Notes. Derived Hα kinematic quantities for the narrow (systemic) component. Horizontal lines distinguish class 0, 1, and 2 (from top to bottom, respectively). Column (1): IRAS name. Column (2): systemic velocity calculated as the Hα radial velocity. A mean error of 5−7 km s^-1 should be added when calibration and fitting errors are considered. Column (3): Hα velocity amplitude defined as the half of the observed “peak-to-peak” velocity (i.e., half the difference between the maximum and minimum values is considered without applying the inclination correction). Column (4): Hα velocity shear defined as the half of the difference between the median of the 5 percentile at each end of the velocity distribution (i.e., and ), as in Gonçalves et al. (2010) (not corrected for the inclination). Column (5): Hα mean velocity dispersion. Column (6): Hα central velocity dispersion, derived as the mean of 4 × 4 spaxels around the VIMOS continuum flux peak. Column (7): dynamical ratio between the velocity shear (corrected for the inclination) and the mean velocity dispersion values. Column (8): inclination of the galaxy, defined as i = cos^-1(b/a) (i.e., where a and b are, respectively, the major and minor axes of the object). When possible, it has been inferred directly from the Hα map or continuum images (i.e., DSS, HST and 2MASS). When the morphology of the object was too complex, we assumed a mean inclination of about 52° ± 26°, equivalent to ⟨ sini ⟩  = 0.79 ± 0.35 (see Appendix in Law et al. 2009). In this case, the uncertainty of the inclination has been computed as the standard deviation of the distribution of the different measures derived when i varies from 0° to 90°, using step of 1°. See details in Col. 12, notes (v, vi, vii). Column (9): velocity gradient (km s^-1) associated with one spaxel derived as explained in the text. Column (10): kinematical classification inferred from the kinematic maps. RD stands for rotating disk, PD perturbed disk and CK are systems with complex kinematics (see text for details). The galaxy IRAS 08424-3130 N is in the edge of the FoV, and its kinematic classification was not possible. For those objects for which the kinematical classification is controversial, the possible classifications are shown in the table. Column (11): dynamical masses (see text). Column (12): comments with the following code: (i) after distributing the total IR luminosity between the individual objects forming the system, this galaxy does not qualify as LIRG as its luminosity is lower 10¹¹  L_⊙. The galaxies IRAS F01341-3735 N and IRAS F09437+0317 N are in the limit to be classified as LIRG (see Col. 6 in Table 1). (ii) Systems for which a mask has been applied to the data-cube in order to analyze separately the sources (e.g., N and S stand for northern and southern galaxies). (iii) No reliable due to AGN contamination (see Arribas et al. 2012 and App. B for details). (iv) For this galaxy two pointings have been combined to derive the kinematic values. (v) The inclination has been derived using the Hα map. (vi) A mean inclination (i.e., 52°    ±    26°) has been considered. (vii) The inclination has been derived using continuum available images (i.e., HST or DSS or 2MASS). (viii) The kinematic classification was not possible due to the poor linear resolution for IRAS F12596-1529, while the emission of the IRAS F08424-3130 N is only partially included in the FoV.