Why reducing the cosmic sound horizon alone can not fully resolve the Hubble tension

Jedamzik, Karsten; Pogosian, Levon; Zhao, Gong-Bo

doi:10.1038/s42005-021-00628-x

Cited by 168 publications

(103 citation statements)

References 50 publications

(62 reference statements)

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“…Such models are favoured by trying to simultaneously fit the SH0ES measurement of H 0 and the angular size of the sound horizon measured with Planck and BAO. Jedamzik et al (2021) show that the S 8 implied by Planck in such models is several sigma away from that measured by lensing (a similar result was found in the context of Early Dark Energy models in Hill et al 2020). This can be understood by noting that S 8 ∝ A 0.…”

Section: Appendix B: Weak Lensing + Bbn As a Standard Ruler Calibratorsupporting

confidence: 79%

“…As the main focus of this paper is a study of how H 0 may be constrained with lensing, we believe our omission of the eBOSS DR16 data is justified. 13 As shown in Jedamzik et al (2021), galaxy lensing can help to constrain models with high Ω m h 2 (and hence low sound horizon) if one is willing to combine Planck primary CMB measurements and cosmic shear in a joint analysis. Such models are favoured by trying to simultaneously fit the SH0ES measurement of H 0 and the angular size of the sound horizon measured with Planck and BAO.…”

Section: Appendix B: Weak Lensing + Bbn As a Standard Ruler Calibratormentioning

confidence: 99%

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Cosmology from weak lensing alone and implications for the Hubble tension

Hall

2021

Monthly Notices of the Royal Astronomical Society

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We investigate the origin of ΛCDM parameter constraints in weak lensing, with a focus on the Hubble constant. We explain why current cosmic shear data are sensitive to the parameter combination $S_8 \propto \sigma _8 \Omega _m^{0.5}$, improving upon previous studies through use of the halo model. Motivated by the ongoing discrepancy in measurements of the Hubble constant from high and low redshift, we explain why cosmic shear provides almost no constraint on H0 by showing how the lensing angular power spectrum depends on physical length scales in the dark matter distribution. We derive parameter constraints from galaxy lensing in KiDS and cosmic microwave background weak lensing from Planck and SPTpol, separately and jointly, showing how degeneracies between σ8 and Ωm can be broken. Using lensing and big bang Nucleosynthesis to calibrate the sound horizon measured in projection by baryon acoustic oscillations gives H0 = 67.4 ± 0.9 km s−1 Mpc−1, consistent with previous results from Planck and the Dark Energy Survey. We find that a toy Euclid-like lensing survey provides only weak constraints on the Hubble constant due to degeneracies with other parameters that affect the shape of the lensing correlation functions. If external priors on ns, the baryon density, and the amplitude of baryon feedback are available then sub-percent H0 constraints are achievable with forthcoming lensing surveys.

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Section: Appendix B: Weak Lensing + Bbn As a Standard Ruler Calibratorsupporting

confidence: 79%

Section: Appendix B: Weak Lensing + Bbn As a Standard Ruler Calibratormentioning

confidence: 99%

Cosmology from weak lensing alone and implications for the Hubble tension

Hall

2021

Monthly Notices of the Royal Astronomical Society

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“…The continued increase in expansion velocity involving a decline in microstates might be validated by the use of more powerful telescopes to determine whether the density of matter at the cosmic horizon exceeds the predicted value based on current measurements. Such a discrepancy already exists in the form of the Hubble tension, which may require new theoretical approaches to cosmic expansion (Jedamzik, Pogosian, & Zhao, 2021).…”

Section: Discussionmentioning

confidence: 99%

A Hypothetical Approach to Cosmic Inflation Incorporating Binary Entropy

Cantor¹

2021

APR

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The current paper presents an alternative hypothesis for the termination of cosmic inflation based on Huang’s model of spacetime involving the movement of a superfluid through a random resistor network. Using this model, we previously derived a mathematical relationship between the velocity of a reference frame and the probability that a random bond is intact. As an extension of this finding, the permutations of open and closed bonds are now shown to represent potential microstates, thus providing a means of relating motion within the network to binary entropy. Applying this concept to cosmic inflation, termination of this process is an expected consequence of the changes in binary entropy associated with the increasing velocity of expansion.

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“…Although the most effective attempts of solutions to the Hubble tension are those that modify the cosmic expansion history at early epochs (see, e.g., Knox & Millea 2020;Schöneberg et al 2021), leading to a reduced sound horizon at recombination, it was shown that this change alone did not fully resolve the H 0 tension while remaining consistent with other cosmological datasets (Jedamzik et al 2021).…”

Section: Parametrizing the Eft Functionsmentioning

confidence: 99%

An exploration of an early gravity transition in light of cosmological tensions

Benevento¹,

Kable²,

Addison³

et al. 2022

Preprint

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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 CMB, BAO, and SNIa 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 +0.96 −0.72 (68% CL). 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 +0.67 −0.86 km s −1 Mpc −1 when the prior is excluded. The TPM model improves χ 2 with respect to ΛCDM by ∆χ 2 = −23.72 with the H 0 prior and ∆χ 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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Why reducing the cosmic sound horizon alone can not fully resolve the Hubble tension

Cited by 168 publications

References 50 publications

Cosmology from weak lensing alone and implications for the Hubble tension

Cosmology from weak lensing alone and implications for the Hubble tension

A Hypothetical Approach to Cosmic Inflation Incorporating Binary Entropy

An exploration of an early gravity transition in light of cosmological tensions

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