Effects on the local dark matter distribution due to the Large Magellanic Cloud

Abstract

We study the local dark matter distribution in two models for the Milky Way (MW)-Large Magellanic Cloud (LMC) interaction. The effect of the LMC on the local dark matter distribution is dependent on the evolution of the MW-LMC system, such that a static model is insufficient to accurately model the dark matter velocity distribution in the solar neighbourhood. An evolved model boosts local LMC dark matter particle velocities by nearly 50%, to a median value of $\approx 750$km/s. MW dark matter particles also experience a velocity boost, which we identify as being caused by reflex motion owing to the infall of the LMC. We study the implications of LMC particles in the solar neighbourhood for dark matter detection experiments. Specifically, the directionality of LMC particles is distinguishable from the MW particles, with a difference in the apparent origin centroid location between the MW and LMC particles of $26\pm 6^{\circ }$. This unique identifier, along with their high velocities, can be utilised by directional detectors to search for dark matter particles originating in the LMC.

6 pages, 3 figures

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• Enhancing Direct Detection of Higgsino Dark Matter
• Dark Matter Velocity Distributions for Direct Detection: Astrophysical Uncertainties are Smaller Than They Appear
• Deciphering the Kinematic Substructure of Local Dark Matter with LAMOST K Giants
• Are there any extragalactic high speed dark matter particles in the Solar neighborhood?
• How do the dynamics of the Milky Way -- Large Magellanic Cloud system affect gamma-ray constraints on particle dark matter?