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Large-scale structure and kinematics of the Magellanic Clouds from carbon star studies

Published online by Cambridge University Press:  19 July 2016

M. Azzopardi  and
E. Rebeirot
M. Azzopardi
Affiliation:
Observatoire de Marseille, 2, Place Le Verrier, 13248 Marseille Cedex 4, France
E. Rebeirot
Affiliation:
Observatoire de Marseille, 2, Place Le Verrier, 13248 Marseille Cedex 4, France

Abstract

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Initially, carbon stars have been searched for through their CN bands in the near infrared. However, C stars can also be identified efficiently by the C2 Swan bands in the blue-green spectral region. Schmidt telescopes with objective-prisms have been used intensively for the detection of C stars. More recently, transmission gratings at the prime foci of large telescopes have made possible deeper surveys at limiting magnitudes that insure carbon star detection in the Magellanic Clouds (MCs) with a reasonable degree of completeness; completeness is even better in the regions where both observational techniques have been used. Statistical studies are now possible. The C star surface distribution and global kinematics derived from radial velocity measurements of selected C stars, when compared to those of other objects, show that the field Small Magellanic Cloud (SMC) C stars are not a young population, in agreement with studies of C stars in SMC clusters.

Type
Large-Scale Structure and Kinematics
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 71 - 76
Copyright
Copyright © Kluwer 1991 

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