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Extended Oh Emission at 1720 Mhz

Published online by Cambridge University Press:  14 August 2015

W. M. Goss ,
L. E. B. Johansson ,
J. Elldér ,
B. Höglund ,
Nguyen-Q-Rieu  and
A. Winnberg
W. M. Goss
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
L. E. B. Johansson
Affiliation:
Onsala Space Observatory, Onsala, Sweden
J. Elldér
Affiliation:
Onsala Space Observatory, Onsala, Sweden
B. Höglund
Affiliation:
Onsala Space Observatory, Onsala, Sweden
Nguyen-Q-Rieu
Affiliation:
Observatoire de Meudon, Meudon, France
A. Winnberg
Affiliation:
Max-Planck-Institut für Radioastronomie, Bonn, F.R.G.

Abstract

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Low-velocity OH emission lines at 1720 MHz have been investigated in the direction of W41, W43, W51, and 3C 353. The emission lines in the directions of W43 and W51 show no detectable circular polarization and are about 27 and 32 arcmin in size, respectively. The inferred peak brightness temperatures are 0.6 K for W43 and 2.0 K for W51. This emission may be similar to the nonthermal 1720-MHz emission in dust clouds.

Type
Part 1: The Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 60: Galactic Radio Astronomy , 1974 , pp. 135 - 136
Copyright
Copyright © Reidel 1974 

References

Goss, W. M.: 1968, Astrophys. J. Suppl. 15, 131.Google Scholar
Goss, W. M. and Robinson, B. J.: 1968, Astrophys. Letters 2, 81.Google Scholar
Hardebeck, E.: 1971, Astrophys. J. 170, 281.Google Scholar