Notable parameter spaces where the combination of morphological metrics separate well different morphologies. In each panel, the red line corresponds to the line of best separation, which corresponds to the minimal contamination 𝒞_min (defined in Appendix C), and the light red area indicates other possible line positions which achieve contamination within 0.01 of the minimal contamination, i.e., C ∈ (𝒞_min, 𝒞_min + 0.01). Left: Gini vs. M₂₀ plane for galaxies with and without bulges. The line G = −0.52M₂₀ − 0.4, separates the main cluster of galaxies with bulges (71%) and those without bulges (74%). Middle: Gini vs. M₂₀ plane for galaxies identified as interacting/mergers. The line G = −0.29M₂₀ + 0.07 (red) shows a systematic separation of the cluster of data points in this parameter space, with 50% of visually classified mergers and 93% of nonmergers correctly separated. For comparison, we show with the black dashed line the boundary line established by Lotz et al. (2008) and discuss the difference in the main text. Right: Gini vs. asymmetry A plane for clumpy and nonclumpy galaxies. The separation line is given by G = 0.229A + 0.448, where 81.8% of clumpy galaxies are below the line and 64.1% of the nonclumpy galaxies are above.