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RXJ0256.5+0006: a merging cluster of galaxies at z=0.36 observed with XMM-Newton | | S. Majerowicz
; D.M. Neumann
; A.K. Romer
; R.C. Nichol
; D.J. Burke
; C.A. Collins
; | | Date: |
22 Jun 2004 | | Subject: | astro-ph | | Affiliation: | CEA/Saclay DSM/DAPNIA/SAP, France Physics Department, Carnegie Mellon University, USA Harvard-Smithsonian Center for Astrophysics, USA Astrophysics Research Institute, Liverpool John Moores University UK | | Abstract: | (abridged) We present a study based on XMM data of RX J0256.5+0006, a medium distant (z=0.36) galaxy cluster found in the Bright SHARC catalog. The intracluster medium shows a bimodal structure: one main cluster component and a substructure in the west. Despite the indication of interaction we do not find any sign of temperature gradients. Due to the non-symmetric form of the main cluster we extract surface brightness profiles in different sectors around its centre. We see large variations between the profiles, which we quantify by beta-model fitting. The corresponding r_c’s vary between 0.1-0.5Mpc and the beta’s between 0.5-1.2. The variations of the beta-model parameters indicate that the main cluster is not entirely relaxed. This hypothesis is strengthened by the fact that the cluster is over-luminous with respect to the (z-evolving) L_x-T relation found for nearby clusters. Comparing our profiles to the reference emission measure profile of Arnaud et al., we find that only the profile extracted north-east (NE) of the main cluster centre is similar to this reference profile. This indicates that only the NE profile is representative for the relaxed part of this cluster component. Using this profile and the spectroscopically fitted temperature of T=4.9^+0.5_-0.4keV we find M_500~4 10^14 solar masses. This value is in agreement with the value obtained using the z-evolving M_500-T relation from the HIFLUGCS sample. For the gas mass fraction we find f_g~18-20% which is in good agreement with other work. We also develop a simple on-axis merger model for the cluster. Together with a simple ram pressure model we find that the most likely physical distance of the subcluster to the main cluster lies between 0.6 | | Source: | arXiv, astro-ph/0406478 | | Services: | Forum | Review | PDF | Favorites | |
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