As in Paper I, standard pre-processing was applied to the raw data, up to the rebinning in wavelength. The galaxy centers (r=0) were determined by a gaussian fitting to a limited range () around the brightest line. In the outer regions, cosmic-ray hits were removed with a median filter, and adjacent lines were combined with a variable weighting function (a gaussian continuously wider faintward). A Fourier-Fitting technique determined the central velocity dispersion and, when possible, the radial profile of the dispersion, together with the projected rotation curve V(r) along the major axis. A two-pass mode (described in Paper I) allowed to remove cosmics on the inner lines, where the spatial resolution must be preserved. We adopted as the systemic velocity the value measured at r=0. Whenever possible, we have measured the maximum rotation velocity , as the mean of representative values on the opposite semi-axes.