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CO Observations in the Small Magellanic Cloud

Published online by Cambridge University Press:  04 August 2017

M. Rubio ,
R. Cohen  and
J. Montani
M. Rubio
Affiliation:
Universidad de Chile, Departamento de Astronomia
R. Cohen
Affiliation:
Columbia University
J. Montani
Affiliation:
Columbia University

Extract

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The dwarf Magellanic irregular galaxies apparently have a very low molecular content compared to the Milky Way. In the LMC, molecular clouds are fairly common, but the ratio of molecular to atomic gas is at least 5 times lower than in the Galaxy (Cohen et al. 1984). Elmegreen et al. (1980) searched for CO in 6 dwarf galaxies and failed to detect any emission even though their sensitivity was adequate to detect galactic giant molecular clouds placed at the distance of these galaxies. Israel (1984) observed the J=2→1 transition of CO at 15 points in the Small Magellanic Cloud and detected CO emission from five of them, but at a level two to six times lower than typical galactic values.

Type
Interstellar Matter
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 399 - 400
Copyright
Copyright © Reidel 1984 

References

Cohen, R.S., Montani, J., Rubio, M. 1984, this volume, p. 401.Google Scholar
Elmegreen, B.G., Elmegreen, D.M., Morris, M. 1980, Astrophys. J. 240, 455.Google Scholar
Hodge, P.W. 1974, Publ. Astron. Soc. Pac. 86, 263.Google Scholar
Israel, F.P. 1984, this volume, p. 319.Google Scholar
Lebrun, F. et al. 1983, Ap. J., in press.Google Scholar
McGee, R.X., Newton, L.M. 1981, Proc. Astron. Soc. Australia, 4, 189.CrossRefGoogle Scholar