using the techniques described in @phillips11 finds a total flux of 19.4$\pm$11.0 mJy, much lower than the one published by @nilsson10. The peak emission in the 870 [${\rm \mu m}$ ]{}map is offset by 13 (i.e., 2/3 of the beam diameter) from the expected star position; therefore, the quoted flux is estimated as an unresolved source at the position of the star. Due to the large offset, we consider it as a non-detection and use 33 mJy as the 3 $\sigma$ upper limit. We adopted this value for further SED analysis. Using similar approaches and grain parameters as in @su15 (minimum and maximum grain sizes of $\sim$1.8 [${\rm \mu m}$ ]{}and 1000 [${\rm \mu m}$]{}, and a particle size distribution in a power law index of $-$3.5), a geometrically thin, constant surface density disk with a radial span of 106-320 au provides a good fit to the ALMA 1.3 mm flux and maximum allowable fluxes in the far infrared (gray squares in Figure \[sed\]). This cold disk SED model also agrees with the observed 7 mm flux (not shown in Figure \[sed\]) obtained by @ricci15b within the uncertainty. Compared to the cold component model presented in @su15, this revised planetesimal 