Clustering dark energy and halo abundances
Autor(a) principal: | |
---|---|
Data de Publicação: | 2017 |
Outros Autores: | |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRN |
Texto Completo: | https://repositorio.ufrn.br/handle/123456789/30828 |
Resumo: | Within the standard paradigm, dark energy is taken as a homogeneous fluid that drives the accelerated expansion of the universe and does not contribute to the mass of collapsed objects such as galaxies and galaxy clusters. The abundance of galaxy clusters—measured through a variety of channels—has been extensively used to constrain the normalization of the power spectrum: it is an important probe as it allows us to test if the standard ΛCDM model can indeed accurately describe the evolution of structures across billions of years. It is then quite significant that the Planck satellite has detected, via the Sunyaev-Zel'dovich effect, less clusters than expected according to the primary CMB anisotropies. One of the simplest generalizations that could reconcile these observations is to consider models in which dark energy is allowed to cluster, i.e., allowing its sound speed to vary. In this case, however, the standard methods to compute the abundance of galaxy clusters need to be adapted to account for the contributions of dark energy. In particular, we examine the case of clustering dark energy—a dark energy fluid with negligible sound speed—with a redshift-dependent equation of state. We carefully study how the halo mass function is modified in this scenario, highlighting corrections that have not been considered before in the literature. We address modifications in the growth function, collapse threshold, virialization densities and also changes in the comoving scale of collapse and mass function normalization. Our results show that clustering dark energy can impact halo abundances at the level of 10%–30%, depending on the halo mass, and that cluster counts are modified by about 30% at a redshift of unity |
id |
UFRN_83e2a25418dace60b47b77360f1967d3 |
---|---|
oai_identifier_str |
oai:https://repositorio.ufrn.br:123456789/30828 |
network_acronym_str |
UFRN |
network_name_str |
Repositório Institucional da UFRN |
repository_id_str |
|
spelling |
Batista, Ronaldo CarlottoMarra, Valério2020-12-04T20:00:48Z2020-12-04T20:00:48Z2017-11-27BATISTA, Ronaldo C.; MARRA, Valerio. Clustering dark energy and halo abundances. Journal of Cosmology and Astroparticle Physics, [S.L.], v. 2017, n. 11, p. 048-048, 27 nov. 2017. Disponível em: https://iopscience.iop.org/article/10.1088/1475-7516/2017/11/048. Acesso em: 02 out. 2020. http://dx.doi.org/10.1088/1475-7516/2017/11/048.1475-7516https://repositorio.ufrn.br/handle/123456789/3082810.1088/1475-7516/2017/11/048IOP PublishingCluster countsDark energy theoryGalaxy clustersClustering dark energy and halo abundancesinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleWithin the standard paradigm, dark energy is taken as a homogeneous fluid that drives the accelerated expansion of the universe and does not contribute to the mass of collapsed objects such as galaxies and galaxy clusters. The abundance of galaxy clusters—measured through a variety of channels—has been extensively used to constrain the normalization of the power spectrum: it is an important probe as it allows us to test if the standard ΛCDM model can indeed accurately describe the evolution of structures across billions of years. It is then quite significant that the Planck satellite has detected, via the Sunyaev-Zel'dovich effect, less clusters than expected according to the primary CMB anisotropies. One of the simplest generalizations that could reconcile these observations is to consider models in which dark energy is allowed to cluster, i.e., allowing its sound speed to vary. In this case, however, the standard methods to compute the abundance of galaxy clusters need to be adapted to account for the contributions of dark energy. In particular, we examine the case of clustering dark energy—a dark energy fluid with negligible sound speed—with a redshift-dependent equation of state. We carefully study how the halo mass function is modified in this scenario, highlighting corrections that have not been considered before in the literature. We address modifications in the growth function, collapse threshold, virialization densities and also changes in the comoving scale of collapse and mass function normalization. Our results show that clustering dark energy can impact halo abundances at the level of 10%–30%, depending on the halo mass, and that cluster counts are modified by about 30% at a redshift of unityengreponame:Repositório Institucional da UFRNinstname:Universidade Federal do Rio Grande do Norte (UFRN)instacron:UFRNinfo:eu-repo/semantics/openAccessCC-LICENSElicense_rdflicense_rdfapplication/rdf+xml; charset=utf-8914https://repositorio.ufrn.br/bitstream/123456789/30828/2/license_rdf4d2950bda3d176f570a9f8b328dfbbefMD52LICENSElicense.txtlicense.txttext/plain; charset=utf-81484https://repositorio.ufrn.br/bitstream/123456789/30828/3/license.txte9597aa2854d128fd968be5edc8a28d9MD53TEXTClusteringDarkEnergy_BATISTA_2017.pdf.txtClusteringDarkEnergy_BATISTA_2017.pdf.txtExtracted texttext/plain48035https://repositorio.ufrn.br/bitstream/123456789/30828/4/ClusteringDarkEnergy_BATISTA_2017.pdf.txt18c3b1e84b5698ce80c3401321a7d621MD54THUMBNAILClusteringDarkEnergy_BATISTA_2017.pdf.jpgClusteringDarkEnergy_BATISTA_2017.pdf.jpgGenerated Thumbnailimage/jpeg1137https://repositorio.ufrn.br/bitstream/123456789/30828/5/ClusteringDarkEnergy_BATISTA_2017.pdf.jpgeda60937f745e3bcb5a31309d84281bcMD55123456789/308282022-10-19 18:17:50.13oai:https://repositorio.ufrn.br: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Repositório de PublicaçõesPUBhttp://repositorio.ufrn.br/oai/opendoar:2022-10-19T21:17:50Repositório Institucional da UFRN - Universidade Federal do Rio Grande do Norte (UFRN)false |
dc.title.pt_BR.fl_str_mv |
Clustering dark energy and halo abundances |
title |
Clustering dark energy and halo abundances |
spellingShingle |
Clustering dark energy and halo abundances Batista, Ronaldo Carlotto Cluster counts Dark energy theory Galaxy clusters |
title_short |
Clustering dark energy and halo abundances |
title_full |
Clustering dark energy and halo abundances |
title_fullStr |
Clustering dark energy and halo abundances |
title_full_unstemmed |
Clustering dark energy and halo abundances |
title_sort |
Clustering dark energy and halo abundances |
author |
Batista, Ronaldo Carlotto |
author_facet |
Batista, Ronaldo Carlotto Marra, Valério |
author_role |
author |
author2 |
Marra, Valério |
author2_role |
author |
dc.contributor.author.fl_str_mv |
Batista, Ronaldo Carlotto Marra, Valério |
dc.subject.por.fl_str_mv |
Cluster counts Dark energy theory Galaxy clusters |
topic |
Cluster counts Dark energy theory Galaxy clusters |
description |
Within the standard paradigm, dark energy is taken as a homogeneous fluid that drives the accelerated expansion of the universe and does not contribute to the mass of collapsed objects such as galaxies and galaxy clusters. The abundance of galaxy clusters—measured through a variety of channels—has been extensively used to constrain the normalization of the power spectrum: it is an important probe as it allows us to test if the standard ΛCDM model can indeed accurately describe the evolution of structures across billions of years. It is then quite significant that the Planck satellite has detected, via the Sunyaev-Zel'dovich effect, less clusters than expected according to the primary CMB anisotropies. One of the simplest generalizations that could reconcile these observations is to consider models in which dark energy is allowed to cluster, i.e., allowing its sound speed to vary. In this case, however, the standard methods to compute the abundance of galaxy clusters need to be adapted to account for the contributions of dark energy. In particular, we examine the case of clustering dark energy—a dark energy fluid with negligible sound speed—with a redshift-dependent equation of state. We carefully study how the halo mass function is modified in this scenario, highlighting corrections that have not been considered before in the literature. We address modifications in the growth function, collapse threshold, virialization densities and also changes in the comoving scale of collapse and mass function normalization. Our results show that clustering dark energy can impact halo abundances at the level of 10%–30%, depending on the halo mass, and that cluster counts are modified by about 30% at a redshift of unity |
publishDate |
2017 |
dc.date.issued.fl_str_mv |
2017-11-27 |
dc.date.accessioned.fl_str_mv |
2020-12-04T20:00:48Z |
dc.date.available.fl_str_mv |
2020-12-04T20:00:48Z |
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 |
BATISTA, Ronaldo C.; MARRA, Valerio. Clustering dark energy and halo abundances. Journal of Cosmology and Astroparticle Physics, [S.L.], v. 2017, n. 11, p. 048-048, 27 nov. 2017. Disponível em: https://iopscience.iop.org/article/10.1088/1475-7516/2017/11/048. Acesso em: 02 out. 2020. http://dx.doi.org/10.1088/1475-7516/2017/11/048. |
dc.identifier.uri.fl_str_mv |
https://repositorio.ufrn.br/handle/123456789/30828 |
dc.identifier.issn.none.fl_str_mv |
1475-7516 |
dc.identifier.doi.none.fl_str_mv |
10.1088/1475-7516/2017/11/048 |
identifier_str_mv |
BATISTA, Ronaldo C.; MARRA, Valerio. Clustering dark energy and halo abundances. Journal of Cosmology and Astroparticle Physics, [S.L.], v. 2017, n. 11, p. 048-048, 27 nov. 2017. Disponível em: https://iopscience.iop.org/article/10.1088/1475-7516/2017/11/048. Acesso em: 02 out. 2020. http://dx.doi.org/10.1088/1475-7516/2017/11/048. 1475-7516 10.1088/1475-7516/2017/11/048 |
url |
https://repositorio.ufrn.br/handle/123456789/30828 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.publisher.none.fl_str_mv |
IOP Publishing |
publisher.none.fl_str_mv |
IOP Publishing |
dc.source.none.fl_str_mv |
reponame:Repositório Institucional da UFRN instname:Universidade Federal do Rio Grande do Norte (UFRN) instacron:UFRN |
instname_str |
Universidade Federal do Rio Grande do Norte (UFRN) |
instacron_str |
UFRN |
institution |
UFRN |
reponame_str |
Repositório Institucional da UFRN |
collection |
Repositório Institucional da UFRN |
bitstream.url.fl_str_mv |
https://repositorio.ufrn.br/bitstream/123456789/30828/2/license_rdf https://repositorio.ufrn.br/bitstream/123456789/30828/3/license.txt https://repositorio.ufrn.br/bitstream/123456789/30828/4/ClusteringDarkEnergy_BATISTA_2017.pdf.txt https://repositorio.ufrn.br/bitstream/123456789/30828/5/ClusteringDarkEnergy_BATISTA_2017.pdf.jpg |
bitstream.checksum.fl_str_mv |
4d2950bda3d176f570a9f8b328dfbbef e9597aa2854d128fd968be5edc8a28d9 18c3b1e84b5698ce80c3401321a7d621 eda60937f745e3bcb5a31309d84281bc |
bitstream.checksumAlgorithm.fl_str_mv |
MD5 MD5 MD5 MD5 |
repository.name.fl_str_mv |
Repositório Institucional da UFRN - Universidade Federal do Rio Grande do Norte (UFRN) |
repository.mail.fl_str_mv |
|
_version_ |
1802117548037111808 |