pith. machine review for the scientific record. sign in

arxiv: 2603.26560 · v2 · submitted 2026-03-27 · 🌌 astro-ph.CO · gr-qc

Recognition: 2 theorem links

· Lean Theorem

Exploring the interplay of late-time dynamical dark energy and new physics before recombination

Adri\`a G\'omez-Valent, Alex Gonz\'alez-Fuentes

Authors on Pith no claims yet

Pith reviewed 2026-05-14 23:09 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc
keywords dynamical dark energyphantom crossingHubble tensionrecombination physicsearly universeweighted function regressionsupernova dataBAO constraints
0
0 comments X

The pith

If recombination physics stays standard, data favor phantom-crossing dark energy and exclude LambdaCDM at up to 3 sigma.

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

The authors apply an improved weighted function regression method to reconstruct the dark energy equation of state from CMB, BAO, and supernova data under two cosmic distance ladder calibrations. When early-universe physics is left unmodified, the reconstruction shows a 96.7-98.5 percent probability of phantom crossing and excludes a cosmological constant at 2.5-3 sigma . Allowing new physics before recombination to ease the Hubble tension removes the need for phantom behavior and leaves only a mild preference for quintessence, yet it forces the matter density parameter to values in strong tension with CMB constraints, especially under the SH0ES calibration. The results depend on the supernova sample and calibration choice, and the authors caution that the matter-density mismatch prevents firm conclusions about late-time dynamics.

Core claim

If physics prior to decoupling remains unmodified, current data indicate a 96.7-98.5 percent probability of phantom crossing in the dark energy equation of state and exclude LambdaCDM at 2.5-3 sigma . Early new physics can reduce the Hubble tension but requires extremely large values of the reduced matter density parameter that conflict with full CMB analyses, rendering phantom crossing no longer required and leaving only a mild quintessence preference; the tension in matter density nevertheless makes firm statements about dynamical dark energy premature.

What carries the argument

The Weighted Function Regression (WFR) method for model-independent reconstruction of the background dark energy equation of state, applied separately with SH0ES and CCHP cosmic-ladder calibrations.

If this is right

  • Phantom crossing occurs with 96.7-98.5 percent probability under unmodified early physics.
  • LambdaCDM is disfavored at 2.5-3 sigma when recombination is standard.
  • Early new physics reduces the Hubble tension but forces matter densities far above CMB-inferred values under SH0ES calibration.
  • With early new physics included, the data show only mild preference for quintessence and no requirement for phantom crossing.
  • The strength of the dynamical dark energy signal varies with the supernova sample and the choice of distance-ladder calibration.

Where Pith is reading between the lines

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

  • Independent large-scale structure measurements of the matter density could distinguish whether the early-physics route to the Hubble tension is viable.
  • Precision observations of recombination parameters would test the assumption that early new physics leaves recombination untouched.
  • If the matter-density tension persists, future data may force a joint revision of both early and late cosmological assumptions rather than isolated fixes.

Load-bearing premise

That new physics introduced before recombination leaves the recombination process itself unchanged and that the SH0ES calibration is free of large systematic errors driving the reported matter-density mismatch.

What would settle it

A CMB-derived upper limit on the matter density parameter in early new physics models that remains consistent with late-time observations, or a direct probe showing that recombination deviates from standard predictions in those models.

read the original abstract

Cosmological models exhibiting crossing of the phantom divide improve the fit to current data, suggesting late-time dark energy (DE) dynamics at $\sim3\sigma$ CL. However, they favor low values of $H_0$, in tension with SH0ES. This may point to the presence of new physics prior to the decoupling era. In this work, we reconstruct the background DE functions using the Weighted Function Regression (WFR) method, introducing three main improvements compared to our previous JCAP 12 (2025) 049. First, we adopt the Frequentist-Bayesian approach for the weights. Second, we combine CMB and BAO with the DES-Dovekie SNIa sample and compare our findings with those derived from Pantheon+, still assuming standard recombination. Third, we study in a model-independent manner the viability of early-time ``solutions'' to the Hubble tension and how they affect the evidence for dynamical DE at late times, under the influence of the SH0ES and the more conservative CCHP calibration of the cosmic ladders, separately. We find that, if the physics prior to decoupling is unmodified, the probability of phantom crossing is $\sim 96.7\text{--}98.5\%$, with $\Lambda$CDM excluded at $\sim 2.5\sigma$ and $\sim 3\sigma$ CL. New physics before recombination can alleviate the Hubble tension, but requires extremely large values of the reduced matter density parameter when the SH0ES calibration is employed, in strong tension with those inferred from full CMB analyses. This raises serious concerns about the actual viability of these models to explain the SH0ES measurement. We find that phantom crossing, while not excluded, is no longer required, with only a very mild preference for quintessence. Nevertheless, given the aforesaid tension in $\omega_m$, it would be rash to draw firm conclusions about how the dynamical DE signal is affected in these scenarios. [abridged]

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. The manuscript applies an improved Weighted Function Regression (WFR) reconstruction to the late-time dark energy equation of state, using Frequentist-Bayesian weights, the DES-Dovekie SNIa sample, and comparisons to Pantheon+. Assuming unmodified pre-decoupling physics, it reports a 96.7–98.5% probability of phantom crossing and excludes ΛCDM at 2.5–3σ. When early-time new physics is allowed to address the Hubble tension, the analysis finds that SH0ES calibration forces extreme ω_m values in tension with CMB constraints, shifting the preference to only mild quintessence-like behavior; the authors conclude that firm statements cannot be drawn until the ω_m inconsistency is resolved.

Significance. If the conditional results hold, the work supplies model-independent evidence favoring dynamical dark energy over ΛCDM at late times while quantifying the tension that arises when early-time extensions are introduced to reconcile H0 measurements. The explicit comparison of SH0ES versus CCHP calibrations and the caveat on ω_m provide a useful framework for assessing the viability of combined early- and late-time solutions to cosmological tensions.

major comments (2)
  1. [Early-time new physics discussion] Section discussing early-time new physics solutions: the statement that SH0ES calibration requires 'extremely large values of the reduced matter density parameter' in 'strong tension' with full CMB analyses should include a quantitative measure of that tension (e.g., Δω_m in units of σ relative to Planck or ACT constraints) to support the viability assessment.
  2. [WFR results and probability statements] WFR reconstruction and probability results: the reported 96.7–98.5% phantom-crossing probability range is derived from data fits, but the propagation of systematic choices (SNIa sample, calibration, and recombination assumption) through the Frequentist-Bayesian weights is not fully detailed; a dedicated error-budget table or subsection would strengthen the central claim.
minor comments (2)
  1. [Abstract] Abstract: the acronym 'DE' appears before 'dark energy' is defined; spell out on first use for clarity.
  2. [Notation and figures] Notation: the symbol ω_m is used interchangeably with the reduced matter density; confirm consistent definition and units throughout the text and figures.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments and positive recommendation. We address each major comment below and will revise the manuscript accordingly to strengthen the presentation.

read point-by-point responses

  1. Referee: [Early-time new physics discussion] Section discussing early-time new physics solutions: the statement that SH0ES calibration requires 'extremely large values of the reduced matter density parameter' in 'strong tension' with full CMB analyses should include a quantitative measure of that tension (e.g., Δω_m in units of σ relative to Planck or ACT constraints) to support the viability assessment.

    Authors: We agree that a quantitative measure of the tension would improve clarity. In the revised manuscript we will report the offset in ω_m (in units of σ) relative to the Planck and ACT constraints, derived directly from our posterior distributions under the SH0ES calibration. This addition will make the viability assessment more precise without altering the qualitative conclusion. revision: yes

  2. Referee: [WFR results and probability statements] WFR reconstruction and probability results: the reported 96.7–98.5% phantom-crossing probability range is derived from data fits, but the propagation of systematic choices (SNIa sample, calibration, and recombination assumption) through the Frequentist-Bayesian weights is not fully detailed; a dedicated error-budget table or subsection would strengthen the central claim.

    Authors: We acknowledge that an explicit error budget would help readers assess robustness. We will add a short subsection (or table) that tabulates the impact of each systematic choice—SNIa sample, calibration, and recombination assumption—on the Frequentist-Bayesian weights and on the final phantom-crossing probability. This will document the propagation without changing the reported probability range. revision: yes

Circularity Check

0 steps flagged

Minor self-citation to prior WFR method; central reconstruction remains data-driven

full rationale

The paper reconstructs DE functions via Weighted Function Regression (WFR) on external datasets (CMB, BAO, DES-Dovekie/Pantheon+ SNIa) under the explicit assumption of standard recombination. Probabilities for phantom crossing (96.7–98.5%) and ΛCDM exclusion (~2.5–3σ) are obtained from this fit; they do not reduce by construction to any parameter fitted to the target result itself. The only self-reference is to the authors’ prior JCAP 12 (2025) 049 work for the base WFR technique, but the present analysis introduces three documented improvements (Frequentist-Bayesian weights, new SNIa sample, early-physics viability study) and performs cross-checks across calibrations. No self-definitional loop, fitted-input-called-prediction, or load-bearing uniqueness theorem is present. The central claims are therefore conditional on external data and stated assumptions rather than internally forced.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

WFR weights are determined from the data; standard FLRW background and recombination assumptions are invoked when testing early modifications. No new entities are postulated.

free parameters (1)
  • WFR weights
    Determined via Frequentist-Bayesian approach on CMB+BAO+SNIa data; central to the reconstruction.
axioms (1)
  • domain assumption Standard recombination physics holds when early new physics is added
    Explicitly stated when studying viability of pre-decoupling solutions.

pith-pipeline@v0.9.0 · 5669 in / 1196 out tokens · 47605 ms · 2026-05-14T23:09:29.276689+00:00 · methodology

discussion (0)

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

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

Forward citations

Cited by 3 Pith papers

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

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

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    Model-independent reconstruction shows that early-universe modifications resolving the Hubble tension exist at the background level, requiring a smooth ~15% pre-recombination expansion rate enhancement.

  2. Double the axions, half the tension: multi-field early dark energy eases the Hubble tension

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    Two-field axion-like early dark energy reduces Hubble tension to 1.5 sigma residual and improves high-ell CMB fits over single-field models.

  3. Constraints on Coupled Dark Energy in the DESI Era

    astro-ph.CO 2026-04 unverdicted novelty 4.0

    New cosmological data mildly favor a small coupling between dark matter and a scalar dark energy field at |β| ≈ 0.03 while allowing an effective phantom-crossing equation of state.

Reference graph

Works this paper leans on

170 extracted references · 170 canonical work pages · cited by 3 Pith papers · 40 internal anchors

  1. [1]

    Efstathiou and S

    G. Efstathiou and S. Gratton,A Detailed Description of the CamSpec Likelihood Pipeline and a Reanalysis of the Planck High Frequency Maps,1910.00483

    work page arXiv 1910

  2. [2]

    Rosenberg, S

    E. Rosenberg, S. Gratton and G. Efstathiou,CMB power spectra and cosmological parameters from Planck PR4 with CamSpec,Mon. Not. Roy. Astron. Soc.517(2022) 4620 [2205.10869]

    work page arXiv 2022

  3. [3]

    The Pantheon+ Analysis: The Full Dataset and Light-Curve Release

    D. Scolnic et al.,The Pantheon+ Analysis: The Full Data Set and Light-curve Release, Astrophys. J.938(2022) 113 [2112.03863]

    work page internal anchor Pith review Pith/arXiv arXiv 2022

  4. [4]

    Rubin et al.,Union Through UNITY: Cosmology with 2,000 SNe Using a Unified Bayesian Framework,Astrophys

    D. Rubin et al.,Union Through UNITY: Cosmology with 2,000 SNe Using a Unified Bayesian Framework,Astrophys. J.986(2025) 231 [2311.12098]. [6]DEScollaboration,The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties,Astrophys. J.975(2024) 86 [2401.02945]. [7]DEScollaboration,The Dark Energy Survey: Cosmology Results with...

    work page arXiv 2025

  5. [5]

    B. Popovic et al.,The Dark Energy Survey Supernova Program: A Reanalysis Of Cosmology Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration,2511.07517. [9]eBOSScollaboration,Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Ap...

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  6. [6]

    Dynamics of dark energy

    E.J. Copeland, M. Sami and S. Tsujikawa,Dynamics of dark energy,Int. J. Mod. Phys. D15 (2006) 1753 [hep-th/0603057]

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  7. [7]

    Mavromatos and J

    N.E. Mavromatos and J. Sol` a Peracaula,Stringy-running-vacuum-model inflation: from primordial gravitational waves and stiff axion matter to dynamical dark energy,Eur. Phys. J. ST230(2021) 2077 [2012.07971]

    work page arXiv 2021

  8. [8]

    Sol` a Peracaula,The cosmological constant problem and running vacuum in the expanding universe,Phil

    J. Sol` a Peracaula,The cosmological constant problem and running vacuum in the expanding universe,Phil. Trans. Roy. Soc. Lond. A380(2022) 20210182 [2203.13757]

    work page arXiv 2022

  9. [9]

    Moreno-Pulido and J

    C. Moreno-Pulido and J. Sol` a Peracaula,Renormalizing the vacuum energy in cosmological spacetime: implications for the cosmological constant problem,Eur. Phys. J. C82(2022) 551 [2201.05827]

    work page arXiv 2022

  10. [10]

    Moreno-Pulido and J

    C. Moreno-Pulido and J. Sol` a Peracaula,Equation of state of the running vacuum,Eur. Phys. J. C82(2022) 1137 [2207.07111]

    work page arXiv 2022

  11. [11]

    Sol` a Peracaula, A

    J. Sol` a Peracaula, A. Gonz´ alez-Fuentes and C. Moreno-Pulido,Towards a unified quantum field theory of dark energy and inflation: unstable de Sitter vacuum and running vacuum, 2601.05218

    work page arXiv

  12. [12]

    Modified Gravity and Cosmology

    T. Clifton, P.G. Ferreira, A. Padilla and C. Skordis,Modified Gravity and Cosmology,Phys. Rept.513(2012) 1 [1106.2476]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  13. [13]

    Amendola and S

    L. Amendola and S. Tsujikawa,Dark Energy: Theory and Observations, Cambridge University Press (1, 2015)

    work page 2015

  14. [14]

    Quintom Cosmology: Theoretical implications and observations

    Y.-F. Cai, E.N. Saridakis, M.R. Setare and J.-Q. Xia,Quintom Cosmology: Theoretical implications and observations,Phys. Rept.493(2010) 1 [0909.2776]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  15. [15]

    Y. Cai, X. Ren, T. Qiu, M. Li and X. Zhang,The Quintom theory of dark energy after DESI DR2,2505.24732

    work page internal anchor Pith review Pith/arXiv arXiv

  16. [16]

    Dark Energy Constraints from the Cosmic Age and Supernova

    B. Feng, X.-L. Wang and X.-M. Zhang,Dark energy constraints from the cosmic age and supernova,Phys. Lett. B607(2005) 35 [astro-ph/0404224]

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  17. [17]

    LXCDM: a cosmon model solution to the cosmological coincidence problem?

    J. Grande, J. Sol` a Peracaula and H. Stefancic,LXCDM: A Cosmon model solution to the cosmological coincidence problem?,JCAP08(2006) 011 [gr-qc/0604057]

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  18. [18]

    Composite dark energy: cosmon models with running cosmological term and gravitational coupling

    J. Grande, J. Sol` a and H. Stefancic,Composite dark energy: Cosmon models with running cosmological term and gravitational coupling,Phys. Lett. B645(2007) 236 [gr-qc/0609083]

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  19. [19]

    U. Alam, V. Sahni, T.D. Saini and A.A. Starobinsky,Is there supernova evidence for dark energy metamorphosis ?,Mon. Not. Roy. Astron. Soc.354(2004) 275 [astro-ph/0311364]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  20. [20]

    U. Alam, V. Sahni and A.A. Starobinsky,The Case for dynamical dark energy revisited, JCAP06(2004) 008 [astro-ph/0403687]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  21. [21]

    Indications of a late-time interaction in the dark sector

    V. Salvatelli, N. Said, M. Bruni, A. Melchiorri and D. Wands,Indications of a late-time interaction in the dark sector,Phys. Rev. Lett.113(2014) 181301 [1406.7297]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  22. [22]

    Model independent evidence for dark energy evolution from Baryon Acoustic Oscillations

    V. Sahni, A. Shafieloo and A.A. Starobinsky,Model independent evidence for dark energy evolution from Baryon Acoustic Oscillations,Astrophys. J. Lett.793(2014) L40 [1406.2209]. – 28 –

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  23. [23]

    Hints of dynamical vacuum energy in the expanding Universe

    J. Sol` a, A. G´ omez-Valent and J. de Cruz P´ erez,Hints of dynamical vacuum energy in the expanding Universe,Astrophys. J. Lett.811(2015) L14 [1506.05793]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  24. [24]

    First evidence of running cosmic vacuum: challenging the concordance model

    J. Sol` a, A. G´ omez-Valent and J. de Cruz P´ erez,First evidence of running cosmic vacuum: challenging the concordance model,Astrophys. J.836(2017) 43 [1602.02103]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  25. [25]

    Dynamical dark energy versus $\Lambda=$const. in light of observations

    J. Sol` a Peracaula, J. de Cruz P´ erez and A. G´ omez-Valent,Dynamical dark energy vs.Λ= const in light of observations,EPL121(2018) 39001 [1606.00450]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  26. [26]

    Dynamical dark energy in light of the latest observations

    G.-B. Zhao et al.,Dynamical dark energy in light of the latest observations,Nature Astron.1 (2017) 627 [1701.08165]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  27. [27]

    Possible signals of vacuum dynamics in the Universe

    J. Sol` a Peracaula, J. de Cruz P´ erez and A. G´ omez-Valent,Possible signals of vacuum dynamics in the Universe,Mon. Not. Roy. Astron. Soc.478(2018) 4357 [1703.08218]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  28. [28]

    The $H_0$ tension in light of vacuum dynamics in the Universe

    J. Sol` a, A. G´ omez-Valent and J. de Cruz P´ erez,TheH0 tension in light of vacuum dynamics in the Universe,Phys. Lett. B774(2017) 317 [1705.06723]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  29. [29]

    Signs of Dynamical Dark Energy in Current Observations

    J. Sol` a Peracaula, A. G´ omez-Valent and J. de Cruz P´ erez,Signs of Dynamical Dark Energy in Current Observations,Phys. Dark Univ.25(2019) 100311 [1811.03505]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  30. [30]

    Chakraborty, T

    A. Chakraborty, T. Ray, S. Das, A. Banerjee and V. Ganesan,Hint of Dark Matter–Dark Energy Interaction in DESI DR2 and Current Cosmological Dataset?,Astrophys. J.998 (2026) 83 [2403.14247]

    work page arXiv 2026

  31. [31]

    G´ omez-Valent and J

    A. G´ omez-Valent and J. Sol` a Peracaula,Phantom Matter: A Challenging Solution to the Cosmological Tensions,Astrophys. J.975(2024) 64 [2404.18845]

    work page arXiv 2024

  32. [32]

    G. Ye, M. Martinelli, B. Hu and A. Silvestri,Hints of Nonminimally Coupled Gravity in DESI 2024 Baryon Acoustic Oscillation Measurements,Phys. Rev. Lett.134(2025) 181002 [2407.15832]

    work page arXiv 2024

  33. [33]

    W.J. Wolf, C. Garc´ ıa-Garc´ ıa, D.J. Bartlett and P.G. Ferreira,Scant evidence for thawing quintessence,Phys. Rev. D110(2024) 083528 [2408.17318]

    work page arXiv 2024

  34. [34]

    Roy Choudhury and T

    S. Roy Choudhury and T. Okumura,Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension, Astrophys. J. Lett.976(2024) L11 [2409.13022]

    work page arXiv 2024

  35. [35]

    C.-G. Park, J. de Cruz P´ erez and B. Ratra,Is the w0waCDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck CMB anisotropy data?,Int. J. Mod. Phys. D34(2025) 2550058 [2410.13627]

    work page arXiv 2025

  36. [36]

    G´ omez-Valent and J

    A. G´ omez-Valent and J. Sol` a Peracaula,Composite dark energy and the cosmological tensions, Phys. Lett. B864(2025) 139391 [2412.15124]

    work page arXiv 2025

  37. [37]

    Odintsov, D

    S.D. Odintsov, D. S´ aez-Chill´ on G´ omez and G.S. Sharov,Modified gravity/dynamical dark energy vsΛCDM: is the game over?,Eur. Phys. J. C85(2025) 298 [2412.09409]

    work page arXiv 2025

  38. [38]

    Giar` e, T

    W. Giar` e, T. Mahassen, E. Di Valentino and S. Pan,An overview of what current data can (and cannot yet) say about evolving dark energy,Phys. Dark Univ.48(2025) 101906 [2502.10264]

    work page arXiv 2025

  39. [39]

    W.J. Wolf, C. Garc´ ıa-Garc´ ıa and P.G. Ferreira,Robustness of dark energy phenomenology across different parameterizations,JCAP05(2025) 034 [2502.04929]

    work page arXiv 2025

  40. [40]

    Silva, M.A

    E. Silva, M.A. Sabogal, M. Scherer, R.C. Nunes, E. Di Valentino and S. Kumar,New constraints on interacting dark energy from DESI DR2 BAO observations,Phys. Rev. D111 (2025) 123511 [2503.23225]

    work page arXiv 2025

  41. [41]

    Chakraborty, P.K

    A. Chakraborty, P.K. Chanda, S. Das and K. Dutta,DESI results: hint towards coupled dark matter and dark energy,JCAP11(2025) 047 [2503.10806]. – 29 –

    work page arXiv 2025

  42. [42]

    Khoury, M.-X

    J. Khoury, M.-X. Lin and M. Trodden,Apparent w<-1 and a Lower S8 from Dark Axion and Dark Baryons Interactions,Phys. Rev. Lett.135(2025) 181001 [2503.16415]

    work page arXiv 2025

  43. [43]

    W.J. Wolf, C. Garc´ ıa-Garc´ ıa, T. Anton and P.G. Ferreira,Assessing Cosmological Evidence for Nonminimal Coupling,Phys. Rev. Lett.135(2025) 081001 [2504.07679]

    work page arXiv 2025

  44. [44]

    S. Roy Choudhury,Cosmology in Extended Parameter Space with DESI Data Release 2 Baryon Acoustic Oscillations: A 2σ+ Detection of Nonzero Neutrino Masses with an Update on Dynamical Dark Energy and Lensing Anomaly,Astrophys. J. Lett.986(2025) L31 [2504.15340]. [50]DESIcollaboration,Dynamical dark energy in light of the DESI DR2 baryonic acoustic oscillatio...

    work page arXiv 2025

  45. [45]

    Scherer, M.A

    M. Scherer, M.A. Sabogal, R.C. Nunes and A. De Felice,Challenging theΛCDM model: 5σ evidence for a dynamical dark energy late-time transition,Phys. Rev. D112(2025) 043513 [2504.20664]

    work page arXiv 2025

  46. [46]

    Y. Yang, Q. Wang, X. Ren, E.N. Saridakis and Y.-F. Cai,Modified Gravity Realizations of Quintom Dark Energy after DESI DR2,Astrophys. J.988(2025) 123 [2504.06784]

    work page arXiv 2025

  47. [47]

    Chen and A

    X. Chen and A. Loeb,Evolving dark energy or dark matter with an evolving equation-of-state?,JCAP07(2025) 059 [2505.02645]

    work page arXiv 2025

  48. [48]

    Giani, R

    L. Giani, R. Von Marttfens and O.F. Piattella,The matter with(in) CPL,2505.08467

    work page arXiv

  49. [49]

    Nojiri, S.D

    S. Nojiri, S.D. Odintsov and V.K. Oikonomou,Phantom crossing and oscillating dark energy with F(R) gravity,Phys. Rev. D112(2025) 104035 [2506.21010]

    work page arXiv 2025

  50. [50]

    Mishra, W.L

    S.S. Mishra, W.L. Matthewson, V. Sahni, A. Shafieloo and Y. Shtanov,Braneworld dark energy in light of DESI DR2,JCAP11(2025) 018 [2507.07193]

    work page arXiv 2025

  51. [51]

    Braglia, X

    M. Braglia, X. Chen and A. Loeb,Exotic dark matter and the DESI anomaly,JCAP11 (2025) 064 [2507.13925]

    work page arXiv 2025

  52. [52]

    G´ omez-Valent and A

    A. G´ omez-Valent and A. Gonz´ alez-Fuentes,Effective phantom divide crossing with standard and negative quintessence,Phys. Lett. B872(2026) 140096 [2508.00621]

    work page arXiv 2026

  53. [53]

    Roy Choudhury, T

    S. Roy Choudhury, T. Okumura and K. Umetsu,Cosmological Constraints on Nonphantom Dynamical Dark Energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3σ+ Lensing Anomaly,Astrophys. J. Lett.994(2025) L26 [2509.26144]

    work page arXiv 2025

  54. [54]

    Sohail, S

    S. Sohail, S. Alam and M.W. Hossain,Observational constraints on early time non-phantom behaviour of dynamical dark energy,2512.19888

    work page arXiv

  55. [55]

    Z. Yao, G. Ye and A. Silvestri,A general model for dark energy crossing the phantom divide, JCAP10(2025) 078 [2508.01378]

    work page arXiv 2025

  56. [56]

    Goh and A.N

    L.W.K. Goh and A.N. Taylor,Phantom Crossing with Quintom Models,Mon. Not. Roy. Astron. Soc.3142(2025) 3157 [2509.12335]

    work page arXiv 2025

  57. [57]

    Tsujikawa,Crossing the phantom divide in scalar-tensor and vector-tensor theories,Phys

    S. Tsujikawa,Crossing the phantom divide in scalar-tensor and vector-tensor theories,Phys. Rev. D113(2026) L041301 [2508.17231]

    work page arXiv 2026

  58. [58]

    Wolf, P.G

    W.J. Wolf, P.G. Ferreira and C. Garc´ ıa-Garc´ ıa,Cosmological constraints on Galileon dark energy with broken shift symmetry,Phys. Rev. D113(2026) 023551 [2509.17586]

    work page arXiv 2026

  59. [59]

    Efstratiou, E.A

    D. Efstratiou, E.A. Paraskevas and L. Perivolaropoulos,Addressing the DESI DR2 Phantom-Crossing Anomaly and EnhancedH 0 Tension with Reconstructed Scalar-Tensor Gravity,2511.04610

    work page arXiv

  60. [60]

    Camarena, K

    D. Camarena, K. Greene, J. Houghteling and F.-Y. Cyr-Racine,Designing concordant distances in the age of precision cosmology: The impact of density fluctuations,Phys. Rev. D 112(2025) 083526 [2507.17969]. – 30 –

    work page arXiv 2025

  61. [61]

    Artola, I

    M. Artola, I. Ayuso, R. Lazkoz and V. Salzano,Is Chevallier-Polarski-Linder dark energy a mirage?,Phys. Rev. D113(2026) 023513 [2510.04191]

    work page arXiv 2026

  62. [62]

    Li, G.-H

    T.-N. Li, G.-H. Du, S.-H. Zhou, Y.-H. Li, J.-F. Zhang and X. Zhang,Robust evidence for dynamical dark energy in light of DESI DR2 and joint ACT, SPT, and Planck data,Phys. Dark Univ.52(2026) 102254 [2511.22512]

    work page arXiv 2026

  63. [63]

    Ghedini, R

    P. Ghedini, R. Hajjar and O. Mena,Dark energy and neutrinos along the cosmic expansion history,Phys. Dark Univ.52(2026) 102237 [2512.16781]

    work page arXiv 2026

  64. [64]

    de Cruz P´ erez, A

    J. de Cruz P´ erez, A. G´ omez-Valent and J. Sol` a Peracaula,Dynamical Dark Energy models in light of the latest observations,2512.20616

    work page arXiv

  65. [65]

    Cheng, S

    H. Cheng, S. Pan and E. Di Valentino,Beyond Two Parameters: Revisiting Dark Energy with the Latest Cosmic Probes,Astrophys. J.999(2026) 190 [2512.09866]

    work page arXiv 2026

  66. [66]

    T.-N. Li, W. Giar` e, G.-H. Du, Y.-H. Li, E. Di Valentino, J.-F. Zhang et al.,Strong Evidence for Dark Sector Interactions,2601.07361

    work page arXiv

  67. [67]

    T. Xu, S. Kumar, Y. Chen, A.J.S. Capistrano and ¨O. Akarsu,Probing Dynamical Dark Energy with Late-Time Data: Evidence, Tensions, and the Limits of thew 0waCDM Framework,2602.11936

    work page arXiv

  68. [68]

    Ibarra-Uriondo and M

    B. Ibarra-Uriondo and M. Bouhmadi-L´ opez,Sign-Switching Dark Energy: Smooth Transitions with Recent DESI DR2 Observations,2602.12347

    work page arXiv

  69. [69]

    Akarsu, M

    ¨O. Akarsu, M. Caruana, K.F. Dialektopoulos, L.A. Escamilla, E.O. Kahya and J. Levi Said, Hints of sign-changing scalar field energy density and a transient acceleration phase atz∼2 from model-agnostic reconstructions,2602.08928

    work page arXiv

  70. [70]

    C.-G. Park, J. de Cruz Perez and B. Ratra,Is thew 0waCDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?,2604.03756. [77]DESIcollaboration,DESI 2024: reconstructing dark energy using crossing statistics with DESI DR1 BAO data,JCAP10(2024) 048 [2405.04216]. [78]DESI...

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  71. [71]

    Gonz´ alez-Fuentes and A

    A. Gonz´ alez-Fuentes and A. G´ omez-Valent,Reconstruction of dark energy and late-time cosmic expansion using the Weighted Function Regression method,JCAP12(2025) 049 [2506.11758]

    work page arXiv 2025

  72. [72]

    Jiang, D

    J.-Q. Jiang, D. Pedrotti, S.S. da Costa and S. Vagnozzi,Nonparametric late-time expansion history reconstruction and implications for the Hubble tension in light of recent DESI and type Ia supernovae data,Phys. Rev. D110(2024) 123519 [2408.02365]

    work page arXiv 2024

  73. [73]

    Berti, E

    M. Berti, E. Bellini, C. Bonvin, M. Kunz, M. Viel and M. Zumalacarregui,Reconstructing the dark energy density in light of DESI BAO observations,Phys. Rev. D112(2025) 023518 [2503.13198]

    work page arXiv 2025

  74. [74]

    Accelerating Universes with Scaling Dark Matter

    M. Chevallier and D. Polarski,Accelerating universes with scaling dark matter,Int. J. Mod. Phys. D10(2001) 213 [gr-qc/0009008]

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  75. [75]

    Exploring the Expansion History of the Universe

    E.V. Linder,Exploring the expansion history of the universe,Phys. Rev. Lett.90(2003) 091301 [astro-ph/0208512]

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  76. [76]

    C.-G. Park, J. de Cruz P´ erez and B. Ratra,Using non-DESI data to confirm and strengthen the DESI 2024 spatially flat w0waCDM cosmological parametrization result,Phys. Rev. D110 (2024) 123533 [2405.00502]

    work page arXiv 2024

  77. [77]

    Z. Lu, T. Simon and P. Zhang,Preference for evolving dark energy in light of the galaxy bispectrum,2503.04602. – 31 –

    work page arXiv

  78. [78]

    Herold and T

    L. Herold and T. Karwal,Bayesian and frequentist perspectives agree on dynamical dark energy,2506.12004

    work page arXiv

  79. [79]

    Bayes in the sky: Bayesian inference and model selection in cosmology

    R. Trotta,Bayes in the sky: Bayesian inference and model selection in cosmology,Contemp. Phys.49(2008) 71 [0803.4089]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  80. [80]

    D.D.Y. Ong, D. Yallup and W. Handley,A Bayesian Perspective on Evidence for Evolving Dark Energy,2511.10631

    work page internal anchor Pith review Pith/arXiv arXiv

Showing first 80 references.