How early is early dark energy?
We investigate constraints on early dark energy (EDE) from the Cosmic Microwave Background (CMB) anisotropy, taking into account data from WMAP9 combined with latest small scale measurements from the South Pole Telescope (SPT). For a constant EDE fraction we propose a new parametrization with one le...
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ftdatacite:10.48550/arxiv.1301.5279 2023-05-15T18:22:39+02:00 How early is early dark energy? Pettorino, Valeria Amendola, Luca Wetterich, Christof 2013 https://dx.doi.org/10.48550/arxiv.1301.5279 https://arxiv.org/abs/1301.5279 unknown arXiv https://dx.doi.org/10.1103/physrevd.87.083009 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ Cosmology and Nongalactic Astrophysics astro-ph.CO High Energy Physics - Phenomenology hep-ph FOS Physical sciences article-journal Article ScholarlyArticle Text 2013 ftdatacite https://doi.org/10.48550/arxiv.1301.5279 https://doi.org/10.1103/physrevd.87.083009 2022-04-01T13:24:27Z We investigate constraints on early dark energy (EDE) from the Cosmic Microwave Background (CMB) anisotropy, taking into account data from WMAP9 combined with latest small scale measurements from the South Pole Telescope (SPT). For a constant EDE fraction we propose a new parametrization with one less parameter but still enough to provide similar results to the ones previously studied in literature. The main emphasis of our analysis, however, compares a new set of different EDE parametrizations that reveal how CMB constraints depend on the redshift epoch at which Dark Energy was non negligible. We find that bounds on EDE get substantially weaker if dark energy starts to be non-negligible later, with early dark energy fraction Omega_e free to go up to about 5% at 2 sigma if the onset of EDE happens at z < 100. Tight bounds around 1-2% are obtained whenever dark energy is present at last scattering, even if its effects switch off afterwards. We show that the CMB mainly constrains the presence of Dark Energy at the time of its emission, while EDE-modifications of the subsequent growth of structure are less important. : 14 pages, 9 figures Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole |
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Cosmology and Nongalactic Astrophysics astro-ph.CO High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
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Cosmology and Nongalactic Astrophysics astro-ph.CO High Energy Physics - Phenomenology hep-ph FOS Physical sciences Pettorino, Valeria Amendola, Luca Wetterich, Christof How early is early dark energy? |
topic_facet |
Cosmology and Nongalactic Astrophysics astro-ph.CO High Energy Physics - Phenomenology hep-ph FOS Physical sciences |
description |
We investigate constraints on early dark energy (EDE) from the Cosmic Microwave Background (CMB) anisotropy, taking into account data from WMAP9 combined with latest small scale measurements from the South Pole Telescope (SPT). For a constant EDE fraction we propose a new parametrization with one less parameter but still enough to provide similar results to the ones previously studied in literature. The main emphasis of our analysis, however, compares a new set of different EDE parametrizations that reveal how CMB constraints depend on the redshift epoch at which Dark Energy was non negligible. We find that bounds on EDE get substantially weaker if dark energy starts to be non-negligible later, with early dark energy fraction Omega_e free to go up to about 5% at 2 sigma if the onset of EDE happens at z < 100. Tight bounds around 1-2% are obtained whenever dark energy is present at last scattering, even if its effects switch off afterwards. We show that the CMB mainly constrains the presence of Dark Energy at the time of its emission, while EDE-modifications of the subsequent growth of structure are less important. : 14 pages, 9 figures |
format |
Text |
author |
Pettorino, Valeria Amendola, Luca Wetterich, Christof |
author_facet |
Pettorino, Valeria Amendola, Luca Wetterich, Christof |
author_sort |
Pettorino, Valeria |
title |
How early is early dark energy? |
title_short |
How early is early dark energy? |
title_full |
How early is early dark energy? |
title_fullStr |
How early is early dark energy? |
title_full_unstemmed |
How early is early dark energy? |
title_sort |
how early is early dark energy? |
publisher |
arXiv |
publishDate |
2013 |
url |
https://dx.doi.org/10.48550/arxiv.1301.5279 https://arxiv.org/abs/1301.5279 |
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South Pole |
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South Pole |
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South pole |
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South pole |
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https://dx.doi.org/10.1103/physrevd.87.083009 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1301.5279 https://doi.org/10.1103/physrevd.87.083009 |
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