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Disk Mass From Large-Scale Dynamics

Published online by Cambridge University Press:  14 August 2015

J.A. Sellwood
J.A. Sellwood*
Affiliation:
Rutgers University Dept. of Physics & Astronomy, PO Box 849, Piscataway, NJ 08855, USA

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The radial distribution of mass in a disk galaxy is strongly constrained by its rotation curve. The separate contributions from the individual stellar populations and dark matter (DM) are not easily disentangled, however, especially since there is generally no feature to indicate where the component dominating the central attraction switches from luminous to dark matter. Here I summarize three recent thesis projects at Rutgers University which all suggest that DM has a low density in the inner parts of bright galaxies, and that most of the mass therefore resides in the disk. In addition, I present some preliminary work on the Milky Way. If we are able to determine the M/L of a typical disk stellar population, it should provide a useful constraint on the numbers of low mass stars.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 1: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part A), 1997 , 1998 , pp. 410 - 411
Copyright
Copyright © Kluwer 1998

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