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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

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

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Autor(es):
Durret, F. [1, 2] ; Lagana, T. F. [3] ; Adami, C. [4] ; Bertin, E. [1, 2]
Número total de Autores: 4
Afiliação do(s) autor(es):
[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
Número total de Afiliações: 4
Tipo de documento: Artigo Científico
Fonte: Astronomy & Astrophysics; v. 517, JUL 2010.
Citações Web of Science: 14
Resumo

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)

Processo FAPESP: 08/04318-7 - Enriquecimento do gás intra-aglomerado e a eficiência de formação estelar em aglomerados de galáxias
Beneficiário:Tatiana Ferraz Laganá
Linha de fomento: Bolsas no Brasil - Pós-Doutorado
Processo FAPESP: 06/56213-9 - Nova física no espaço: formação e evolução de estruturas no universo
Beneficiário:Claudia Lucia Mendes de Oliveira
Linha de fomento: Auxílio à Pesquisa - Temático