Cosmological simulations with rare and frequent dark matter self-interactions

Author:

Fischer Moritz S1ORCID,Brüggen Marcus1,Schmidt-Hoberg Kai2,Dolag Klaus34,Kahlhoefer Felix56,Ragagnin Antonio789,Robertson Andrew10ORCID

Affiliation:

1. Hamburger Sternwarte, Universität Hamburg , Gojenbergsweg 112, D-21029 Hamburg, Germany

2. Deutsches Elektronen-Synchrotron DESY , Notkestr. 85, D-22607 Hamburg, Germany

3. Universitäts-Sternwarte München, Faculty of Physics, Ludwig-Maximilians-Universität , Scheinerstr. 1, D-81679 München, Germany

4. Max-Planck-Institut für Astrophysik , Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany

5. Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University , D-52056 Aachen, Germany

6. Institute for Theoretical Particle Physics (TTP), Karlsruhe Institute of Technology (KIT) , D-76128 Karlsruhe, Germany

7. Dipartimento di Fisica e Astronomia ‘Augusto Righi’, Alma Mater Studiorum Università di Bologna , via Gobetti 93/2, I-40129 Bologna, Italy

8. INAF-Osservatorio Astronomico di Trieste , via G. B. Tiepolo 11, I-34143 Trieste, Italy

9. IFPU – Institute for Fundamental Physics of the Universe , Via Beirut 2, I-34014 Trieste, Italy

10. Jet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, Pasadena, CA 91109, USA

Abstract

ABSTRACT Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self-scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function, and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall, we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide – for the first time – upper limits on the cross-section for frequent self-interactions.

Funder

Deutsche Forschungsgemeinschaft

European Research Council

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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