From top to bottom and from left to right: Hα, Hβ, [O II], [O III], [N II], and [S II] observed (i.e., dust extincted) luminosity functions of the main-ELG sample (full black dots). The contributions of ELGs classified in different ways are shown by empty colored markers, with colors as indicated in the legend. We compare our results – both tabulated in Appendix B and at the CDS – with several observed published measurements in the local Universe: Hα ELGs from Ly et al. (2007) at z = 0.07 − 0.09, Gilbank et al. (2010) at 0.032 < z < 0.2, Pirzkal et al. (2013) at 0 < z < 0.5, and Hα AGN from Schulze et al. (2009) at z < 0.3; Hβ ELGs from Comparat et al. (2016) at z = 0.3, Hβ AGN from Schulze et al. (2009) at z < 0.3; [O II] ELGs from Gilbank et al. (2010) at 0.032 < z < 0.2, Gallego et al. (2002) at z ≤ 0.045, Comparat et al. (2015) at z = 0.17, and Pirzkal et al. (2013) at 0.5 < z < 1.5; [O III] ELGs from Comparat et al. (2016) at z = 0.3, from Pirzkal et al. (2013) at 0.1 < z < 0.9, and [O III] AGN from Bongiorno et al. (2010) at 0.15 < z < 0.92. We overplot our Saunders fits as lines; the parameters are in Table 3 and were obtained considering only the points above the luminosity completeness thresholds discussed in Sect. 2.5 and Appendix A and represented as cyan shades in the panels (for those lines whose completeness limit falls within the L range shown in the figure). The error bars are computed from 50 jackknife resamplings (see Sect. 5.2).