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The data obtained by the recent modern sky surveys enable detailed studies ofthe stellar distribution in the multi-dimensional space spanned by spatialcoordinates, velocity and metallicity, from the solar neighborhood all the wayout to the outer Milky Way halo. While these results represent excitingobservational breakthroughs, their interpretation is not simple. For example,traditional decomposition of the thin and thick disks predicts a strongcorrelation in metallicity and kinematics at $\sim$1 kpc from the Galacticplane; however, recent SDSS--based work has demonstrated an absence of thiscorrelation for disk stars. Instead, the variation of the metallicity androtational velocity distributions can be modeled using non--Gaussian functionsthat retain their shapes and only shift as the distance from the mid--planeincreases. To fully contextualize these recent observational results, adetailed comparison with sophisticated numerical models is necessary. Modernsimulations have sufficient resolution and physical detail to study theformation of stellar disks and spheroids over a large baseline of masses andcosmic ages. We discuss preliminary comparisons of various observed maps andN--body model predictions and find them encouraging. In particular, the N--bodydisk models of Ro\v{s}kar et al. \cite{Roskar 2008} reproduce a change of diskscale height reminiscent of thin/thick disk decomposition, as well asmetallicity and rotational velocity gradients, while not inducing a correlationof the latter two quantities, in qualitative agreement with SDSS observations.

SDSS Observations of the Milky Way vs. N-body Models: A Comparison of Stellar Distributions in the Position-Velocity-Metallicity Space