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 _ { \odot } .
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 .