  Recent work by several groups has established the properties of the dwarf
satellites to M31. We reexamine the reported kinematics of this group employing
a fresh technique we have developed previously. By calculating the distribution
of a chi statistic (which we define in the paper) for the M31 system, we
conclude that the total mass (disk plus halo) of the primary is unlikely to be
as great as that of our own Milky Way. In fact the chi distribution for M31
indicates that, like NGC 3992, it does not have a massive halo. In contrast,
the analysis of the satellites of NGC 1961 and NGC 5084 provides strong
evidence for massive halos surrounding both spiral galaxies.
