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Carbon Monoxide in the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

F. P. Israel  and
Th. De Graauw
F. P. Israel
Affiliation:
Sterrewacht Leiden, PO Box 9513, 2300 RA Leiden, The Netherlands
Th. De Graauw
Affiliation:
Laboratory for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands

Abstract

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Molecular gas is a major constituent of the interstellar medium of all late-type galaxies. Virtually all of it is in the form of cold molecular hydrogen (H2) which today cannot be observed directly. However, the tracer molecule carbon monoxide (CO) (relative abundance 10−5) is easily detected. For the Magellanic Clouds (MCs), CO studies are of specific importance. The Clouds are rich in HI, and if we can establish the presence of significant amounts of H2 as well, this will influence our estimates of the global rate of star formation and its history. Complexes of presently quiescent molecular gas may betray regions primed for star formation, but not yet in action. Detailed studies of the HI, HII and H2 and young star content may provide estimates of star formation efficiences on scales of a kiloparsec.

Type
Large-Scale Structure and Kinematics
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 45 - 49
Copyright
Copyright © Kluwer 1991 

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