CO observations of the supernova remnant G78.2+2.1

Details CO observations of the supernova remnant G78.2+2.1 CO observations of the supernova remnant G78.2+2.1

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983aj.....88...97h&link_type=abstract

Astronomical Journal, vol. 88, Jan. 1983, p. 97-103.

Astronomy and Astrophysics

Astronomy

5

Astronomical Spectroscopy, Carbon Monoxide, Emission Spectra, Radio Emission, Supernova Remnants, Data Reduction, Molecular Clouds, Propagation Velocity, Shock Wave Propagation, Spectrum Analysis

Scientific paper

The area of most intense radio emission in the shell of the supernova remnant G78.2+2.1 has been observed in the 115-GHz line of (C-12)O. Previous H I observations of this region had revealed the presence of several dense cloudlets apparently accelerated by the SNR blast. No corresponding features are apparent in the CO observations. The absence of accelerated CO is interpreted as evidence that either the SNR shock velocity is so high that any pre-existing CO is chemically dissociated by the shock, or the pre-shock cloudlets were too diffuse to contain CO. The undisturbed CO in this region is found to be confined to four main clouds having typical angular sizes of 10-15 arcmin.

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