Five examples of spectra illustrating our fitting method. For each object, we show on the left the spectrum (black curve) and the best-fit model (red curve). Central and right panels show the zoomed regions around the Hβ and Hα emission, respectively. The dashed vertical lines indicate the location of Hβ, [O III] doublet, Hα, [N II], and [S II] doublets. Best-fit NC and BC profiles are highlighted with green curves (panels a) to e)); OC and Fe II emission are shown with blue (panels a) to e)) and magenta (panel a)) curves, respectively. Finally, black Gaussian profiles (in panel e)) show a second set of NC used to fit doublet peaked galaxies. In the rows the spectra of various AGN types are shown. From top to bottom, the plots represent a) a blue spectrum of a type 1 AGN with broad BLR Lorentzian profiles, Fe II emission, and blue wings associated with outflows; b) a reddened type 1 AGN without evidence of outflow; c) a low-luminosity broad line AGN, whose continuum is dominated by stellar emission, in which we observe a complex BLR Hα profile, modelled with two strong BC and no BLR Hβ emission; d) a candidate type 2 AGN without evidence of BLR emission but with strong emission from outflowing gas detected for all the optical emission lines; and e) a candidate type 2 AGN with double peaked emission lines and an outflow component.