Astronomy and Astrophysics – Astrophysics
Scientific paper
1997-07-02
Astronomy and Astrophysics
Astrophysics
53 pages, LaTex (aaspp4), 2 tables, 1 in .tex mode; 1 as ADC-format data table with its own readme file; 17 figures. *.gz file
Scientific paper
10.1086/118570
The kappa-space three-dimensional parameter system was originally defined for the physical properties of dynamically hot galaxies. Here we define self-consistent kappa-parameters for disk galaxies, galaxy groups and clusters, and globular clusters and project an integrated view of the major classes of self-gravitating, equilibrium stellar systems in the universe. Six different fundamental planes exist that are interrelated and interconnected - the ``cosmic metaplane.'' The kappa-3 vs. kappa-1 projection (M/L vs. Mass) views all planes edge-on, M/L increasing or constant with Mass. Within the cosmic metaplane (kappa-2 vs. kappa-1 projection), no stellar system violates the rule that kappa-1 + kappa-2 < 8, meaning the maximum volume luminosity density of stellar systems varies as a (K times M^{-4/3}; the ``zone of exclusion''). Galaxies march away from ZOE as a function of Hubble type: DHGs closest, Sm-Irr's furthest away. We test current ideas of galaxy formation via hierarchical clustering and merging and find them to be broadly consistent with the properties of the cosmic metaplane. Four key questions are raised by this study: Why do galaxy groups form a bridge between galaxy clusters and galaxies? Why do galaxies march away from the ZOE? Why are isotropic galaxies only found in a limited mass range? What causes M/L to vary so smoothly with M to produce the cosmic metaplane? This study is but the first step along a long road, limited by existing data to the B passband of major stellar systems, whose light is dominated by stars. K-band data would be high desirable, as well as data that can probe the gaseous content (cold and hot) of stellar systems, and data for other classes of stellar systems.
Bender Ralf
Burstein David
Faber Sandra
Nolthenius Richard
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