77.4, and a rms of 7.5 $\mu$Jy beam$^{-1}$. The ring’s circumference is detected at signal-to-noise (S/N) $\gtrsim$15 $\sigma$ per beam, and is slightly inclined from face-on. We estimate the pointing accuracy of the data, $\sim$resolution/signal-to-noise, to be 013 since the main ring is detected at S/N$\gtrsim$10.

We adopt two approaches to explore the best-fit parameters for the HD 95086 system: (1) visibilities fitting and (2) image plane fitting. In both approaches, we assume the millimeter emission can be described by an optically and geometrically thin (no scale height) model plus a point source offset from the center. We explore two simple axi-symmetric models to describe the disk: (1) a two-boundary disk confined in a radial span of $R_{in}$ and $R_{out}$ with a surface density power law of $\Sigma(r) \propto r^{p}$ where $r$ is the stellocentric distance, and (2) a Gaussian ring defined by the peak ($R_p$) and the width (FWHM) of the ring ($R_w$). For the millimeter emission of the disk (i.e., dominated by large grains), we expect the dust temperatures follow $T_d(r) = 278.3 L_{\ast}^{0.25}
r^{-0.5}$ where $L_{\ast}$ is the stellar luminosity in units of the solar luminosity (6 $L_{\sun}$ for HD 95086 using the new distance) and $r$ 