The Ups and Downs of Early Dark Energy solutions to the Hubble tension: A review of models, hints and constraints circa 2023

Poulin, Vivian; Smith, Tristan L.; Karwal, Tanvi

doi:10.1016/j.dark.2023.101348

Cited by 66 publications

(20 citation statements)

References 243 publications

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“…There, we plot the evolution for 3 modes that cross the Hubble radius well before (k = 0.1 Mpc −1 ), shortly before 5 (k = 0.05 Mpc −1 ) and long after (k = 0.001 Mpc −1 ) z c , similarly to the analysis in ref. [17]. As we can see, the effective density perturbations in the EMG sector feature a dip in their evolution at early times z ≳ z c .…”

Section: Comparison With the Rock'n'roll Ede Modelmentioning

confidence: 60%

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Probing early modification of gravity with Planck, ACT and SPT

Franco Abellán,

Braglia,

Ballardini

et al. 2023

J. Cosmol. Astropart. Phys.

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We consider a model of early modified gravity (EMG) that was recently proposed as a candidate to resolve the Hubble tension. The model consists of a scalar fieldσwith a nonminimal coupling (NMC) to the Ricci curvature of the formF(σ) = Mpl2+ξσ2and an effective mass induced by a quartic potentialV(σ) = λσ4/4. We present the first analyses of the EMG model in light of the latest ACT DR4 and SPT-3G data in combination with fullPlanckdata, and find a ≳ 2σ preference for a non-zero EMG contribution from a combination of primary CMB data alone, mostly driven by ACT-DR4 data. This is different from popular `Early Dark Energy' models, which are detected only when the high-ℓ information fromPlancktemperature is removed. We find that the NMC plays a key role in controlling the evolution of density perturbations that is favored by the data over the minimally coupled case. Including measurements of supernovae luminosity distance from Pantheon+, baryonic acoustic oscillations and growth factor from BOSS, and CMB lensing ofPlanckleaves the preference unaffected. In the EMG model, the tension with SH0ES is alleviated from ∼ 6σto ∼ 3σ. Further adding SH0ES data raises the detection of the EMG model above 5σ.

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Section: Comparison With the Rock'n'roll Ede Modelmentioning

confidence: 60%

“…One possible way to reduce r s is to briefly increase the Hubble rate around matter-radiation equality, for instance via a new form of Dark Energy active at early time [15,16] dubbed 'early dark energy' (EDE) (see refs. [12,17] for reviews), or by modifying general relativity (GR).…”

Section: Introductionmentioning

confidence: 99%

Probing early modification of gravity with Planck, ACT and SPT

Franco Abellán,

Braglia,

Ballardini

et al. 2023

J. Cosmol. Astropart. Phys.

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“…(6.32 × 10 −10 GeV) 4 1.45247 × 10 −47 GeV 4 0.3569 0.1044 on the H 0 tension and solutions see [26,27]. For recent reviews on EDE models see [67,68]).…”

Section: Early and Late Dark Energymentioning

confidence: 99%

“…should not exceed values around 12% (see e.g. [67,68]). This requirement is satisfied in our set-up, see figure 5.…”

Section: Early and Late Dark Energymentioning

confidence: 99%

Dark energy, D-branes and pulsar timing arrays

Chowdhury,

Tasinato,

Zavala

2023

J. Cosmol. Astropart. Phys.

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Several pulsar timing array (PTA) collaborations recently announced the first detection of a stochastic gravitational wave (GW) background, leaving open the question of its source. We explore the possibility that it originates from cosmic inflation, a guaranteed source of primordial GW. The inflationary GW background amplitude is enhanced at PTA scales by a non-standard early cosmological evolution, driven by Dirac-Born-Infeld (DBI) scalar dynamics motivated by string theory. The resulting GW energy density has a broken power-law frequency profile, entering the PTA band with a peak amplitude consistent with the recent GW detection. After this initial DBI kination epoch, the dynamics starts a new phase mainly controlled by the scalar potential. It provides a realization of an early dark energy scenario aimed at relaxing the H 0 tension, and a late dark energy model which explains the current cosmological acceleration with no need of a cosmological constant. Hence our mechanism — besides providing a possible explanation for the recent PTA results — connects them with testable properties of the physics of the dark universe.

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“…Here, we do not distinguish the behaviour of early dark energy and late dark energy [29,30] but assume that the early dark energy component evolves to become the present cosmological constant (Λ) with fractional energy density Ω Λ . With this understanding, we compute the Hubble parameter during inflation using the equation ( 8) in Friedmann's equation for a flat FLRW universe and obtain [24]…”

Section: The Hybrid Inflationary Modelmentioning

confidence: 99%

A possible solution to the Hubble tension from quantum gravity

Suresh

2024

Class. Quantum Grav.

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We investigate the relevance of quantum gravity during inﬂation to address the Hubble tension that arises from Planck 2018 and SH0ES data sets. We show that the eﬀect of quantum gravity during inﬂation can increase the rate of change of H0, thereby accounting for a wide range of observed H0. Further, we show that due to the quantum gravity eﬀect on inﬂation, the temperature at the onset of reheating can be lower than the standard case, causing delays in the reheating process. The role of quantum gravity is inevitable in settling the Hubble tension. The results of the present study may ﬁnd use in resolving the Hubble tension, in validating inﬂationary model and quantum gravity.

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The Ups and Downs of Early Dark Energy solutions to the Hubble tension: A review of models, hints and constraints circa 2023

Cited by 66 publications

References 243 publications

Probing early modification of gravity with Planck, ACT and SPT

Probing early modification of gravity with Planck, ACT and SPT

Dark energy, D-branes and pulsar timing arrays

A possible solution to the Hubble tension from quantum gravity

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