Mass function of our simulations using the B15b approach compared with the results presented in Mayor et al. (2011), for planets with a_final > 0.1 AU. The upper graph represents the simulations with embryos starting at t = 1.5 Myr of the evolution of the disc and the lower one the embryos starting after t = 2 Myr. The green line represents the results presented in Mayor et al. (2011), the black line shows all the planets we form beyond 0.1 AU, and the purple one indicates the planets considered as observed once the detection probability is applied.