a center ${r_\mathrm{g}}$ and a full width half maximum (FWHM) ${w_\mathrm{g}}=2\sqrt{2\ln(2)}{\sigma_\mathrm{g}}$. We leave as a free parameter the total dust mass ${M_\mathrm{d}}$, which is the surface integral of $\Sigma(r)$. Although the disc is close to face on, we still model the dust distribution in three dimensions adding the scale height $h$ as an extra parameter (i.e. vertical standard deviation of $hr$), and imposing a prior of $h>0.03$.

We solve for the dust equilibrium temperature and compute images at 0.86 and 1.13 mm using <span style="font-variant:small-caps;">RADMC-3D</span>[^4]. We assume a weighted mean dust opacity corresponding to dust grains made of a mix of astrosilicates [@Draine2003], amorphous carbon and water ice [@LiGreenberg1998], with mass fractions of 70%, 15% and 15%, respectively, and assuming a size distribution with an exponent of -3.5 and minimum and maximum sizes of 1$\mu$m and 1cm. This translates to a dust opacity of 1.5 cm$^2$ g$^{-1}$ at 1.1 mm. We note that these choices in dust composition and size distribution have no significant effect on our modeling apart from the derived total dust mass. We then use these images to compute model visibilities at the same *uv* points as the 12m band 6, 12m band 7 and ACA band 