2015/12/31 by J.A Schewtschenko, J. A. Schewtschenko, C. M. Baugh +8 · 72 citations
Physics and Astronomy · #Astronomy #Astrophysics #Cold dark matter #Cosmology #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark energy #Dark matter #Dwarf galaxy problem #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy group #Hot dark matter #Milky Way #Neutrino #Particle physics #Physics #Satellite #Satellite galaxy #astro-ph.CO #hep-ph
paper · pdf · doi:10.1093/mnras/stw1078
published in Monthly Notices of the Royal Astronomical Society 461(3), 2282-2287 (Oxford University Press) · 6 pages, 3 figures, 1 table. Augmented content available for figures (cf. 'Augmented Content' section). V3: Matches version in MNRAS
arxiv created 2016/04/13 · openalex publication_date 2016/05/06 · arxiv updated 2016/05/16 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In the thermal dark matter (DM) paradigm, primordial interactions between DM and Standard Model particles are responsible for the observed DM relic density. In Bœhm et al., we showed that weak-strength interactions between DM and radiation (photons or neutrinos) can erase small-scale density fluctuations, leading to a suppression of the matter power spectrum compared to the collisionless cold DM (CDM) model. This results in fewer DM subhaloes within Milky Way-like DM haloes, implying a reduction in the abundance of satellite galaxies. Here we use very high-resolution N-body simulations to measure the dynamics of these subhaloes. We find that when interactions are included, the largest subhaloes are less concentrated than their counterparts in the collisionless CDM model and have rotation curves that match observational data, providing a new solution to the ‘too big to fail’ problem.