results because the ALMA primary beam is comparable in size to the HR 8799 emission region, and the ALMA observations provide very little data at spatial frequencies inside the first null of the visibility function to limit the total disk emission. To obtain constraints on these parameters from the ALMA data alone, we must impose strong priors on both $R_\text{out}$ and $F_\text{tot}$. As an example, we implemented a Gaussian prior on the total belt flux density, $3.0\leq F_\text{tot} \leq 4.0$ mJy, motivated by submillimeter observations [@matthews14] that predict a flux density of $\sim3.5$ mJy at 1.3 mm assuming a millimeter spectral index of $2.5$, typical of debris disks [@macgregor16]. We note that the fit to the SMA data alone yields a higher flux density of $5.13^{+0.34}_{-1.01}$ mJy, but still comparable within the uncertainties. In addition, we implemented a logistic function $f(x) = 1/(1+e^{-k(x-x_0)})$ prior for the outer radius with $k=-10$ and $x_0 = 512$ AU, the primary beam diameter. With these assumptions, fitting the ALMA observations alone yields $F_\text{tot} = 3.5\pm0.5$ mJy and $R_\text{out} = 497.(+2.,-150)$ AU, effectively recovering the priors. We suspect that the $\sim10\%$ uncertainties on the disk parameters quoted by @booth16 from an image-based analysis of the 