in the ALMA data, the “translated” pointing accuracy cannot confirm such an offset. The disk is very broad ($\Delta R/R\sim$0.84) in the millimeter continuum, and its width is resolved by $\sim$1.7 beam widths. As a result, we cannot determine the exact disk density distribution nor the offset between the star and disk center. For the two-boundary model, the disk can be described as having sharp boundaries at $R_{in}=$106$\pm$5 au and $R_{out}=$320$\pm$10 au with a surface density power index of –0.5$\pm$0.3. For the Gaussian ring, the disk is peaked at $R_p=$200$\pm$6 au with a width of $R_w=$168$\pm$7 au. The reduced chi-squared ($\chi^2$) is 1.20 for the two-boundary model, but 1.15 for the Gaussian ring model with the total number of visibilities (574358) in the fitting; similar $\chi^2$ numbers are also found using the image plane approach. Based on the $\chi^2$, the Gaussian ring model gives a slightly better fit; however, the number of free parameters is different (7 vs. 8), and some of the parameters are correlated.

Discussion
==========

Revised 3-Component SED Model
-----------------------------

\[sed\]

@su15 examined the resolved disk images of HD 95086 from [*Herschel*]{} and argued, by a detailed SED analysis, that the system is likely to possess three 