Kinematical tests for the intrinsic shapes of galaxies

Details Kinematical tests for the intrinsic shapes of galaxies Kinematical tests for the intrinsic shapes of galaxies

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.209..317c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 209, July 15, 1984, p. 317-334.

Astronomy and Astrophysics

Astronomy

9

Astronomical Models, Elliptical Galaxies, Galactic Evolution, Galactic Structure, Kinematics, Astronomical Catalogs, Monte Carlo Method, Shapes, Velocity Distribution

Scientific paper

Determining the intrinsic shape of elliptical galaxies has been an illusive enterprise, but one fundamental to the understanding of their internal dynamics and formation. Here, a dynamic approach to the problem is used; noting that the velocity dispersion is largest when sighted down the longest axis, the expected correlations of velocity dispersion with observed eccentricity are derived after the known trend of velocity dispersion with luminosity is removed. Using a compilation of published data, the relation between luminosity and velocity dispersion is determined more accurately. The residuals are examined as a function of axis ratio in order to construct a test for the intrinsic shape of galaxies. The effects of projection are modeled and possible intrinsic variations are examined. Model catalogues, generated from the theory by a Monte Carlo technique, are compared to the observational data. This test is inconclusive, since it excludes only one of the four proposed configurations, but further probes which are capable of untangling intrinsic variations from those of projection are discussed.

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