Left: dust surface density profile of the best-fit radiative transfer model as a function of the distance to the star. The upper limit on the dust surface density (small + large grains) in the inner disk and the gap is overplotted (dotted line). Right: azimuthally averaged gas surface density profiles at various times in a gaseous disk perturbed by a 3.4 M_Jup planet. The green line is the initial gas surface density profile; the two thinner and faded solid lines represent the gas surface density profiles after 10 000 (~10⁵ yrs) and 100 000 orbits (~1 Myr), without including the planet.