Rock 'n' Roll Solutions to the Hubble Tension

Agrawal, Prateek; Cyr-Racine, Francis-Yan; Pinner, David; Randall, Lisa

doi:10.48550/arxiv.1904.01016

Cited by 171 publications

(304 citation statements)

References 45 publications

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“…This is in fact suggested by previous analyses in the literature, see e.g. (Poulin et al 2019;Agrawal et al 2019;Smith et al 2020;Chudaykin et al 2020;Niedermann & Sloth 2020. Our results are presented in Tables 3-5, and also in Fig.…”

Section: Results For Tomographic Dark Energysupporting

confidence: 90%

“…A nonzero coupling impacts indeed the tensions in cosmological observations (Pettorino 2013;Ade et al 2016) -for a recent update see (Gómez-Valent et al 2020) and references therein. In the present paper we investigate the case of uncoupled quintessence in order to find out if some appropriate time evolution of EDE could remove the tensions, as advocated, for example, in different versions of "new EDE" (Poulin et al 2019;Agrawal et al 2019;Smith et al 2020;Niedermann & Sloth 2020.…”

Section: Introductionmentioning

confidence: 99%

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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: Results For Tomographic Dark Energysupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

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

Gómez-Valent,

Zheng,

Amendola

et al. 2021

Preprint

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“…This potential, of the form first proposed in [34], is a generalization of the usual axion potential, corresponding to a careful fine-tuning of an instanton expansion or of other non-perturbative effects (see, e.g., the discussion in [3]). Alternative realizations and variations on the EDE model abound, see, e.g., [1,[57][58][59][60][61][62][63][64][65].…”

Section: From Early Dark Energy To the Early Dark Sectormentioning

confidence: 99%

“…( 4), whereas [29] considered a monomial V (φ) = λφ 4 . These two choices for V (φ) are known to exhibit different phenomenology; see, e.g., the discussion in [57,58].…”

Section: From Early Dark Energy To the Early Dark Sectormentioning

confidence: 99%

The Early Dark Sector, the Hubble Tension, and the Swampland

McDonough¹,

Lin²,

Hill³

et al. 2021

Preprint

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We consider the interplay of the Early Dark Energy (EDE) model, the Swampland Distance Conjecture (SDC), and cosmological parameter tensions. EDE is a proposed resolution of the Hubble tension relying upon a near-Planckian scalar field excursion, while the SDC predicts an exponential sensitivity of masses of other fields to such an excursion, m ∝ e −c|∆φ|/M pl with c ∼ O(1). Meanwhile, EDE is in tension with large-scale structure (LSS) data, due to shifts in the standard ΛCDM parameters necessary to fit the cosmic microwave background (CMB). One might hope that a proper treatment of the model, e.g., accounting for the SDC, may ameliorate the tension with LSS. Motivated by these considerations, we introduce the Early Dark Sector (EDS) model, wherein the mass of dark matter is exponentially sensitive to super-Planckian field excursions of the EDE scalar. The EDS model exhibits new phenomenology in both the early and late universe, the latter due to an EDE-mediated dark matter self-interaction, which manifests as an enhanced gravitational constant on small scales. This EDE-induced dark matter-philic "fifth force", while constrained to be small, remains active in the late universe and is not screened in virialized halos. We find that the new interaction with dark matter partially resolves the LSS tension. However, the marginalized posteriors are nonetheless consistent with fEDE = 0 at 95% CL once the Dark Energy Survey Year 3 measurement of S8 is included. We additionally study constraints on the model from Atacama Cosmology Telescope data, and find a factor of two improvement on the error bar on the SDC parameter c, along with an increased preference for the EDE component. We discuss the implications of these constraints for the SDC, and find the tightest observational constraints to date on a swampland parameter, suggesting that an EDE description of cosmological data is in tension with the SDC.

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“…By means of many independent probes, and efforts spanning multiple decades, a picture has now emerged in which there appears to be a clear discrepancy between early and late-time cosmological studies (Planck Collaboration et al 2020;Riess et al 2019;Wong et al 2020;Abbott et al 2018;Pesce et al 2020;Verde et al 2019). At the heart of this debate is nothing less than our understanding of our standard cosmological model and, at face value, this discrepancy can only be resolved by yet unknown and unaccounted physics (e.g., Poulin et al 2019;Agrawal et al 2019;Knox & Millea 2020) or by our lack of accounting for systematic uncertainties in the methods (e.g., Freedman et al 2019;Shanks et al 2019).…”

Section: Introductionmentioning

confidence: 99%

TDCOSMO VIII: Cosmological distance measurements in light of the mass-sheet degeneracy -- forecasts from strong lensing and IFU stellar kinematics

Yıldırım¹,

Suyu²,

Chen³

et al. 2021

Preprint

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Time-delay distance measurements of strongly lensed quasars have provided a powerful and independent probe of the current expansion rate of the Universe (H 0 ). However, in light of the discrepancies between early and late-time cosmological studies, current efforts revolve around the characterisation of systematic uncertainties in the methods. In this work, we focus on the mass-sheet degeneracy (MSD), which is commonly considered as being a significant source of systematics in time-delay strong lensing studies, and aim to assess the constraining power provided by integral field unit (IFU) stellar kinematics. To this end, we approximate the MSD with a cored, two-parameter extension to the adopted lensing mass profiles (with core radius r c and mass-sheet parameter λ int ), which introduces a full degeneracy between λ int and H 0 from lensing data alone. In addition, we utilise spatially resolved mock IFU stellar kinematics of time-delay strong lenses, given the prospects of obtaining such high-quality data with the James Webb Space Telescope (JWST) in the near future. We construct joint strong lensing and generalised two-integral axisymmetric Jeans models, where the time delays, mock imaging and IFU observations are used as input to constrain the mass profile of lens galaxies at the individual galaxy level, and consequently yield joint constraints on the time-delay distance (D ∆t ) and angular diameter distance (D d ) to the lens. We find that mock JWST-like stellar kinematics constrain the amount of internal mass sheet that is physically associated with the lens galaxy and limit its contribution to the uncertainties of D ∆t and D d , each at the ≤ 4% level, without assumptions on the background cosmological model. Incorporating additional uncertainties due to external mass sheets associated with mass structures along the lens line-of-sight, these distance constraints would translate to a 4% precision measurement on H 0 in flat ΛCDM cosmology for a single lens. Our study shows that future IFU stellar kinematics of time-delay lenses will be key in lifting the MSD on a per lens basis, assuming reasonable and physically motivated core sizes. However, even in the limit of infinite r c , where D ∆t is fully degenerate with λ int and is thus not constrained, stellar kinematics of the deflector, time delays and imaging data will provide powerful constraints on D d , which becomes the dominant source of information in the cosmological inference.

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Rock 'n' Roll Solutions to the Hubble Tension

Cited by 171 publications

References 45 publications

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

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

The Early Dark Sector, the Hubble Tension, and the Swampland

TDCOSMO VIII: Cosmological distance measurements in light of the mass-sheet degeneracy -- forecasts from strong lensing and IFU stellar kinematics

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