [C I] emission arises from ambient cloud material swept-up by the outflow.
The presence of carbon in the swept-up component of the outflows indicates that gas phase carbon is present deep within molecular clouds and is not confined solely to surface layers.

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