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Oh as a Constituent of the Interstellar Medium

Published online by Cambridge University Press:  30 March 2016

B. E. Turner

Abstract

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OH is at present the most ubiquitous molecule known in the interstellar medium. It is primarily associated with galactic continuum sources, both thermal and nonthermal. The fraction of all sources showing OH decreases monotonically with galactic longitude away from the Galactic Center region. However, neither the projected density of OH nor the abundance relative to hydrogen or other molecules seems to depend on location within the galactic plane. OH also occurs in many dark dust clouds, where its density is typically 10−5—10−4 cm−3 and its abundance relative to hydrogen is very high. OH is not found in the heavily reddened stellar clusters of Reddish, in Wolf Rayet stars, in planetary nebulae, or in globules. Recent surveys have indicated that OH both in emission and in absorption, is highly correlated with H2CO in direction and in velocity. OH emission, but not absorption, is also highly correlated with anomalous H2O emission. These relationships are important in deciding between various processes for interstellar molecule formation. On present information, it appears that more than one such process is operative in different regions of the interstellar medium.

Type
III. Joint Discussions
Information
Highlights of Astronomy , Volume 2: Highlights of Astronomy. As presented at the XIVth General Assembly of the IAU, 1970 , 1971 , pp. 378 - 390
Copyright
Copyright © Reidel 1971

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