Abstract
We study the effects of galaxy formation on dark matter direct detection using hydrodynamic simulations obtained from the “Evolution and Assembly of GaLaxies and their Environments” (EAGLE) and APOSTLE projects. We extract the local dark matter density and velocity distribution of the simulated Milky Way analogues, and use them directly to perform an analysis of current direct detection data. The local dark matter density of the Milky Way-like galaxies is 0.41–0.73 GeV/cm3, and a Maxwellian distribution (with best fit peak speed of 223–289 km/s) describes well the local dark matter speed distribution. We find that the consistency between the result of different direct detection experiments cannot be improved by using the dark matter distribution of the simulated haloes.
Highlights
Direct dark matter (DM) detection experiments search for the energy deposited by a recoiling nucleus due to the scattering of a DM particle in an underground detector
In addition to the hydrodynamic simulations used in this work, we present results for dark matter only (DMO) companion simulations in eagle and apostle which were run assuming all the matter content is collisionless
We directly use the DM density and velocity distribution of the Milky Way (MW) analogues to perform an analysis of data from direct detection experiments, and study how the preferred regions and exclusion limits set by different experiments vary in the DM mass and scattering cross section plane
Summary
Direct dark matter (DM) detection experiments search for the energy deposited by a recoiling nucleus due to the scattering of a DM particle in an underground detector. The range of the best fit local circular speed for the Maxwellian distribution is 223 – 289 km/s in the hydrodynamic case.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
