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We use the distribution of accreted stars in SDSS-Gaia DR2 to demonstratethat a non-trivial fraction of the dark matter halo within Galactocentric radiiof 7.5-10 kpc and $|z| > 2.5$ kpc is in substructure, and thus may not be inequilibrium. Using a mixture likelihood analysis, we separate the contributionsof an old, isotropic stellar halo and a younger anisotropic population. Thelatter dominates and is uniform within the region studied. It can be explainedas the tidal debris of a disrupted massive satellite on a highly radial orbit,and is consistent with mounting evidence from recent studies. Simulations thattrack the tidal debris from such mergers find that the dark matter traces thekinematics of its stellar counterpart. If so, our results indicate that acomponent of the nearby dark matter halo that is sourced by luminous satellitesis in kinematic substructure referred to as debris flow. These resultschallenge the Standard Halo Model, which is discrepant with the distributionrecovered from the stellar data, and have important ramifications for theinterpretation of direct detection experiments.

Inferred Evidence For Dark Matter Kinematic Substructure with SDSS-Gaia