000477165 001__ 477165
000477165 005__ 20230214113514.0
000477165 0247_ $$2INSPIRETeX$$aFischer:2022rko
000477165 0247_ $$2inspire$$ainspire:2077888
000477165 0247_ $$2arXiv$$aarXiv:2205.02243
000477165 0247_ $$2datacite_doi$$a10.3204/PUBDB-2022-01926
000477165 037__ $$aPUBDB-2022-01926
000477165 041__ $$aEnglish
000477165 088__ $$2DESY$$aDESY-22-072
000477165 088__ $$2arXiv$$aarXiv:2205.02243
000477165 1001_ $$0M.S.Fischer.2$$aFischer, Moritz S.$$b0$$eCorresponding author
000477165 245__ $$aCosmological simulations with rare and frequent dark matter self-interactions
000477165 260__ $$c2022
000477165 3367_ $$0PUB:(DE-HGF)25$$2PUB:(DE-HGF)$$aPreprint$$bpreprint$$mpreprint$$s1652183155_13616
000477165 3367_ $$2ORCID$$aWORKING_PAPER
000477165 3367_ $$028$$2EndNote$$aElectronic Article
000477165 3367_ $$2DRIVER$$apreprint
000477165 3367_ $$2BibTeX$$aARTICLE
000477165 3367_ $$2DataCite$$aOutput Types/Working Paper
000477165 500__ $$a13 pages, 16 figures + appendices, submitted to MNRAS
000477165 520__ $$aDark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide - for the first time - upper limits on the cross-section for frequent self-interactions.
000477165 536__ $$0G:(DE-HGF)POF4-611$$a611 - Fundamental Particles and Forces (POF4-611)$$cPOF4-611$$fPOF IV$$x0
000477165 536__ $$0G:(GEPRIS)390833306$$aEXC 2121 - Das Quantisierte Universum (390833306)$$c390833306$$fDFG EXC 2121$$x1
000477165 588__ $$aDataset connected to INSPIRE
000477165 650_7 $$2INSPIRE$$adark matter, density
000477165 650_7 $$2INSPIRE$$ascattering, small-angle
000477165 650_7 $$2INSPIRE$$adark matter, halo
000477165 650_7 $$2INSPIRE$$amatter, power spectrum
000477165 650_7 $$2INSPIRE$$adark matter, scattering
000477165 650_7 $$2INSPIRE$$ahalo, density
000477165 650_7 $$2INSPIRE$$asatellite
000477165 650_7 $$2INSPIRE$$awide-angle
000477165 650_7 $$2INSPIRE$$acorrelation function
000477165 650_7 $$2INSPIRE$$asuppression
000477165 650_7 $$2INSPIRE$$acosmological model
000477165 693__ $$0EXP:(DE-MLZ)NOSPEC-20140101$$5EXP:(DE-MLZ)NOSPEC-20140101$$eNo specific instrument$$x0
000477165 7001_ $$0M.Brueggen.1$$aBrüggen, Marcus$$b1
000477165 7001_ $$0P:(DE-H253)PIP1022003$$aSchmidt-Hoberg, Kai$$b2
000477165 7001_ $$0K.Dolag.1$$aDolag, Klaus$$b3
000477165 7001_ $$aKahlhoefer, Felix$$b4
000477165 7001_ $$0A.Ragagnin.1$$aRagagnin, Antonio$$b5
000477165 7001_ $$0A.Robertson.5$$aRobertson, Andrew$$b6
000477165 8564_ $$uhttps://bib-pubdb1.desy.de/record/477165/files/HTML-Approval_of_scientific_publication.html
000477165 8564_ $$uhttps://bib-pubdb1.desy.de/record/477165/files/PDF-Approval_of_scientific_publication.pdf
000477165 8564_ $$uhttps://bib-pubdb1.desy.de/record/477165/files/2205.02243v1.pdf$$yOpenAccess
000477165 8564_ $$uhttps://bib-pubdb1.desy.de/record/477165/files/2205.02243v1.pdf?subformat=pdfa$$xpdfa$$yOpenAccess
000477165 909CO $$ooai:bib-pubdb1.desy.de:477165$$pdnbdelivery$$pdriver$$pVDB$$popen_access$$popenaire
000477165 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1022003$$aDeutsches Elektronen-Synchrotron$$b2$$kDESY
000477165 9131_ $$0G:(DE-HGF)POF4-611$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vFundamental Particles and Forces$$x0
000477165 9141_ $$y2022
000477165 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000477165 915__ $$0LIC:(DE-HGF)CCBY4$$2HGFVOC$$aCreative Commons Attribution CC BY 4.0
000477165 915__ $$0StatID:(DE-HGF)0580$$2StatID$$aPublished
000477165 9201_ $$0I:(DE-H253)T-20120731$$kT$$lTheorie-Gruppe$$x0
000477165 980__ $$apreprint
000477165 980__ $$aVDB
000477165 980__ $$aUNRESTRICTED
000477165 980__ $$aI:(DE-H253)T-20120731
000477165 9801_ $$aFullTexts