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Mass-to-light ratio of intermediate and old clusters in the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

Patrick Seitzer
Patrick Seitzer*
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MC 21218, USA

Abstract

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The observed central velocity dispersion of a stellar system is dependent on the mass distribution and the velocity distribution function. For the past several years a program has been undertaken to determine central velocity dispersions of LMC and SMC clusters for comparison with galactic clusters. The mass-to-light ratio (M/L) estimates so obtained should be considerably more accurate than those obtained by tidal arguments (Chun 1978, Elson & Freeman 1985).

Accurate radial velocities (mean error = 1.3 km s−1) have been obtained for a sample of K-type giants with the CTIO 4m telescope and échelle spectrograph with CCD detector. All of the stars observed were within two core radii of the cluster centre. Multiple observations at several epochs (1984 and 1989) were used to determine the velocity errors.

The central M/L in solar units has been estimated from single component isotropic King models (King 1966), with the assumption that the distribution of mass follows that of the light. Observed values for the total integrated light and core radius were taken from the literature (in particular, from Chun 1978, van den Bergh 1981, Mateo 1987).

Type
Star Formation and Clustering
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 213 - 214
Copyright
Copyright © Kluwer 1991 

References

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