Top panel: radius of giant planets as a function of their stellar insolation flux S_eff. The open circles indicate the secured planets, the Epen squares the likely ones, and the dots the non-Kepler objects. The solid line represent the best model of Eq. (7) and the grey regions represent the 1, 2, 3σ (from dark to light grey) confidence interval for this best model, as described by the covariance matrix provided in Eq. (8). Bottom panel: normalised cumulative distribution (CDF) of the radius of giant planets listed in Table B.7 for objects receiving more (dashed thick line) or less (solid thick line) insolation flux than 10⁸ erg cm^-2 s^-1. The prediction from Mordasini et al. (2012b) is shown for comparison (age of 5 Gyr – solid thin line). This prediction is for planet with orbit >0.1 au, which correspond to 1.4 × 10⁸ erg cm^-2 s^-1 for a Sun-like star.