peculiar velocity data to determine the fit parameters. An equivalent way of exploring the same information is to use the scalar velocity correlation function, computed under the assumption of a homogeneous and isotropic flow. The results of this analysis can then be compared directly to model predictions using linear theory and an ensemble average of cosmic flow realizations for different cosmological models. The statistics of the model velocity field is parameterized by the amplitude, $\eta_8$, and by the shape parameter, $\Gamma$, of a CDM–like power spectrum. Applying the velocity correlation statistics to the SFI[@borgani1] and ENEAR[@borgani2] data sets one finds $\eta_8=0.34$ (SFI) and $\eta_8=0.51$ (ENEAR) for $\Gamma=0.25$. These values translate to $\beta_I=0.45-0.67$, assuming $b_I/b_o\sim 1.3$, results which agree within the uncertainties with the lower values of $\beta$ obtained by other methods presented above. More importantly, in contrast to the PS analyses, the region of acceptable solutions comfortably overlaps with other constraints on $\eta_8$ derived from the $rms$ of cluster peculiar velocities and cluster abundances, and on $\Gamma$ as determined for the galaxy power spectrum. One possible explanation for the discrepancy between the results of the PS analysis and the velocity correlation statistics is the different way the errors in the 