LBGs to the distribution of circular velocities $V_{c7}$. We compared this distribution against the predicted distribution for $V_{c7}$ for the massive–halo model. The LBG circular velocities are too small by a factor $1.4\pm0.15$. As noted earlier, our analysis does not account for the increase in the circular velocity of the galaxies due to baryonic dissipation, so the quoted factor is a lower limit. With this in mind we can compute an upper limit to the median dynamical halo virial mass, by taking the median value of $\sigma$, and multiplying by 1.9 to convert to $V_{c7}$. Selecting an appropriate value of $c$, our median estimated dynamical halo mass is $<10^{11.6\pm0.3}$[${\mathrm M_{\odot}\thinspace}$]{}. Our new dynamical mass limit is a factor 3 larger than our earlier estimate (Paper I) which neglected the effects of seeing and slit width. Our dynamical mass limit is inconsistent with the value of $10^{12.3}$[${\mathrm M_{\odot}\thinspace}$]{}predicted by the massive–halo model. The broad spread in measured velocity widths (Figure \[fig:lbg\_mmwdistribution\]), which translates to a broad spread in inferred $V_{c7}$ is further evidence against the massive–halo model, which predicts a narrow spread in $V_{c7}$. A consistent picture is one in which LBGs inhabit only a fraction of the most–massive haloes. In 