Galactic structure
Above we have concentrated on sub-stellar objects. But ordinary low
mass stars, mostly M dwarfs, will be detected in huge numbers. Stars
at the very bottom end of the main sequence, with absolute magnitude
MJ=10, can be seen to a distance of 1kpc. With the second epoch
survey, proper motions will be available for huge numbers of the
nearer brighter objects. The star counts and kinematics from this
immense database will provide a valuable addition to our knowledge of
Galactic structure. In particular, the number of halo subdwarfs
identified in the survey will make them become almost as numerous as
the number of disc M dwarfs now known.