We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

Lovell, Mark R and Cautun, Marius and Frenk, Carlos S and Hellwing, Wojciech A and Newton, Oliver (2021) 'The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter.', Monthly Notices of the Royal Astronomical Society, 507 (4). pp. 4826-4839.


The spatial distribution of Milky Way (MW) subhaloes provides an important set of observables for testing cosmological models. These include the radial distribution of luminous satellites, planar configurations, and the abundance of dark subhaloes whose existence or absence is key to distinguishing among dark matter models. We use the COCON-body simulations of cold dark matter (CDM) and 3.3 keV thermal relic warm dark matter (WDM) to predict the satellite spatial distribution in the limit that the impact of baryonic physics is minimal. We demonstrate that the radial distributions of CDM and 3.3 keV-WDM luminous satellites are identical if the minimum pre-infall halo mass to form a galaxy is >108.5 M⊙⁠. The distribution of dark subhaloes is significantly more concentrated in WDM due to the absence of low mass, recently accreted substructures that typically inhabit the outer parts of a MW halo in CDM. We show that subhaloes of mass [107, 108] M⊙ and within 30 kpc of the centre are the stripped remnants of larger haloes in both models. Therefore, their abundance in WDM is 3× higher than one would anticipate from the overall WDM subhalo population. We estimate that differences between CDM and WDM concentration–mass relations can be probed for subhalo–stream impact parameters <2 kpc. Finally, we find that the impact of WDM on planes of satellites is likely negligible. Comprehensive comparisons with observations will require further work with high resolution, self-consistent hydrodynamical simulations.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Date accepted:20 August 2021
Date deposited:15 November 2021
Date of first online publication:28 August 2021
Date first made open access:15 November 2021

Save or Share this output

Look up in GoogleScholar