Early modified gravity in light of the 
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 tension and LSS data

Braglia, Matteo; Ballardini, M.; Finelli⋆, F.; Koyama, K.

doi:10.1103/physrevd.103.043528

Cited by 111 publications

(47 citation statements)

References 124 publications

(237 reference statements)

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“…Hence, the H 0 tension in this model is alleviated, but at the expense of worsening the S 8 /σ 8 one (Hill et al 2020;Ivanov et al 2020;D'Amico et al 2021). Something similar happens in the New EDE model proposed in (Niedermann & Sloth 2021 or the early modified gravity model studied in (Braglia et al 2021). Although the S 8 /σ 8 tension is not as statistically significant as the H 0 one (cf.…”

Section: Weak Lensingsupporting

confidence: 61%

Early dark energy in the pre- and post-recombination epochs

Gómez-Valent,

Zheng,

Amendola

et al. 2021

Preprint

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Dark energy could play a role at redshifts z O(1). Many quintessence models possess scaling or attractor solutions where the fraction of dark energy follows the dominant component in previous epochs of the Universe's expansion, or phase transitions may happen close to the time of matter-radiation equality. A non-negligible early dark energy (EDE) fraction around matter-radiation equality could contribute to alleviate the well-known H0 tension. In this work we constrain the fraction of EDE 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. The latter allows us to reconstruct the evolution of Ω de (z) before and after the decoupling of the Cosmic Microwave Background (CMB) photons. We have employed Planck data 2018, the Pantheon compilation of supernovae of Type Ia (SNIa), data on galaxy clustering, the prior on the absolute magnitude of SNIa by SH0ES, and weak lensing 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. We show how 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, 0.4% at 2σ c.l. We confirm previous results that a significant EDE fraction in the radiation-dominated epoch loosens the H0 tension, but tends to worsen the tension for σ8. A subsequent presence of EDE in the matter-dominated era helps to alleviate this issue. When both the SH0ES prior and weak lensing 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 2.6% in the radiation-dominated epoch and 1.5% in the redshift range z ∈ (100, 1000) at 2σ c.l. The two tensions remain with a statistical significance of ∼ 2 − 3σ c.l.

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Section: Weak Lensingsupporting

confidence: 61%

Early dark energy in the pre- and post-recombination epochs

Gómez-Valent,

Zheng,

Amendola

et al. 2021

Preprint

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“…27 For this model, the combination of the Planck 2018 + BAO + FS + Pantheon + R19 + H0LiCOW datasets gives H 0 = 71.00 +0. 87 −0.79 km s −1 Mpc −1 at 68% CL [859], reducing the Hubble tension at 1.4σ with R20. The analysis already includes a Gaussian prior on H 0 .…”

Section: F(q) Gravity Theorymentioning

confidence: 93%

“…Early modified gravity. The scenario described by the action in equation (102) with F(σ) = 1 + ξσ 2 and with the potential V(σ) = λσ 4 /4 (λ is a free parameter) has been recently studied in reference [859], where it has been named 'early modified gravity model'. 27 For this model, the combination of the Planck 2018 + BAO + FS + Pantheon + R19 + H0LiCOW datasets gives H 0 = 71.00 +0.…”

Section: F(q) Gravity Theorymentioning

confidence: 99%

In the realm of the Hubble tension—a review of solutions ^*

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,419

760

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The simplest ΛCDM model provides a good fit to a large span of cosmological data but harbors large areas of phenomenology and ignorance. With the improvement of the number and the accuracy of observations, discrepancies among key cosmological parameters of the model have emerged. The most statistically significant tension is the 4σ to 6σ disagreement between predictions of the Hubble constant, H 0, made by the early time probes in concert with the ‘vanilla’ ΛCDM cosmological model, and a number of late time, model-independent determinations of H 0 from local measurements of distances and redshifts. The high precision and consistency of the data at both ends present strong challenges to the possible solution space and demands a hypothesis with enough rigor to explain multiple observations—whether these invoke new physics, unexpected large-scale structures or multiple, unrelated errors. A thorough review of the problem including a discussion of recent Hubble constant estimates and a summary of the proposed theoretical solutions is presented here. We include more than 1000 references, indicating that the interest in this area has grown considerably just during the last few years. We classify the many proposals to resolve the tension in these categories: early dark energy, late dark energy, dark energy models with 6 degrees of freedom and their extensions, models with extra relativistic degrees of freedom, models with extra interactions, unified cosmologies, modified gravity, inflationary models, modified recombination history, physics of the critical phenomena, and alternative proposals. Some are formally successful, improving the fit to the data in light of their additional degrees of freedom, restoring agreement within 1–2σ between Planck 2018, using the cosmic microwave background power spectra data, baryon acoustic oscillations, Pantheon SN data, and R20, the latest SH0ES Team Riess, et al (2021 Astrophys. J. 908 L6) measurement of the Hubble constant (H 0 = 73.2 ± 1.3 km s−1 Mpc−1 at 68% confidence level). However, there are many more unsuccessful models which leave the discrepancy well above the 3σ disagreement level. In many cases, reduced tension comes not simply from a change in the value of H 0 but also due to an increase in its uncertainty due to degeneracy with additional physics, complicating the picture and pointing to the need for additional probes. While no specific proposal makes a strong case for being highly likely or far better than all others, solutions involving early or dynamical dark energy, neutrino interactions, interacting cosmologies, primordial magnetic fields, and modified gravity provide the best options until a better alternative comes along.

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“…Here, we consider the so called Rock n Roll (RnR) model of Ref. [43] as representative of EDE (see [40,42,43,[60][61][62][63][64][65][66][67] for an incomplete list of EDE models). The Lagrangian is that of a minimally coupled, canonical scalar field φ:…”

Section: Early Dark Energymentioning

confidence: 99%

Probing pre-Recombination Physics by the Cross-Correlation of Stochastic Gravitational Waves and CMB Anisotropies

Braglia,

Kuroyanagi

2021

Preprint

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We study the effects of pre-recombination physics on the Stochastic Gravitational Wave Background (SGWB) anisotropies induced by the propagation of gravitons through the large-scale density perturbations and their cross-correlation with Cosmic Microwave Background (CMB) temperature and E-mode polarization ones. As examples of Early Universe extensions to the ΛCDM model, we consider popular models featuring extra relativistic degrees of freedom, a massless non-minimally coupled scalar field, and an Early Dark Energy component. Assuming the detection of a SGWB, we perform a Fisher analysis to assess in a quantitative way the capability of future gravitational wave interferometers (GWIs) in conjunction with a future large-scale CMB polarization experiment to constrain such variations. Our results show that the cross-correlation of CMB and SGWB anisotropies will help tighten the constraints obtained with CMB alone, with an improvement that significantly depends on the specific model as well as the maximum angular resolution GW max of the GWIs, their designed sensitivity, and the amplitude A * of the monopole of the SGWB.

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Early modified gravity in light of the H0 tension and LSS data

Cited by 111 publications

References 124 publications

Early dark energy in the pre- and post-recombination epochs

Early dark energy in the pre- and post-recombination epochs

In the realm of the Hubble tension—a review of solutions ^*

Probing pre-Recombination Physics by the Cross-Correlation of Stochastic Gravitational Waves and CMB Anisotropies

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Early modified gravity in light of the H0 tension and LSS data

Cited by 111 publications

References 124 publications

Early dark energy in the pre- and post-recombination epochs

Early dark energy in the pre- and post-recombination epochs

In the realm of the Hubble tension—a review of solutions *

Probing pre-Recombination Physics by the Cross-Correlation of Stochastic Gravitational Waves and CMB Anisotropies

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In the realm of the Hubble tension—a review of solutions ^*