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An overview of the structure and kinematics of the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

B. E. Westerlund
B. E. Westerlund*
Affiliation:
Astronomical Observatory, Box 515, S-751 20 Uppsala, Sweden

Abstract

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A vast amount of observational data concerning the structure and kinematics of the Magellanic Clouds is now available. Many basic quantities (e.g. distances and geometry) are, however, not yet sufficiently well determined. Interactions between the Small Magellanic Cloud (SMC), the Large Magellanic Cloud (LMC) and our Galaxy have dominated the evolution of the Clouds, causing bursts of star formation which, together with stochastic self-propagating star formation, produced the observed structures. In the youngest generation in the LMC it is seen as an intricate pattern imitating a fragmented spiral structure. In the SMC much of the fragmentation is along the line of sight complicating the reconstruction of its history. The violent events in the past are also recognizable in complex velocity patterns which make the analysis of the kinematics of the Clouds difficult.

Type
Large-Scale Structure and Kinematics
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 15 - 23
Copyright
Copyright © Kluwer 1991 

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