Are there any extragalactic high speed dark matter particles in the Solar neighborhood?

Abstract

We use the APOSTLE suite of cosmological hydrodynamical simulations of the Local Group to examine the high speed tail of the local dark matter velocity distribution in simulated Milky Way analogues. The velocity distribution in the Solar neighborhood is well approximated by a generalized Maxwellian distribution sharply truncated at a well-defined maximum ``escape" speed. The truncated generalized Maxwellian distribution accurately models the local dark matter velocity distribution of all our Milky Way analogues, with no evidence for any separate extragalactic high-speed components. The local maximum speed is well approximated by the terminal velocity expected for particles able to reach the Solar neighborhood in a Hubble time from the farthest confines of the Local Group. This timing constraint means that the local dark matter velocity distribution is unlikely to contain any high-speed particles contributed by the Virgo Supercluster ``envelope", as argued in recent works. Particles in the Solar neighborhood with speeds close to the local maximum speed can reach well outside the virial radius of the Galaxy, and, in that sense, belong to the Local Group envelope posited in earlier work. The local manifestation of such envelope is thus not a distinct high-speed component, but rather simply the high-speed tail of the truncated Maxwellian distribution.

16 pages, 8 figures. To be submitted to JCAP

References in corpus (9)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
• Baryon effects on the internal structure of LCDM halos in the EAGLE simulations
• Bent by baryons: the low mass galaxy-halo relation
• Magellanic satellites in $\Lambda$CDM cosmological hydrodynamical simulations of the Local Group
• The impact of the Large Magellanic Cloud on dark matter direct detection signals
• Effects on the local dark matter distribution due to the Large Magellanic Cloud
• Enhanced prospects for direct detection of inelastic dark matter from a non-galactic diffuse component
• The local dark matter distribution in self-interacting dark matter halos