at redshift $z=3$, which are all indirect, cover a wide range, $10^{11.1}$[${\mathrm M_{\odot}\thinspace}$]{}to $10^{12.3}$[${\mathrm M_{\odot}\thinspace}$]{}. Motivated by this large uncertainty, in an earlier paper (Weatherley & Warren, 2003; hereafter Paper I) we presented a simplified analysis of the kinematic data on LBGs, to estimate the halo virial masses. The $\Lambda$CDM paradigm for structure formation permits computation of the detailed properties of the dark matter yielding predictions of the masses of haloes, their mass profiles, and their assembly history (e.g. Lacey & Cole, 1993; Navarro, Frenk & White, 1997, hereafter NFW). Baryonic processes, including star formation and feedback, on the other hand are too complex to allow [*ab initio*]{} predictions of the distribution and state of the baryons within the haloes. Therefore the best tests of the $\Lambda$CDM paradigm will be those which measure the properties of the dark matter. Instead, at high redshift, we are largely limited to studies of luminous matter in the brightest central regions of galaxies, where the baryons dominate the mass budget. For example, in most cases the kinematic data on LBGs is limited to the measured line velocity widths. These data, on their own, are not useful for measuring halo masses; fortunately, in a handful 