Size–mass relation of BGGs using sSFR-only classification. Each panel shows results for a redshift bin of width Δz = 0.5 spanning z = 0 to z = 3.7. Star-forming and quiescent BGGs are identified based on whether their log₁₀(sSFR) falls above or below the redshift-dependent threshold log₁₀(0.2/t_obs), where t_obs is the age of the universe in Gyr. As in previous figures, dashed (SFGs) and solid (QGs) lines show best-fit power-law relations, and shaded regions represent 1σ confidence intervals. The sSFR-based method yields similar trends but may misclassify dusty SFGs at intermediate redshift. Results from Faisst et al. 2017 are shown as cyan dashed-dotted (SFGs) and orange dotted (QGs) lines in matching redshift bins for comparison. While dashed lime and dashed magenta lines show van der Wel et al. 2014 results.