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Fig. 14.


Composite HST F140W (red), F105W (green), and F606W (blue) images with contours from the smoothed Chandra surface brightness map (yellow dashed; upper right panel in Fig. 11) and from the 2.1 GHz ATCA data after subtraction of the core radio emission, and imaged using Briggs weighting with robust parameter equal to 0.00 and a uv-tapering at 10 kλ (white solid, covering the 3σ − 5.5σ range in steps of 0.5σ; upper panel of Fig. 5). The resulting synthesized beam is shown in the bottom right corner. We denote the position of the subtracted radio core model with a red ellipse, whose axes and position angle correspond to the synthesized beam of the uniformly weighted 2.1 GHz ATCA image used to subtract the core emission. The morphology of the central region of the extended radio emission, consistent with a wide-angle tailed radio galaxy (Sect. 4.1.1; Sakelliou & Merrifield 2000), appears to align in the same direction as the optical filament.

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