Results from Kinemetry. Left: Best-fit kinematic inclination as a function of nuclear distance obtained by Kinemetry on the CO (red), [N II] λ6583 (brown), and stellar (blue) velocity fields, with the PA fixed to 355°. For reference, the equivalent (morphology) results from running Kinemetry on the HST/WFC3 F160W image are shown in black; at radii ≤15″ these latter fits are not reliable, due to the prominent dust lanes, and are shown with a dotted black line. Error bars are as reported by Kinemetry. Right: Kinemetry-derived k1 coefficient (the – projected for inclination – amplitude of the “pure-rotative” component k1 cos θ) as a function of radius when fitting the velocity fields of CO (red symbols), [N II] λ6583 (brown symbols) and stars (blue symbols). Error bars shown are as reported by Kinemetry. Overlaid (see Sect. 4) are the adopted best fit inclination-projected rotation curves due to the stellar potential for the arctangent (brown dotted lines) and the MGEFit solution (blue dotted lines): two curves (inclinations of 78° and 65°) are shown for each. The solid lines in the corresponding colors show the total expected inclination-projected rotation curve if our adopted best-fit value (3.34 × 10⁹ M_⊙) for the black hole mass is considered.