Notes. Columns: (1) Sub-sample and identification according to the IRAS code, or other common name. For those systems with enough spatial resolution to separate the individual galaxies they are identified with N, S, E, W, and C (i.e. centre) according to their relative location; (2) redshift according to NED; (3) Luminosity distance; (4) Morphological class, where 0, 1, 2, distinguish isolated discs, interacting, and mergers, respectively. For interacting systems 1.0 and 1.1 distinguish between the total system and individuals, respectively. In five cases (F06035−7102, F23128−5919, F08572+3515, Mrk463, F18580+6527) the individuals members, as well as the global system are considered; (5) Logarithmic of the infrared luminosity in solar units. For individual galaxies in multiple U/LIRGs, these are estimated dividing the total luminosity taking into account the relative fluxes in the MIPS images. The uncertainty has been estimated as three times the typical error in the IRAS fluxes. For individual objects in multiple systems, an uncertainty of 0.2 dex has been considered; (6) Hα half-light radius using the A/2 method (Arribas et al. 2012). Values in brackets correspond to upper limits. Lower limits in the radii values due to limitations in the FoV are not distinguished, as the effect is estimated to be within the quoted uncertainties and the FoV effect is (partially) compensated in the Σ(Hα) determination; (7) SFRs obtained from the reddening corrected Hα luminosity from RZ11 and GM09, transformed for a Chabrier (2003) IMF. For Arp220 and Mrk273, the SFRs were obtained from the works by Veilleux et al. (1999) and Colina et al. (2004), respectively; (8) Hα star formation rate density; (9) Dynamical masses for the VIMOS sub-sample are from Bellocchi et al. (2013). For the INTEGRAL data they are derived following the same methodology; (10) “y” indicates evidence of an AGN from the optical spectra, as indicated by either the emission line ratios or the presence of a very broad Hα (see also notes in table A1). For IRAS F06035-7102, the spectra show evidence of a (weak) AGN in the southern component, but not in the whole system.