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Interstellar Phases in the Magellanic Clouds

Published online by Cambridge University Press:  25 May 2016

John M. Dickey,
Monika Marx-Zimmer,
Christian Düsterberg,
Ulrich Mebold,
Snezana Stanimirović,
Lister Staveley-Smith and
H. A. Kobulnicky
John M. Dickey
Affiliation:
Univ. of Minnesota, 116 Church St. SE, Minneapolis, MN 55455, USA
Monika Marx-Zimmer
Affiliation:
Radioastronomisches Instutut der Universität Bonn, Bonn, Germany
Christian Düsterberg
Affiliation:
Radioastronomisches Instutut der Universität Bonn, Bonn, Germany
Ulrich Mebold
Affiliation:
Radioastronomisches Instutut der Universität Bonn, Bonn, Germany
Snezana Stanimirović
Affiliation:
Australia Telescope National Facility, Epping, NSW1710, Australia
Lister Staveley-Smith
Affiliation:
Australia Telescope National Facility, Epping, NSW1710, Australia
H. A. Kobulnicky
Affiliation:
Astronomy Dept., Univ. of California, Santa Cruz, CA 95064, USA

Abstract

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Surveys of λ21-cm absorption in the Magellanic System show that the cool phase of the HI is less abundant in the SMC than in the Milky Way, and may be so also in the LMC. The typical cool cloud temperature is colder than in the Milky Way, 30 to 40 K rather than 60 to 75 K. The lower abundance of cool phase HI can be traced to the lower heavy element abundances in the Magellanic environment. The cooler cloud temperatures are somewhat mysterious.

Information

Type
Part 2. Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 190: New Views of the Magellanic Clouds , 1999, pp. 45 - 50
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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