Late-transition versus smooth 
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-deformation models for the resolution of the Hubble crisis

Alestas, George; Camarena, David; Valentino, Eleonora Di; Kazantzidis, Lavrentios; Marra, Valerio; Nesseris, Savvas; Perivolaropoulos, Leandros

doi:10.1103/physrevd.105.063538

Cited by 56 publications

(13 citation statements)

References 260 publications

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“…[11][12][13][14][15][16][17][18][19][20][21][22][23][24], as well as the σ 8 tension, see e.g. [10,[25][26][27][28][29][30][31][32][33][34] (see also [35][36][37][38][39][40] for an overview of observations and models). Among these solutions, those that modify the behaviour of dark energy either at late or early times have received special attention.…”

Section: Introductionmentioning

confidence: 99%

Can late-time extensions solve the $H_0$ and $σ_8$ tensions?

Heisenberg¹,

Villarrubia-Rojo²,

Zosso³

2022

Preprint

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We analyze the properties that any late-time modification of the ΛCDM expansion history must have in order to consistently solve both the H0 and the σ8 tensions. Taking a model-independent approach, we obtain a set of necessary conditions that can be applied to generic late-time extensions. Our results are fully analytical and merely based on the assumptions that the deviations from the ΛCDM background remain small. For the concrete case of a dark energy fluid with equation of state w(z), we derive the following general requirements: (i) Solving the H0 tension demands w(z) < −1 at some z (ii) Solving both the H0 and σ8 tensions requires w(z) to cross the phantom divide. Finally, we also allow for small deviations on the effective gravitational constant. In this case, our method is still able to constrain the functional form of these deviations. Contents

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Section: Introductionmentioning

confidence: 99%

Can late-time extensions solve the $H_0$ and $σ_8$ tensions?

Heisenberg¹,

Villarrubia-Rojo²,

Zosso³

2022

Preprint

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“…A number of studies have prescribed to use in the statistical analyses a prior on the intrinsic magnitude rather than on the Hubble constant H 0 [7,[34][35][36][37]. A prior on M B is more robust and avoids double-counting issues when using simultaneously luminosity distance measurements from the SN Ia Pantheon sample and measurements of H 0 from SH0ES.…”

Section: Introductionmentioning

confidence: 99%

Late-time interacting cosmologies and the Hubble constant tension

et al. 2022

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“…This assumption is reminiscent of what happens to w EDE in EDE models. Similar transitions in the Planck Mass have been also considered during inflation (Ashoorioon et al 2014), during the matter-dominated epoch (Sakr & Sapone 2022), and at very low redshift (Marra & Perivolaropoulos 2021;Alestas et al 2022). More complex parameterizations are possible; for instance, one could explore the case of a double transition in M å at both early and late times.…”

Section: Parameterizing the Eft Functionsmentioning

confidence: 69%

An Exploration of an Early Gravity Transition in Light of Cosmological Tensions

Benevento

Kable

Addison

et al. 2022

ApJ

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We study a step-like transition in the value of the effective Planck mass (or effective gravitational constant) on cosmological scales prior to recombination. We employ cosmic microwave background, baryon acoustic oscillations, and Type Ia supernova data and find they are sufficient to strongly constrain our implementation of the effective field theory of dark energy and modified gravity, used to model the transition, to a limited parameter space. The data prefer a ∼5% shift in the value of the effective Planck mass (<10% at 2σ) prior to recombination. This Transitional Planck Mass (TPM) model is free to undergo its transition at any point over multiple decades of scale factor prior to recombination, log 10 ( a ) = − 5.32 − 0.72 + 0.96 (68% confidence level). This lowers the sound horizon at last scattering, which increases the Hubble constant to 71.09 ± 0.75 km s−1 Mpc−1 with a combination of local measurements as prior and to 69.22 − 0.86 + 0.67 km s−1 Mpc−1 when the prior is excluded. The TPM model improves χ 2 with respect to ΛCDM by Δχ 2 = −23.72 with the H 0 prior and Δχ 2 = −4.8 without the prior. The model allows for both H 0 > 70 kms−1 Mpc−1 and S 8 < 0.80 simultaneously with lower values of S 8 due to a reduction in the matter density Ω m to offset the increase in H 0 relative to ΛCDM. While this is a particular modified gravity model, studying other variants of modified gravity may be a productive path for potentially resolving cosmological tensions while avoiding the need for a cosmological constant.

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Late-transition versus smooth H(z) -deformation models for the resolution of the Hubble crisis

Abstract: This is a repository copy of Late-transition versus smooth H(z)-deformation models for the resolution of the Hubble crisis.

Cited by 56 publications

References 260 publications

Can late-time extensions solve the $H_0$ and $σ_8$ tensions?

Can late-time extensions solve the $H_0$ and $σ_8$ tensions?

Late-time interacting cosmologies and the Hubble constant tension

An Exploration of an Early Gravity Transition in Light of Cosmological Tensions

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