Notes. Column (1) Target name. Column (2) 2R_e from Isophote fits of available HST/F160W images for all but the Seyfert 1 systems IZw1 and I01572 (for which we used the Veilleux et al. 2006 measurements) and the two systems without HST data: I16090 and I10190. The geometric parameters of the latter two sources are derived from MUSE narrow-band images (at λ ∼ 7500 Å). Columns (3) and (4) Inclination and PA of the galaxy. The PA is taken anti-clockwise from the north on the sky. These parameters are derived with Isophote, at the distance reported in Col. (2). Columns (5) and (6) Stellar and gas PA^kin, taken anti-clockwise from the north on the sky. Column (7) and (8) Maximum stellar and gas velocity variations along PA^kin, non-corrected for galaxy inclination. The velocity amplitudes are computed along an intermediate PA^kin when PA and PA are consistent within the errors (3σ); alternatively, stellar (gas) velocity amplitudes are computed along PA (PA); for those sources with a missing PA^kin measurement, the gas and stellar δv are computed along the only available PA^kin measurement. Velocity uncertainties are derived with a bootstrap. Columns (9) and (10) Median velocity dispersion along PA^kin. All velocity and velocity dispersion values for the gas component are derived from the narrow Hα velocity maps. Column (11) Kinematic classification according to the two criteria defined in Sect. 3.2: ‘s’ for stellar disk-like kinematics; ‘g’ for gas disk-like kinematics. ^( * *)The effective radius measurement is highly uncertain due to prominent tidal tails (and, for I10190 W, the nearby E nucleus). ^(s)In Cols. (3) and (4), the label identifies those sources whose geometric parameters do not vary significantly at r > R_e, i.e. whose inclination and PA are relatively stable. ^(u)In Cols. 3 and 4, the label identifies those sources whose inclination and PA vary significantly at r > R_e. These sources generally have prominent tails that strongly affect the isophote fit.