  We perform a series of simulations of a Galactic mass dark matter halo at
different resolutions, our largest uses over three billion particles and has a
mass resolution of 1000 M_sun. We quantify the structural properties of the
inner dark matter distribution and study how they depend on numerical
resolution. We can measure the density profile to a distance of 120 pc (0.05%
of R_vir) where the logarithmic slope is -0.8 and -1.4 at (0.5% of R_vir). We
propose a new two parameter fitting function that has a linearly varying
logarithmic density gradient which fits the GHALO and VL2 density profiles
extremely well. Convergence in the density profile and the halo shape scales as
N^(-1/3), but the shape converges at a radius three times larger at which point
the halo becomes more spherical due to numerical resolution. The six
dimensional phase-space profile is dominated by the presence of the
substructures and does not follow a power law, except in the smooth
under-resolved inner few kpc.
