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Fig. 11.

image

Comparison of the SZ effect (upper left), smoothed X-ray surface brightness (upper right), signal-to-noise map of the weak-lensing convergence (middle left; Kim et al. 2019), X-ray hardness ratio (middle right) maps, and EMU (lower left) and ATCA (lower right) images for SPT-CL J2106-5844. The black contours appearing in all panels represent the unfiltered SZ model derived in Sect. 3.2.3. To facilitate comparison between the main cluster features, we overlay to the Chandra, EMU, and ATCA the same contours as in Figs. 1, 3, and 5, respectively, while the ones for the mass distribution reproduce the contours in Fig. 6 of Kim et al. (2019). The symbols in all the maps denote the positions of the BCG (triangle; Song et al. 2012), the peak in the galaxy number density (circle; Kim et al. 2019), and the SZ centroid as measured by SPT (diamond; Bleem et al. 2015). The two SZ features can be seen to correspond to two weak-lensing mass peaks, as well as mildly soft components of the X-ray emission, in turn corresponding to the X-ray peak and the southern extension. We note that, interestingly, the curved morphology of the southern feature in the SZ dirty image (thick black contours in the middle right panel) appears to trace an arc-shaped patch of hard X-ray emission.

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