Effects of shear and rotation on the spherical collapse model for clustering dark energy
Autor(a) principal: | |
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Data de Publicação: | 2014 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRN |
Texto Completo: | https://repositorio.ufrn.br/handle/123456789/30830 |
Resumo: | 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. |
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Pace, FrancescoBatista, Ronaldo CarlottoPopolo, Antonino del2020-12-04T20:09:59Z2020-12-04T20:09:59Z2014-11-21PACE, 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/stu1782.0035-87111365-2966https://repositorio.ufrn.br/handle/123456789/3083010.1093/mnras/stu1782Oxford University PressMethods: analyticalDark energyCosmology: theoryEffects of shear and rotation on the spherical collapse model for clustering dark energyinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleIn 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.engreponame:Repositório Institucional da UFRNinstname:Universidade Federal do Rio Grande do Norte (UFRN)instacron:UFRNinfo:eu-repo/semantics/openAccessLICENSElicense.txtlicense.txttext/plain; charset=utf-81484https://repositorio.ufrn.br/bitstream/123456789/30830/2/license.txte9597aa2854d128fd968be5edc8a28d9MD52ORIGINALEffectsOfShearAndRotation_2014.pdfEffectsOfShearAndRotation_2014.pdfapplication/pdf2443704https://repositorio.ufrn.br/bitstream/123456789/30830/1/EffectsOfShearAndRotation_2014.pdf1a5bea708095c3104c2289bcb44c2442MD51TEXTEffectsOfShearAndRotation_2014.pdf.txtEffectsOfShearAndRotation_2014.pdf.txtExtracted texttext/plain60053https://repositorio.ufrn.br/bitstream/123456789/30830/3/EffectsOfShearAndRotation_2014.pdf.txt638daaa7d5c9a7dec4f7d097f74db2f6MD53THUMBNAILEffectsOfShearAndRotation_2014.pdf.jpgEffectsOfShearAndRotation_2014.pdf.jpgGenerated Thumbnailimage/jpeg1780https://repositorio.ufrn.br/bitstream/123456789/30830/4/EffectsOfShearAndRotation_2014.pdf.jpgec50cd6a349155fc15ce4521e17f7ccaMD54123456789/308302020-12-06 05:06:53.744oai:https://repositorio.ufrn.br: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Repositório de PublicaçõesPUBhttp://repositorio.ufrn.br/oai/opendoar:2020-12-06T08:06:53Repositório Institucional da UFRN - Universidade Federal do Rio Grande do Norte (UFRN)false |
dc.title.pt_BR.fl_str_mv |
Effects of shear and rotation on the spherical collapse model for clustering dark energy |
title |
Effects of shear and rotation on the spherical collapse model for clustering dark energy |
spellingShingle |
Effects of shear and rotation on the spherical collapse model for clustering dark energy Pace, Francesco Methods: analytical Dark energy Cosmology: theory |
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 |
author |
Pace, Francesco |
author_facet |
Pace, Francesco Batista, Ronaldo Carlotto Popolo, Antonino del |
author_role |
author |
author2 |
Batista, Ronaldo Carlotto Popolo, Antonino del |
author2_role |
author author |
dc.contributor.author.fl_str_mv |
Pace, Francesco Batista, Ronaldo Carlotto Popolo, Antonino del |
dc.subject.por.fl_str_mv |
Methods: analytical Dark energy Cosmology: theory |
topic |
Methods: analytical Dark energy Cosmology: theory |
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. |
publishDate |
2014 |
dc.date.issued.fl_str_mv |
2014-11-21 |
dc.date.accessioned.fl_str_mv |
2020-12-04T20:09:59Z |
dc.date.available.fl_str_mv |
2020-12-04T20:09:59Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.citation.fl_str_mv |
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. |
dc.identifier.uri.fl_str_mv |
https://repositorio.ufrn.br/handle/123456789/30830 |
dc.identifier.issn.none.fl_str_mv |
0035-8711 1365-2966 |
dc.identifier.doi.none.fl_str_mv |
10.1093/mnras/stu1782 |
identifier_str_mv |
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 10.1093/mnras/stu1782 |
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https://repositorio.ufrn.br/handle/123456789/30830 |
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eng |
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eng |
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info:eu-repo/semantics/openAccess |
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openAccess |
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Oxford University Press |
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Oxford University Press |
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