Star formation, radio sources, cooling x-ray sas, and galaxy interactions in the brightest cluster galaxy in 2A0335+096

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Title: Star formation, radio sources, cooling x-ray sas, and galaxy interactions in the brightest cluster galaxy in 2A0335+096
Author: Donahue, Megan; Ming, Sun; O'Dea, Christopher; Voit, G. Mark; Cavagnolo, Kenneth
Abstract: We present deep emission-line imaging taken with the new SOAR Optical Imaging Camera of the brightest cluster galaxy (BCG) in the nearby (z = 0:035) X-ray cluster of galaxies 2A0335+096. We also present our analysis of additional, multi-wavelength observations for the BCG, including long-slit optical spectroscopy, archival VLA radio data, Chandra X-ray imaging, and XMM UVimaging. Cluster 2A0335+096 is a bright, cool-core X-ray cluster, once known as a cooling ow. Within the highly disturbed core revealed by Chandra Xray observations, 2A0335+096 hosts a luminous and highly structured optical emission-line system, spanning the brightest cluster galaxy (BCG) and its companion. We con rm that the redshift of the companion is within 100 km s􀀀1 of the BCG and has certainly interacted with the BCG, and is likely bound to it. The comparison of optical and radio images shows curved laments in H emission surrounding the newly resolved radio source. The velocity structure of the emission-line bar between the BCG nucleus and the companion galaxy provides strong evidence for an interaction between the BCG and its northeast companion in the last 50 million years. The age of the radio source is similar to the interaction time, so this interaction may have provoked an episode of radio activity. We estimate a star formation rate of & 7 M yr􀀀1 from the H and archival UV arXiv:0705.1659v1 [astro-ph] 11 May 2007 { 2 { data. This rate is similar to, but somewhat lower than, the revised X-ray cooling rate of 10􀀀30 M yr􀀀1 in the vicinity of the BCG, estimated from XMM spectra by Peterson et al. (2003). The H nebula is limited to a region of high X-ray surface brightness and cool X-ray temperatures. However, the detailed structures of H and X-ray gas di er. The peak of the X-ray surface brightness is not the peak of H emission, nor does it lie in the BCG. The estimated age of the radio lobes and their interaction with the optical emission-line gas, the estimated timescale for depletion and accumulation of cold gas, and the dynamical time in the system are all similar, suggesting a common trigger mechanism.
Description: Also archived in: arXiv:0705.1659 v1 May 11 2007RIT community members may access full-text via RIT Libraries licensed databases:
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Date: 2007-05-10

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