EDP Sciences
Free Access
Issue
A&A
Volume 392, Number 3, September IV 2002
Page(s) 795 - 805
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361:20020940
Published online 09 September 2002


A&A 392, 795-805 (2002)
DOI: 10.1051/0004-6361:20020940

Abell 1451 and 1RXS J131423.6-251521: A multi-wavelength study of two dynamically perturbed clusters of galaxies

I. Valtchanov1, T. Murphy2, M. Pierre1, R. Hunstead2 and L. Lémonon1

1  CEA/DSM/DAPNIA, Service d'Astrophysique, 91191 Gif-sur-Yvette, France
2  School of Physics, University of Sydney, NSW 2006, Australia

(Received 9 April 2002 / Accepted 20 June 2002)

Abstract
We present results from optical, X-ray and radio observations of two X-ray bright ( $L_{\rm X} \sim 10^{45}$ erg s -1) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion $\sigma_{\rm v} = 1330$ km s -1 as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and $\sigma_{\rm v} = 1100$ km s -1 from 37 galaxies. There are two distinct galaxy groups with a projected separation of $\approx$700 kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700 km s -1, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.


Key words: galaxies: clusters: individual: Abell 1451, 1RXS J131423.6-251521 -- X-rays: galaxies -- radio lines: galaxies -- galaxies: distances and redshifts -- galaxies: clusters: general

Offprint request: I. Valtchanov, ivaltchanov@cea.fr

SIMBAD Objects in preparation



© ESO 2002

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