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Fig. 5.


Spatially resolved BPT diagrams (left) of NGC 1365 and corresponding spatial distribution (right), obtained from the fit of the star-subtracted Voronoi-binned cube (so as to have an average signal-to-noise ratio of at least 4 per bin in each wavelength channel around Hβ). The N-BPT ([N II]λ6584/Hα vs. [O III]λ5007/Hβ, upper panels), S-BPT ([S II]λλ6716,6731/Hα vs. [O III]λ5007/Hβ, central panels), and O-BPT ([O I]λ6300/Hα vs. [O III]λ5007/Hβ, lower panels) diagrams for each bin with S/N > 3 in each line are shown on the left, while the corresponding maps are reported on the right (each bin in the maps corresponds to a single dot in the diagrams). The solid curves in the diagrams define the theoretical upper bound for pure star formation (Kewley et al. 2001), while the dashed one in the N-BPT is the Kauffmann et al. (2003) empirical classification, and all bins under this curve are star-formation dominated. Finally, the dashed line in S-BPT and O-BPT diagrams separates Seyfert galaxies from LI(N)ERs (Kewley et al. 2006). SF-dominated regions are then marked in blue, Seyfert-type ionization is displayed in red, green marks LI(N)ER regions in the S-BPT and O-BPT, while light blue denotes composite regions in the N-BPT lying between Kewley et al. (2001) and Kauffmann et al. (2003) curves. A 6px-radius circle around the center has been masked, because of BLR contamination (see text).

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