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Rotational Fine Structure Lines of Interstellar C2 Toward ζ Persei

Published online by Cambridge University Press:  14 August 2015

Frederic H. Chaffee Jr. ,
Barry L. Lutz ,
John H. Black ,
Paul A. Vanden Bout  and
Ronald L. Snell
Frederic H. Chaffee Jr.
Affiliation:
Smithsonian Astrophysical Observatory, Mt. Hopkins Observatory
Barry L. Lutz
Affiliation:
Lowell Observatory
John H. Black
Affiliation:
Harvard-Smithsonian Center for Astrophysics
Paul A. Vanden Bout
Affiliation:
University of Texas at Austin
Ronald L. Snell
Affiliation:
University of Texas at Austin

Abstract

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We have detected 9 of the rotational fine structure lines of the 2-0 Phillips band of interstellar C2 toward ζ Persei using the Tull spectrograph and Reticon detector on the 2.7 m telescope at the McDonald Observatory. These data yield a total C2 column density of 1.2 × 1013 cm-2 and a rotational temperature of 97 K compared to 1.4 × 1013 cm-2 and 45 K predicted by the detailed model of the cloud by Black, Hartquist and Dalgarno. We suggest that radiative pumping through the Mulliken and Phillips systems has modified the C2 level populations in such a way as to produce an observed rotational temperature which exceeds that arising in pure thermal equilibrium.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 87: Interstellar Molecules , 1980 , pp. 263 - 267
Copyright
Copyright © Reidel 1980 

References

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