The Density and Structure of CS Emission in the Milky Way Plane

Details The Density and Structure of CS Emission in the Milky Way Plane The Density and Structure of CS Emission in the Milky Way Plane

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.7105b&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #71.05; Bulletin of the American Astronomical Society, Vol. 30, p.1356

Astronomy and Astrophysics

Astronomy

Scientific paper

In an earlier survey of CS(J=2--1) emission in the plane of the Milky Way, Helfer & Blitz (1997) found that emission from this high dipole moment molecule was more commonly detected in the Galactic plane than in solar-neighborhood Giant Molecular Clouds, albeit at a weaker level than in starforming cores in GMCS. Here, we present observations of CS(J=3--2) and CS(J=2--1) from twenty-one pc-scale ``features'' along nine lines of sight in the first quadrant of the Milky Way plane. Using a Large Velocity Gradient (LVG) radiative transfer model of the observed line temperatures, we derive moderate (log n(H_2) cm(-3) = 3--5) densities for the features. The moderate densities suggest that these features are not cloud cores; they may instead be similar to the envelopes around starforming cores. For one line of sight that was specially selected for strong molecular emission, we derive a density of log n(H_2) cm(-3) = 5.4; this special position appears to be the only core candidate in our sample. We also present interferometric observations of one of the cloud features; these observations place limits on the size scale of the emitting region.

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