\
${r_\mathrm{g}}$ \[au\] & $75.4^{+0.8}_{-0.7}$ & radius of the gap\
${w_\mathrm{g}}$ \[au\] & $42.2^{+1.7}_{-2.2}$ & width of the gap\
${\delta_\mathrm{g}}$ & $0.43\pm0.02$ & depth of the gap\
\
${e_\mathrm{d}}$ & &lt;0.03 & disc global eccentricity\
\
${r_{\min}}$ \[au\] & $41.9^{+1.2}_{-1.4}$ & disc inner radius\
$\gamma_1$ & $11.6^{+3.0}_{-2.7}$ & inner edge’s slope\
$\gamma_2$ & $0.03^{+0.19}_{-0.26}$ & disc slope\
${r_\mathrm{g}}$ \[au\] & $72.1^{+2.2}_{-2.9}$ & radius of the gap\
${w_\mathrm{g}}$ \[au\] & $51^{+12}_{-8}$& FWHM of the gap\
${\delta_\mathrm{g}}$ & $0.58^{+0.08}_{-0.06}$ & fractional depth of the gap\
${M_\mathrm{c}}$ \[$M_{\earth}$\] & $3.0^{+0.9}_{-0.6}\times10^{-3}$ & dust mass inner component\
${r_\mathrm{c}}$ \[au\] & $19.3^{+2.8}_{-2.8}$ & radius of inner component\
${\Delta r_\mathrm{c}}$ \[au\] & $35.8^{+9.1}_{-6.7}$ & radial width of inner component\
${\omega_\mathrm{c}}$ \[$\degr$\] & $85^{+9}_{-9}$ & PA of inner component south of disc PA,\
& & and in the disc plane\
${\sigma_{\phi}}$ \[$\degr$\] & $94^{+15}_{-12}$ & azimuthal width of inner component\

In Table \[tab:mcmc\] we present the best fit parameters of our 3-power law model with a Gaussian gap. We find a disc inner radius of 47 au that is significantly larger than the inner edge of $\sim25-30$ au derived by [@Ricci2015]. This is because in their model they considered a sharp inner edge, while in ours we allow 