$R_\text{out}$, respectively. The surface brightness power law index, $x$, encapsulates both the radial surface density and temperature profiles of the emitting grains. The total flux density of the belt is normalized to $F_\text{belt} = \int I_\nu d\Omega$. We also fit for the belt geometry, specifically an inclination, $i$ (where $0\degr$ is face-on), and a position angle, $PA$ (measured East from North). For comparison with observed visibilities, the model emission is multiplied by the appropriate primary beam response of each telescope. Since imaging with both [*Herschel*]{} [@matthews14] and JCMT [@holland17] shows the presence of a compact background source to the northwest of the disk, we also include an unresolved point source at this location in the model, described by a total flux, $F_\text{pt}$, and an offset from the phase center of the observations, $\{\Delta\alpha_\text{pt},\Delta\delta_\text{pt}\}$. When modeling the ALMA data alone, this additional background source is omitted on account of primary beam attenuation at the offset location.

This simple two-dimensional parametric model for the disk emission is incorporated into a Markov Chain Monte Carlo (MCMC) framework. For each model image, we calculate synthetic visibilities using [vissample]{}[^1], a python package for visibility sampling that improves on the sampling and interpolation of the [uvmodel]{} 