Monte Carlo sampling plot of the planet mass vs. the stellar metallicity, 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 stellar mass. The gray dashed lines represent the averaged metallicities for the planets with M_p ≤ 20 M_⊕ and M_p > 20  M_⊕. The formation of low-mass planets (M_p ≤ 20 M_⊕) is barely dependent on the stellar metallicity, whereas massive planets (M_p > 20  M_⊕) prefers to grow in metal-rich systems.