no easy way to mask out the contribution of the bright source in the visibility domain since the bright source contributes to all baselines. We tried to minimize the impact of the bright source by fitting it as a Gaussian profile in visibilities, allowing for some sort of extension. The results are also given in Table \[tab4\_disk\]. Similar to the image plane approach, the disk size parameters are also slightly smaller than the ones derived in Section 3.2. The Gaussian parameters for the bright source are basically the same as the synthesized beam, but with much less flux compared to the fits derived from the long baseline data (Table \[tab3\_twops\]). The residual maps (not shown) are neither better than the ones in Figures \[residual\_disk\]a and \[residual\_disk\]b nor than those in Figures \[mcmc\_model\]a and \[mcmc\_model\]b as a result.

We synthesized the various fitting results as follows. The disk has a total flux density of 2.79$\pm$0.1 mJy at 1.3 mm, and is inclined by 30$\pm$3 from face-on with a P.A. of 97$\pm$3. It is interesting to note that the best-fit models (Table \[tab4\_disk\]) all prefer to have the ring center east of the star by $\sim$01. Since the star is not detected 