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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

The clusters Abell 222 and Abell 223: a multi-wavelength view

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Author(s):
Durret, F. [1, 2] ; Lagana, T. F. [3] ; Adami, C. [4] ; Bertin, E. [1, 2]
Total Authors: 4
Affiliation:
[1] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris - France
[2] Univ Paris 06, UPMC, Inst Astrophys Paris, UMR 7095, F-75014 Paris - France
[3] Univ Sao Paulo, IAG, Sao Paulo - Brazil
[4] LAM, Pole Etoile Site Chateau Gombert, F-13388 Marseille 13 - France
Total Affiliations: 4
Document type: Journal article
Source: Astronomy & Astrophysics; v. 517, JUL 2010.
Web of Science Citations: 14
Abstract

Context. The Abell 222 and 223 clusters are located at an average redshift z similar to 0.21 and are separated by 0.26 deg. Signatures of mergers have been previously found in these clusters, both in X-rays and at optical wavelengths, thus motivating our study. In X-rays, they are relatively bright, and Abell 223 shows a double structure. A filament has also been detected between the clusters both at optical and X-ray wavelengths. Aims. We analyse the optical properties of these two clusters based on deep imaging in two bands, derive their galaxy luminosity functions (GLFs) and correlate these properties with X-ray characteristics derived from XMM-Newton data. Methods. The optical part of our study is based on archive images obtained with the CFHT Megaprime/Megacam camera, covering a total region of about 1 deg(2), or 12.3 x 12.3 Mpc(2) at a redshift of 0.21. The X-ray analysis is based on archive XMM-Newton images. Results. The GLFs of Abell 222 in the g' and r' bands are well fit by a Schechter function; the GLF is steeper in r' than in g'. For Abell 223, the GLFs in both bands require a second component at bright magnitudes, added to a Schechter function; they are similar in both bands. The Serna \& Gerbal method allows to separate well the two clusters. No obvious filamentary structures are detected at very large scales around the clusters, but a third cluster at the same redshift, Abell 209, is located at a projected distance of 19.2 Mpc. X-ray temperature and metallicity maps reveal that the temperature and metallicity of the X-ray gas are quite homogeneous in Abell 222, while they are very perturbed in Abell 223. Conclusions. The Abell 222/Abell 223 system is complex. The two clusters that form this structure present very different dynamical states. Abell 222 is a smaller, less massive and almost isothermal cluster. On the other hand, Abell 223 is more massive and has most probably been crossed by a subcluster on its way to the northeast. As a consequence, the temperature distribution is very inhomogeneous. Signs of recent interactions are also detected in the optical data where this cluster shows a ``perturbed{''} GLF. In summary, the multiwavelength analyses of Abell 222 and Abell 223 are used to investigate the connection between the ICM and the cluster galaxy properties in an interacting system. (AU)

FAPESP's process: 08/04318-7 - Intracluster gas enrichment and star formation efficiency in clusters of galaxies
Grantee:Tatiana Ferraz Laganá
Support type: Scholarships in Brazil - Post-Doctorate
FAPESP's process: 06/56213-9 - New physics from space: formation and evolution of structures in the universe
Grantee:Claudia Lucia Mendes de Oliveira
Support type: Research Projects - Thematic Grants