Results of the ^3DBarolo dynamical modelling of the [CII] emission line. Top and bottom left: PV diagrams of the [CII] emission line along the line of nodes (PA = 200 deg) and orthogonal to it (PA = 290 deg), performed with ^3DBarolo. Contours are at 2, 3, 6, and 12σ, with σ = 0.22 mJy, for the data (solid black lines) and the best-fit model (dashed orange lines). Sampling is performed with five radii, spaced by 0.045 arcsec. Yellow stars show the disk model. Top and bottom right: rotational velocity, v_rot, and gas velocity dispersion, σ_gas, as a function of radius for the best-fit disk model. To compute the top and bottom error bars for the rotational velocity, we performed the modelling by varying the disk inclination i = 20 and 45 deg, respectively. The grey shaded area marks the central beam (r_beam ∼ 0.08 arcsec), and grey points are those computed including the central beam.