Chemistry of the Hot Core Region in OMC-1

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Session 61 -- Molecular Clouds, Star Formation
Display presentation, Thursday, 9:20-4:00, Pauley Room

[61.05] Chemistry of the Hot Core Region in OMC-1

E.C.Sutton, R.S.Peng (U. Illinois), W.C.Danchi (UCB), P.A.Jaminet (SAO), G.Sandell (JAC), A.P.G.Russell (ROE)

We have carried out a survey of molecular line emission in the 334-343 GHz region from several positions in the core of the Orion molecular cloud. These observations were carried out using the 15 m JCMT, which gave a beam width of approximately 14 arcsec at these frequencies. Good spatial selectivity is essential in analyzing the chemistry of a region as complex as the Orion core. Analysis of spectra taken towards the hot core position reveals approximately 140 identifiable lines indicative of an oxygen and nitrogen-rich environment. Excitation analysis yields typical excitation temperatures of about 150 K, indicating physical temperature in excess of 200 K and densities of order $10^{7}$ $cm^{-3}$. Spectra from nearby positions in the central regions of OMC-1 differ sharply, indicating the presence of small scale variations in both chemical abundances and excitation. This work has been supported in part by the National Science Foundation under grants AST 91-96077 and AST 91-17740.

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