In an effort to more precisely define the spatial distribution of Galactic field stars , we present an analysis of the photometric parallaxes of stars in seven Kapteyn Selected Areas .
Our photometry database covers \sim 14.9 square degrees and contain over 130,000 stars , of which approximately 70,000 are in a color range ( 0.4 \leq R - I \leq 1.5 ) for which relatively unambiguous photometric parallaxes can be derived .
We discuss our photometry pipeline , our method of determining photometric parallaxes and our analysis efforts .
We also address the affects of Malmquist Bias , subgiant/giant contamination , metallicity and binary stars upon the derived density laws .
The affect of binary stars is the most significant of these biases – a binary star fraction of 50 % could result in derived scale heights that are 80 % of the actual values .

We find that while the disk-like populations of the Milky Way are easily constrained in a simultaneous analysis of all seven fields , no good simultaneous solution for the halo is found .
We have applied halo density laws taken from other studies and find that the Besançon flattened power law halo model ( \frac { c } { a } = 0.6 , \rho \propto r ^ { -2.75 } ) produces the best fit to our data .
With this halo , the thick disk has a scale height of 750 pc with an 8.5 % normalization to the old disk .
The old disk scale height is \sim 280-300 pc for our early type ( 5.8 \leq M _ { R } < 6.8 ) dwarfs and rises to \sim 350 pc for our late type ( 8.8 \leq M _ { R } \leq 10.2 ) dwarf stars .
Corrected for a binary fraction of 50 % , these scale heights are 940 pc and 350-375 pc , respectively .

Even with this model , there are systematic discrepancies between the observed and predicted density distributions – discrepancies only apparent at the faint magnitudes reached by our survey .
Specifically , our model produces density overpredictions in the inner Galaxy and density underpredictions in the outer Galaxy .
A possible escape from this dilemma is offered by modeling the stellar halo as a two-component system , as favored by studies of BHB/RR Lyrae stars and recent analyses of the kinematics of metal-poor stars .
In this paradigm , the halo has a flattened inner distribution and a roughly spherical , but substructured outer distribution .
Further reconciliation could be provided by a flared thick disk , a structure consistent with a merger origin for that population .