An interstellar cloud density from Copernicus observations of CO in the spectrum of Zeta Ophiuchi

Details An interstellar cloud density from Copernicus observations of CO in the spectrum of Zeta Ophiuchi An interstellar cloud density from Copernicus observations of CO in the spectrum of Zeta Ophiuchi

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..138s&link_type=abstract

Astrophysical Journal, Part 1, vol. 220, Feb. 15, 1978, p. 138-148.

Astronomy and Astrophysics

Astrophysics

34

Carbon Monoxide, Gas Density, Interstellar Matter, Satellite Observation, Absorption Spectra, Black Body Radiation, Gas Temperature, Radial Velocity, Stellar Envelopes, Supernova Remnants

Scientific paper

Interstellar CO absorption bands in Copernicus spectra of Zeta Oph have been studied. Absorption profiles, computed under the assumption that excitation is due to collisions with H2 molecules and interaction with the 3-K background radiation field, were fitted to the reduced data of nine bands. When a gas kinetic temperature of 56 K is assumed, the best-fit condition implies a hydrogen-nucleus density of 120 per cu cm, a CO column density of 1.2 by 10 to the 15th power per sq cm, and a radial-velocity dispersion of 0.9 km/s. The relevance of these results to existing ideas concerning the Zeta Oph interstellar clouds is discussed. It is suggested that the strongest interstellar component is not circumstellar in origin but is instead part of a supernova remnant. Simple calculations are made to establish the plausibility of the supernova-remnant identification. This suggestion is also supported by Heiles's (1976) 21-cm pictures.

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