Alexander Knebe
Published 1998-08-31Version 1
The formation process, 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 in order to compare statistical measures such as mass spectra, merging histories, correlation functions, and clustering power spectra with relevant observations. The study of the time evolution shows that the internal structure of galaxy groups and clusters is connected with their merging history. Here we discuss the virialisation and the halo's spin parameters.
Comments: 2 pages, 2 figures, to appear in: Large Scale Structures: Tracks and Traces, Proceedings of the 12th Potsdam Cosmology Workshop 1997
Quantifying the Morphologies and Dynamical Evolution of Galaxy Clusters. II. Application to a Sample of ROSAT Clusters
Quantifying Substructure in Galaxy Clusters
Dynamical Search for Substructures in Galaxy Clusters, A Hierarchical Clustering Method
