Application of V0, V1, and V2 stellar abundance estimates: cdfs of sampled 1D marginal posterior (green to blue) and prior (red) for HD 219134b, 55 Cnc e^S, 55 Cnc e^L, and HD 97658b: a) m_water, c) r_mantle, d) r_c, and e) Fe/Si_mantle. Posterior cdfs refer to the different host star abundance estimates (V1 – iron rich, V2 – iron poor) listed in Table 3. The dashed lines are the 95% lower and upper confidence bounds, which almost completely overlap the solid lines. Depending on the stellar abundance proxy estimates, the upper prior bound in e) differs, which is indicated by the vertical colored lines corresponding to the respective proxy.