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tokens: concentration and asymmetry derived with pyca ; and (11) [O iii ] luminosity in units of 10 40 erg s −1 . Table 2. Control sample parameters. (1) identification of the AGN host associated with the control galaxy; (2)–(12) same as (1)–(11) of Table 1 . Twelve control sample objects have been paired to more than one AGN hosts and appear more than once in the table. In order to assess quantitatively the morphological variety of the AGN and control samples, we have derived the concentration index C and asymmetry index A of the sample galaxies using the publicly available code pyca (Menanteau et al. 2005 ). This calculation was made using the r -band images in order to maximize the galaxy signal-to-noise ratio. We have also obtained for all galaxies of the sample the morphological classifications from GZ1 (Lintott et al. 2011 ). From the GZ1 classification probabilities, we have separated the galaxies in four large classes: ellipticals (E), spirals (S), merging (M) and intermediate elliptical/spiral (E/S); this last class corresponds to galaxies whose GZ1 elliptical and spiral probabilities are rigorously the same and exceed 50 per cent when combined. Most of the 62 AGN in our sample have luminosities erg s −1 , with only 17 having larger luminosities. We use this threshold – postulated by Kauffmann et al. ( 2003 ) – to characterize these 17 AGNs as ‘strong AGN’. SDSS-III ugriz negative images (Fukugita et al. 1996 ) of the four most luminous of these strong AGNs are shown in Fig. 1 ; the remainder are available online. Figure 1. SDSS-III ugriz negative images of the four strongest AGN from our sample (left-hand columns) and their control sample equivalents (centre and right-hand columns). The mangaID of each host is indicated above its respective panel. Each chart is 51 arcsec on a side; north is up, east to the left. Inspection of the SDSS-III spectra showed that most of the strong AGN in our sample present coronal lines: at least one of the lines [NeV] λ3425 Å, [FeV ii ] λ3760 Å or [FeX] λ6374 Å are detectable above 3σ. A small number of objects among the most [O iii ]-luminous ‘weak AGN’ also present some of these lines. Coronal lines are thought to be produced by photoionization from the AGN (Mazzalay, Rodríguez-Ardila Komossa 2010 ; Rodríguez-Ardila et al. 2011 ) and to be associated with outflows (Müller-Sánchez et al. 2011 ). Being insensitive to star formation as opposed to the [O iii ] λ5007 Å, the presence of coronal lines reinforces the AGN nature of the 17 most [O iii ]-luminous objects in our sample, and suggests a transition between high- and low-ionization AGN at erg s −1 , in concordance with Kauffmann et al. ( 2003 ). We note that our AGN selection is based on single-fibre SDSS-III observations, which limits us to sources with AGN-photoionization signatures within 3 arcsec of the galactic centre. Wylezalek et al. (in preparation) has recently developed an AGN selection algorithm taking full advantage of the spatial dimension of