Resulting planet population for three solar-mass stars of varying composition. At low metallicity, it is difficult to form any planets beyond a few AU in the protoplanetary disc, so very few water-rich planets above 1 M_⊕ form in that case. For solar metallicity and above (middle and bottom panels), we start to form water-rich planets up to around a few M_⊕ far out in the disc. We note that due to our abundance scaling of the remaining elements, the middle panel has a slightly higher metallicity of 0.016 for solar [Fe/H] compared to the solar metallicity of 0.014.