Results from hydrodynamical simulations performed with FARGO3D assuming a planet-to-star mass ratio of 4 × 10⁻³ (10 M_Jup around a 2.5 M_⊙ star) at 60 au and ~0.15 Myr of evolution (~500 orbits, where the exact output is taken when the vortex is opposite the planet). Each set of panels assumes a different planet eccentricity: e = 0.0,0.1,0.2 from the top to the bottom. The simulation assumes an α viscosity of 10⁻⁴. For each eccentricity, the top left panel shows the gas surface density, the panels from the top middle to the bottom right show the dust surface density of 1, 10, 100, and 1000 µm-sized particles, respectively.