Light concentration (top), image asymmetry (middle top), Gini coefficient (middle bottom), and moment of light (bottom) as a function of stellar mass. We add to all panels the relation for the global sample at M_⋆ >  10¹⁰ M_⊙ as empty grey squares. In each panel, we show the Spearman correlation coefficient, ρ, and the corresponding probability of an uncorrelated dataset having the same distribution in parenthesis (considering only M_⋆ >  10¹⁰ M_⊙). We find quiescent galaxies to have a higher concentration of light than star-forming galaxies at similar stellar masses. We also find quiescent galaxies to have less disturbed profiles at stellar masses greater than 10¹⁰ M_⊙. This is likely a reflection of the lack of star formation that is clumpier in nature (Conselice 2003). We also find quiescent galaxies to have their light concentrated on a smaller area (higher value of G) than star-forming galaxies at similar stellar masses. Finally, quiescent galaxies are smoother (lower values of M₂₀) at all stellar masses, as also seen in the asymmetry parameter.