obtained  spectra for nine of their sample, with the slit aligned along the major axis. Contrary to expectation, rotation velocities were secured for only two of the galaxies. They proposed that these results could be explained if some of the elongated galaxies are in fact merging sub-units, rather than relaxed edge–on disks. It is worth noting, nevertheless, that the majority of these observations were undertaken in typical seeing of 0.8arcsec, somewhat worse than for the data analysed here. Of the nine galaxies selected as elongated, in six cases the (deconvolved) extent of the  emission is smaller than the seeing, which would make it difficult to detect rotation. Of the three cases where the emission is more extended than the seeing, rotation velocities were secured for two. This analysis further underscores the desirability of high–spatial resolution 2D spectroscopy, to remove some of these uncertainties of interpretation. In the meantime, our goal in this paper has been to maximise the useful information on the dynamical virial masses of the haloes of LBGs from existing kinematic data.

Acknowledgments {#acknowledgments .unnumbered}
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We thank Dawn Erb and Max Pettini for their helpful comments regarding their data, and their constructive criticism of Paper I. We 