Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component

Autores
Chimento, Luis Pascual; Forte, Mónica; Richarte, Martín Gustavo
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We examine a Friedmann-Robertson-Walker universe filled with interacting dark matter, modified holographic Ricci dark energy (MHRDE), and a decoupled baryonic component.The estimations of the cosmic parameters with Hubble data lead to an age of the universe of 13.17 Gyr and show that the MHRDE is free from the cosmic-age problem at low redshift (0 ≤ z ≤ 2) in contrast to holographic Ricci dark energy (HRDE) case. We constrain the parameters with the Union2 data set and contrast with the Hubble data. We also study the behavior of dark energy at early times by taking into account the severe bounds found at recombination era and/or at big bang nucleosynthesis. The inclusion of a non interacting baryonic matter forces that the amount of dark energy at zt ∼ O(1) changes abruptly implying that Ωx(z ≃ 1100) = 0.03, so the bounds reported by the forecast of Planck and CMBPol experiments are more favored for the MHRDE model than in the case of HRDE cutoff. For the former model, we also obtain that at high redshift the fraction of dark energy varies from 0.006 to 0.002, then the amount of Ωx at the big bang nucleosynthesis era does not disturb the observed Helium abundance in the universe provided that the bound Ωx(z ≃ 1010) < 0.21 is hold.
Fil: Chimento, Luis Pascual. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Fil: Forte, Mónica. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina
Fil: Richarte, Martín Gustavo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Materia
Interacting Dark Sector
Holographic Dark Energy
Triple Cosmic Coincidence
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/698
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic componentChimento, Luis PascualForte, MónicaRicharte, Martín GustavoInteracting Dark SectorHolographic Dark EnergyTriple Cosmic Coincidencehttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We examine a Friedmann-Robertson-Walker universe filled with interacting dark matter, modified holographic Ricci dark energy (MHRDE), and a decoupled baryonic component.The estimations of the cosmic parameters with Hubble data lead to an age of the universe of 13.17 Gyr and show that the MHRDE is free from the cosmic-age problem at low redshift (0 ≤ z ≤ 2) in contrast to holographic Ricci dark energy (HRDE) case. We constrain the parameters with the Union2 data set and contrast with the Hubble data. We also study the behavior of dark energy at early times by taking into account the severe bounds found at recombination era and/or at big bang nucleosynthesis. The inclusion of a non interacting baryonic matter forces that the amount of dark energy at zt ∼ O(1) changes abruptly implying that Ωx(z ≃ 1100) = 0.03, so the bounds reported by the forecast of Planck and CMBPol experiments are more favored for the MHRDE model than in the case of HRDE cutoff. For the former model, we also obtain that at high redshift the fraction of dark energy varies from 0.006 to 0.002, then the amount of Ωx at the big bang nucleosynthesis era does not disturb the observed Helium abundance in the universe provided that the bound Ωx(z ≃ 1010) < 0.21 is hold.Fil: Chimento, Luis Pascual. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; ArgentinaFil: Forte, Mónica. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; ArgentinaFil: Richarte, Martín Gustavo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; ArgentinaSpringer2013-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/698Chimento, Luis Pascual; Forte, Mónica; Richarte, Martín Gustavo; Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component; Springer; European Physical Journal C: Particles and Fields; C73; 2352; 1-2013; 1-91434-6044enginfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1301.2737info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1140/epjc/s10052-013-2285-1info:eu-repo/semantics/altIdentifier/doi/10.1140/epjc/s10052-013-2285-1info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:02:18Zoai:ri.conicet.gov.ar:11336/698instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-03 10:02:18.819CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
title Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
spellingShingle Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
Chimento, Luis Pascual
Interacting Dark Sector
Holographic Dark Energy
Triple Cosmic Coincidence
title_short Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
title_full Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
title_fullStr Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
title_full_unstemmed Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
title_sort Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component
dc.creator.none.fl_str_mv Chimento, Luis Pascual
Forte, Mónica
Richarte, Martín Gustavo
author Chimento, Luis Pascual
author_facet Chimento, Luis Pascual
Forte, Mónica
Richarte, Martín Gustavo
author_role author
author2 Forte, Mónica
Richarte, Martín Gustavo
author2_role author
author
dc.subject.none.fl_str_mv Interacting Dark Sector
Holographic Dark Energy
Triple Cosmic Coincidence
topic Interacting Dark Sector
Holographic Dark Energy
Triple Cosmic Coincidence
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We examine a Friedmann-Robertson-Walker universe filled with interacting dark matter, modified holographic Ricci dark energy (MHRDE), and a decoupled baryonic component.The estimations of the cosmic parameters with Hubble data lead to an age of the universe of 13.17 Gyr and show that the MHRDE is free from the cosmic-age problem at low redshift (0 ≤ z ≤ 2) in contrast to holographic Ricci dark energy (HRDE) case. We constrain the parameters with the Union2 data set and contrast with the Hubble data. We also study the behavior of dark energy at early times by taking into account the severe bounds found at recombination era and/or at big bang nucleosynthesis. The inclusion of a non interacting baryonic matter forces that the amount of dark energy at zt ∼ O(1) changes abruptly implying that Ωx(z ≃ 1100) = 0.03, so the bounds reported by the forecast of Planck and CMBPol experiments are more favored for the MHRDE model than in the case of HRDE cutoff. For the former model, we also obtain that at high redshift the fraction of dark energy varies from 0.006 to 0.002, then the amount of Ωx at the big bang nucleosynthesis era does not disturb the observed Helium abundance in the universe provided that the bound Ωx(z ≃ 1010) < 0.21 is hold.
Fil: Chimento, Luis Pascual. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Fil: Forte, Mónica. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina
Fil: Richarte, Martín Gustavo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
description We examine a Friedmann-Robertson-Walker universe filled with interacting dark matter, modified holographic Ricci dark energy (MHRDE), and a decoupled baryonic component.The estimations of the cosmic parameters with Hubble data lead to an age of the universe of 13.17 Gyr and show that the MHRDE is free from the cosmic-age problem at low redshift (0 ≤ z ≤ 2) in contrast to holographic Ricci dark energy (HRDE) case. We constrain the parameters with the Union2 data set and contrast with the Hubble data. We also study the behavior of dark energy at early times by taking into account the severe bounds found at recombination era and/or at big bang nucleosynthesis. The inclusion of a non interacting baryonic matter forces that the amount of dark energy at zt ∼ O(1) changes abruptly implying that Ωx(z ≃ 1100) = 0.03, so the bounds reported by the forecast of Planck and CMBPol experiments are more favored for the MHRDE model than in the case of HRDE cutoff. For the former model, we also obtain that at high redshift the fraction of dark energy varies from 0.006 to 0.002, then the amount of Ωx at the big bang nucleosynthesis era does not disturb the observed Helium abundance in the universe provided that the bound Ωx(z ≃ 1010) < 0.21 is hold.
publishDate 2013
dc.date.none.fl_str_mv 2013-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/698
Chimento, Luis Pascual; Forte, Mónica; Richarte, Martín Gustavo; Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component; Springer; European Physical Journal C: Particles and Fields; C73; 2352; 1-2013; 1-9
1434-6044
url http://hdl.handle.net/11336/698
identifier_str_mv Chimento, Luis Pascual; Forte, Mónica; Richarte, Martín Gustavo; Modified holographic Ricci dark energy coupled to interacting dark matter and a non interacting baryonic component; Springer; European Physical Journal C: Particles and Fields; C73; 2352; 1-2013; 1-9
1434-6044
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1301.2737
info:eu-repo/semantics/altIdentifier/url/https://link.springer.com/article/10.1140/epjc/s10052-013-2285-1
info:eu-repo/semantics/altIdentifier/doi/10.1140/epjc/s10052-013-2285-1
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Springer
publisher.none.fl_str_mv Springer
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.13397

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