DescriptionA set of four paired cosmological simulations of Milky Way-mass galaxies are used to examine the dark matter structure. Particular attention is paid to the ability of simulated velocity distributions to inform the experimental search for dark matter and the change in dark matter velocity distributions due to the addition of baryons. It is found that the dark matter distributions from hydrodynamic simulations are better described by the Standard Halo Model (which assumes a Maxwellian distribution for dark matter velocities) than dark matter-only simulations. Thus, the additional of baryonic physics to simulations does not alleviate tension in results from dark matter direct detection experiments which generally assume the Standard Halo Model.
The dark matter and stellar content of these galaxies is examined in both the virialized and the debris components. Previous works have yielded contradictory results on whether there is a stellar population that could be used observationally to infer the underlying dark matter velocity distributions in the solar neighborhood. The stellar material is not found - in either case - to be a particularly good tracer of dark matter material, especially at the extreme velocities. The diversity in Milky Way mass galaxies shows the need to carefully match the Milky Way in a variety of categories. The specific merger history is found to be important for velocity structures, even for old merger events.