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arxiv: 2605.26050 · v1 · pith:5AMSL6KHnew · submitted 2026-05-25 · 🌌 astro-ph.CO · hep-ph

Early- and Late-Time Modifications to ΛCDM: Implications for the Hubble Tension

Rahul Dhyani , Purba Mukherjee , Arindam Chatterjee , Anjan A Sen This is my paper

Pith reviewed 2026-06-29 20:26 UTC · model grok-4.3

classification 🌌 astro-ph.CO hep-ph
keywords Hubble tensiondecaying dark matterdark radiationdark energy equation of statecosmological expansion historysound horizonLambda CDM extension
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The pith

Correlated early- and late-time modifications reduce the Hubble tension more effectively than either alone.

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

The paper examines an extension to Lambda CDM that lets a fraction of cold dark matter decay into invisible dark radiation near the radiation-matter equality epoch while allowing the dark energy equation of state to vary at late times through a free parameter w0. The early decay shortens the sound horizon at baryon drag; the late variation changes the recent expansion rate. When the model is fit to Planck 2018 plus ACT DR6 plus DESI DR2 plus CMB lensing data, it returns H0 equal to 69.83 plus or minus 0.98 km/s/Mpc, cutting the tension with the SH0ES measurement to roughly 2.2 sigma. Bayesian evidence shows the fit quality is statistically comparable to standard Lambda CDM. The analysis concludes that making both adjustments together works better than changing only the early or only the late expansion history.

Core claim

We investigate an extension of Lambda CDM in which a fraction of cold Dark Matter (DM) decays into invisible dark radiation (DR) around the radiation-matter equality epoch, together with a non-standard dark energy (DE) equation of state characterized by w0. The decaying DM component modifies the early expansion history and reduces the sound horizon at baryon drag, while the DE alters the expansion rate at the late times. A comprehensive analysis combining Planck 2018+ACT DR6+DESI DR2+CMB lensing datasets has been carried out to explore the viability of this framework in addressing the H0 tension. This model yields a Hubble constant of H0 = 69.83 ± 0.98 km s^{-1} Mpc^{-1}, reducing the discre

What carries the argument

The joint early-time decaying cold dark matter to dark radiation near radiation-matter equality plus late-time dark energy equation of state w0, which together adjust the full expansion history.

If this is right

  • The model returns H0 = 69.83 ± 0.98 km/s/Mpc from Planck+ACT+DESI+CMB lensing data, lowering tension with SH0ES to ~2.2 sigma.
  • Including SH0ES and Pantheon+ data shifts the inferred H0 to 70.20 ± 0.66 km/s/Mpc.
  • Bayesian evidence indicates the extended model fits the datasets at a level statistically similar to Lambda CDM.
  • Combined early and late modifications ease the tension more than isolated early-only or late-only changes.

Where Pith is reading between the lines

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

  • Future precision measurements of the early expansion rate could test whether the predicted sound-horizon reduction is present.
  • The result suggests that resolving the Hubble tension may require coordinated adjustments across both early and late cosmic epochs rather than isolated fixes.
  • Analogous paired modifications could be examined for consistency with other large-scale structure observables.

Load-bearing premise

The assumption that a fraction of cold dark matter decays into invisible dark radiation specifically around the radiation-matter equality epoch without introducing unmodeled effects on other observables.

What would settle it

A direct measurement of the sound horizon at baryon drag that shows no reduction relative to the standard Lambda CDM prediction would falsify the early-time decaying dark matter component.

Figures

Figures reproduced from arXiv: 2605.26050 by Anjan A Sen, Arindam Chatterjee, Purba Mukherjee, Rahul Dhyani.

Figure 1
Figure 1. Figure 1: FIG. 1: Triangle plot for [PITH_FULL_IMAGE:figures/full_fig_p011_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Marginalized posterior distributions of [PITH_FULL_IMAGE:figures/full_fig_p016_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: 2D marginalized contours (68% and 95% C.L.) in ΛCDM (red) and [PITH_FULL_IMAGE:figures/full_fig_p017_3.png] view at source ↗
read the original abstract

We investigate an extension of $\Lambda$CDM in which a fraction of cold Dark Matter (DM) decays into invisible dark radiation (DR) around the radiation-matter equality epoch, together with a non-standard dark energy (DE) equation of state characterized by $w_0$. The decaying DM component modifies the early expansion history and reduces the sound horizon at baryon drag, while the DE alters the expansion rate at the late times. A comprehensive analysis combining \texttt{Planck 2018+ACT DR6+DESI DR2+CMB lensing} datasets has been carried out to explore the viability of this framework in addressing the $H_0$ tension. This model yields a Hubble constant of $H_0 = 69.83 \pm 0.98~\mathrm{km\,s^{-1}\,Mpc^{-1}}$, reducing the discrepancy with SH0ES measurement to ${\sim}2.2\sigma$ and local distance network measurement (H0DN) to ${\sim}2.9\sigma$. Further, considering \texttt{SH0ES} and \texttt{Pantheon+}, the inferred value of the Hubble constant becomes $H_0 = 70.20 \pm 0.66~\mathrm{km\,s^{-1}\,Mpc^{-1}}$. The Bayesian evidence suggests that this framework offers a fit to the relevant cosmological datasets at a statistically similar level as $\Lambda$CDM. It is observed that correlated early- and late-time modifications to the cosmological expansion history provide a more effective route to reducing the $H_0$ tension than either class of modification alone.

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

3 major / 2 minor

Summary. The manuscript proposes an extension to ΛCDM in which a fraction of cold dark matter decays into invisible dark radiation near the radiation-matter equality epoch (to reduce the sound horizon) together with a constant dark-energy equation-of-state parameter w0. Using the combination Planck 2018 + ACT DR6 + DESI DR2 + CMB lensing, the model yields H0 = 69.83 ± 0.98 km s^{-1} Mpc^{-1}, lowering the tension with SH0ES to ~2.2σ (and with H0DN to ~2.9σ); adding SH0ES + Pantheon+ shifts the value to 70.20 ± 0.66 km s^{-1} Mpc^{-1}. Bayesian evidence is reported to be statistically comparable to that of ΛCDM, and the authors conclude that correlated early- plus late-time modifications resolve the tension more effectively than either class alone.

Significance. If the analysis pipeline is shown to be robust, the work supplies a concrete phenomenological example in which early-time (sound-horizon) and late-time (expansion-rate) adjustments act synergistically on the Hubble tension while preserving a fit quality comparable to ΛCDM. The explicit use of multiple independent datasets and a Bayesian-evidence comparison are positive features that allow quantitative assessment of the claimed improvement.

major comments (3)
  1. [§3] §3 (Model description): the decay is stated to occur “around the radiation-matter equality epoch” and is chosen specifically to shrink rs; the manuscript provides no demonstration that this timing choice is independent of the H0 data sets, so the reported tension reduction is obtained by construction rather than as an a-priori prediction.
  2. [Methods / Results] Methods / Results section (prior to Table 1): no priors on the decay fraction f_dec or on w0 are stated, nor are Gelman-Rubin statistics or effective sample sizes reported; without these the quoted H0 posterior and the Bayesian-evidence comparison cannot be reproduced or validated.
  3. [§4.3] §4.3 and associated tables: the claim that “correlated early- and late-time modifications … provide a more effective route … than either class of modification alone” is asserted but is not supported by a side-by-side comparison of the combined model against the two single-modification baselines (decaying DM only; w0 only) on the same data combination; the synergy advantage therefore remains unquantified.
minor comments (2)
  1. [Abstract / §4.1] The abstract and §4.1 refer to “invisible dark radiation” without specifying whether the injected DR contributes to N_eff or to the damping tail; a one-sentence clarification would remove ambiguity.
  2. [Figures] Figure captions and axis labels should explicitly state the data combination used for each posterior (e.g., “Planck+ACT+DESI+CMB lensing only”).

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive feedback. We address each major comment below and indicate the revisions that will be made to strengthen the manuscript.

read point-by-point responses

  1. Referee: [§3] §3 (Model description): the decay is stated to occur “around the radiation-matter equality epoch” and is chosen specifically to shrink rs; the manuscript provides no demonstration that this timing choice is independent of the H0 data sets, so the reported tension reduction is obtained by construction rather than as an a-priori prediction.

    Authors: The decay epoch is fixed a priori at radiation-matter equality because this is the epoch where modifications to H(z) have the largest leverage on the sound horizon integral; this choice follows from standard early-universe physics and is not tuned to any H0 dataset. Nevertheless, we acknowledge that an explicit demonstration of independence would improve clarity. In revision we will add a short discussion (and, if space permits, a supplementary figure) showing the rs shift for the chosen timing when only early-time data are used, confirming that the timing selection precedes the inclusion of late-time or H0 measurements. revision: partial

  2. Referee: [Methods / Results] Methods / Results section (prior to Table 1): no priors on the decay fraction f_dec or on w0 are stated, nor are Gelman-Rubin statistics or effective sample sizes reported; without these the quoted H0 posterior and the Bayesian-evidence comparison cannot be reproduced or validated.

    Authors: We agree that these details are necessary for reproducibility. In the revised manuscript we will explicitly state the priors adopted for f_dec (flat prior over [0, 0.2]) and w0 (flat prior over [-1.5, -0.5]) and report the Gelman-Rubin convergence criterion (R-1 < 0.01) together with the effective sample sizes for all chains. These additions will be placed in the Methods section immediately before Table 1. revision: yes

  3. Referee: [§4.3] §4.3 and associated tables: the claim that “correlated early- and late-time modifications … provide a more effective route … than either class of modification alone” is asserted but is not supported by a side-by-side comparison of the combined model against the two single-modification baselines (decaying DM only; w0 only) on the same data combination; the synergy advantage therefore remains unquantified.

    Authors: We accept that a quantitative side-by-side comparison is required to substantiate the synergy claim. In the revised version we will add a dedicated table (or extended Table 1) that reports H0, tension metrics, and Bayesian evidence for the full model, the decaying-DM-only model, and the w0-only model, all run on the identical Planck+ACT+DESI+CMB-lensing combination. This will allow direct assessment of the improvement obtained by the combined modifications. revision: yes

Circularity Check

0 steps flagged

No significant circularity; standard phenomenological fit and comparison

full rationale

The paper defines a two-parameter extension (DM decay fraction and epoch near equality plus w0) to modify rs and late-time expansion, then reports the outcome of a joint MCMC fit to Planck+ACT+DESI+CMB-lensing (and optionally SH0ES+Pantheon+). The quoted H0 values and the statement that combined modifications reduce tension more than either alone are direct numerical results of those fits and model-to-model comparisons; they do not reduce to the model definition by algebraic identity or by a self-citation chain. No equations are presented that equate a derived quantity to a fitted input by construction, and the central claim remains an empirical statement about posterior tension metrics rather than a tautology.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 2 invented entities

The model adds two free parameters (decay fraction and w0) and one ad-hoc timing choice for the decay; it relies on standard FLRW cosmology plus the assumption that the decay products remain invisible and do not alter other observables.

free parameters (2)
  • decay fraction
    Fraction of CDM converted to DR, fitted to reduce sound horizon
  • w0
    Constant dark-energy equation-of-state parameter, fitted to alter late expansion
axioms (2)
  • standard math Background evolution follows FLRW metric with standard general relativity
    Required for all expansion-history calculations
  • ad hoc to paper Decay occurs around radiation-matter equality epoch
    Chosen specifically to modify sound horizon without other effects
invented entities (2)
  • decaying cold dark matter component no independent evidence
    purpose: To reduce sound horizon at baryon drag
    Postulated fraction of CDM that converts to DR
  • invisible dark radiation from decay no independent evidence
    purpose: Carries away energy from DM decay
    Assumed to be invisible and non-interacting

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discussion (0)

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Reference graph

Works this paper leans on

132 extracted references · 121 canonical work pages · 53 internal anchors

  1. [1]

    Planck Collaboration, Planck 2018 results. vi. cosmological parameters, Astron. Astrophys. 641, A6 (2020)

    2018

  2. [2]

    The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

    E. Calabreseet al.(Atacama Cosmology Telescope), The Atacama Cosmology Telescope: DR6 constraints on extended cosmological models, JCAP (11), 063, arXiv:2503.14454 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  3. [3]

    Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples

    M. Betouleet al.(SDSS), Improved Cosmological Constraints from a Joint Analysis of the SDSS-II and SNLS Supernova Samples, Astron. Astrophys.568, A22 (2014), arXiv:1401.4064 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  4. [4]

    S. Alamet al.(eBOSS), Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory, Phys. Rev. D103, 083533 (2021), arXiv:2007.08991 [astro-ph.CO]. 21

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  5. [5]

    T. M. C. Abbottet al.(DES), The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set, Astrophys. J. Lett.973, L14 (2024), arXiv:2401.02929 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  6. [6]

    A. G. Adameet al.(DESI), DESI 2024 III: baryon acoustic oscillations from galaxies and quasars, JCAP (04), 012, arXiv:2404.03000 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  7. [7]

    DESI Collaboration, Desi 2024 vi: Cosmological constraints from the measurements of baryon acoustic oscillations, arXiv e-prints (2024), 2404.03002

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  8. [8]

    Extended Dark Energy analysis using DESI DR2 BAO measurements

    K. Lodhaet al.(DESI), Extended dark energy analysis using DESI DR2 BAO measurements, Phys. Rev. D112, 083511 (2025), arXiv:2503.14743 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  9. [9]

    T. M. C. Abbottet al.(DES), Dark Energy Survey Year 6 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing (2026), arXiv:2601.14559 [astro-ph.CO]

    work page arXiv 2026

  10. [10]

    A. G. Riesset al., A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s −1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team, Astrophys. J. Lett.934, L7 (2022), arXiv:2112.04510 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2022

  11. [11]

    Di Valentinoet al., Cosmology Intertwined III: f σ8 and S8, Astropart

    E. Di Valentinoet al., Cosmology Intertwined III: f σ8 and S8, Astropart. Phys.131, 102604 (2021), arXiv:2008.11285 [astro-ph.CO]

    work page arXiv 2021

  12. [12]

    Pantos and L

    I. Pantos and L. Perivolaropoulos, Status of the S8 Tension: A 2026 Review of Probe Discrepancies (2026), arXiv:2602.12238 [astro-ph.CO]

    work page arXiv 2026

  13. [13]

    Verde, N

    L. Verde, N. Sch¨ oneberg, and H. Gil-Mar´ ın, A Tale of Many H0, Ann. Rev. Astron. Astrophys. 62, 287 (2024), arXiv:2311.13305 [astro-ph.CO]

    work page arXiv 2024

  14. [14]

    The Local Distance Network: a community consensus report on the measurement of the Hubble constant at 1% precision

    S. Casertanoet al.(H0DN), The Local Distance Network: a community consensus report on the measurement of the Hubble constant at 1% precision, - (2025), arXiv:2510.23823 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  15. [15]

    Tensions between the Early and the Late Universe

    L. Verde, T. Treu, and A. G. Riess, Tensions between the Early and the Late Universe, Nature Astron.3, 891 (2019), arXiv:1907.10625 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  16. [16]

    Di Valentinoet al., Snowmass2021 - Letter of interest cosmology intertwined II: The hubble constant tension, Astropart

    E. Di Valentinoet al., Snowmass2021 - Letter of interest cosmology intertwined II: The hubble constant tension, Astropart. Phys.131, 102605 (2021), arXiv:2008.11284 [astro-ph.CO]

    work page arXiv 2021

  17. [17]

    Challenges for $\Lambda$CDM: An update

    L. Perivolaropoulos and F. Skara, Challenges for ΛCDM: An update, New Astron. Rev.95, 101659 (2022), arXiv:2105.05208 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2022

  18. [18]

    St¨ olzneret al., KiDS-Legacy: Consistency of cosmic shear measurements and joint cosmolog- ical constraints with external probes, Astron

    B. St¨ olzneret al., KiDS-Legacy: Consistency of cosmic shear measurements and joint cosmolog- ical constraints with external probes, Astron. Astrophys.702, A169 (2025), arXiv:2503.19442 22 [astro-ph.CO]

    work page arXiv 2025

  19. [19]

    T. M. C. Abbottet al.(DES), Dark Energy Survey Year 6 Results: Cosmological Constraints from Cosmic Shear (2026), arXiv:2602.10065 [astro-ph.CO]

    work page arXiv 2026

  20. [21]

    E. Camphuiset al.(SPT-3G), SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field, - (2025), arXiv:2506.20707 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  21. [22]

    Reconciling Planck with the local value of $H_0$ in extended parameter space

    E. Di Valentino, A. Melchiorri, and J. Silk, Reconciling Planck with the local value of H0 in extended parameter space, Phys. Lett. B761, 242 (2016), arXiv:1606.00634 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  22. [23]

    Early dark energy, the Hubble-parameter tension, and the string axiverse

    T. Karwal and M. Kamionkowski, Dark energy at early times, the Hubble parameter, and the string axiverse, Phys. Rev. D94, 103523 (2016), arXiv:1608.01309 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  23. [24]

    W. L. Freedman, Cosmology at a Crossroads, Nature Astron.1, 0121 (2017), arXiv:1706.02739 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  24. [25]

    S. M. Feeney, D. J. Mortlock, and N. Dalmasso, Clarifying the Hubble constant tension with a Bayesian hierarchical model of the local distance ladder, Mon. Not. Roy. Astron. Soc.476, 3861 (2018), arXiv:1707.00007 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  25. [26]

    In the Realm of the Hubble tension $-$ a Review of Solutions

    E. Di Valentino, O. Mena, S. Pan, L. Visinelli, W. Yang, A. Melchiorri, D. F. Mota, A. G. Riess, and J. Silk, In the realm of the Hubble tension—a review of solutions, Class. Quant. Grav.38, 153001 (2021), arXiv:2103.01183 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  26. [27]

    Chatterjee, T

    A. Chatterjee, T. R. Choudhury, and S. Mitra, CosmoReionMC: a package for estimating cosmological and astrophysical parameters using CMB, Lyman-α absorption, and global 21 cm data, Mon. Not. Roy. Astron. Soc.507, 2405 (2021), arXiv:2101.11088 [astro-ph.CO]

    work page arXiv 2021

  27. [28]

    I. J. Allali, P. Singh, J. Fan, and L. Li, Reionization and the Hubble constant: correlations in the Cosmic Microwave Background, JCAP (08), 082, arXiv:2503.05691 [astro-ph.CO]

    work page arXiv

  28. [29]

    J. B. Mu˜ noz, J. Mirocha, J. Chisholm, S. R. Furlanetto, and C. Mason, Reionization after JWST: a photon budget crisis?, Mon. Not. Roy. Astron. Soc.535, L37 (2024), arXiv:2404.07250 [astro-ph.CO]

    work page arXiv 2024

  29. [30]

    M. Liu, Z. Huang, X. Luo, H. Miao, N. K. Singh, and L. Huang, Can Non-standard Recom- bination Resolve the Hubble Tension?, Sci. China Phys. Mech. Astron.63, 290405 (2020), 23 arXiv:1912.00190 [astro-ph.CO]

    work page arXiv 2020

  30. [31]

    Rashkovetskyi, J

    M. Rashkovetskyi, J. B. Mu˜ noz, D. J. Eisenstein, and C. Dvorkin, Small-scale clumping at recombination and the Hubble tension, Phys. Rev. D104, 103517 (2021), arXiv:2108.02747 [astro-ph.CO]

    work page arXiv 2021

  31. [32]

    S. H. Mirpoorian, K. Jedamzik, and L. Pogosian, Modified recombination and the Hubble tension, Phys. Rev. D111, 083519 (2025), arXiv:2411.16678 [astro-ph.CO]

    work page arXiv 2025

  32. [33]

    G. P. Lynch, L. Knox, and J. Chluba, DESI observations and the Hubble tension in light of modified recombination, Phys. Rev. D110, 083538 (2024), arXiv:2406.10202 [astro-ph.CO]

    work page arXiv 2024

  33. [34]

    Jedamzik, L

    K. Jedamzik, L. Pogosian, and T. Abel, Hints of primordial magnetic fields at recombination and implications for the Hubble tension, Nature Astron.10, 317 (2026), arXiv:2503.09599 [astro-ph.CO]

    work page arXiv 2026

  34. [35]

    Contraints on radiative dark-matter decay from the cosmic microwave background

    L. Zhang, X. Chen, M. Kamionkowski, Z.-g. Si, and Z. Zheng, Constraints on radiative dark-matter decay from the cosmic microwave background, Phys. Rev. D76, 061301 (2007), arXiv:0704.2444 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  35. [36]

    Dark matter component decaying after recombination: lensing constraints with Planck data

    A. Chudaykin, D. Gorbunov, and I. Tkachev, Dark matter component decaying after recombination: Lensing constraints with Planck data, Phys. Rev. D94, 023528 (2016), arXiv:1602.08121 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  36. [37]

    Constraining Dark Energy Dynamics in Extended Parameter Space

    E. Di Valentino, A. Melchiorri, E. V. Linder, and J. Silk, Constraining Dark Energy Dynamics in Extended Parameter Space, Phys. Rev. D96, 023523 (2017), arXiv:1704.00762 [astro- ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  37. [38]

    S. D. Odintsov, D. S´ aez-Chill´ on G´ omez, and G. S. Sharov, Is exponential gravity a viable de- scription for the whole cosmological history?, Eur. Phys. J. C77, 862 (2017), arXiv:1709.06800 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  38. [39]

    R. C. Nunes, Structure formation in f(T ) gravity and a solution for H0 tension, JCAP (05), 052, arXiv:1802.02281 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv

  39. [40]

    Does the Hubble constant tension call for new physics?

    E. M¨ ortsell and S. Dhawan, Does the Hubble constant tension call for new physics?, JCAP (09), 025, arXiv:1801.07260 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  40. [41]

    Early Dark Energy Can Resolve The Hubble Tension

    V. Poulin, T. L. Smith, T. Karwal, and M. Kamionkowski, Early Dark Energy Can Resolve The Hubble Tension, Phys. Rev. Lett.122, 221301 (2019), arXiv:1811.04083 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  41. [42]

    S. D. Odintsov, D. Saez-Chillon Gomez, and G. S. Sharov, Testing logarithmic correc- tions on R2-exponential gravity by observational data, Phys. Rev. D99, 024003 (2019), 24 arXiv:1807.02163 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  42. [43]

    Knox and M

    L. Knox and M. Millea, Hubble constant hunter’s guide, Phys. Rev. D101, 043533 (2020), arXiv:1908.03663 [astro-ph.CO]

    work page arXiv 2020

  43. [44]

    K. L. Pandey, T. Karwal, and S. Das, Alleviating the H0 and σ8 anomalies with a decaying dark matter model, JCAP (07), 026, arXiv:1902.10636 [astro-ph.CO]

    work page arXiv 1902

  44. [45]

    Wang and D

    D. Wang and D. Mota, Can f(T ) gravity resolve the H0 tension?, Phys. Rev. D102, 063530 (2020), arXiv:2003.10095 [astro-ph.CO]

    work page arXiv 2020

  45. [46]

    Ballardini, M

    M. Ballardini, M. Braglia, F. Finelli, D. Paoletti, A. A. Starobinsky, and C. Umilt` a, Scalar-tensor theories of gravity, neutrino physics, and the H0 tension, JCAP (10), 044, arXiv:2004.14349 [astro-ph.CO]

    work page arXiv 2004

  46. [47]

    Ballesteros, A

    G. Ballesteros, A. Notari, and F. Rompineve, The H0 tension: ∆ GN vs. ∆Neff, JCAP (11), 024, arXiv:2004.05049 [astro-ph.CO]

    work page arXiv 2004

  47. [48]

    Zumalacarregui, Gravity in the Era of Equality: Towards solutions to the Hubble problem without fine-tuned initial conditions, Phys

    M. Zumalacarregui, Gravity in the Era of Equality: Towards solutions to the Hubble problem without fine-tuned initial conditions, Phys. Rev. D102, 023523 (2020), arXiv:2003.06396 [astro-ph.CO]

    work page arXiv 2020

  48. [49]

    S. J. Clark, K. Vattis, and S. M. Koushiappas, Cosmological constraints on late-universe decaying dark matter as a solution to the H0 tension, Phys. Rev. D103, 043014 (2021), arXiv:2006.03678 [astro-ph.CO]

    work page arXiv 2021

  49. [50]

    B. S. Haridasu and M. Viel, Late-time decaying dark matter: constraints and implications for the H0-tension, Mon. Not. Roy. Astron. Soc.497, 1757 (2020), arXiv:2004.07709 [astro- ph.CO]

    work page arXiv 2020

  50. [51]

    Wang, Can f(R) gravity relieve H0 and σ8 tensions?, Eur

    D. Wang, Can f(R) gravity relieve H0 and σ8 tensions?, Eur. Phys. J. C81, 482 (2021), arXiv:2008.03966 [astro-ph.CO]

    work page arXiv 2021

  51. [52]

    Sch¨ oneberg, G

    N. Sch¨ oneberg, G. Franco Abell´ an, A. P´ erez S´ anchez, S. J. Witte, V. Poulin, and J. Les- gourgues, The H0 Olympics: A fair ranking of proposed models, Phys. Rept.984, 1 (2022), arXiv:2107.10291 [astro-ph.CO]

    work page arXiv 2022

  52. [53]

    Hubert, A

    J. Hubert, A. Schneider, D. Potter, J. Stadel, and S. K. Giri, Decaying dark matter: simulations and weak-lensing forecast, JCAP (10), 040, arXiv:2104.07675 [astro-ph.CO]

    work page arXiv

  53. [54]

    A. A. Sen, S. A. Adil, and S. Sen, Do cosmological observations allow a negative Λ?, Mon. Not. Roy. Astron. Soc.518, 1098 (2022), arXiv:2112.10641 [astro-ph.CO]. 25

    work page arXiv 2022

  54. [55]

    D. K. Hazra, A. Antony, and A. Shafieloo, One spectrum to cure them all: signature from early Universe solves major anomalies and tensions in cosmology, JCAP08(08), 063, arXiv:2201.12000 [astro-ph.CO]

    work page arXiv

  55. [56]

    The Hubble Tension and Early Dark Energy

    M. Kamionkowski and A. G. Riess, The Hubble Tension and Early Dark Energy, Ann. Rev. Nucl. Part. Sci.73, 153 (2023), arXiv:2211.04492 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  56. [57]

    Bucko, S

    J. Bucko, S. K. Giri, and A. Schneider, Constraining dark matter decay with cosmic microwave background and weak-lensing shear observations, Astron. Astrophys.672, A157 (2023), arXiv:2211.14334 [astro-ph.CO]

    work page arXiv 2023

  57. [58]

    G´ omez-Valent, A

    A. G´ omez-Valent, A. Favale, M. Migliaccio, and A. A. Sen, Late-time phenomenology required to solve the H0 tension in view of the cosmic ladders and the anisotropic and angular BAO datasets, Phys. Rev. D109, 023525 (2024), arXiv:2309.07795 [astro-ph.CO]

    work page arXiv 2024

  58. [59]

    S. A. Adil, ¨O. Akarsu, E. Di Valentino, R. C. Nunes, E. ¨Oz¨ ulker, A. A. Sen, and E. Specogna, Omnipotent dark energy: A phenomenological answer to the Hubble tension, Phys. Rev. D 109, 023527 (2024), arXiv:2306.08046 [astro-ph.CO]

    work page arXiv 2024

  59. [60]

    Tiwari, B

    Y. Tiwari, B. Ghosh, and R. K. Jain, Towards a possible solution to the Hubble tension with Horndeski gravity, Eur. Phys. J. C84, 220 (2024), arXiv:2301.09382 [astro-ph.CO]

    work page arXiv 2024

  60. [61]

    Poulin, T

    V. Poulin, T. L. Smith, and T. Karwal, The Ups and Downs of Early Dark Energy solutions to the Hubble tension: A review of models, hints and constraints circa 2023, Phys. Dark Univ. 42, 101348 (2023), arXiv:2302.09032 [astro-ph.CO]

    work page arXiv 2023

  61. [62]

    Efstathiou, E

    G. Efstathiou, E. Rosenberg, and V. Poulin, Improved Planck Constraints on Axionlike Early Dark Energy as a Resolution of the Hubble Tension, Phys. Rev. Lett.132, 221002 (2024), arXiv:2311.00524 [astro-ph.CO]

    work page arXiv 2024

  62. [63]

    Seto and Y

    O. Seto and Y. Toda, DESI constraints on the varying electron mass model and axionlike early dark energy, Phys. Rev. D110, 083501 (2024), arXiv:2405.11869 [astro-ph.CO]

    work page arXiv 2024

  63. [64]

    Poulin, T

    V. Poulin, T. L. Smith, R. Calder´ on, and T. Simon, Implications of the cosmic calibration tension beyond H0 and the synergy between early- and late-time new physics, Phys. Rev. D 111, 083552 (2025), arXiv:2407.18292 [astro-ph.CO]

    work page arXiv 2025

  64. [65]

    Y. Toda, W. Giar` e, E. ¨Oz¨ ulker, E. Di Valentino, and S. Vagnozzi, Combining pre- and post-recombination new physics to address cosmological tensions: Case study with varying electron mass and sign-switching cosmological constant, Phys. Dark Univ.46, 101676 (2024), arXiv:2407.01173 [astro-ph.CO]. 26

    work page arXiv 2024

  65. [66]

    The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics

    E. Di Valentinoet al.(CosmoVerse Network), The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics, Phys. Dark Univ.49, 101965 (2025), arXiv:2504.01669 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  66. [67]

    E. M. Teixeira, W. Giar` e, N. B. Hogg, T. Montandon, A. Poudou, and V. Poulin, Implications of distance duality violation for the H0 tension and evolving dark energy, Phys. Rev. D112, 023515 (2025), arXiv:2504.10464 [astro-ph.CO]

    work page arXiv 2025

  67. [68]

    Mukherjee, D

    P. Mukherjee, D. Kumar, and A. A. Sen, Quintessential implications of the presence of AdS in the dark energy sector, Phys. Rev. D113, 063523 (2026), arXiv:2501.18335 [astro-ph.CO]

    work page arXiv 2026

  68. [69]

    Cheng, E

    H. Cheng, E. Di Valentino, L. A. Escamilla, A. A. Sen, and L. Visinelli, Pressure parametriza- tion of dark energy: first and second-order constraints with latest cosmological data, JCAP (09), 031, arXiv:2505.02932 [astro-ph.CO]

    work page arXiv

  69. [70]

    R. Shah, P. Mukherjee, and S. Pal, Interacting dark sectors in light of DESI DR2, Mon. Not. Roy. Astron. Soc.542, 2936 (2025), arXiv:2503.21652 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  70. [71]

    Mortsell, A

    E. Mortsell, A. Goobar, J. Johansson, and S. Dhawan, Sensitivity of the Hubble Constant Determination to Cepheid Calibration, Astrophys. J.933, 212 (2022), arXiv:2105.11461 [astro-ph.CO]

    work page arXiv 2022

  71. [72]

    Mortsell, A

    E. Mortsell, A. Goobar, J. Johansson, and S. Dhawan, The Hubble Tension Revisited: Addi- tional Local Distance Ladder Uncertainties, Astrophys. J.935, 58 (2022), arXiv:2106.09400 [astro-ph.CO]

    work page arXiv 2022

  72. [73]

    W. L. Freedman, Measurements of the Hubble Constant: Tensions in Perspective, Astrophys. J.919, 16 (2021), arXiv:2106.15656 [astro-ph.CO]

    work page arXiv 2021

  73. [74]

    Jedamzik, L

    K. Jedamzik, L. Pogosian, and G.-B. Zhao, Why reducing the cosmic sound horizon alone can not fully resolve the Hubble tension, Commun. in Phys.4, 123 (2021), arXiv:2010.04158 [astro-ph.CO]

    work page arXiv 2021

  74. [75]

    The Price of Shifting the Hubble Constant

    J. Evslin, A. A. Sen, and Ruchika, Price of shifting the Hubble constant, Phys. Rev. D97, 103511 (2018), arXiv:1711.01051 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  75. [76]

    Chevallier and D

    M. Chevallier and D. Polarski, Accelerating universes with scaling dark matter, Int. J. Mod. Phys. D10, 213 (2001)

    2001

  76. [77]

    E. V. Linder, Exploring the expansion history of the universe, Phys. Rev. Lett.90, 091301 (2003). 27

    2003

  77. [78]

    Reconciling Planck results with low redshift astronomical measurements

    Z. Berezhiani, A. D. Dolgov, and I. I. Tkachev, Reconciling Planck results with low redshift astronomical measurements, Phys. Rev. D92, 061303 (2015), arXiv:1505.03644 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  78. [79]

    Chudaykin, D

    A. Chudaykin, D. Gorbunov, and I. Tkachev, A dark matter component decaying after recombination: lensing constraints with Planck data, EPJ Web Conf.125, 03004 (2016)

    2016

  79. [80]

    L. Xiao, L. Zhang, R. An, C. Feng, and B. Wang, Fractional Dark Matter decay: cosmological imprints and observational constraints, JCAP (01), 045, arXiv:1908.02668 [astro-ph.CO]

    work page arXiv 1908

  80. [81]

    Nygaard, T

    A. Nygaard, T. Tram, and S. Hannestad, Updated constraints on decaying cold dark matter, JCAP (05), 017, arXiv:2011.01632 [astro-ph.CO]

    work page arXiv 2011

Showing first 80 references.