Cosmological constraints on nonadiabatic dark energy perturbations

The exact nature of dark energy is currently unknown and its cosmological perturbations, when dark energy is assumed not to be the cosmological constant, are usually modeled as adiabatic. Here we explore the possibility that dark energy might have a nonadiabatic component and we examine how it would...

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Detalles Bibliográficos
Autores: Arjona, Rubén, García-Bellido, Juan, Nesseris, Savvas
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2020
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/233261
Acceso en línea:http://hdl.handle.net/10261/233261
Access Level:acceso abierto
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spelling Cosmological constraints on nonadiabatic dark energy perturbationsArjona, RubénGarcía-Bellido, JuanNesseris, SavvasThe exact nature of dark energy is currently unknown and its cosmological perturbations, when dark energy is assumed not to be the cosmological constant, are usually modeled as adiabatic. Here we explore the possibility that dark energy might have a nonadiabatic component and we examine how it would affect several key cosmological observables. We present analytical solutions for the growth rate and growth index of matter density perturbations and compare them to both numerical solutions of the fluid equations and an implementation in the Boltzmann code CLASS, finding that they all agree to well below one percent. We also perform a Monte Carlo analysis to derive constraints on the parameters of the nonadiabatic component using the latest cosmological data, including the temperature and polarization spectra of the cosmic microwave background as observed by Planck, the baryon acoustic oscillations, the Pantheon type Ia supernovae compilation and last, measurements of redshift space distortions (RSDs) of the growth rate of matter perturbations. We find that the amplitude of the nonadiabatic pressure perturbation is consistent with zero within 1σ. Finally, we also present a new, publicly available, RSD likelihood for MONTE PYTHON based on the "Gold 2018"growth-rate data compilation.American Physical SocietyConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versionPublisher's versioninfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/233261reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://dx.doi.org/10.1103/PhysRevD.102.103526Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2332612026-05-22T06:33:51Z
dc.title.none.fl_str_mv Cosmological constraints on nonadiabatic dark energy perturbations
title Cosmological constraints on nonadiabatic dark energy perturbations
spellingShingle Cosmological constraints on nonadiabatic dark energy perturbations
Arjona, Rubén
title_short Cosmological constraints on nonadiabatic dark energy perturbations
title_full Cosmological constraints on nonadiabatic dark energy perturbations
title_fullStr Cosmological constraints on nonadiabatic dark energy perturbations
title_full_unstemmed Cosmological constraints on nonadiabatic dark energy perturbations
title_sort Cosmological constraints on nonadiabatic dark energy perturbations
dc.creator.none.fl_str_mv Arjona, Rubén
García-Bellido, Juan
Nesseris, Savvas
author Arjona, Rubén
author_facet Arjona, Rubén
García-Bellido, Juan
Nesseris, Savvas
author_role author
author2 García-Bellido, Juan
Nesseris, Savvas
author2_role author
author
dc.contributor.none.fl_str_mv Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
description The exact nature of dark energy is currently unknown and its cosmological perturbations, when dark energy is assumed not to be the cosmological constant, are usually modeled as adiabatic. Here we explore the possibility that dark energy might have a nonadiabatic component and we examine how it would affect several key cosmological observables. We present analytical solutions for the growth rate and growth index of matter density perturbations and compare them to both numerical solutions of the fluid equations and an implementation in the Boltzmann code CLASS, finding that they all agree to well below one percent. We also perform a Monte Carlo analysis to derive constraints on the parameters of the nonadiabatic component using the latest cosmological data, including the temperature and polarization spectra of the cosmic microwave background as observed by Planck, the baryon acoustic oscillations, the Pantheon type Ia supernovae compilation and last, measurements of redshift space distortions (RSDs) of the growth rate of matter perturbations. We find that the amplitude of the nonadiabatic pressure perturbation is consistent with zero within 1σ. Finally, we also present a new, publicly available, RSD likelihood for MONTE PYTHON based on the "Gold 2018"growth-rate data compilation.
publishDate 2020
dc.date.none.fl_str_mv 2020
2021
2021
2021
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
Publisher's version
info:eu-repo/semantics/publishedVersion
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/233261
url http://hdl.handle.net/10261/233261
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv http://dx.doi.org/10.1103/PhysRevD.102.103526
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv American Physical Society
publisher.none.fl_str_mv American Physical Society
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,811543

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