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Fig. 11.

image

Panel a: 0.3–1.2 keV Chandra ACIS-S soft X-ray emission (contours) superimposed on the [O III] (green) and Hα (red) emission fitted from the star-subtracted smoothed MUSE data cube (same as in Fig. 4(a)). Panel b: soft X-ray emission extracted from the yellow polygonal region in Fig. 9. The data are in black, resulting from the merging of the six extracted spectra. Red is the best fit, having used a thermal emission model. The residuals are reported on the bottom. The labeled blue lines on top indicate the statistically significant (at 95% level) emission lines in the Chandra HETG spectra, after accounting for the collisional component, from Nardini et al. (2015a). Panel c: unsmoothed 0.3–0.4 keV emission and [O III] contours from MUSE, zooming in the central regions of MUSE FOV. Panel d: spectrum extracted from the inner contour of [O III] in panel c (excluding the nucleus)

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