Constraining dark matter candidates from structure formation
By C. Bœhm, P. Fayet, R. Schaeffer. 2000
163 citations recorded by the source corpus.
Abstract We show that collisional damping of adiabatic primordial fluctuations yields constraints on the possible range of mass and interaction rates of dark matter particles. Our analysis relies on a general classification of dark matter candidates, that we establish independently of any specific particle theory or model. It holds for very weakly as well as very strongly interacting particles. From a relation between the collisional damping scale and the dark matter interaction rate, we find that dark matter candidates must have cross-sections at decoupling ≲10 −33 m dm 1 MeV cm 2 with photons and ≲10 −37 m dm 1 MeV cm 2 with neutrinos, to explain the observed primordial structures of 10 9 M ⊙ . When marginally satisfied, these damping constraints provide warm dark matter candidates whose astrophysical relevance is worth to be explored. They also leave open less known regions of parameter space corresponding to particles having much higher interaction rates with other species than neutrinos and photons.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/54ac14b0122af2c3c8f2e41288901c4b8442e125
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In Astronomy and Astrophysics
- E. di Valentino
- C. Bœhm
- R. Wilkinson
- Céline Boehm
- E. Hivon
- F. Bouchet
- Julien Lesgourgues
- S. Vagnozzi
In Nuclear and High Energy Physics
- E. di Valentino
- C. Bœhm
- R. Wilkinson
- Céline Boehm
- E. Hivon
- F. Bouchet
- Julien Lesgourgues
- S. Vagnozzi
Citations in the corpus
- Constraining dark matter-neutrino interactions using the CMB and large-scale structure (2014, background): “Interactions of DM beyond gravity lead to a suppression of the primordial density fluctuations, erasing structures with a size smaller than the “collisional damping scale” [5, 7].”
- Reducing the H0 and σ8 tensions with dark matter-neutrino interactions. (2017, background): “Dark matter-baryon and dark matter self-interactions can also erase the DM fluctuations but the u ratio needs to be of order 1 to produce the same effects as the one considered here [2,3], given that there are many less baryons than radiation in the Universe and baryons are nonrelativistic.”