Same as Fig. B.1, now for Δσ_⋆ against the fraction of young stars. Similarly to the case of Δv_⋆ against the fraction of young stars we find almost vertical distributions of the mean values of Δσ_⋆ in all the regions of each galaxy. The only exception is the nucleus in NGC 1097 where we find a slight trend of increasing velocity dispersion differences with increasing fractions, but we find mean values of Δσ_⋆ very similar to the typical error. Thus, we rule out any kind of trend with the fraction of young stars.