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The Stellar Cluster

Published online by Cambridge University Press:  23 September 2016

K. Sellgren
K. Sellgren*
Affiliation:
Institute for Astronomy, University of Hawaii 2680 Woodlawn Drive Honolulu, Hawaii 96822 USA

Abstract

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Observations of the stellar cluster in the central 10 pc of the Galaxy are reviewed. The stellar density law derived from the observed light distribution and the effects on this density law of variable extinction, the possibility of a varying mass-to-light ratio, and the current debate as to the core radius of the cluster are all important for establishing the true mass distribution of the stellar cluster. The presence of the supergiant IRS 7 in the Galactic Center establishes that some recent star formation has occurred, but the age and extent of a possible starburst are still being established. The kinematics of the stellar cluster show predominantly velocity dispersion, in contrast to the systematic gas motion observed, yet the total mass distributions derived from stellar and gas kinematics agree reasonably well. The core radius of the cluster is critical to establishing whether or not a central dark mass is required to explain the total mass distribution.

Type
Stars and the Central Mass Distribution
Information
Symposium - International Astronomical Union , Volume 136: The Galactic Center , 1989 , pp. 477 - 486
Copyright
Copyright © Kluwer 1989 

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