Using the Milky Way satellites to study interactions between cold dark matter and radiation
By C. Bœhm, Jascha A. Schewtschenko, R. Wilkinson, C. Baugh, Silvia Pascoli. 2014
136 citations recorded by the source corpus.
The cold dark matter (CDM) model faces persistent challenges on small scales. In particular, the model significantly overestimates the number of satellite galaxies around the Milky Way. Attempts to solve this problem remain controversial and have even led some to abandon CDM altogether. However, current simulations are limited by the assumption that dark matter feels only gravity. Here we show that including interactions between CDM and radiation (photons or neutrinos) leads to a dramatic reduction in the number of satellite galaxies, providing a potential solution to the Milky Way satellite problem and indicating that physics beyond gravity may be essential to make accurate predictions of structure formation on small scales. The methodology introduced here gives constraints on dark matter interactions that are significantly improved over those from the cosmic microwave background.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/87b34e0cce7ec21b20485141af29170ead8e1975
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Citations in the corpus
- “Non-cold” dark matter at small scales: a general approach (2017, background): “heses potentially able to induce a smallscale suppression in the matter power spectrum: a mixed (cold and warm) DM uid [23{26], DM particles coupled to dark energy [27{29] or to some relativistic uid [30,31], or Self-Interacting Dark Matter (SIDM) [32,33]. Dierent scenarios lead to dierent shapes in”
- Reducing the H0 and σ8 tensions with dark matter-neutrino interactions. (2017, background): “Such high values of the u ratio would question our understanding of structure formation, as it is expected that there would be little satellite companions left in the Milky Way [10].”
- ETHOS - an effective theory of structure formation: dark matter physics as a possible explanation of the small-scale CDM problems (2015, background): “…leading to cutoff scales of the primordial linear power spectrum that are on mass scales of order of dwarf galaxies and hence alleviate the overabundance problem of these (sub)halos in CDM cosmologies (Van den Aarssen et al. 2012; Bœhm et al. 2014; Schewtschenko et al. 2014; Buckley et al. 2014).”