an offset of the star from the center of the disk. If any such asymmetries are present in the millimeter emission from the HR 8799 disk, observations with a significantly higher signal-to-noise ratio will be required to reveal them. This outer belt of large fractional width joins a growing list other young debris disks with similar characteristics, e.g. HD 95086 [@su17], that are much broader than the classical Kuiper Belt of our Solar System [especially the low excitation “kernel” component discussed by @bannister16].

VLA 9 millimeter Flux Estimate
------------------------------

In the VLA image, the disk is detected only at the $\sim3\sigma$ per beam level, and we do not apply the same MCMC modeling technique to these data. For simplicity, we measure the flux density in [CASA]{} within a circular aperture centered at the location of the disk, assuming the diameter of the disk determined from the combined modeling of the SMA and ALMA data. We determine the uncertainty by measuring the flux density in the same circular aperture at ten random locations in the image and taking the average. The measured total flux density of the disk from our VLA observations is $F_\text{9mm} = 32.6\pm9.9$ $\mu$Jy (correction for primary beam 