We present the results of a detailed analysis of the XMM-Newton observation of the galaxy cluster Abell 3921. The X-ray morphology of the cluster is elliptical, with the centroid offset from the brightest cluster galaxy by 17´´, and with a pronounced extension toward the NW. Subtraction of a 2D β-model fit to the main cluster emission reveals a large scale, irregular residual structure in the direction of the extension, containing both diffuse emission from the intra cluster medium, and extended emission from the second and third-brightest cluster galaxies (BG2 and BG3). The greatest concentration of galaxies in the subcluster lies at the extreme northern edge of the residual. The cluster exhibits a remarkable temperature structure, in par...
Aims. We study the X-ray morphology and dynamics of the galaxy cluster Abell 514. Also, the relation...
Aims: We study the X-ray morphology and dynamics of the galaxy cluster Abell 514. Also, the relation...
We have observed the cluster of galaxies Abell 85 with XMM-Newton. These data have allowed us to con...
We present the results of a detailed analysis of the XMM-Newton observation of the galaxy cluster A...
We present the results of a detailed analysis of the XMM-Newton observation of the galaxy cluster Ab...
Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) that exhibit...
Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) th...
(Abridged) The galaxy cluster Abell 2218, at z=0.171, is well-known for the discrepancy between mass...
We present structural analysis results of Abell 0141 (z = 0.23) based on X-ray data. The X-ray lumin...
We present the Chandra analysis of the rich galaxy cluster Abell 521 ($z=0.247$). The high resoluti...
We have observed the cluster of galaxies Abell 85 with XMM-Newton. These data have allowed us in a p...
Context. A 2163 is among the richest and most distant Abell clusters, presenting outstanding prop...
International audienceAims. We present the joint analysis of the X-ray and Sunyaev–Zel’dovich (SZ) s...
Abell 3266 is one of the X-ray brightest galaxy clusters in the sky and is a well-known merging syst...
Aims. We present the results of a joint XMM-Newton and NuSTAR observation (200 ks) of the galaxy clu...
Aims. We study the X-ray morphology and dynamics of the galaxy cluster Abell 514. Also, the relation...
Aims: We study the X-ray morphology and dynamics of the galaxy cluster Abell 514. Also, the relation...
We have observed the cluster of galaxies Abell 85 with XMM-Newton. These data have allowed us to con...
We present the results of a detailed analysis of the XMM-Newton observation of the galaxy cluster A...
We present the results of a detailed analysis of the XMM-Newton observation of the galaxy cluster Ab...
Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) that exhibit...
Located at z = 0.203, A2163 is a rich galaxy cluster with an intra-cluster medium (ICM) th...
(Abridged) The galaxy cluster Abell 2218, at z=0.171, is well-known for the discrepancy between mass...
We present structural analysis results of Abell 0141 (z = 0.23) based on X-ray data. The X-ray lumin...
We present the Chandra analysis of the rich galaxy cluster Abell 521 ($z=0.247$). The high resoluti...
We have observed the cluster of galaxies Abell 85 with XMM-Newton. These data have allowed us in a p...
Context. A 2163 is among the richest and most distant Abell clusters, presenting outstanding prop...
International audienceAims. We present the joint analysis of the X-ray and Sunyaev–Zel’dovich (SZ) s...
Abell 3266 is one of the X-ray brightest galaxy clusters in the sky and is a well-known merging syst...
Aims. We present the results of a joint XMM-Newton and NuSTAR observation (200 ks) of the galaxy clu...
Aims. We study the X-ray morphology and dynamics of the galaxy cluster Abell 514. Also, the relation...
Aims: We study the X-ray morphology and dynamics of the galaxy cluster Abell 514. Also, the relation...
We have observed the cluster of galaxies Abell 85 with XMM-Newton. These data have allowed us to con...