Distribution of galaxies in the M_H2–SFR plane, i.e., a deprojected version of the KS plane, at redshifts 4, 3, 2, 1, and 0.25, from left to right, as a function of galaxy mass (top) and effective radius (bottom). Dash-dotted lines are fits in the logarithmic space at each redshift, with the slope, a, and the standard deviation of residuals, σ. The coefficient R is the Pearson correlation coefficient. At all redshifts, more massive galaxies tend to have higher SFRs and M_H2 values compared to their lower-mass counterparts. As galaxies grow in mass, they also grow in size; however, no obvious correlation is seen between R_eff, the SFR, and the molecular gas mass.