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For refcode 1995AJ....109.2293D:
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1995AJ....109.2293D THE FORMATION OF COMPACT GROUPS OF GALAXIES. II. X-RAY PROPERTIES ANTONALDO DIAFERIO Universita di Pavia, Dipartimento di Fisica Nucleare e Teorica, Via Bassi 6,27100, Pavia, Italy, and Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge Massachusetts 02138 Electronic mail: diaferio@cfa.harvard.edu MARGARET J. GELLER Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge Massachusetts 02138 Electronic mail: mjg@cfa.harvard.edu MASSIMO RAMELLA Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11,34131 Trieste, Italy Electronic mail: ramella@oat.ts.astro.it Received 1994 September 9; revised 1995 February 22 ABSTRACT We use N-body/hydrodynamic simulations of collapsing rich galaxy groups to predict X-ray properties of compact groups. The model is consistent with the X-ray observations of a few compact groups and naturally explains the correlation between the spiral fraction and the velocity dispersion and crossing time observed in compact groups. The model predicts a correlation between X-ray luminosity and gas temperature only if the systems are bound. The model is an extension of the one used by Diaferio et at. [AJ, 107,868(1994)] to show that substructures within collapsing rich loose groups have dynamical properties and a multiplicity function similar to the Hickson compact groups. So far, both X-ray and optical results suggest that most observed compact groups are three- dimensional systems rather than chance alignments of unrelated galaxies. We propose some direct observational tests to discriminate among models.
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