The comparison between the observed ΔR_pl,obs and synthetic ΔR_pl,model radius spread values as a function of planetary mass for the whole temperature range and for planets cooler or hotter than 956 K. Bottom panels: Comparison between the measured (squares) and synthetic (areas) spread in planetary radii as a function of planetary mass (ΔR_pl = R_pl,max – R_pl,min) for the entire sample (left), for planets cooler than 956 K (middle), and for planets hotter than 956 K (right). The relative values for the observed ΔR_pl distribution are listed in Tables B.1–B.3, respectively, but with the difference that for visualisation purposes, we combined neighbouring bins whose ΔR_pl values differed by less than 1% in the plots. In the high-mass range, the blue and black squares have been obtained by accounting and disregarding, respectively, planets affected by atmospheric inflation (i.e., planets with a radius larger than 11 R_⊕). The green area is for the basic scenario and accounts for the variability in the initial stellar rotation rate affecting atmospheric mass loss. The yellow area is for the migrated scenario, and thus it accounts for larger initial atmospheric mass fractions (assuming the host star was a slow rotator). To guide the eye, the dashed red line is a smoothed distribution of the black squares. Top panels: Histograms of the number of observed planets within each mass bin for the entire sample (left), for planets cooler than 956 K (middle), and for planets hotter than 956 K (right). The dark blue and bright blue areas account for and disregard, respectively, planets affected by atmospheric inflation.