XMM-Newton and Chandra Observations of Abell 2626
Physics and Astronomy
We present a detailed analysis of the XMM-Newton and Chandra observations of Abell 2626 focused on the X-ray and radio interactions. Within the cooling radius of ˜ 70 kpc, we find considerable substructure, which is probably the result of effects of the central radio source. From the radio image of Abell 2626, the most unusual features are the two elongated radio bars to the north and south of the radio core. Their symmetric positions suggests they are radio lobes, which further suggests that these features are candidates for cooling core X-ray/radio bubbles. However, we find that there is no obvious correlation between the radio bars and the X-ray image. The X-ray image residual map shows that the southern radio bar lies in a region with a slight X-ray excess, while the northern one lies in both regions of X-ray excess and deficit. A cool extension connects the central core to the southern bar, but there is no similarly strong feature to the north. The hardness ratio map shows that the southern bar appears to be located in a hotter region, while the X-ray emission near the northern bar appears soft. Thus, the morphology of Abell 2626 is different from that of the standard cooling core X-ray/radio bubbles, which may indicate that the situation in Abell 2626 is much more complicated than in simpler systems. Thus, Abell 2626 provides a challenging problem for studying cooling core --- radio source interaction. Besides the study of the X-ray and radio interaction, we also studied various interesting structures in Abell 2626, such as possible subclusters, possible AGNs, and an SO galaxy. We find a possible alignment of X-ray substructure in the cluster with the Perseus-Pegasus supercluster filament, and suggest that Abell 2626 is preferentially accreting subclusters and groups from this large-scale structure.
XMM-Newton and Chandra Observations of Abell 2626. Wong, K.-W., Sarazin, C. L., Blanton, E. L., & Reiprich, T. H. American Astronomical Society Meeting, 207, No.177; Bulletin of the American Astronomical Society, Vol. 37, p1450.
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