Outflow velocity as given by (see explanation in Sect. 4.1) inferred from [OIII] (upper panel) and Hα emission (bottom panel), plotted as a function of SFR, stellar velocity dispersion (as obtained from the fit to the stellar continuum), and sSFR. The same bins as Fig. 17 are plotted, excluding those for which . In the middle panels, the dashed lines indicate the locus of points where v_out = σ_stars. The Spearman rank correlation coefficient (0 <ρ< 1, higher values of ρ indicate stronger correlation) is reported for each plot, along with the corresponding two-sided p value (if the p value is ≤ α, where α = 0.05 is the level of significance, the observed correlation is statistically significant).