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Published December 2010 | Published
Journal Article Open

Spitzer observations of A1763. II. Constraining the nature of activity in the cluster-feeding filament with VLA and XMM-Newton data

Abstract

The A1763 superstructure at z = 0.23 contains the first galaxy filament to be directly detected using mid-infrared observations. Our previous work has shown that the frequency of starbursting galaxies, as characterized by 24μm emission is much higher within the filament than at either the center of the rich galaxy cluster, or the field surrounding the system. New Very Large Array and XMM-Newton data are presented here. We use the radio and X-ray data to examine the fraction and location of active galaxies, both active galactic nuclei (AGNs) and starbursts (SBs). The radio far-infrared correlation, X-ray point source location, IRAC colors, and quasar positions are all used to gain an understanding of the presence of dominant AGNs. We find very few MIPS-selected galaxies that are clearly dominated by AGN activity. Most radio-selected members within the filament are SBs. Within the supercluster, three of eight spectroscopic members detected both in the radio and in the mid-infrared are radio-bright AGNs. They are found at or near the core of A1763. The five SBs are located further along the filament. We calculate the physical properties of the known wide angle tail (WAT) source which is the brightest cluster galaxy of A1763. A second double lobe source is found along the filament well outside of the virial radius of either cluster. The velocity offset of the WAT from the X-ray centroid and the bend of the WAT in the intracluster medium are both consistent with ram pressure stripping, indicative of streaming motions along the direction of the filament. We consider this as further evidence of the cluster-feeding nature of the galaxy filament.

Additional Information

© 2010 American Astronomical Society. Received 2010 January 15; accepted 2010 September 24; published 2010 November 9. We thank the scientific staff at the NRAO, in particular G. Van Moorsel for help with observation planning and F. Owen for help with data reduction techniques. We thank A. Biviano for his reading and comments on this manuscript and for constructing the FIR SEDs. We also thank the anonymous referee for extremely helpful comments that contributed to a much improved version of this paper. Support for this work was provided by NASA through an award issued by JPL/Caltech. This work is based in part on original observations using the Very Large Array operated by the NRAO. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is also based in part on archival observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA and observations made with Spitzer, a space telescope operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, then Participating Institutions, the National Science Foundation, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions (see list at http://www.sdss.org/collaboration/credits.html). We have made use of the ROSAT Data Archive of theMax-Planck-Institut für extraterrestrische Physik (MPE) at Garching, Germany as well as the XMM-Newton Data Archive. Facilities: Spitzer (IRAC, MIPS), VLA, XMM, WIYN (Hydra)

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August 19, 2023
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