Dust distributions in the Three-Giants configuration case: in the left panels, the velocity of the gas used as an input for the dust evolution model is the averaged velocity as presented in Fig. A.7; in the right panels, the gas velocity is taken to be null. The first row presents the integrated dust distribution along all the dust sizes, representingthe total dust distribution in the disk, whereas the second row presents the classic dust distributions as in Sect. 3.1. The presence of spikes in the left panel shows that the radial gas velocities are indeed responsible for the dust accumulations in additional rings exterior to the positions of the planets.