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

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...

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Detalles Bibliográficos
Autores principales: Chimento, Luis Pascual, Forte, Mónica Isabel, Richarte, Martín Gustavo
Publicado: 2013
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_14346044_v73_n1_p1_Chimento
http://hdl.handle.net/20.500.12110/paper_14346044_v73_n1_p1_Chimento
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_14346044_v73_n1_p1_Chimento
record_format dspace
spelling paper:paper_14346044_v73_n1_p1_Chimento2023-06-08T16:14:51Z Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component Chimento, Luis Pascual Forte, Mónica Isabel Richarte, Martín Gustavo 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 find 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. © 2013 Springer-Verlag Berlin Heidelberg and Società Italiana di Fisica. Fil:Chimento, L.P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Forte, M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Richarte, M.G. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2013 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_14346044_v73_n1_p1_Chimento http://hdl.handle.net/20.500.12110/paper_14346044_v73_n1_p1_Chimento
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
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 find 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. © 2013 Springer-Verlag Berlin Heidelberg and Società Italiana di Fisica.
author Chimento, Luis Pascual
Forte, Mónica Isabel
Richarte, Martín Gustavo
spellingShingle Chimento, Luis Pascual
Forte, Mónica Isabel
Richarte, Martín Gustavo
Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component
author_facet Chimento, Luis Pascual
Forte, Mónica Isabel
Richarte, Martín Gustavo
author_sort Chimento, Luis Pascual
title Modified holographic Ricci dark energy coupled to interacting dark matter and a non-interacting baryonic component
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
publishDate 2013
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_14346044_v73_n1_p1_Chimento
http://hdl.handle.net/20.500.12110/paper_14346044_v73_n1_p1_Chimento
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AT fortemonicaisabel modifiedholographicriccidarkenergycoupledtointeractingdarkmatterandanoninteractingbaryoniccomponent
AT richartemartingustavo modifiedholographicriccidarkenergycoupledtointeractingdarkmatterandanoninteractingbaryoniccomponent
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