Mass of planetesimals formed in the dust trap generated by a planet at 10 au by the end of our simulations for a range of viscosity α_visc, local turbulence δ_turb and planet mass M_p. We see that under specific conditions, dust traps can be strong enough to form planetesimals. In that case, a large fraction of the available outer disc dust mass (see Fig. 5) may be transferred into planetesimals.