Effects of shear and rotation on the spherical collapse model for clustering dark energy

In the framework of the spherical collapse model, we study the influence of shear and rotation terms for dark matter fluid in clustering dark energy models. We evaluate, for different equations of state, the effects of these terms on the linear overdensity threshold parameter, δc, and on the virial...

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Principais autores: Pace, Francesco, Batista, Ronaldo Carlotto, Popolo, Antonino del
Formato: article
Idioma:English
Publicado em: Oxford University Press
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Methods: analytical
Dark energy
Cosmology: theory
Endereço do item:https://repositorio.ufrn.br/handle/123456789/30830
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spelling ri-123456789-308302020-12-06T08:06:53Z Effects of shear and rotation on the spherical collapse model for clustering dark energy Pace, Francesco Batista, Ronaldo Carlotto Popolo, Antonino del Methods: analytical Dark energy Cosmology: theory In the framework of the spherical collapse model, we study the influence of shear and rotation terms for dark matter fluid in clustering dark energy models. We evaluate, for different equations of state, the effects of these terms on the linear overdensity threshold parameter, δc, and on the virial overdensity, ΔV. The evaluation of their effects on δc allows us to infer the modifications occurring on the mass function. Due to ambiguities in the definition of the halo mass in the case of clustering dark energy, we consider two different situations: the first is the classical one where the mass is of the dark matter halo only, while the second one is given by the sum of the mass of dark matter and dark energy. As previously found, the spherical collapse model becomes mass dependent and the two additional terms oppose the collapse of the perturbations, especially on galactic scales, with respect to the spherical non-rotating model, while on cluster scales the effects of shear and rotation become negligible. The values for δc and ΔV are higher than the standard spherical model. Regarding the effects of the additional non-linear terms on the mass function, we evaluate the number density of haloes. As expected, major differences appear at high masses and redshifts. In particular, quintessence (phantom) models predict more (less) objects with respect to the Λ colddarkmatter model, and the mass correction due to the contribution of the dark energy component has negligible effects on the overall number of structures. 2020-12-04T20:09:59Z 2020-12-04T20:09:59Z 2014-11-21 article PACE, Francesco; BATISTA, Ronaldo C.; POPOLO, Antonino del. Effects of shear and rotation on the spherical collapse model for clustering dark energy. Monthly Notices of the Royal Astronomical Society, [S.L.], v. 445, n. 1, p. 648-659, 29 set. 2014. Disponível em: https://academic.oup.com/mnras/article/445/1/648/1749251. Acesso em: 02 out. 2020. http://dx.doi.org/10.1093/mnras/stu1782. 0035-8711 1365-2966 https://repositorio.ufrn.br/handle/123456789/30830 10.1093/mnras/stu1782 en application/pdf Oxford University Press
institution Repositório Institucional
collection RI - UFRN
language English
topic Methods: analytical
Dark energy
Cosmology: theory
spellingShingle Methods: analytical
Dark energy
Cosmology: theory
Pace, Francesco
Batista, Ronaldo Carlotto
Popolo, Antonino del
Effects of shear and rotation on the spherical collapse model for clustering dark energy
description In the framework of the spherical collapse model, we study the influence of shear and rotation terms for dark matter fluid in clustering dark energy models. We evaluate, for different equations of state, the effects of these terms on the linear overdensity threshold parameter, δc, and on the virial overdensity, ΔV. The evaluation of their effects on δc allows us to infer the modifications occurring on the mass function. Due to ambiguities in the definition of the halo mass in the case of clustering dark energy, we consider two different situations: the first is the classical one where the mass is of the dark matter halo only, while the second one is given by the sum of the mass of dark matter and dark energy. As previously found, the spherical collapse model becomes mass dependent and the two additional terms oppose the collapse of the perturbations, especially on galactic scales, with respect to the spherical non-rotating model, while on cluster scales the effects of shear and rotation become negligible. The values for δc and ΔV are higher than the standard spherical model. Regarding the effects of the additional non-linear terms on the mass function, we evaluate the number density of haloes. As expected, major differences appear at high masses and redshifts. In particular, quintessence (phantom) models predict more (less) objects with respect to the Λ colddarkmatter model, and the mass correction due to the contribution of the dark energy component has negligible effects on the overall number of structures.
format article
author Pace, Francesco
Batista, Ronaldo Carlotto
Popolo, Antonino del
author_facet Pace, Francesco
Batista, Ronaldo Carlotto
Popolo, Antonino del
author_sort Pace, Francesco
title Effects of shear and rotation on the spherical collapse model for clustering dark energy
title_short Effects of shear and rotation on the spherical collapse model for clustering dark energy
title_full Effects of shear and rotation on the spherical collapse model for clustering dark energy
title_fullStr Effects of shear and rotation on the spherical collapse model for clustering dark energy
title_full_unstemmed Effects of shear and rotation on the spherical collapse model for clustering dark energy
title_sort effects of shear and rotation on the spherical collapse model for clustering dark energy
publisher Oxford University Press
publishDate 2020
url https://repositorio.ufrn.br/handle/123456789/30830
work_keys_str_mv AT pacefrancesco effectsofshearandrotationonthesphericalcollapsemodelforclusteringdarkenergy
AT batistaronaldocarlotto effectsofshearandrotationonthesphericalcollapsemodelforclusteringdarkenergy
AT popoloantoninodel effectsofshearandrotationonthesphericalcollapsemodelforclusteringdarkenergy
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