Evidence for AGN Feedback in Galaxy Clusters and Groups
Figure 3
(a) 1.4 GHz VLA radio contours (obtained by combining observations in A-, B-, and C-array configurations) overlaid onto the smoothed 0.5–2.0 keV Chandra X-ray image of the galaxy cluster RBS 797. The combined radio map has a resolution of , and is able to reveal the morphology of the central radio source, showing its elongation in the cavity direction (see Figure 1(b)), without losing sensitivity at the larger scales. In particular, the extended radio emission is detected out to ~90 kpc. By subtracting the contribution of the central nuclear source, the residual flux density of the diffuse radio emission is mJy, indicating the likely presence of a radio mini-halo. (b) Integrated radio power at 1.4 GHz, , versus cooling flow power, , for the mini-halo clusters which have relevant X-ray and radio data available (data from [111, 183–186]).
