Gaussian centers of CH₃CN 12₃ – 11₃ emission at different velocities from the uv-domain fitting in comparison with the line-of-sight velocity of a Keplerian disk model (V ∝ r^−0.5), shown at the top. These models adopte three sets of V_lsr, PA, θ_inc listed in the upper-left corner from Diaz-Rodriguez et al. (2022) for VLA4A/B circumstellar disks and the circumbinary disk. Line-of-sight velocities of these points as a function of the inclination-corrected radius, shown at the bottom. The solid and dotted lines show modeled velocities at the corresponding emitting positions assuming Keplerian motion (V ∝ r^−0.5) and conservation of angular momentum (V ∝ r⁻¹), respectively. We note that the modeled curves will only shift vertically if the velocity of the model is scaled.