Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.2207b&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #22.07; Bulletin of the American Astronomical Society, Vol. 24, p.1157
Other
Scientific paper
Using the Owens Valley millimeter interferometer, we have observed W3 in the \h40a, HCN, HNC, and CS transitions at 3 mm at 3'' resolution. We have also observed the \c34s\ transition at 10'' resolution. Three fields were mapped covering an area of about 2' east-west by 1.5' north-south. encompassing the core of the molecular cloud and surrounding the compact H II regions W3(B) and W3(C). The molecular maps show eight condensations with sizes ranging from ~ 4'' to over 20'' and virial masses from roughly 20 to 500 M\sun. Apparent optical depths in CS determined from the \c34s/C(32) S flux ratios are typically 2--4, though a value of about 20 is seen in the largest observed condensation (15'' south of W3(C)). Several regions stand out as quite disparate in the relative intensities of the HCN/HNC/CS transitions, suggesting significant variations in the relative abundances of these molecules throughout the cloud core. The most dramatic case is W3 IRS 5, a possible protostar with supersonic molecular outflows. At the position of IRS 5, the integrated intensity of HCN reaches its greatest value in the mapped area; however, HNC is completely undetected, and, while a strong CS condensation is present 4'' north-east of IRS 5, no CS emission associated with IRS 5 itself is detected. The 3sigma upper limit to the HNC/HCN abundance ratio is determined to be 0.25 in this region, assuming similar excitation temperatures for the two species. Furthermore, the HCN emission at IRS 5 exhibits a very broad line-width ( ~ 20 km s(-1) ); the other clumps show line-widths of 2--5 km s(-1) , more typical of cold, turbulent molecular clumps.
Bryant Peter M.
Scoville Nicholas Z.
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