A Multitransitional Molecular and Atomic Line Study of S:140

Details A Multitransitional Molecular and Atomic Line Study of S:140 A Multitransitional Molecular and Atomic Line Study of S:140

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...277..595m&link_type=abstract

Astronomy and Astrophysics, Vol. 277, NO. 2/OCT(I), P. 595, 1993

Astronomy and Astrophysics

Astrophysics

49

Stars: Early-Type - Interstellar Medium: H Ii Regions - Ism: Radio Lines: Interstellar - Jets And Outflows - Ism: Individual Objects: S14O

Scientific paper

We present high-angular resolution maps of the S 140 molecular cloud in various transitions of the 12CO, 13CO and C18 O molecules and single-channel observations of the 3P1 H3P0 line of neutral atomic carbon (CI). Velocity channel maps of the 12CO lines show a systematic shift of the emission peak away from the outflow source with increasing velocity offset from the line centre. The blue and redshifted outflow lobes are separated by ˜35 arcsec (0.15 pc) in projection and the outflow axis is believed to be directed close to the observers' line- of-sight. The masses of the blue and redshifted outflow lobes were found to be 19.5 and 8.1Msun respectively, giving a total mass for the outflow of 27.6Msun. The higher J-level 12CO lines are strongly self-absorbed, with the amount of self-absorption varying with position across the mapped region.
All the 12CO, 13CO and C18O lines show enhanced main beam brightness temperatures at the molecular cloud/H II region interface. The 13CO line intensities imply the excitation temperature increases from ˜65-70K at the position of the outflow source, to ˜250K at the interface region. The CI emission is mainly confined to a clumpy, elongated ridge-like feature adjacent to the edge of the molecular cloud and is coincident with a similar feature seen in 12CO line emission. The coincidence of these features contradicts homogeneous cloud models and is interpreted as evidence that the molecular material is composed of dense clumps interspersed with a more tenuous interclump medium. A second region of intense CI emission is located inside a ring of CS emission, implying that 12CO here is dissociated by the radiation field from the embedded infrared cluster and not the external radiation field. Observed positions on the PDR have significantly higher values Of Tmb(CI)/Tmb(13CO) than for the general cloud, implying N(CI)IN(13CO) is likely to be significantly higher for positions on the PDR than in the general molecular cloud.

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