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Structural and Kinematic Properties of Populations of the Andromeda Galaxy

Published online by Cambridge University Press:  14 August 2015

J. Einasto
J. Einasto*
Affiliation:
W. Struve Astrophysical Observatory, Tartu, Estonia, U.S.S.R.

Abstract

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New observational data (Spinrad, 1970; Van den Bergh, 1970; Rubin and Ford, 1970) are used to determine structural and kinematic parameters of the nucleus, the subsystem of globular clusters, and interstellar hydrogen in M31.

The mass derived for the nucleus from the new spectrophotometric data is in good agreement with the virial mass 6 × 108M⊙. Model calculations show that there is no appreciable exchange of stars between the nucleus and the bulge. The rotation energy of the nucleus is only 7.5% of the total kinetic energy; the central density is 2 × 106M⊙ pc−3.

The mean radius of the subsystem of globular clusters is 4.5 kpc. This indicates that the subsystem of old stars is not identical with the spheroidal component of the galaxy, whose mean radius is only 1 kpc. Radial velocity dispersion of globular clusters is only half of that of the nucleus. This shows a strong dependence of the velocity dispersion on distance to the center of the galaxy and a bias in mass determination of a galaxy from velocity dispersion near the nucleus.

On the basis of data on rotation two mass distribution models have been found, differing from each other in respect of the mass concentration to the center. Spectrophotometric data on the stellar content of the bulge are urgently needed to solve the mass distribution problem.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 44: External Galaxies and Quasi-Stellar Objects , 1972 , pp. 37 - 45
Copyright
Copyright © Reidel 1972 

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