Internal dynamics of the z ~ 0.8 cluster RX J0152.7-1357

Free access article

Issue		A&A Volume 442, Number 1, October IV 2005


Page(s)		29 - 41
Section		Cosmology (including clusters of galaxies)
DOI		http://dx.doi.org/10.1051/0004-6361:20053232

A&A 442, 29-41 (2005)
DOI: 10.1051/0004-6361:20053232

Internal dynamics of the z ~ 0.8 cluster RX J0152.7-1357

M. Girardi¹, R. Demarco^{2, 3}, P. Rosati² and S. Borgani¹

¹ Dipartimento di Astronomia, Università degli Studi di Trieste, via Tiepolo 11, 34100 Trieste, Italy
e-mail: girardi@ts.astro.it
² ESO-European Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
³ Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA

(Received 12 April 2005 / Accepted 1 June 2005 )

Abstract
We present the results from the dynamical analysis of the cluster of galaxies RX J0152.7-1357, which shows a complex structure in its X-ray emission, with two major clumps in the central region and a third clump in the Eastern region. Our analysis is based on redshift data for 187 galaxies. We find that RX J0152.7-1357 $\,$ appears as a well isolated peak in the redshift space at z=0.836, which includes 95 galaxies recognized as cluster members. We compute the line-of-sight velocity dispersion of galaxies, $\sigma_{\rm V}=1322^{+74}_{-68}$ km s^-1, which is significantly larger than what is expected in the case of a relaxed cluster with an observed X-ray temperature of 5-6 keV. We find evidence that this cluster is far from dynamical equilibrium, as shown by the non Gaussianity of the velocity distribution, the presence of a velocity gradient and a significant substructure. Our analysis shows that the high value of $\sigma_{\rm V}$ is due to the complex structure of RX J0152.7-1357, i.e. to the presence of three galaxy clumps of different mean velocities. Using optical data we detect a low-velocity clump (with $\sigma_{\rm V}=300$ -500 km s^-1) in the central southwest region and a high-velocity clump (with $\sigma_{\rm V} \sim 700$ km s^-1) in the Eastern region, corresponding well to the South-West and East peaks detected in the X-ray emission. The central North-East X-ray peak is associated to the main galaxy structure with a velocity which is intermediate between those of the other two clumps and $\sigma_{\rm V}\sim 900$ km s^-1. The mass of the whole system within 2 Mpc is estimated to lie in the range $(1.2{-}2.2)\times 10^{15}$ $M_{\odot}$ , depending on the model adopted to describe the cluster dynamics. Such values are comparable to those of very massive clusters at lower redshifts. Analytic calculations based on the two-body model indicate that the system is most likely bound and currently undergoing merging. In particular, we suggest that the southwestern clump is not a small group, but rather the dense cluster-core of a massive cluster, most likely destined to survive tidal disruption during the merger.

Key words: galaxies: clusters: general -- galaxies: clusters: individual: RX J0152.7-1357 $\,$ -- galaxies: distances and redshifts -- cosmology: observations

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