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The Kinematics of the Magellanic Clouds

Published online by Cambridge University Press:  07 August 2017

B.E. Westerlund
B.E. Westerlund*
Affiliation:
Astronomical Observatory, Uppsala University Box 515, S-75120 Uppsala, Sweden

Abstract

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It is essential for our understanding of the evolution of the Magellanic System, comprising the Large and the Small Magellanic Cloud, the Intercloud or Bridge region and the Magellanic Stream, to know its motions in the past. The Clouds have a common envelope of neutral hydrogen; this indicates that they have been bound to each others for a long time. The Magellanic System moves in the gravitational potential of our Galaxy; it is exposed to ram pressure through its movement in the galactic halo. Both effects ought to be noticeable in their present structure and kinematics. It is generally assumed, but not definitely proven, that the Clouds have been bound to our Galaxy for at least the last 7 Gyr. Most models assume that the Clouds lead the Magellanic Stream. The interaction between the Clouds has influenced their structure and kinematics severely. The effects should be possible to trace in the motions of their stellar and gaseous components as pronounced disturbances. Recent astrometric contributions in this field show a great promise for the future if still higher accuracy can be achieved.

Type
2. Current and Future Needs for Very Accurate Astrometry
Information
Symposium - International Astronomical Union , Volume 166: Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry , 1995 , pp. 273 - 282
Copyright
Copyright © Kluwer 1995 

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