for the presence of dust within this inner radius, but decreasing towards smaller radii. We find that $r_{\min}$ matches well the radius at which the surface density peaks as seen in Figure \[fig:radial\_profile\]. Similarly, our estimate of the outer radius (136 au) is significantly smaller than their outer edge (150 au). We find that the disc inner edge has a power law index (slope hereafter) of $\sim2.6$, while the outer edge is much steeper with a slope of $-11$. The intermediate component has a very flat slope of $\sim0.3$, $2.7\sigma$ flatter than the previous estimate (0.59), although the difference could be simply due to different parametrizations, i.e. considering a three vs a single power law parametrization or leaving the gap’s depth as a free parameter vs fixed to 1. Note that the slope derived from the intermediate component does not imply that the mass surface density of planetesimals is flat. In fact, from collisional evolution models we expect the surface density of mm-sized dust and optical depth to have a lower slope than the total mass surface density in regions of the disc where the largest planetesimals are not yet in collisional equilibrium [i.e. have a lifetime longer than the 