Early dark energy in the pre- and postrecombination epochs
| Autor: | Adrià Gómez-Valent, Valeria Pettorino, Ziyang Zheng, Christof Wetterich, Luca Amendola |
|---|---|
| Přispěvatelé: | Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS) |
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Cosmology and Nongalactic Astrophysics (astro-ph.CO)
cosmic background radiation: decoupling satellite: Planck constraint Cosmic microwave background quintessence FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Type (model theory) baryon: oscillation: acoustic 01 natural sciences Omega dark matter gravitation: lens statistical analysis cosmological model: parameter space 0103 physical sciences dark energy 010303 astronomy & astrophysics Weak gravitational lensing Physics supernova: Type I density Hubble constant 010308 nuclear & particles physics background Cosmology: observations photon scaling parametrization cosmological model: fluid critical phenomena tension redshift Redshift velocity: acoustic recombination attractor Dark energy galaxy: cluster cosmological parameter Baryon acoustic oscillations Cosmology: theory [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Astrophysics - Cosmology and Nongalactic Astrophysics Quintessence |
| Zdroj: | Phys.Rev.D Phys.Rev.D, 2021, 104 (8), pp.083536. ⟨10.1103/PhysRevD.104.083536⟩ |
| DOI: | 10.1103/PhysRevD.104.083536⟩ |
| Popis: | Many quintessence models possess scaling or attractor solutions where the fraction of dark energy follows the dominant component in previous epochs of the expansion, or phase transitions may happen close to matter-radiation equality time. A non-negligible early dark energy (EDE) fraction around matter-radiation equality could contribute to alleviate the $H_0$ tension. We constrain the EDE fraction using two approaches: first, we use a fluid parameterization that mimics the plateaux of the dominant components in the past. An alternative tomographic approach constrains the EDE density in binned redshift intervals. This allows us to reconstruct $\Omega_{de}(z)$ before and after the decoupling of the CMB photons. We have employed Planck data 2018, the Pantheon supernovae of Type Ia (SNIa), galaxy clustering data, the prior on the absolute magnitude of SNIa by SH0ES, and weak lensing (WL) data from KiDS+VIKING-450 and DES-Y1. When we use a minimal parameterization mimicking the background plateaux, EDE has only a small impact on current cosmological tensions. The constraints on the EDE fraction weaken considerably when its sound speed is allowed to vary. By means of our binned analysis we put very tight constraints on the EDE fraction around the CMB decoupling time, $\lesssim 0.4\%$ at $2\sigma$ c.l. We confirm previous results that a significant EDE fraction in the radiation-dominated epoch (RDE) loosens the $H_0$ tension, but tends to worsen the $\sigma_8$ one. The presence of EDE in the matter-dominated era helps to alleviate this issue. When the SH0ES prior and WL data are considered in the fitting analysis in combination with data from CMB, SNIa and baryon acoustic oscillations, the EDE fractions are constrained to be $\lesssim 2.6\%$ in the RDE epoch and $\lesssim 1.5\%$ in the redshift range $z\in (100,1000)$ at $2\sigma$ c.l. The tensions remain at $\sim 2-3\sigma$ c.l. Comment: 17 pages, 5 figures, 5 tables. Version accepted for publication in PRD |
| Databáze: | OpenAIRE |
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