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Spherical Galaxies: Methods and Models

Published online by Cambridge University Press:  04 August 2017

Douglas O. Richstone
Douglas O. Richstone*
Affiliation:
Department of Astronomy, University of Michigan

Abstract

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Over the last 5 years, considerable progress has been made in our ability to construct self-gravitating stellar equilibria. One of these new methods is essentially a variant of Eddington's (1916) method. Two other key approaches are logical extensions of Schwarzschild's Linear Programming method, and can be applied to nonspherical models as well. These methods are reviewed below.

The application of these methods to galaxies has yielded a few very interesting results within the last year or two. The methods described below unambiguously establish M/L's for M87 and M32 within about 30 arc seconds. They strongly support Tonry's contention that the nucleus of M32 contains a large invisible mass, possibly a 107M⊙ black hole. They also suggest that observational recovery of the projected velociy distribution might permit the observer to distinguish between a massive halo and an increasingly tangential velocity distribution function.

Type
Invited Reviews
Information
Symposium - International Astronomical Union , Volume 127: Structure and Dynamics of Elliptical Galaxies , 1987 , pp. 261 - 269
Copyright
Copyright © Reidel 1987 

References

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