Running Hubble tension and a H0 diagnostic

Krishnan, Chethan; Colgáin, Eoin Ó; Sheikh-Jabbari, M. M.; Yang, Tao

doi:10.1103/physrevd.103.103509

Cited by 93 publications

(53 citation statements)

References 112 publications

(193 reference statements)

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“…The shaded blue and red envelopes are the 1σ confidence intervals, while the grey region is the overlap. That this ratio is basically a constant confirms there is no H 0 running in the sense discussed in [23].…”

Section: Resultssupporting

confidence: 53%

“…In figure 2 we offer visual confirmation that the reconstructed E(z) rec does not differ enough from flat ΛCDM E(z) ΛCDM . There is no evidence for running in H 0 with redshift [23] as is clear from the 1σ confidence intervals for the ratio presented. For completeness, we compare to flat ΛCDM defined with respect to our MCMC chains (table 2) and the Planck MCMC chains [2].…”

Section: Resultsmentioning

confidence: 70%

“…In this letter we have explored a modification of the DE sector consistent with a recent determination of the age of Universe, t U [17,29]. As explained, a fixed t U consistent with Planck results allows a higher H 0 , but lower E(z) relative to Planck-ΛCDM, thus providing a realisation of a running H 0 [23]. Ultimately, the rigidity of the DE sector precludes this.…”

Section: Discussionmentioning

confidence: 92%

“…Only when the two models are identical the left-hand side can remain a constant. Such a running must follow if Hubble tension can find a resolution within FLRW [23]. Tentative hints of such a feature already exist [24][25][26][27][28].…”

Section: Introductionmentioning

confidence: 99%

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Does Hubble tension signal a breakdown in FLRW cosmology?

Krishnan

Mohayaee

Colgáin

et al. 2021

Class. Quantum Grav.

114

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The tension between early and late Universe probes of the Hubble constant has motivated various new FLRW cosmologies. Here, we reanalyse the Hubble tension with a recent age of the Universe constraint. This allows us to restrict attention to matter and a dark energy sector that we treat without assuming a specific model. Assuming analyticity of the Hubble parameter H(z), and a generic low redshift modification to flat ΛCDM, we find that low redshift data (z 2.5) and well-motivated priors only permit a dark energy sector close to the cosmological constant Λ. This restriction rules out late Universe modifications within FLRW. We show that early Universe physics that alters the sound horizon can yield an upper limit of H 0 ∼ 71 ± 1 km s −1 Mpc −1 . Since various local determinations may be converging to H 0 ∼ 73 km s −1 Mpc −1 , a breakdown of the FLRW framework is a plausible resolution. We outline how future data, in particular strongly lensed quasar data, could also provide further confirmations of such a resolution.

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Section: Resultssupporting

confidence: 53%

Section: Resultsmentioning

confidence: 70%

Section: Discussionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Does Hubble tension signal a breakdown in FLRW cosmology?

Krishnan

Mohayaee

Colgáin

et al. 2021

Class. Quantum Grav.

114

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“…In reference [1015] a running of H 0 as a function of redshift is proposed to alleviate the Hubble tension, although a full data analysis is missing. A similar idea has been explored in reference [1016] to analyse the Pantheon SNIa data.…”

Section: Running Hubble Tensionmentioning

confidence: 99%

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

Valentino

Mena²,

Pan³

et al. 2021

Class. Quantum Grav.

1,086

694

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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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Stepped partially acoustic dark matter, large scale structure, and the Hubble tension

Buen-Abad

Chacko

Kılıç

et al. 2023

J. High Energ. Phys.

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We propose a new interacting dark sector model, Stepped Partially Acoustic Dark Matter (SPartAcous), that can simultaneously address the two most important tensions in current cosmological data, the H0 and S8 problems. As in the Partially Acoustic Dark Matter (PAcDM) scenario, this model features a subcomponent of dark matter that interacts with dark radiation at high temperatures, suppressing the growth of structure at small scales and thereby addressing the S8 problem. However, in the SPartAcous model, the dark radiation includes a component with a light mass that becomes non-relativistic close to the time of matter-radiation equality. As this light component annihilates away, the remaining dark radiation heats up and its interactions with dark matter decouple. The heating up of the dark sector results in a step-like increase in the relative energy density in dark radiation, significantly reducing the H0 tension, while the decoupling of dark matter and dark radiation ensures that the power spectrum at larger scales is identical to ΛCDM.

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Running Hubble tension and a H0 diagnostic

Cited by 93 publications

References 112 publications

Does Hubble tension signal a breakdown in FLRW cosmology?

Does Hubble tension signal a breakdown in FLRW cosmology?

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

Stepped partially acoustic dark matter, large scale structure, and the Hubble tension

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Running Hubble tension and a H0 diagnostic

Cited by 93 publications

References 112 publications

Does Hubble tension signal a breakdown in FLRW cosmology?

Does Hubble tension signal a breakdown in FLRW cosmology?

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

Stepped partially acoustic dark matter, large scale structure, and the Hubble tension

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