Similar to Fig. 2, but assuming the inter-correlated IBP derived by MD17. Analogous to what we have found while adopting an IBP draw from flat distributions, any combination of the parameters such that K ≳ 50 and η ≳ 50 is able to reasonably well explain the huge reduction of systems at ∼0.5 M_⊙. However, with a more realistic IBP, we can also reproduce the high fraction of systems for M dwarf masses ≲0.3 M_⊙.