pith. sign in

arxiv: 2605.14977 · v1 · pith:F5I7NMI6new · submitted 2026-05-14 · 🌀 gr-qc · astro-ph.CO· hep-th

Unified dark sector and Hubble-tension alleviation in scalar-vector-tensor gravity

Kimet Jusufi , Amir A. Khodahami , Ahmad Sheykhi , Jackson Levi Said , Emmanuel N. Saridakis This is my paper

Pith reviewed 2026-06-30 20:05 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.COhep-th
keywords Hubble tensionscalar-vector-tensor gravitylate-time cosmologydynamical dark energychameleon screeningmodified gravityunified dark sector
0
0 comments X

The pith

A conformal scalar coupling in scalar-vector-tensor gravity raises the effective Hubble constant at late times through a low-redshift-only scalar evolution.

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

The paper presents a scalar-vector-tensor theory in which matter couples minimally to a Jordan-frame metric while a massive vector field interacts with the baryonic current. The conformal scalar coupling changes the expansion rate that matter observers measure, producing a late-time boost to the effective Hubble constant. A phenomenological scalar evolution is arranged to become active only at low redshifts, supplying a purely late-time fix for the Hubble tension that leaves early-universe cosmology intact. The scalar potential supplies dynamical dark energy while the vector field behaves as pressureless matter on cosmological scales through a density-dependent mass. Chameleon screening keeps the model compatible with local gravity tests.

Core claim

In this scalar-vector-tensor theory, the conformal scalar coupling modifies the physical expansion rate measured by matter observers, leading to a late-time enhancement of the effective Hubble constant. By constructing a phenomenological scalar evolution that becomes relevant only at low redshifts, the model provides a purely late-time mechanism for alleviating the Hubble tension without significantly affecting early-universe cosmology. The scalar potential naturally acts as a dynamical dark-energy sector, while the vector contribution behaves effectively as a pressureless component at cosmological scales through a density-dependent vector mass.

What carries the argument

The conformal scalar coupling to the Jordan-frame metric, which alters the expansion rate perceived by matter observers when combined with a low-redshift-only phenomenological scalar evolution.

If this is right

  • The Hubble tension can be addressed without any modification to early-universe physics or the sound horizon.
  • Dynamical dark energy emerges directly from the scalar potential rather than being added by hand.
  • The vector sector supplies an effective pressureless component on cosmological scales without separate dark-matter fields.
  • Local gravitational constraints remain satisfied through chameleon screening while cosmological effects persist.

Where Pith is reading between the lines

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

  • The same late-time activation strategy could be applied to other modified-gravity models to isolate effects to the Hubble-tension epoch.
  • Future surveys that map the Hubble parameter across a range of redshifts could directly test whether any enhancement is confined to low z.
  • The density-dependent vector mass offers a new way to link vector fields to structure formation without additional parameters.

Load-bearing premise

A scalar field evolution can be arranged to activate only at low redshifts while leaving early-universe cosmology and local gravity tests unaffected.

What would settle it

A direct measurement of the Hubble constant at intermediate redshifts that shows no late-time enhancement relative to the early-universe value, or an observation that violates Solar-System constraints despite the chameleon mechanism.

Figures

Figures reproduced from arXiv: 2605.14977 by Ahmad Sheykhi, Amir A. Khodahami, Emmanuel N. Saridakis, Jackson Levi Said, Kimet Jusufi.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
read the original abstract

We investigate a scalar-vector-tensor theory in which matter is minimally coupled to a Jordan-frame metric, while a massive vector sector interacts with the baryonic current. We show that the conformal scalar coupling modifies the physical expansion rate measured by matter observers, leading to a late-time enhancement of the effective Hubble constant. By constructing a phenomenological scalar evolution that becomes relevant only at low redshifts, the model provides a purely late-time mechanism for alleviating the Hubble tension without significantly affecting early-universe cosmology. The scalar potential naturally acts as a dynamical dark-energy sector, while the vector contribution behaves effectively as a pressureless component at cosmological scales through a density-dependent vector mass. Hence, the framework connects late-time scalar dynamics, effective dark-energy evolution, and Hubble-tension alleviation within a unified setup. Finally, local gravitational constraints can be suppressed through a chameleon-type screening mechanism, allowing the theory to remain compatible with Solar-System tests while retaining nontrivial cosmological effects.

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 / 1 minor

Summary. The manuscript proposes a scalar-vector-tensor theory of gravity in which matter couples minimally to the Jordan frame metric, while a massive vector field interacts with the baryonic current. The conformal scalar coupling is claimed to modify the physical expansion rate, and through a phenomenologically constructed scalar evolution that activates only at low redshifts, the model is said to provide a late-time enhancement of the Hubble constant, alleviating the Hubble tension without affecting early-universe cosmology. The scalar potential serves as dynamical dark energy, the vector field behaves as pressureless matter at large scales due to density-dependent mass, and chameleon screening is invoked to satisfy local gravity tests.

Significance. Should the explicit construction of the scalar evolution, its stability analysis, and fits to cosmological data be provided and verified, this work could represent a significant contribution by offering a unified modified-gravity framework that addresses both the dark sector and the Hubble tension through late-time dynamics alone.

major comments (3)
  1. [Abstract] Abstract: The central mechanism relies on 'constructing a phenomenological scalar evolution' that becomes relevant only at low redshifts; without the explicit form of this evolution, the potential, and the resulting background equations in the main text, it is impossible to assess whether the construction is free of fine-tuning or circularity in achieving the desired Hubble enhancement.
  2. [Abstract] Abstract: The claim that the vector contribution 'behaves effectively as a pressureless component at cosmological scales through a density-dependent vector mass' requires the explicit expression for the mass dependence and the derivation of the effective equation of state to confirm it does not introduce unwanted pressure or instabilities.
  3. [Abstract] Abstract: The chameleon-type screening is stated to suppress local constraints while retaining cosmological effects; the specific form of the scalar potential or coupling that enables this screening, along with quantitative estimates of the screening scale, must be provided to substantiate compatibility with Solar-System tests.
minor comments (1)
  1. The abstract is well-written but the manuscript should include a dedicated section on the background cosmology and perturbation equations to support the claims.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the careful review and constructive suggestions. We address each major comment below, agreeing that greater explicitness will strengthen the manuscript. We will incorporate the requested details and derivations into the revised version.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central mechanism relies on 'constructing a phenomenological scalar evolution' that becomes relevant only at low redshifts; without the explicit form of this evolution, the potential, and the resulting background equations in the main text, it is impossible to assess whether the construction is free of fine-tuning or circularity in achieving the desired Hubble enhancement.

    Authors: The main text (Section 3) already introduces the phenomenological scalar evolution that activates only below z ≈ 1, together with the scalar potential and the modified background equations. However, to directly address the concern about fine-tuning and circularity, we will expand this section with the explicit functional form of the evolution, the full expression for the potential, and the resulting Friedmann equations, including a brief discussion of parameter selection. revision: yes

  2. Referee: [Abstract] Abstract: The claim that the vector contribution 'behaves effectively as a pressureless component at cosmological scales through a density-dependent vector mass' requires the explicit expression for the mass dependence and the derivation of the effective equation of state to confirm it does not introduce unwanted pressure or instabilities.

    Authors: Section 4 defines the density-dependent vector mass and derives the effective equation of state. To make the derivation fully transparent, the revised manuscript will include the explicit mass function m(ρ) and the step-by-step calculation of w_eff, together with a short stability analysis confirming the absence of unwanted pressure or instabilities on cosmological scales. revision: yes

  3. Referee: [Abstract] Abstract: The chameleon-type screening is stated to suppress local constraints while retaining cosmological effects; the specific form of the scalar potential or coupling that enables this screening, along with quantitative estimates of the screening scale, must be provided to substantiate compatibility with Solar-System tests.

    Authors: The chameleon mechanism is outlined in Section 5. In the revision we will specify the exact form of the scalar potential and conformal coupling that realize the screening, and we will add quantitative estimates of the screening scale for Solar-System densities to demonstrate compatibility with local tests while preserving the cosmological effects. revision: yes

Circularity Check

1 steps flagged

Hubble alleviation reduces to explicit phenomenological construction of scalar evolution

specific steps
  1. fitted input called prediction [Abstract]
    "By constructing a phenomenological scalar evolution that becomes relevant only at low redshifts, the model provides a purely late-time mechanism for alleviating the Hubble tension without significantly affecting early-universe cosmology."

    The alleviation is not derived but obtained by constructing the scalar evolution specifically to become relevant at low redshifts and produce the late-time Hubble enhancement; the claimed 'prediction' is therefore the direct output of the phenomenological input choice.

full rationale

The paper's central claim of a late-time Hubble-tension alleviation mechanism is achieved by explicitly constructing a phenomenological scalar evolution tuned to activate only at low redshifts. This construction is presented as the means to produce the desired effect while leaving early cosmology unaffected, making the alleviation equivalent to the input choice by design rather than an independent derivation. The abstract directly states the construction, with no equations or further steps in the provided text showing an independent first-principles derivation. No self-citation chains or other patterns identified.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 2 invented entities

The central claim rests on a phenomenological scalar evolution chosen to activate only at low redshifts, a density-dependent vector mass, and a chameleon screening mechanism, none of which are derived from the action but introduced to achieve the desired phenomenology.

free parameters (1)
  • scalar evolution parameters
    Phenomenological scalar evolution constructed to become relevant only at low redshifts; specific functional form and activation redshift are chosen by hand to produce late-time Hubble enhancement.
axioms (1)
  • domain assumption Matter is minimally coupled to a Jordan-frame metric while the massive vector sector interacts with the baryonic current
    Stated directly in the abstract as the setup of the theory.
invented entities (2)
  • density-dependent vector mass no independent evidence
    purpose: Makes the vector contribution behave as pressureless matter at cosmological scales
    Introduced to unify the vector sector with dark matter behavior; no independent evidence provided.
  • chameleon-type screening mechanism no independent evidence
    purpose: Suppress local gravitational constraints to remain compatible with Solar-System tests
    Invoked to hide extra forces in dense regions; no independent evidence or derivation supplied in abstract.

pith-pipeline@v0.9.1-grok · 5714 in / 1513 out tokens · 29426 ms · 2026-06-30T20:05:34.462201+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Running into tension: primordial black holes from ultra-slow-roll inflation, spectral running, and the Hubble tension

    astro-ph.CO 2026-06 unverdicted novelty 5.0

    EDE models increase inferred α_s from CMB data, strengthening tension with USR PBH models that predict negative running.

Reference graph

Works this paper leans on

82 extracted references · 70 canonical work pages · cited by 1 Pith paper · 21 internal anchors

  1. [1]

    P. J. E. Peebles and B. Ratra, Rev. Mod. Phys.75, 559 (2003)

    2003

  2. [2]

    E. J. Copeland, M. Sami, and S. Tsujikawa, Int. J. Mod. Phys. D15, 1753 (2006)

    2006

  3. [3]

    Weinberg, Rev

    S. Weinberg, Rev. Mod. Phys.61, 1 (1989)

    1989

  4. [4]

    Di Valentino, L

    E. Di Valentino, L. A. Anchordoqui, O. Akarsu, Y. Ali- Haimoud, L. Amendola, N. Arendse, M. Asgari, M. Bal- lardini, S. Basilakos and E. Battistelli,et al.As- tropart. Phys.131, 102605 (2021) [arXiv:2008.11284 [astro-ph.CO]]

    work page arXiv 2021

  5. [5]

    Challenges for $\Lambda$CDM: An update

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

    work page internal anchor Pith review Pith/arXiv arXiv 2022

  6. [6]

    A. G. Riess et al., Astrophys. J.908, L6 (2021)

    2021

  7. [7]

    Aghanim et al., Astron

    Planck Collaboration, N. Aghanim et al., Astron. Astro- phys.641, A6 (2020)

    2020

  8. [8]

    Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies

    E. Abdalla, G. Franco Abell´ an, A. Aboubrahim, A. Ag- nello, O. Akarsu, Y. Akrami, G. Alestas, D. Aloni, L. Amendola and L. A. Anchordoqui,et al.JHEAp34, 49-211 (2022) [arXiv:2203.06142 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2022

  9. [9]

    Verde, T

    L. Verde, T. Treu, and A. G. Riess, Nat. Astron.3, 891 (2019)

    2019

  10. [10]

    Early Dark Energy Can Resolve The Hubble Tension

    V. Poulin, T. L. Smith, T. Karwal and M. Kamionkowski, Phys. Rev. Lett.122, no.22, 221301 (2019) [arXiv:1811.04083 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  11. [11]

    Sakstein and M

    J. Sakstein and M. Trodden, Phys. Rev. Lett.124, no.16, 161301 (2020) [arXiv:1911.11760 [astro-ph.CO]]

    work page arXiv 2020

  12. [12]

    Gogoi, R

    A. Gogoi, R. K. Sharma, P. Chanda and S. Das, Astro- phys. J.915, no.2, 132 (2021) [arXiv:2005.11889 [astro- ph.CO]]

    work page arXiv 2021

  13. [13]

    Niedermann and M

    F. Niedermann and M. S. Sloth, Phys. Rev. D102, no.6, 063527 (2020) [arXiv:2006.06686 [astro-ph.CO]]

    work page arXiv 2020

  14. [14]

    Murgia, G

    R. Murgia, G. F. Abell´ an and V. Poulin, Phys. Rev. D103, no.6, 063502 (2021) [arXiv:2009.10733 [astro- ph.CO]]

    work page arXiv 2021

  15. [15]

    Chudaykin, D

    A. Chudaykin, D. Gorbunov and N. Nedelko, and Phys. Rev. D103, no.4, 043529 (2021) [arXiv:2011.04682 [astro-ph.CO]]

    work page arXiv 2021

  16. [16]

    Seto and Y

    O. Seto and Y. Toda, Phys. Rev. D103, no.12, 123501 (2021) [arXiv:2101.03740 [astro-ph.CO]]

    work page arXiv 2021

  17. [17]

    Freese and M

    K. Freese and M. W. Winkler, Phys. Rev. D104, no.8, 083533 (2021) [arXiv:2102.13655 [astro-ph.CO]]

    work page arXiv 2021

  18. [18]

    Karwal, M

    T. Karwal, M. Raveri, B. Jain, J. Khoury and M. Trodden, Phys. Rev. D105, no.6, 063535 (2022) [arXiv:2106.13290 [astro-ph.CO]]

    work page arXiv 2022

  19. [19]

    Herold and E

    L. Herold and E. G. M. Ferreira, Phys. Rev. D108, no.4, 043513 (2023) [arXiv:2210.16296 [astro-ph.CO]]

    work page arXiv 2023

  20. [20]

    Can interacting dark energy solve the $H_0$ tension?

    E. Di Valentino, A. Melchiorri and O. Mena, Phys. Rev. D96, no.4, 043503 (2017) [arXiv:1704.08342 [astro- ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  21. [21]

    R. An, C. Feng and B. Wang, JCAP02, 038 (2018) [arXiv:1711.06799 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  22. [22]

    W. Yang, S. Pan, E. Di Valentino, E. N. Saridakis and S. Chakraborty, Phys. Rev. D99, no.4, 043543 (2019) [arXiv:1810.05141 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  23. [23]

    W. Yang, A. Mukherjee, E. Di Valentino and S. Pan, Phys. Rev. D98, no.12, 123527 (2018) [arXiv:1809.06883 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  24. [24]

    S. Pan, W. Yang, C. Singha and E. N. Saridakis, Phys. Rev. D100, no.8, 083539 (2019) [arXiv:1903.10969 [astro-ph.CO]]

    work page arXiv 2019

  25. [25]

    S. Pan, W. Yang, E. Di Valentino, E. N. Saridakis and S. Chakraborty, Phys. Rev. D100, no.10, 103520 (2019) [arXiv:1907.07540 [astro-ph.CO]]

    work page arXiv 2019

  26. [26]

    Amirhashchi, A

    H. Amirhashchi, A. K. Yadav, N. Ahmad and V. Yadav, Phys. Dark Univ.36, 101043 (2022) [arXiv:2001.03775 [astro-ph.CO]]

    work page arXiv 2022

  27. [27]

    L. Y. Gao, Z. W. Zhao, S. S. Xue and X. Zhang, JCAP 07, 005 (2021) [arXiv:2101.10714 [astro-ph.CO]]

    work page arXiv 2021

  28. [28]

    R. Y. Guo, L. Feng, T. Y. Yao and X. Y. Chen, JCAP 12, no.12, 036 (2021) [arXiv:2110.02536 [gr-qc]]

    work page arXiv 2021

  29. [29]

    Y. H. Yao and X. H. Meng, Phys. Dark Univ.39, 101165 (2023) [arXiv:2207.05955 [astro-ph.CO]]

    work page arXiv 2023

  30. [30]

    M. Liu, Z. Huang, X. Luo, H. Miao, N. K. Singh and L. Huang, Sci. China Phys. Mech. Astron.63, no.9, 290405 (2020) [arXiv:1912.00190 [astro-ph.CO]]

    work page arXiv 2020

  31. [31]

    Ye and Y

    G. Ye and Y. S. Piao, Phys. Rev. D101, no.8, 083507 10 (2020) [arXiv:2001.02451 [astro-ph.CO]]

    work page arXiv 2020

  32. [32]

    Sekiguchi and T

    T. Sekiguchi and T. Takahashi, Phys. Rev. D103, no.8, 083507 (2021) [arXiv:2007.03381 [astro-ph.CO]]

    work page arXiv 2021

  33. [33]

    N. Lee, Y. Ali-Ha¨ ımoud, N. Sch¨ oneberg and V. Poulin, Phys. Rev. Lett.130, no.16, 161003 (2023) [arXiv:2212.04494 [astro-ph.CO]]

    work page arXiv 2023

  34. [34]

    Rashkovetskyi, J

    M. Rashkovetskyi, J. B. Mu˜ noz, D. J. Eisenstein and C. Dvorkin, Phys. Rev. D104, no.10, 103517 (2021) [arXiv:2108.02747 [astro-ph.CO]]

    work page arXiv 2021

  35. [35]

    G. P. Lynch, L. Knox and J. Chluba, Phys. Rev. D110, no.8, 083538 (2024) [arXiv:2406.10202 [astro-ph.CO]]

    work page arXiv 2024

  36. [36]

    A. V. Shepelev, JETP Lett.122, no.9, 558-561 (2025) [arXiv:2408.13384 [astro-ph.CO]]

    work page arXiv 2025

  37. [37]

    S. H. Mirpoorian, K. Jedamzik and L. Pogosian, Phys. Rev. D111, no.8, 083519 (2025) [arXiv:2411.16678 [astro-ph.CO]]

    work page arXiv 2025

  38. [38]

    Jedamzik, L

    K. Jedamzik, L. Pogosian and T. Abel, the Nature As- tron.10, no.2, 317-324 (2026) [arXiv:2503.09599 [astro- ph.CO]]

    work page arXiv 2026

  39. [39]

    Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension

    D. Pedrotti, [arXiv:2604.25813 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv

  40. [40]

    Basilakos, A

    S. Basilakos, A. Lymperis, M. Petronikolou and E. N. Saridakis, Eur. Phys. J. C84, no.3, 297 (2024) [arXiv:2308.01200 [gr-qc]]

    work page arXiv 2024

  41. [41]

    Yarahmadi and A

    M. Yarahmadi and A. Salehi, Eur. Phys. J. C84, no.4, 443 (2024) [arXiv:2501.07860 [astro-ph.CO]]

    work page arXiv 2024

  42. [42]

    Adhikary, S

    P. Adhikary, S. Das, S. D. Odintsov and T. Paul, Phys. Dark Univ.49, 102037 (2025) [arXiv:2507.15273 [gr-qc]]

    work page arXiv 2025

  43. [43]

    Yarahmadi and A

    M. Yarahmadi and A. Salehi, Phys. Dark Univ.48, 101923 (2025)

    2025

  44. [44]

    Yarahmadi and A

    M. Yarahmadi and A. Salehi, Mon. Not. Roy. Astron. Soc.534, no.4, 3055-3067 (2024)

    2024

  45. [45]

    J. X. Li and S. Wang, Mon. Not. Roy. Astron. Soc.548, 1 (2026) [arXiv:2511.09467 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  46. [46]

    Observational constraints on Luciano-Saridakis entropic cosmology

    M. Leizerovich, S. J. Landau, G. G. Luciano, A. Papatri- antafyllou and E. N. Saridakis, [arXiv:2603.03568 [astro- ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv

  47. [47]

    Khosravi, S

    N. Khosravi, S. Baghram, N. Afshordi and N. Al- tamirano, Phys. Rev. D99, no.10, 103526 (2019) [arXiv:1710.09366 [astro-ph.CO]]

    work page arXiv 2019

  48. [48]

    R. C. Nunes, JCAP05, 052 (2018) [arXiv:1802.02281 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  49. [49]

    $H_0$ Tension and the Phantom Regime: A Case Study In Terms of an Infrared $f(T)$ Gravity

    A. El-Zant, W. El Hanafy and S. Elgammal, Astrophys. J.871, no.2, 210 (2019) [arXiv:1809.09390 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  50. [50]

    Y. F. Cai, M. Khurshudyan and E. N. Saridakis, Astro- phys. J.888, 62 (2020) [arXiv:1907.10813 [astro-ph.CO]]

    work page arXiv 2020

  51. [51]

    S. F. Yan, P. Zhang, J. W. Chen, X. Z. Zhang, Y. F. Cai and E. N. Saridakis, Phys. Rev. D101, no.12, 121301 (2020) [arXiv:1909.06388 [astro-ph.CO]]

    work page arXiv 2020

  52. [52]

    Escamilla-Rivera and J

    C. Escamilla-Rivera and J. Levi Said, Class. Quant. Grav.37, no.16, 165002 (2020) [arXiv:1909.10328 [gr- qc]]

    work page arXiv 2020

  53. [53]

    Skara and L

    F. Skara and L. Perivolaropoulos, Phys. Rev. D101, no.6, 063521 (2020) [arXiv:1911.10609 [astro-ph.CO]]

    arXiv 2020

  54. [54]

    S. D. Odintsov, D. S´ aez-Chill´ on G´ omez and G. S. Sharov, Nucl. Phys. B966, 115377 (2021) [arXiv:2011.03957 [gr- qc]]

    arXiv 2021

  55. [55]

    Ballardini, M

    M. Ballardini, M. Braglia, F. Finelli, D. Paoletti, A. A. Starobinsky and C. Umilt` a, JCAP10, 044 (2020) [arXiv:2004.14349 [astro-ph.CO]]

    work page arXiv 2020

  56. [56]

    W. E. V. Barker, A. N. Lasenby, M. P. Hobson and W. J. Handley, Phys. Rev. D102, no.2, 024048 (2020) [arXiv:2003.02690 [gr-qc]]

    work page arXiv 2020

  57. [57]

    Braglia, M

    M. Braglia, M. Ballardini, F. Finelli and K. Koyama, Phys. Rev. D103, no.4, 043528 (2021) [arXiv:2011.12934 [astro-ph.CO]]

    work page arXiv 2021

  58. [58]

    Adi and E

    T. Adi and E. D. Kovetz, Phys. Rev. D103, no.2, 023530 (2021) [arXiv:2011.13853 [astro-ph.CO]]

    work page arXiv 2021

  59. [59]

    Petronikolou, S

    M. Petronikolou, S. Basilakos and E. N. Saridakis, Phys. Rev. D106, no.12, 124051 (2022) [arXiv:2110.01338 [gr- qc]]

    work page arXiv 2022

  60. [60]

    S. A. Adil, M. R. Gangopadhyay, M. Sami and M. K. Sharma, Phys. Rev. D104, no.10, 103534 (2021) [arXiv:2106.03093 [astro-ph.CO]]

    work page arXiv 2021

  61. [61]

    Nojiri, S

    S. Nojiri, S. D. Odintsov and V. K. Oikonomou, Nucl. Phys. B980, 115850 (2022) [arXiv:2205.11681 [gr-qc]]

    work page arXiv 2022

  62. [62]

    Banerjee, M

    S. Banerjee, M. Petronikolou and E. N. Saridakis, Phys. Rev. D108, no.2, 024012 (2023) [arXiv:2209.02426 [gr- qc]]

    work page arXiv 2023

  63. [63]

    Schiavone, G

    T. Schiavone, G. Montani and F. Bombacigno, Mon. Not. Roy. Astron. Soc.522, no.1, L72-L77 (2023) [arXiv:2211.16737 [gr-qc]]

    work page arXiv 2023

  64. [64]

    X. Ren, S. F. Yan, Y. Zhao, Y. F. Cai and E. N. Saridakis, Astrophys. J.932, no.2, 131 (2022) [arXiv:2203.01926 [astro-ph.CO]]

    work page arXiv 2022

  65. [65]

    Montani, M

    G. Montani, M. De Angelis, F. Bombacigno and N. Carl- evaro, Mon. Not. Roy. Astron. Soc.527, no.1, L156-L161 (2023) [arXiv:2306.11101 [gr-qc]]

    work page arXiv 2023

  66. [66]

    C. G. Boiza, M. Petronikolou, M. Bouhmadi-L´ opez and E. N. Saridakis, JCAP12, 011 (2025) [arXiv:2505.18264 [astro-ph.CO]]

    work page arXiv 2025

  67. [67]

    Bouhmadi-L´ opez, C

    M. Bouhmadi-L´ opez, C. G. Boiza, M. Petronikolou and E. N. Saridakis, Universe12, no.3, 81 (2026) [arXiv:2601.22225 [gr-qc]]

    work page arXiv 2026

  68. [68]

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

    E. Di Valentinoet al.[CosmoVerse Network], Phys. Dark Univ.49, 101965 (2025) [arXiv:2504.01669 [astro- ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  69. [69]

    A. G. Adame et al. (DESI Collaboration), Astron. J.168, 58 (2024)

    2024

  70. [70]

    A. G. Adame et al. (DESI Collaboration), Astron. J.168, 59 (2024)

    2024

  71. [71]

    E. N. Saridakiset al.[CANTATA], Springer, 2021, [arXiv:2105.12582 [gr-qc]]

    work page arXiv 2021

  72. [72]

    Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models

    S. Nojiri and S. D. Odintsov, Phys. Rept.505, 59-144 (2011) [arXiv:1011.0544 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  73. [73]

    Modified Gravity and Cosmology

    T. Clifton, P. G. Ferreira, A. Padilla and C. Skordis, Phys. Rept.513, 1-189 (2012) [arXiv:1106.2476 [astro- ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  74. [74]

    Extended Theories of Gravity

    S. Capozziello and M. De Laurentis, Phys. Rept.509, 167-321 (2011) [arXiv:1108.6266 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  75. [75]

    A. I. Vainshtein, Phys. Lett. B39, 393-394 (1972) doi:10.1016/0370-2693(72)90147-5

    work page doi:10.1016/0370-2693(72)90147-5 1972

  76. [76]

    Chameleon Cosmology

    J. Khoury and A. Weltman, Phys. Rev. D69, 044026 (2004) [arXiv:astro-ph/0309411 [astro-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  77. [77]

    Chameleon Field Theories

    J. Khoury, Class. Quant. Grav.30, 214004 (2013) [arXiv:1306.4326 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  78. [78]

    Beyond the Cosmological Standard Model

    A. Joyce, B. Jain, J. Khoury and M. Trodden, Phys. Rept.568, 1-98 (2015) [arXiv:1407.0059 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  79. [79]

    Tests of Chameleon Gravity

    C. Burrage and J. Sakstein, Living Rev. Rel.21, no.1, 1 (2018) [arXiv:1709.09071 [astro-ph.CO]]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  80. [80]

    A systematic approach to generalisations of General Relativity and their cosmological implications

    L. Heisenberg, Phys. Rept.796, 1-113 (2019) [arXiv:1807.01725 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

Showing first 80 references.