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Fig. 2.


IC 5063. (a) [O III] flux integrated from the fitted profile in the velocity range ±|200–1000| km s−1 (blue when negative, i.e. approaching, red when positive, i.e. receding) with respect to the stellar velocity in each pixel (to avoid including the contribution to the flux from the gas that rotates in the disc). It shows the bulk of the high-velocity outflow. (b) [O III] W70 map, i.e. the difference between the 85th and 15th percentile velocities of the modelled line profile. The map has been re-smoothed with a Gaussian kernel having σ = 1 pixel for better visual clarity. The radio contours are the same as in Fig. 1c. Magenta circles indicate 4-spaxel radius extraction apertures of the spectra displayed in Fig. 3. (c) [O III]λ5007/Hβ vs. [S II]λλ6716,6731/Hα BPT diagram and (d) associated spatial distribution. The colour intensity in the diagram and the map is coded according to the [O III] W70. The solid curve defines the theoretical upper bound for pure star formation (Kewley et al. 2001). The dashed line represents the Kewley et al. (2006) demarcation between Seyfert galaxies and shocks or LI(N)ERs, while the dotted line is the Sharp & Bland-Hawthorn (2010) bisector line between AGN- and shock-ionisation. SF-dominated regions are then marked in blue, AGN-dominated ionisation in red, and purple and green mark shock-ionised or LI(N)ER regions. As in Fig. 1c, the maps are zoomed in the central 40″ × 40″ compared to the full-FOV image in Fig. 1b. An S/N cut of 3 has been applied to the maps, together with a cut on high velocity dispersions resulting from poor fits (see text for details).

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