Distribution of galaxies in the KS plane at different redshifts (rows) and in four equally populated stellar mass quartiles at each redshift (columns). The mass range of each quartile is shown in square brackets (in log M_⊙). The colors indicate the sSFR of the galaxies, measured over a timescale of 10 Myr. Dash-dotted lines are fits at each redshift and mass bin, with the slopes (a) and the standard deviation of residuals of the best-fit relation (σ) shown in the lower-right corners. The coefficient R, shown at the bottom right of each panel, is the Pearson correlation coefficient. The solid black and dotted black lines show the sequence of disks and starbursts, respectively, from Daddi et al. (2010) for reference. Note, however, that our fitting method differs from theirs. Regardless of stellar mass, the distributions of galaxies move within the KS plane toward lower values of Σ_H2 and Σ_SFR with decreasing redshift. At each redshift and in each stellar mass bin, the sSFR of galaxies strongly correlates with Σ_SFR. Figure A.1 shows the same but using the neutral gas.