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Astron. Astrophys. 341, 1-7 (1999)

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Formation of groups and clusters of galaxies

Alexander Knebe and Volker Müller

Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany

Received 30 March 1998 / Accepted 25 September 1998


The formation, inner properties, and spatial distribution of galaxy groups and clusters are closely related to the background cosmological model. We use numerical simulations of variants of the CDM model with different cosmological parameters and distinguish relaxed objects from recent mergers using the degree of virialisation. Mergers occur mostly in deep potential wells and mark the most important structure formation processes. As a consequence, the autocorrelation function of merged halos has a higher amplitude and is steeper than that of the virialized clusters. This can be directly connected to the same result found from the observation of luminous infrared galaxies; they are as well more strongly correlated and can primarily be identified with ongoing merging events.

Key words: cosmology: observations – cosmology: large-scale structure of Universe

This article contains no SIMBAD objects.


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© European Southern Observatory (ESO) 1999

Online publication: November 26, 1998