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CO Emission toward HI Absorption Sources in the Large Magellanic Cloud

Published online by Cambridge University Press:  25 May 2016

M. Marx-Zimmer ,
F. Zimmer ,
U. Herbstmeier  and
J. M. Dickey
M. Marx-Zimmer
Affiliation:
Radioastronomisches Institut der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
F. Zimmer
Affiliation:
Radioastronomisches Institut der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
U. Herbstmeier
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
J. M. Dickey
Affiliation:
Department of Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA

Extract

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In the Large Magellanic Cloud (LMC) a large number of cool HI clouds have been detected with temperatures much lower than those found for atomic clouds in the Milky Way (Dickey et al. 1994; Mebold et al. 1997; Marx-Zimmer et al. 1998). Apparently, the population of cool HI clouds reaches kinetic gas temperatures down to as low as 10 or 20 K. These clouds may play an important role in the formation of stars in the LMC. We studied the association between the cool atomic gas and molecular gas in the LMC by 12CO(1–0) line observations in directions of cool HI clouds using the 15-m Swedish-ESO Submillimetre Telescope (SEST).

Type
Part 2. Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 190: New Views of the Magellanic Clouds , 1999 , pp. 124 - 125
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

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