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CO emission from supernova remnants

Scoville, N. Z. and Irvine, W. M. and Wannier, P. G. and Predmore, C. R. (1977) CO emission from supernova remnants. Astrophysical Journal, 216 . pp. 320-328. ISSN 0004-637X. doi:10.1086/155473.

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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.

Item Type:Article
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Scoville, N. Z.0000-0002-0438-3323
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.
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NSFMPS 73-04949
McDonald ObservatoryUNSPECIFIED
Subject Keywords:interstellar: molecules — nebulae: supernovae remnants
Record Number:CaltechAUTHORS:20190403-153007434
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94419
Deposited By: George Porter
Deposited On:05 Apr 2019 17:36
Last Modified:16 Nov 2021 17:05

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