Illustration of the differences in interior models between the previous work (Baumeister et al. 2020, black line) and this work (blue and red lines, for two different equilibrium temperatures T_eq = 100K and T_eq = 1000K, respectively). The figure shows density profiles of a representative 5 M_⊕ planet with w_Core = 0.2, w_Mantle = 0.49, w_Water = 0.3, and w_Gas = 0.01 (Panel a). Panel b shows a zoomed-in view of only the water and atmosphere layers. The dashed lines mark the respective planets’ radii.