  We use broadband photometry and low-resolution spectra of a complete sample
of late-K and M dwarfs brighter than I=22 in three fields at high galactic
latitude to study issues relating to galactic structure and large scale
abundance gradients in the Galaxy. The observed starcounts in each field are a
good match to the predictions of models based on deep starcount data in other
intermediate-latitude fields, and these models identify the late-type stars as
members of the Galactic disk. Abundances for these late type stars are
estimated via narrowband indices that measure the strength of the TiO and CaH
bands in their spectra. Our results show that the average abundance in the
Galactic disk remains close to solar even at heights of more than 2 kpc above
the Plane.
