Radial profile of the gas surface density Σ_g (upper panels) and disc viscosity α_visc (lower panels) including a dust trap caused by a different planet mass and location, whose shape and depth is computed using empirical fits from Kanagawa et al. (2017). We pick here our lowest value of the viscosity (α_visc,0 = 10⁻³) that produces the deepest gaps in our parameter study. For comparison, M_p = 300 M_⊕ corresponds to an approximately Jupiter-mass planet.