Properties of Local Group galaxies in hydrodynamical simulations of sterile neutrino dark matter cosmologies

TL;DR

This study uses hydrodynamical simulations to compare galaxy formation in sterile neutrino dark matter models with cold dark matter, revealing differences in subhalo concentration and galaxy counts that could distinguish dark matter types.

Contribution

First hydrodynamical simulations of Local Group-like galaxies in sterile neutrino dark matter models, highlighting differences from cold dark matter in subhalo properties and galaxy populations.

Findings

Sterile neutrino models have lower subhalo concentration than CDM.

LA10 sterile neutrino model matches CDM galaxy counts when accounting for scatter.

LA120 model requires more low-mass halos to match observed dwarf galaxy counts.

Abstract

We study galaxy formation in sterile neutrino dark matter models that differ signifi- cantly from both cold and from `warm thermal relic' models. We use the EAGLE code to carry out hydrodynamic simulations of the evolution of pairs of galaxies chosen to resemble the Local Group, as part of the APOSTLE simulations project. We compare cold dark matter (CDM) with two sterile neutrino models with 7 keV mass: one, the warmest among all models of this mass (LA120) and the other, a relatively cold case (LA10). We show that the lower concentration of sterile neutrino subhalos compared to their CDM counterparts makes the inferred inner dark matter content of galaxies like Fornax (or Magellanic Clouds) less of an outlier in the sterile neutrino cosmologies. In terms of the galaxy number counts the LA10 simulations are indistinguishable from CDM when one takes into account halo-to-halo (or `simulation-to-simulation') scatter. In order for the LA120 model to match the number of Local Group dwarf galaxies, a higher fraction of low mass haloes is required to form galaxies than is predicted by the EAGLE simulations. As the census of the Local Group galaxies nears completion, this population may provide a strong discriminant between cold and warm dark matter models.