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Distribution of young stars and gas in the Small Magellanic Cloud

Published online by Cambridge University Press:  19 July 2016

J. Lequeux
J. Lequeux*
Affiliation:
Observatoire de Meudon, 92195 Meudon CEDEX, France, and Ecole Normale Supérieure

Abstract

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The relations between the distributions of interstellar gas and young stars in the central parts of the SMC are discussed, based on their distributions over the sky, radial velocities and distances. There are large differences between stars and gas. The existence of two main complexes is confirmed. There is no strong evidence for a distance in depth between these complexes larger than about 10 kpc, although Cepheid observations suggest a large total depth in some regions. Further, more accurate observations of Cepheids, especially of their mean radial velocities, are required for a better understanding of the structure of the SMC.

Type
Large-Scale Structure and Kinematics
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 25 - 29
Copyright
Copyright © Kluwer 1991 

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