the long baseline data, the flux of the bright source is 9% lower than the derived flux by fitting the disk and point source simultaneously.

\[residual\_disk\]

We then generated a “disk-only” map by subtracting the best-fit point sources in the visibility domain. The “disk-only” map is shown in Figure \[pts\_ring\]b. The subtraction of the bright source is far from perfect. There is still significant flux ($\gtrsim$25 $\sigma$) near the east side of the bright source, which could be part of the disk structure or the bright source has a non-symmetric, extended shape. If the bright source is a dusty galaxy in nature (see Section 4.3), it is very likely to have an irregular shape, making it challenging to separate it from the disk without high angular resolution observations. The subtraction of the faint source is better. The emission near the position of the faint source is more smooth, but it does appear that the disk flux extends toward the faint source, explaining the residual in Figure \[mcmc\_model\]. Similarly, the observed resolution prevents further assessment.

To evaluate the impact of the two sources on the derived disk parameters, we searched for the best-fit disk parameters using the visibility approach by fixing 