Notes. Column (1) Target name. (2) 3D-Barolo fit analysis methodology: ‘I’ for a two-step strategy, to first constrain the inclination and then all remaining disk parameters, and ‘II’ for a single-step strategy considering the i^morph (Sect. 2.2.2) as initial guess for the inclination. (3) 3D-Barolo disk inclination i. (4) 3D-Barolo kinematic PA of the major axis on the receding half of the galaxy, taken anti-clockwise from the north on the sky. (5) 3D-Barolo rotation velocity. (6) Measured velocity dispersion in the outer part of the galaxy, after subtracting the instrumental resolution (in quadrature). (7) Maximum rotation velocity over velocity dispersion. (8) Effective radius measurements from Table 1; these values have been preferred to those obtained from the Hα flux map, reported in parenthesis, as less affected by dust obscuration. They are however totally consistent with R_e(Hα), in the range 1 − 2.9 kpc. The only exceptions are represented by I14348 NE and I20100 SE, the R_e(Hα) values of which are strongly affected by the presence of strong off-nuclear Hα emission. (9) Dynamical masses within 2R_e. (10) (spectral-energy-distribution-based) stellar masses from Rodríguez Zaurín et al. (2010) and da Cunha et al. (2010). For the former, no uncertainties were reported in the original paper. ^( † )R_e from Veilleux et al. (2006); see Sect. 2.2.2. ^( * )Mean R_e of local (U)LIRGs, from Bellocchi et al. (2013).