with sizes $>$31 (i.e., the disk emission) is filtered out. The long baseline map is shown in Figure \[pts\_ring\]a. Within 35 radius from the star, there are two sources (detected above 8 $\sigma$) that appear in the long baseline map. The measured FWHM of the faint source is 079$\times$064, the same as the synthesized beam in the long baseline map, while the FWHM of the bright source is $\sim$8% broader, 085$\times$070. To evaluate whether the threshold defining the long baseline data affects the FWHM of the bright source, we also generated the long baseline maps with different thresholds between 60 to 80 $k\lambda$. The FWHM of the bright source is consistently broader than the synthesized beam by 8%. Furthermore, we generated individual, long baseline maps per data set to see if there exists a flux difference between the two data sets for the bright source. Taken at face value, the bright source is about 5% brighter in data set B. Given the typical absolute flux uncertainty (10%) in the ALMA data, the flux difference is not significant. The properties (offset and flux density) of the two point sources are determined using ’uvmodelfit’ in CASA, and given in Table \[tab3\_twops\]. Using 