  We model the NFW potential to determine if, and under what conditions, the
NFW halo appears consistent with the observed velocity fields of low surface
brightness (LSB) galaxies. We present mock DensePak IFU velocity fields and
rotation curves of axisymmetric and non-axisymmetric potentials that are
well-matched to the spatial resolution and velocity range of our sample
galaxies. We find that the DensePak IFU can accurately reconstruct the velocity
field produced by an axisymmetric NFW potential and that a tilted-ring fitting
program can successfully recover the corresponding NFW rotation curve. We also
find that non-axisymmetric potentials with fixed axis ratios change only the
normalization of the mock velocity fields and rotation curves and not their
shape. The shape of the modeled NFW rotation curves does not reproduce the
data: these potentials are unable to simultaneously bring the mock data at both
small and large radii into agreement with observations. Indeed, to match the
slow rise of LSB galaxy rotation curves, a specific viewing angle of the
non-axisymmetric potential is required. For each of the simulated LSB galaxies,
the observer's line-of-sight must be along the minor axis of the potential, an
arrangement which is inconsistent with a random distribution of halo
orientations on the sky.
