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Dark matter haloes in interacting dark energy models: Formation history, density profile, spin, and shape

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dc.contributor.authorYun Liu-
dc.contributor.authorShihong Liao-
dc.contributor.authorXiangkun Liu-
dc.contributor.authorJiajun Zhang-
dc.contributor.authorRui An-
dc.contributor.authorZuhui Fan-
dc.date.accessioned2022-03-24T02:30:04Z-
dc.date.available2022-03-24T02:30:04Z-
dc.date.created2022-03-15-
dc.date.issued2022-04-
dc.identifier.issn0035-8711-
dc.identifier.urihttps://pr.ibs.re.kr/handle/8788114/11301-
dc.description.abstract© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.The interacting dark energy (IDE) model, which considers the interaction between dark energy and dark matter, provides a natural mechanism to alleviate the coincidence problem and can also relieve the observational tensions under the ΛCDM model. Previous studies have put constraints on IDE models by observations of cosmic expansion history, cosmic microwave background, and large-scale structures. However, these data are not yet enough to distinguish IDE models from ΛCDM effectively. Because the non-linear structure formation contains rich cosmological information, it can provide additional means to differentiate alternative models. In this paper, based on a set of N-body simulations for IDE models, we investigate the formation histories and properties of dark matter haloes and compare with their ΛCDM counterparts. For the model with dark matter decaying into dark energy and the parameters being the best-fitting values from previous constraints, the structure formation is markedly slowed down, and the haloes have systematically lower mass, looser internal structure, higher spin, and anisotropy. This is inconsistent with the observed structure formation, and thus this model can be safely ruled out from the perspective of non-linear structure formation. Moreover, we find that the ratio of halo concentrations between IDE and ΛCDM counterparts depends sensitively on the interaction parameter and is independent of halo mass. This can act as a powerful probe to constrain IDE models. Our results concretely demonstrate that the interaction of the two dark components can affect the halo formation considerably, and therefore the constraints from non-linear structures are indispensable.-
dc.language영어-
dc.publisherOxford University Press-
dc.titleDark matter haloes in interacting dark energy models: Formation history, density profile, spin, and shape-
dc.typeArticle-
dc.type.rimsART-
dc.identifier.wosid000767859900011-
dc.identifier.scopusid2-s2.0-85125439384-
dc.identifier.rimsid77882-
dc.contributor.affiliatedAuthorJiajun Zhang-
dc.identifier.doi10.1093/mnras/stac229-
dc.identifier.bibliographicCitationMonthly Notices of the Royal Astronomical Society, v.511, no.2, pp.3076 - 3088-
dc.relation.isPartOfMonthly Notices of the Royal Astronomical Society-
dc.citation.titleMonthly Notices of the Royal Astronomical Society-
dc.citation.volume511-
dc.citation.number2-
dc.citation.startPage3076-
dc.citation.endPage3088-
dc.description.journalClass1-
dc.description.journalClass1-
dc.description.isOpenAccessN-
dc.description.journalRegisteredClassscie-
dc.description.journalRegisteredClassscopus-
dc.relation.journalWebOfScienceCategoryAstronomy & Astrophysics-
dc.subject.keywordPlusANGULAR-MOMENTUM-
dc.subject.keywordPlusMASS FUNCTION-
dc.subject.keywordPlusINITIAL CONDITIONS-
dc.subject.keywordPlusEVOLUTION-
dc.subject.keywordPlusCLUSTERS-
dc.subject.keywordPlusQUINTESSENCE-
dc.subject.keywordPlusSIMULATIONS-
dc.subject.keywordPlusGALAXIES-
dc.subject.keywordPlusORIGIN-
dc.subject.keywordPlusSECTOR-
dc.subject.keywordAuthorCosmology: theory-
dc.subject.keywordAuthorDark energy-
dc.subject.keywordAuthorDark matter-
dc.subject.keywordAuthorMethods: numerical-
Appears in Collections:
Center for Fundamental Theory(순수물리이론 연구단) > 1. Journal Papers (저널논문)
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