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arxiv: 2606.12980 · v1 · pith:W72SV6HCnew · submitted 2026-06-11 · 🌌 astro-ph.CO

A Review on Resolving the Hubble Tension via Late-Universe Physics

Xuan-Dong Jia , Xin-Yi Dai , Yu-Peng Yang , Fa-Yin Wang This is my paper

Pith reviewed 2026-06-27 06:07 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords Hubble tensionDESIBAOType Ia supernovaelate-universe physicsLambda CDMcosmologydark energy
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The pith

DESI BAO and uncalibrated supernovae data indicate the Hubble tension arises from new physics at low redshifts.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This review examines recent progress on the Hubble tension by focusing on late-universe modifications to the standard cosmological model. The central evidence is that Dark Energy Spectroscopic Instrument baryon acoustic oscillation measurements combined with uncalibrated Type Ia supernovae produce a Hubble constant higher than the value predicted by Lambda CDM when fit only to early-universe data. The authors argue that remaining observational systematics fall short of explaining the full offset, which therefore requires undiscovered physical mechanisms operating after the early universe. A reader would care because the result reframes the tension as a problem of recent cosmic expansion rather than a mismatch between local and primordial measurements.

Core claim

The combination of DESI BAO and uncalibrated Type Ia supernovae data yields a value for H0 that is significantly higher than the ΛCDM prediction based on early-universe probes, indicating that the origin of the Hubble tension lies in new physics at low redshifts.

What carries the argument

The combination of DESI baryon acoustic oscillation measurements and uncalibrated Type Ia supernovae, which together infer a higher Hubble constant without distance-ladder calibration.

If this is right

  • Modifications to the expansion history must occur at low redshifts to reconcile the datasets.
  • Changes confined to the early universe are not sufficient to resolve the tension.
  • Current levels of observational systematics cannot account for the discrepancy.
  • New physical mechanisms active after recombination are likely required.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Model-building efforts should prioritize mechanisms that change the expansion rate between recombination and the present epoch.
  • Independent late-universe probes such as gravitational-wave standard sirens could provide decisive cross-checks.
  • Confirmation would lower the priority of revising early-universe parameters like the sound horizon scale.

Load-bearing premise

The DESI BAO measurements and uncalibrated supernova samples are free of systematics large enough to produce the observed offset from early-universe ΛCDM predictions.

What would settle it

A future joint analysis in which the H0 value from DESI BAO plus uncalibrated supernovae falls into agreement with the early-universe ΛCDM prediction within uncertainties.

Figures

Figures reproduced from arXiv: 2606.12980 by Fa-Yin Wang, Xin-Yi Dai, Xuan-Dong Jia, Yu-Peng Yang.

Figure 1
Figure 1. Figure 1: Three-rung distance ladder. The lower-left panel depicts geometric distance measurements to Cepheid variables, which are used to calibrate their period–luminosity relationship. In the central panel, SNe Ia in host galaxies that also contain Cepheids are calibrated against these Cepheid-derived distances. Finally, the upper-right panel displays SNe Ia residing in the Hubble flow; once the calibration is est… view at source ↗
Figure 2
Figure 2. Figure 2: Conceptual overview of the Local Distance Network. The Hubble constant is ultimately measured by combining different distance measurement methods. A non-exhaustive list of baseline linkages is labeled on the right. Background rectangles in orange, light blue, and gray indicate the first, second, and third rungs, respectively. Figure is adapted from [54]. For more detailed information, please refer to it. T… view at source ↗
Figure 3
Figure 3. Figure 3: Comparisons of H0 between HST Cepheids and other measures (JWST Cepheids, JWST JAGB, and JWST NIR-TRGB) for SN Ia host subsamples. The data demonstrate that HST and JWST distance measurements are in good agreement, with the selection of different subsamples by teams (CCHP vs. SH0ES) accounting for the primary variations rather than instrumental systematics or differences in distances to galaxies in common.… view at source ↗
Figure 4
Figure 4. Figure 4: The impact on H0 of the various systematic uncertainties tabulated. The units of these measurements are km s−1 Mpc−1 . More details can be seen in Ref. [23]. 2.2. Tip of the Red Giant Branch The TRGB serves as a precise method for distance measurement [81]. Prior to the onset of the helium flash, red giants reach a peak luminosity that is nearly the same from stat. This allows distances to be derived direc… view at source ↗
Figure 5
Figure 5. Figure 5: The best fit values with uncertainties for the SNe Ia absolute magnitude MB and for H0, derived from SNe within and beyond the transition distance Dc. More details can be seen in Ref. [157]. In addition, there have been studies focusing on the standardization relations used for SNe Ia. For example, recent work [161] re-examined the well-known “mass step”—the correlation between standardized SN Ia brightnes… view at source ↗
Figure 6
Figure 6. Figure 6: Fit of the flat ΛCDM model with Ωm and H0 as free parameters. More details can be seen in Ref. [166]. 3.3. Theoretical Models The analyses of systematics have so far proven insufficient to fully account for the current Hubble tension, suggesting that it may arise from new physics beyond the standard cosmological model [168]. To date, numerous theories have been proposed to attempt to resolve or alleviate t… view at source ↗
Figure 7
Figure 7. Figure 7: The best-fit results for the binned data. The decline trend is 2.1σ significance. More details can be seen in Ref. [185]. Building upon the ΛCDM and wCDM cosmological frameworks, Dainotti et al. [186] performed fits under the assumption that the Hubble constant evolves with redshift accord￾ing to a functional form g(z) as: g(z) = H0(z) = H˜ 0 (1 + z) a , (12) where H˜ 0 and α are free parameters, with α in… view at source ↗
Figure 8
Figure 8. Figure 8: Smoothed H(z) function (blue solid line) with 2σ errors (gray regions) obtained from the 36 H(z) data (31 CC + 5 BAO) employing GP method. More details can be seen in Ref. [196]. 0.2 0.5 1.0 zmax 55 60 65 70 75 80 85 90 H 0(z m a x) [k m/s/M p c] 55 60 65 70 75 80 85 90 H 0(zle ns) [k m/s/M p c] zlens Matern kernel Latest SH0ES result Plank 2018 result z = 0.49 Our results Quasar lensing 0.2 0.5 1.0 zmax 5… view at source ↗
Figure 9
Figure 9. Figure 9: Predictions of H0(zmax) derived from a sample of 36 H(z) measurements (31 CC + 5 BAO). Here, H0(zmax) denotes the Hubble constant inferred from a dataset truncated at a maximum redshift zmax. The red points represent the predicted values of H0(zmax) obtained from our analysis. The gray and purple shaded regions indicate the constraints reported by the SH0ES and Planck collaborations, respectively. The blue… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison between the Hubble parameter H(z) in the standard ΛCDM model and that derived from Equation (15). H0 = H0,zi = 70 km s−1 Mpc−1 , Ωk0 = 0, and Ωm0 = 0.3 are assumed. More details can be seen in Ref. [198]. By combining SNe, BAO, and H(z) data within a Markov Chain Monte Carlo (MCMC) framework, they obtained the posterior distribution of H0. However, the inferred H0 values across different redshi… view at source ↗
Figure 11
Figure 11. Figure 11: Fitting results for H0(z) using equal-width binning across ten redshift intervals. (a): H0(z) as a function of redshift. A clear decreasing trend is observed, with a significance of 5.6σ at z > 0.3. (b): Normalized probability distributions of H0(z) for ten redshift bins, which are well-approximated by Gaussian profiles. More details can be seen in Ref. [198]. With the availability of additional observati… view at source ↗
Figure 12
Figure 12. Figure 12: The descending trend of the Hubble constant H0 derived from the dark energy equation of state w(z). (Top panel). Green data points represent the maximum a posteriori estimates of H0(z) with 1σ error bars, obtained from the combination of DESI DR2 BAO measurements and the Pantheon plus SNe Ia sample. The redshifts of these points correspond to the midpoints of their respective bins. The inferred H0 is cons… view at source ↗
Figure 13
Figure 13. Figure 13: Predicted H0(z) curves in the void models and according to observations. The horizontal blue band at the top shows the local cz′ measurement [3], while the lower magenta band shows H0. https://doi.org/10.3390/galaxies1010000 [PITH_FULL_IMAGE:figures/full_fig_p022_13.png] view at source ↗
read the original abstract

The $\Lambda$CDM cosmological model has been successful in explaining many astronomical observations. However, recent observations increasingly point to deviations from the standard $\Lambda$CDM framework. Among these, one of the most significant discrepancies is the \textit{Hubble tension}, which refers to the difference in values obtained for the Hubble constant $H_0$ from high-redshift measurement and local observation. To address this issue, numerous cosmological models and methodological approaches have been proposed. This review offers a concise overview of recent progress in resolving the Hubble tension. The combination of Dark Energy Spectroscopic Instrument (DESI) Baryon Acoustic Oscillations (BAO) and uncalibrated Type Ia supernovae data yields a value for $H_0$ that is significantly higher than the $\Lambda$CDM predication based on early-universe probes, even without incorporating local distance ladder constraints. This result indicates that the origin of the Hubble tension lies in new physics at low redshifts. Our findings suggest that although many unresolved systematics persist in current observations, they are insufficient to account for the magnitude of the current Hubble tension. This implies the likely existence of new physical mechanisms that have yet to be discovered.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. This review summarizes recent progress on resolving the Hubble tension through late-universe physics. Its central claim, stated in the abstract, is that the combination of DESI BAO and uncalibrated Type Ia supernovae already produces an H0 value significantly higher than the early-universe ΛCDM prediction, even without local distance-ladder constraints, thereby locating the tension in new low-redshift physics; the review further asserts that unresolved systematics are insufficient to explain the full discrepancy.

Significance. If the cited DESI+SN result is robust against systematics, the review would usefully redirect attention from early-universe solutions toward late-time modifications. As a review it offers a concise overview of models and methods, but its significance is limited by the absence of quantitative error budgets or sensitivity tests for the key claim.

major comments (2)
  1. [Abstract] Abstract: the load-bearing claim that 'existing systematics are insufficient to account for the magnitude of the current Hubble tension' is not supported by any explicit error budget, sensitivity analysis, or marginalization over 1–2 % shifts in the distance scale or sound-horizon calibration. Without such a demonstration the inference that the offset survives all plausible systematics cannot be assessed.
  2. [Abstract] Abstract: the statement that DESI BAO + uncalibrated SN Ia 'yields a value for H0 that is significantly higher' does not report the numerical H0 value, the tension level in sigma, or the precise reference to the external analysis being summarized, preventing evaluation of whether the joint posterior remains discrepant after calibration uncertainties are included.
minor comments (2)
  1. [Abstract] Abstract: 'predication' is a typographical error and should read 'prediction'.
  2. [Abstract] Abstract: the phrase 'Our findings suggest' is inappropriate for a review that reports external results rather than new derivations; rephrase to 'The reviewed analyses indicate'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful comments on our review manuscript. We address each major comment below and will revise the abstract to improve clarity and support for the key claims while remaining faithful to the summarized literature.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the load-bearing claim that 'existing systematics are insufficient to account for the magnitude of the current Hubble tension' is not supported by any explicit error budget, sensitivity analysis, or marginalization over 1–2 % shifts in the distance scale or sound-horizon calibration. Without such a demonstration the inference that the offset survives all plausible systematics cannot be assessed.

    Authors: The abstract condenses conclusions drawn from the DESI BAO + uncalibrated SN Ia analyses discussed in the body of the review. Those cited works do address calibration uncertainties and systematics at the percent level. To make this explicit in the abstract, we will add a parenthetical reference to the quantitative error budgets and marginalization procedures presented in the primary analyses being summarized. As this is a review, we do not perform new sensitivity tests ourselves but will ensure the abstract points readers directly to the relevant error-budget discussions in the cited literature. revision: yes

  2. Referee: [Abstract] Abstract: the statement that DESI BAO + uncalibrated SN Ia 'yields a value for H0 that is significantly higher' does not report the numerical H0 value, the tension level in sigma, or the precise reference to the external analysis being summarized, preventing evaluation of whether the joint posterior remains discrepant after calibration uncertainties are included.

    Authors: We agree that the abstract would be clearer with these specifics. In the revised version we will insert the numerical H0 value reported by the DESI+uncalibrated SN analysis, the tension significance relative to early-universe ΛCDM, and the exact citation of the external study being summarized. This will allow readers to evaluate the claim directly. revision: yes

Circularity Check

0 steps flagged

Review reports external DESI+SN results; no internal derivation or self-referential steps

full rationale

The paper is a review that summarizes literature on the Hubble tension. Its strongest claim cites the combination of DESI BAO and uncalibrated SN Ia data as yielding a higher H0 than early-universe ΛCDM, but this is presented as a reported outcome from external datasets and analyses rather than any derivation, fit, or prediction performed within the paper itself. No equations, ansatzes, uniqueness theorems, or self-citations are invoked to generate new quantities from the paper's own inputs. The text explicitly flags that systematics are 'insufficient to account for the magnitude' but does not derive this assessment from its own fitted parameters or reduce any result to a self-definition. The derivation chain is therefore self-contained against external benchmarks, with no load-bearing steps that reduce by construction to the paper's own content.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a review paper; it introduces no new free parameters, axioms, or invented entities of its own.

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Forward citations

Cited by 1 Pith paper

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