of any of the individual main nearby clusters. Bulk flow estimates from TF-like relations are traditionally featureless [e.g. @Dek94], in contrast to velocity dipoles estimated by from the distribution of galaxies in redshift surveys [e.g. @nd94]. In the analysis here, we have collapsed clusters and therefore, signatures of individual clusters, in our estimated bulk flows, could be smeared out. It is instructive to explore how much we are missing by collapsing clusters and wether signature of infall on clusters of nearby galaxies can actually be clearly seen in SFI++ or similar data. As an illustrative representative case we plot in figure \[fig:virgo\] individual peculiar velocities of 54 SFI++ galaxies contained in a cylinder of $6^\circ$ in radius and of $2600\kms$ centered on the Virgo cluster. The individual distances, $d_{\rm TF}$ to galaxies are obtained from the observed galaxy deviation from the straight line describing the inverse TF relation as determined by the 54 galaxies. The individual radial peculiar velocities are then given by $V_{\rm TF}=cz-H_0 d_{\rm TF}$. Red circles in this figure show $V_{\rm TF}$ versus $cz$ while the blue plus signs correspond to $V_{\rm TF} $ versus $d_{\rm TF}$. The solid line is obtained by statistical regression of $V_{\rm 