  We interpret published CCD UBVI data to deduce the stellar density
distribution and metallicity distribution function in the region from 2-8 kpc
from the Galactic Plane, and compare our results to several star count models.
A feature of extant star count models is degeneracy between the adopted scale
heights of the thin and thick disks, and their local normalisation. We
illustrate the utility of this small data set, and future larger sets (e.g.
SDSS), by explicitly considering consistency between the derived density laws,
and the implied solar neighbourhood luminosity function. Our data set, from
Hall et al.(1996) (l=52, b=-39) contains 566 stars, selected to be consistent
with stellar loci in colour-colour diagrams. Our analysis supports the
parameterisation of the recent SDSS galaxy model of Chen et al.(2001), except
in preferring the stellar halo axis ratio to be 0.84. Photometric
metal-abundances have been derived for 329 stars using a new calibration. The
vertical distance-dependent metallicity distribution function, if parameterised
by a single mean value, can be described by a metallicity gradient -0.2$
dex/kpc for the thin disk and thick disk, and -0.1$ dex/kpc for the inner halo.
The data are however better described as the sum of three discrete distribution
functions, each of which has a small or zero internal gradient. The changing
mix of thin disk, thick disk and halo populations with distance from the plane
generates an illusion of a smooth gradient.
