Artículos de revistas
The clusters Abell 222 and Abell 223: a multi-wavelength view
Fecha
2010Registro en:
ASTRONOMY & ASTROPHYSICS, v.517, 2010
0004-6361
10.1051/0004-6361/201014566
Autor
DURRET, F.
LAGANA, T. F.
ADAMI, C.
BERTIN, E.
Institución
Resumen
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.
Ítems relacionados
Mostrando ítems relacionados por Título, autor o materia.
-
Analysis of aeronautical clusters referring to the development of the Colombian aerospace cluster
Bello Zapata, Andrés Felipe -
Analysis of Most Representative Aerospace Cluster Models Worldwide and Their Incidence for the Development of Valle del Cauca Aerospace Cluster
López Martínez, Wilson Estiven; Morante Granobles, Diego Fernando -
Clúster y coo-petencia (cooperación y competencia) industrial: algunos elementos teóricos por considerar
GARCÍA GARNICA, ALEJANDRO; LARA RIVERO, ARTURO A.