The total stellar mass of the binary M_*, systemic velocity υ_LSRK, geometrical parameters (x_c,y_c offset from the central binary, PA position angle measured from the North to the redshifted major axis, and negative inclination i₀ indicates anti-clockwise disk rotation), and emission surface parameters (z₀, p, R_t, q describe an exponentially tapered power law) were inferred from the high-resolution cubes for ¹²CO and ¹³CO and the fiducial cube for C¹⁸O . The reported MCMC uncertainties are represented by the 16th and 84th percentiles drawn from the posterior distribution of the final 10% walkers of each model. These discminer-model uncertainties can increase by a factor of ∼10 due to spatially correlated noise, as shown by Hilder et al. (2025). The strongest correlation between model parameters is observed between the stellar mass and the disk inclination, which are known to be degenerate (e.g. Teague et al. 2018). This M_* ∙ sin i₀ degeneracy is evident through the varying best-fit parameters among CO isotopologs. Note that the inferred inclinations i₀ and position angles PA between the CO tracers are significantly different, which we interpret as a sign of disk warping.

^†Stellar masses for ¹²CO and C¹⁸O models with geometrical parameters fixed to the best-fit ¹³CO ones are 3.58 M_⊙ and 5.01 M_⊙, respectively.