The morphological and dynamical evolution of simulated galaxy clusters

Free access article

Issue		A&A Volume 379, Number 2, November IV 2001


Page(s)		412 - 425
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:20011319

A&A 379, 412-425 (2001)
DOI: 10.1051/0004-6361:20011319

The morphological and dynamical evolution of simulated galaxy clusters

C. Beisbart^{1, 2}, R. Valdarnini³ and T. Buchert^{4, 5, 1}

¹ Theoretische Physik, Ludwig-Maximilians-Universität, Theresienstr. 37, 80333 München, Germany
² Astrophysics, Nuclear and Astrophysics Laboratory, Keble Road, Oxford OX1 3RH, UK
³ SISSA, Via Beirut 4, Trieste 34014, Italy
⁴ Theoretical Astrophysics Division, National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
⁵ Département de Physique Théorique, Université de Genève, 24 quai E. Ansermet, 1211 Genève, Switzerland

(Received 7 May 2001 / Accepted 14 September 2001 )

Abstract
We explore the morphological and dynamical evolution of galaxy clusters in simulations using scalar and vector-valued Minkowski valuations and the concept of fundamental plane relations. In this context, three questions are of fundamental interest: 1. How does the average cluster morphology depend on the cosmological background model? 2. Is it possible to discriminate between different cosmological models using cluster substructure in a statistically significant way? 3. How is the dynamical state of a cluster, especially its distance from a virial equilibrium, correlated to its visual substructure? To answer these questions, we quantify cluster substructure using a set of morphological order parameters constructed on the basis of the Minkowski valuations (MVs). The dynamical state of a cluster is described using global cluster parameters: in certain spaces of such parameters fundamental band-like structures are forming indicating the emergence of a virial equilibrium. We find that the average distances from these fundamental structures are correlated to the average amount of cluster substructure for our cluster samples during the time evolution. Furthermore, significant differences show up between the high- and the low- $\Omega_{\rm m}$ models. We pay special attention to the redshift evolution of morphological characteristics and find large differences between the cosmological models even for higher redshifts.

Key words: galaxies: clusters: general -- X-rays: galaxies: clusters -- methods: N-body simulations -- methods: statistical.

Offprint request: C. Beisbart, beisbart@astro.ox.ac.uk

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