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Explaining Compact Groups as Chance Alignments

Published online by Cambridge University Press:  12 April 2016

Gary A. Mamon
Gary A. Mamon*
Affiliation:
Observatoire de Meudon Meudon, France

Extract

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The physical nature of the apparently densest groups of galaxies, known as compact groups is a topic of some recent controversy, despite the detailed observations (Hickson, in these proceedings, and references therein) of a well-defined catalog of 100 isolated compact groups compiled by Hickson (1982). Whereas many authors have espoused the view that compact groups are bound systems, typically as dense as they appear in projection on the sky (e.g., Williams & Rood 1987; Sulentic 1987; Hickson & Rood 1988), others see them as the result of chance configurations within larger systems, either in ID (chance alignments: Mamon 1986; Walke & Mamon 1989), or in 3D (transient cores: Rose 1979). As outlined in the companion review to this contribution (Mamon, in these proceedings), the implication of Hickson’s compact groups (hereafter, HCGs) being dense bound systems is that they would then constitute the densest isolated systems of galaxies in the Universe and the privileged site for galaxy interactions.

Type
VIII. Classical Theory of Multiplets
Information
International Astronomical Union Colloquium , Volume 124: Paired and Interacting Galaxies , 1990 , pp. 619 - 627
Copyright
Copyright © NASA 1990

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