Comparison between the remaining sample of galaxies once the g-band fraction or aperture correction criteria are considered. Left:g-band flux fraction covered within the fiber with respect to the total magnitude (“modelMag” in the SDSS catalogue) of the galaxy. The horizontal line at 0.2 corresponds to the cut suggested by Kewley et al. (2005) and used in D’Andrea et al. (2011) and Wolf et al. (2016) to justify that objects below the line on the shaded region have spectra that are not representative of the whole galaxy and therefore were excluded from those analyses. Middle:g-band fiber flux fraction vs. radii of the galaxy normalized to the Petrosian R₅₀ radius (radius of a circle that contains 50% of the galaxy light). The horizontal line is the Kewley et al. (2005) limit, under which all objects (in the shaded region) would be excluded. The vertical line corresponds to the range where our aperture corrections are applied, and objects in the shaded region to the left (r/R₅₀ < 0.3) are excluded because Iglesias-Páramo et al. (2013, 2016) corrections cannot be applied. We note that those galaxies with r/R₅₀ ≥ 0.3 (to the right of the vertical line) but a g-band fiber flux fraction lower than 0.2 (below the horizontal line) would have been excluded but are included in this work. Right: normalized radii (r/R₅₀) of the galaxies vs. redshift. Dots with black edges correspond to the 159 objects that we would have discarded using the g-band fraction criterion. In our selection we have mostly lost galaxies at low redshifts.