BPT (top; Baldwin et al. 1981) and WHaN (bottom; Cid Fernandes et al. 2010, 2011) diagnostic diagrams. The dots represent the flux values at the centre (left) or median values at a galactocentric distance of R = 1 HLR (right), coloured by the measurements of EW(Hα) (top) or by morphological type (bottom). The grey shadow on the left shows the distribution of the values of all pixels of all galaxies. On the right, the blue distribution corresponds to the late-type galaxies (LTGs; Sa, Sb, Sc or Sd) and the red to the earl- type galaxies (ETGs; E or S0). The transparency of the colour of both morphological distributions is normalised to the total distribution, as in the panels of the left column. The dotted and dashed lines demarcate the limit between star formation and AGN following the criteria of Kauffmann et al. (2003) and Kewley et al. (2006), respectively. The continuous line differentiates Seyferts from LINERs (Schawinski et al. 2007). The dashed-dotted lines in the two bottom panels mark the retired galaxies (EW(Hα) < 3). Measurements below this limit are coloured black in the top panels.