Monte Carlo sampling plot of the planet mass vs. the stellar mass, with the ice line planet formation model (scenario A) in the left, the log-uniform distributed planet formation model (scenario B) in the right, α_t = 10⁻³ in the top and α_t = 10⁻⁴ in the bottom. The color corresponds to the water mass fraction in the planetary core. The black line represents the characteristic mass of the simulated super-Earths, set by the pebble isolation mass from Eq. (39). The M_p − M_⋆ scaling is almost insensitive to the explored disk turbulent α_t values and embryos’ birth locations r₀. The planet with moderate water fraction can form from the water ice line in less turbulent disks. Planets formed over a wide range of disk distances end up with a distinctive, bimodal water mass distribution.