Published August 15, 1977
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Journal Article
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CO emission from supernova remnants
Abstract
In a search for molecular gas associated with supernova remnants, the CO line has been observed in three optical remnants: the Cygnus Loop, IC 443, and Cas A. In both the Cygnus Loop and IC 443, CO molecules are detected from dense clouds of the order of 100 solar masses, probably located at the edge of the expanding remnants. These are locations of particularly bright optical filaments and strong radio continuum emission. The foreground emission seen in Cas A exhibits changes on a small scale compared with the radio continuum, implying a low filling factor for molecular absorption lines in Cas A.
Additional Information
© 1977. The American Astronomical Society. Received 1976 November 29. We thank Arno Penzias for use of telescope time, Paul Vanden Bout for loaning a klystron, and Peter Goldreich for discussions. This research is partially supported by NSF grant MPS 73-04949. This is Contribution No. 240 of the Five College Observatories. The Millimeter Wave Observatory is operated by the Electrical Engineering Research Laboratory, The University of Texas at Austin, with support from the National Aeronautics and Space Administration, the National Science Foundation, and McDonald Observatory.Attached Files
Published - 1977ApJ___216__320S.pdf
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1977ApJ___216__320S.pdf
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Additional details
- Eprint ID
- 94419
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- CaltechAUTHORS:20190403-153007434
- NSF
- MPS 73-04949
- NASA
- McDonald Observatory
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2019-04-05Created from EPrint's datestamp field
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2021-11-16Created from EPrint's last_modified field