Notes.The kinematic properties were obtained from a 2-Gaussian component fit to the integrated Hα-[NII] spectra of the clumps, except when otherwise stated (see notes). Columns: (1) Identification: First digits of the IRAS code for the galaxy and clump identification according to Fig. 1; (2) Half-light radii, r_hl. They correspond to intrinsic values (i.e., deconvolved by the PSF) calculated from the IFS based Hα maps using the CoG method (e.g., Arribas et al. 2012). Their uncertainties are estimated to be 30 percent. (3) FWHM of the narrower component; (4) FWHM of the broad component; (5) difference in the central velocity of the broad component with respect to the narrow component; (6) flux ratio between the broad and the narrow Hα lines; (7) Maximum velocity defined as V_max = abs(–ΔV + FWHM/2) following, e.g., Rupke et al. (2005). (8) Observed (i.e. no reddening corrected) star-forming rate derived from the Hα luminosities. (9) Observed (i.e., no reddening corrected) star-forming rate density within half-light radius. (10) Notes: (a) Only the FWHM of the 1-Gaussian fit is reported as for this clump the 2-Gaussian fit does not give a good fit, which suggests that if a second component exits, it must be very weak. (b) For this clump the fit for the [NII] lines was not good, but the results for Hα reported here were okay. (c) IRAS06035 was observed under no photometric conditions (see Rodriguez-Zaurin et al. 2011), so the SRF value may be in error. (d) as the clump size is not resolved (i.e., ~PSF), only an upper limit on the radius (lower limit on Σ_SFR) could be obtained Quoted errors are only those associated with the fit, except for the SFR for which considered 30 per cent (errors from the fit were too small to be meaningful). SFR are obtained from the observed Hα flux using the Kennicutt (1998) relation.