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Session 10 - Interstellar Medium and Star Formation.
Display session, Monday, June 08
Atlas Ballroom,
The HII region S140 appears to be a prototype ``blister'' HII region seen approximately edge-on. It is primarily excited by a B0V star, which also produces an ionization front and a photodissociation region at the edge of the molecular cloud L1204. Strong infrared sources, including a bipolar outflow source, embedded in the molecular cloud near the cloud edge, makes this region a good example of an interacting complex of star formation. LWS spectra were taken at a series of positions covering both the HII region and the molecular cloud. Here we consider the dust continuum, the [OI]63 micron, and the [CII]156 micron emission from the HII region and compare to model results assuming a blister (2-D) geometry. Recently available NLTE model atmospheres for the ionizing star are employed. The continuum emission peaks at longer wavelengths than can be explained by the MRN dust sizes and optical properties, and we investigate the possible required changes in the sizes, shapes, and FIR emissivities of the dust. Also, the source of the strong 63 micron emission, which cannot originate in the HII region, will be discussed.
This work is supported by NATO Collaborative Research Grant No. 960326.
