Cartoon depicting the variations induced in the M_★ (left) and SFR (right) completeness limits by changes in the shape of the completeness function (black line). We plot some hypothetical SFR and M_★ limits as dashed lines. The hatched green region encloses the SFR and M_★ values above both completeness limits. The hatched blue region highlights the locus of galaxies that would be detected thanks to their high SFR, but that lie below the M_★ limit. The hatched orange region contains galaxies above the M_★ limit that would be hard to detect because of their low SFR. The white region is occupied by galaxies that are below the M_★ and SFR limits. In yellow (pink), we show how the curve should change in order to increase (decrease) both the M_★ and SFR limits independently. Histograms above each panel exemplify how changes in M_★ or SFR completeness would affect our final sample. Bins are color-coded according to the regions they would occupy in the log SFR−log M_★ plane. We display two mirrored histograms, showing galaxies that lie above (blue and green) and below (white and red) the SFR limit. The quiescent or dormant histogram is centered at a lower M_★, as bursty star formation rules at lower M_★ (i.e., quiescence is not permanent and these galaxies should be included in an MS analysis). At higher M_★ galaxies that fall below the MS are more prone to remain quiescent, and thus would be discarded through UVJ and sSFR cuts. Vertical and horizontal lines are color-coded following the bottom panels. The last two histograms exemplify how objects would move from the top to the mirrored histograms, and vice versa, as we change the SFR limit.