Published 1992
| Version public
Book Section - Chapter
The Orion Nebula
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Abstract
As one of the nearest and brightest massive star forming molecular clouds, the core of the Orion nebula presents a unique opportunity to examine the complexity and evolution of interstellar chemistry. We present here an overview of the results gleaned from high resolution millimeter and submillimeter spectral line surveys of the region along with aperture synthesis maps of molecular emission obtained with interferometers such as the Owens Valley (OVRO) and Hat Creek millimeter-wave instruments and the VLA. Emphasis will be placed on the alteration of the chemical composition of the parent molecular cloud by the star formation process.
Additional Information
© 1992 University of Tokyo Press. It is a pleasure to acknowledge the tireless efforts of a number of coworkers, longstanding members of "the Orion community" (as R. Genzel has described it), who have contributed much to this work. In particular, T. Groesbeck played a critical role in the CSO 345 GHz surveys, while E. Sutton, C. Masson, and T. Phillips were essential to the OVRO 230 GHz spectral line survey. The author also acknowledges many helpful discussions and successful OVRO sessions with L. Mundy and A. Sargent. Figure 2 from the Hat Creek Array was kindly provided by R. Plambeck. Astronomy at the OVRO and at the CSO is support by the NSF, grants #AST 84-12473 and #AST 83-11849.Additional details
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- 34662
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- CaltechAUTHORS:20121003-105552646
Funding
- NSF
- AST 84-12473
- NSF
- AST 83-11849
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2012-10-04Created from EPrint's datestamp field
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2019-10-03Created from EPrint's last_modified field
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- Division of Geological and Planetary Sciences (GPS)