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Testing Cosmological Models with Clusters of Galaxies

Published online by Cambridge University Press:  25 May 2016

S. Gottlöber ,
J. Retzlaff  and
A. Klypin
S. Gottlöber
Affiliation:
Astrophysical Institute Potsdam An der Sternwarte 16, D-14482 Potsdam
J. Retzlaff
Affiliation:
Astrophysical Institute Potsdam An der Sternwarte 16, D-14482 Potsdam
A. Klypin
Affiliation:
Department of Astronomy, New Mexico State University Las Cruces, NM 88001, USA

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Currently little is known about the mass distribution on intermediate scales between those probed by deep redshift surveys of galaxies and those probed by COBE. Catalogs of galaxy clusters reach depths of several hundred megaparsecs, and, thus, are very useful for those scales. Only the Las Campanas Redshift Survey (LCRS) is comparable with that depth. However, the LCRS samples only narrow slices whereas cluster catalogs cover a large fraction of the sky. Clusters seems to be the most suitable objects to fill the gap between scales probed by COBE and the galaxy samples. Moreover, clusters are advantageous over galaxies as probes of the matter distribution in the Universe because our understanding of its formation and evolution is better established than it is for galaxies. Clusters are high peaks (mass scale M ≃ 1015M⊙) in the density field, which have collapsed relatively recently. Because of that, it is easy to identify clusters in numerical simulations. But the number of clusters is much smaller than the number of galaxies, which makes the statistics of clusters noisier. Nevertheless, clusters are exceptionally useful objects for the investigation of the matter distribution on scales well above 100 h–1 Mpc. Thus, it is worth to apply different statistical tests to these objects.

Type
IV. Structure Formation and Dark Matter
Information
Symposium - International Astronomical Union , Volume 183: Cosmological Parameters and the Evolution of the Universe , 1999 , pp. 221 - 228
Copyright
Copyright © Kluwer 1999 

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