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CO and OH in the Galactic Center Region

Published online by Cambridge University Press:  14 August 2015

Junji Inatani  and
Nobuharu Ukita
Junji Inatani
Affiliation:
Department of Astronomy, University of Tokyo Norio Kaifu, Tokyo Astronomical Observatory Shinji Kodaira and Koichi Ishii Kisarazu Technical College
Nobuharu Ukita
Affiliation:
Department of Astronomy, University of Tokyo Norio Kaifu, Tokyo Astronomical Observatory Shinji Kodaira and Koichi Ishii Kisarazu Technical College

Extract

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The two-dimensional distribution of molecular clouds in the galactic center region has been investigated in the CO 115 GHz line and in the OH 1665 and 1667 MHz lines. As the former is an emission line, we can find molecular clouds without the unavoidable bias to continuum sources which is inherent in a survey of OH absorption lines. Because the CO line is usually optically thick, the brightness temperature of the line is directly related to the kinetic temperature of the cloud. On the other hand, the real optical depth of the OH line can be obtained from the intensity ratio between 1665 and 1667 MHz lines (assuming LTE). From this point of view we have compared the CO and OH observational results.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 87: Interstellar Molecules , 1980 , pp. 111 - 112
Copyright
Copyright © Reidel 1980 

References

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