$150{{\rm \,km\,s^{-1}}}\le V_{max} < 300{{\rm \,km\,s^{-1}}}$                                      
  morphology, isolation                                             0.28   0.85   1.19   1.64   3.30           2815
  morphology, no isolation                                          0.22   0.77   1.16   1.64   3.38           3532
  no morphology, isolation                                          0.31   0.89   1.23   1.76   4.06          16479
  no morphology, no isolation                                       0.18   0.79   1.19   1.78   4.46          23429

In Table \[tb\_a200\] we show the effect of weakening the cut on relative radial velocity to require only that the two main galaxies be approaching. Again this has remarkably little effect on the median $A_{200}$ values. A comparison with Table \[tb\_a200\_vra\] shows them all to be increased by about 10%-15%. The effects on the tails of the distributions are more substantial. The 95% point is typically increased by about a factor of $2$. This is because the sample now includes a substantial number of pairs with small $V_{ra}$ (and thus smaller TA mass estimate) for which tangential motion is important for their current orbit. The 5% point of the distribution is significantly reduced, reflecting the fact that our restrictions on relative approach velocity exclude a non negligible number of systems with approach velocities [*larger*]{} than $195{{\rm \,km\,s^{-1}}}$, and thus with large TA mass estimates. Such systems must have more mass [*outside*]{} the conventional virial radii of the two 