pith. sign in

arxiv: 2607.01199 · v1 · pith:QGNBNAWAnew · submitted 2026-07-01 · 🌌 astro-ph.CO

Interpretation of the binned SNe Ia Master Sample data via a scalar quintessence component: phantom transition?

Giovanni Montani , Iolanda Navone , Maria Giovanna Dainotti , Shigehiro Nagataki This is my paper

Pith reviewed 2026-07-02 06:15 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords dark energyquintessencesupernovae Iaequation of statephantom transitionbulk viscosityrunning Hubble constantlate universe
0
0 comments X

The pith

Best-fit viscous quintessence model to binned SNe Ia data keeps effective equation of state below -1 at all redshifts with no transition.

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

The paper models late-universe dark energy as a self-interacting scalar field that includes a viscous term, allowing its effective equation of state to reach values below -1. It compares the resulting effective running Hubble constant against binned Master Sample supernova data that were themselves constructed under a LambdaCDM assumption in each bin. For the parameter values that give the best fit, the scalar field remains in a slow-roll regime and its effective equation of state stays below -1 across the entire redshift range examined. Consequently the data show no sign that dark energy must change its character from quintessence-like to phantom-like behavior.

Core claim

Within the viscous scalar-field framework the effective running Hubble constant is fitted to the binned SNe Ia Master Sample. The best-fit solution satisfies the slow-rolling condition because kinetic energy remains small compared with the potential throughout the redshift interval. For those same parameter values the effective equation of state parameter remains below -1 at every redshift, so no quintessence-to-phantom transition occurs. Supernovae data alone therefore supply no indication of a change in the nature of dark energy.

What carries the argument

Viscous contribution added to the scalar-field energy-momentum tensor, allowing an effective equation-of-state parameter that can lie below -1 while the underlying field remains quintessence-like.

If this is right

  • The slow-rolling condition holds because kinetic energy stays small relative to potential energy over the full redshift interval.
  • Any transition that might appear is pushed to redshifts significantly lower than the value reported by the DESI Collaboration.
  • When the model is restricted to the parameter region that best matches the data, the effective equation of state never crosses -1.

Where Pith is reading between the lines

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

  • The result applies only to supernova data; joint analyses with BAO or CMB measurements could still permit a transition at higher redshift.
  • If future supernova surveys reach higher redshifts with smaller errors, they could directly test whether the effective w remains below -1.
  • The viscosity term itself is an effective description; a microscopic derivation of the bulk-viscosity coefficient would be needed before the model can be extrapolated to early times.

Load-bearing premise

The binned Master Sample data are constructed by performing an MCMC fit that assumes a LambdaCDM model inside each redshift bin.

What would settle it

An independent re-binning or re-fitting of the same SNe Ia catalog performed without assuming LambdaCDM inside each bin that yields a best-fit transition at redshift greater than zero would falsify the no-transition result.

Figures

Figures reproduced from arXiv: 2607.01199 by Giovanni Montani, Iolanda Navone, Maria Giovanna Dainotti, Shigehiro Nagataki.

Figure 1
Figure 1. Figure 1: Comparison between (on the left) the values of [PITH_FULL_IMAGE:figures/full_fig_p012_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Fit of the effective running Hubble constant of the cosmological model using the Master [PITH_FULL_IMAGE:figures/full_fig_p013_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Trend of the effective equation of state parameter in Eq. (19) (using also Eq. (11)) after [PITH_FULL_IMAGE:figures/full_fig_p013_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Trend of the potential numerically integrated using Eq. (13) and Eq. (10), for different [PITH_FULL_IMAGE:figures/full_fig_p014_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Posteriors for the parameters in Tab. 3, corresponding to the fit of the cosmological [PITH_FULL_IMAGE:figures/full_fig_p015_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Ratio of the bulk viscosity contribution to the total equilibrium pressure (see Eq. (18)) [PITH_FULL_IMAGE:figures/full_fig_p016_6.png] view at source ↗
read the original abstract

We study a modified cosmological scenario for the late Universe, involving an evolutionary dark energy model associated with the dynamics of a self-interacting scalar field in a potential-dominated regime. Through the analogy with a fluid energy-momentum tensor, we introduce a viscous contribution to the scalar dynamics, accounting for effective non-equilibrium behaviour of the self-interacting scalar cluster. The resulting picture is that of an intrinsic quintessence contribution which, due to the bulk viscosity, admits an effective equation of state parameter that can also take values below -1. Within this framework, we set up the diagnostic tool of the so-called "effective running Hubble constant", which allows us to trace possible deviations from a standard LambdaCDM model. We then compare this theoretical function with binned data from the Master Sample of Supernovae Ia, constructed assuming a LambdaCDM model in the MCMC procedure performed in each bin. We show that the self-interacting scalar field corresponding to the best fit satisfies a slow-rolling condition, since the kinetic energy remains small compared to the potential contribution throughout the redshift interval. The key finding is that, when limiting the model to specific regions of the parameter space and fitting it to the data, the transition only occurs at redshifts significantly lower than the redshift value identified by the DESI Collaboration. Furthermore, for the parameter values ensuring the best fit, no quintessence-to-phantom transition occurs (i.e., the effective equation of state parameter remains below -1 across the whole redshift domain). In other words, Supernovae data alone provide no indication of a change in the nature of the dark energy.

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 / 1 minor

Summary. The manuscript introduces a viscous quintessence model for late-universe dark energy, where bulk viscosity allows an effective equation-of-state parameter w_eff that can fall below -1. An effective running Hubble constant is used as a diagnostic to fit the model to binned SNe Ia Master Sample data (constructed via per-bin LambdaCDM MCMC). The central result is that the best-fit parameters satisfy a slow-roll condition and yield w_eff < -1 at all redshifts, implying no quintessence-to-phantom transition and that SNe Ia data alone show no evidence for a change in the nature of dark energy.

Significance. If the no-transition result is robust, the work supplies a concrete counter-example to claims of evolving dark energy from other probes (e.g., DESI) by demonstrating consistency of SNe Ia with a non-transitioning viscous quintessence scenario. The explicit acknowledgment of the LambdaCDM-based binning procedure is a point of transparency, though it does not resolve the dependence of the conclusion on that preprocessing.

major comments (2)
  1. [Abstract] Abstract: The claim that 'Supernovae data alone provide no indication of a change in the nature of the dark energy' rests on fits to binned Master Sample data whose construction explicitly assumes a LambdaCDM cosmology in each bin's MCMC. Because this preprocessing embeds the constant-w = -1 hypothesis, any signature of a w_eff transition could be attenuated before the viscous-quintessence fit is performed; the no-transition conclusion is therefore not an independent test of the data but a consequence of the binning step. This is load-bearing for the central claim.
  2. [Abstract] Abstract (key-finding paragraph): The statement that 'for the parameter values ensuring the best fit, no quintessence-to-phantom transition occurs' follows after restricting the model to 'specific regions of the parameter space.' No explicit justification, prior ranges, or post-fit robustness checks against these restrictions are referenced, leaving open whether the w_eff < -1 result is selected by the data or imposed by the chosen parameter domain.
minor comments (1)
  1. [Abstract] The abstract supplies no derivation outline or explicit expression for the effective equation-of-state parameter that incorporates the viscous term, nor any mention of error bars or covariance on the reported best-fit values; these omissions hinder immediate assessment of the quantitative support for the no-transition statement.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on our manuscript. Below we respond point-by-point to the major comments, indicating where revisions will strengthen the presentation while preserving the core analysis.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The claim that 'Supernovae data alone provide no indication of a change in the nature of the dark energy' rests on fits to binned Master Sample data whose construction explicitly assumes a LambdaCDM cosmology in each bin's MCMC. Because this preprocessing embeds the constant-w = -1 hypothesis, any signature of a w_eff transition could be attenuated before the viscous-quintessence fit is performed; the no-transition conclusion is therefore not an independent test of the data but a consequence of the binning step. This is load-bearing for the central claim.

    Authors: We acknowledge that the binned Master Sample is constructed via per-bin LambdaCDM MCMC fits, as already stated in the manuscript. This is the published form of the data set and the standard preprocessing used in the literature for such binned analyses. While the referee is correct that this step can limit sensitivity to transitions, our result remains that the viscous quintessence model provides a good fit to these data without requiring a transition at the redshifts suggested by DESI. We will revise the abstract to qualify the central claim explicitly as applying to the binned SNe Ia Master Sample constructed under LambdaCDM assumptions, thereby making the dependence transparent rather than overstating independence. revision: partial

  2. Referee: [Abstract] Abstract (key-finding paragraph): The statement that 'for the parameter values ensuring the best fit, no quintessence-to-phantom transition occurs' follows after restricting the model to 'specific regions of the parameter space.' No explicit justification, prior ranges, or post-fit robustness checks against these restrictions are referenced, leaving open whether the w_eff < -1 result is selected by the data or imposed by the chosen parameter domain.

    Authors: The phrase 'specific regions of the parameter space' refers to the slow-roll regime in which the kinetic energy remains negligible compared with the potential energy, a condition we verify explicitly for the best-fit parameters in the main text. The MCMC fit was performed over the full physically allowed ranges consistent with this regime; the best-fit point lies inside it. In revision we will (i) state the explicit prior ranges employed, (ii) add a short robustness paragraph confirming that the w_eff < -1 result is stable under modest excursions around the best-fit values, and (iii) clarify that the slow-roll restriction is theoretically motivated rather than arbitrarily imposed. revision: yes

Circularity Check

0 steps flagged

No circularity: standard model fit to externally provided binned data

full rationale

The paper constructs a viscous quintessence model with an effective running Hubble constant diagnostic, then performs a fit to the binned Master Sample data (explicitly noting the per-bin LambdaCDM MCMC construction). The reported outcome—that best-fit parameters yield w_eff < -1 with no transition—is the direct numerical result of that fit rather than a quantity defined to equal the input by construction. No self-definitional loop, fitted-input-renamed-as-prediction, load-bearing self-citation, uniqueness theorem, or ansatz smuggling appears in the derivation chain. The analysis is therefore self-contained against the supplied data.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 1 invented entities

The central claim rests on an ad-hoc viscous term introduced to permit w < -1, the slow-roll assumption verified only after fitting, and pre-binned data whose construction assumes LambdaCDM.

free parameters (1)
  • viscosity coefficient and scalar potential parameters
    Fitted to the binned supernova data to obtain the best-fit model.
axioms (2)
  • domain assumption Scalar field remains in potential-dominated slow-roll regime throughout the redshift range.
    Invoked to justify the model dynamics and stated as satisfied by the best fit.
  • standard math Standard FLRW background cosmology.
    Implicit throughout the cosmological setup.
invented entities (1)
  • viscous contribution to scalar dynamics no independent evidence
    purpose: To model effective non-equilibrium behavior allowing effective EoS below -1.
    Introduced via fluid analogy without independent physical justification beyond enabling the desired phenomenology.

pith-pipeline@v0.9.1-grok · 5842 in / 1513 out tokens · 35147 ms · 2026-07-02T06:15:00.114159+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

81 extracted references · 61 canonical work pages · 12 internal anchors

  1. [1]

    G.Dainotti, etal., A NewMaster Supernovae Iasample andthe investigation of the Hubble tension, JHEAp 48 (2025) 100405.arXiv:2501.11772,doi: 10.1016/j.jheap.2025.100405

    M. G.Dainotti, etal., A NewMaster Supernovae Iasample andthe investigation of the Hubble tension, JHEAp 48 (2025) 100405.arXiv:2501.11772,doi: 10.1016/j.jheap.2025.100405

    work page doi:10.1016/j.jheap.2025.100405 2025

  2. [2]

    DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints

    M. Abdul Karim, et al., DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints (3 2025).arXiv:2503.14738

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  3. [3]

    A. G. Adame, et al., DESI 2024 VI: cosmological constraints from the measure- ments of baryon acoustic oscillations, JCAP 02 (2025) 021.arXiv:2404.03002, doi:10.1088/1475-7516/2025/02/021. 17

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2025/02/021 2024

  4. [4]

    A. G. Riess, W. Yuan, L. M. Macri, et al., A comprehensive measurement of the local value of the Hubble constant with 1 km s−1 Mpc−1uncertainty from the Hubble Space Telescope and the SH0ES team, The Astrophysical journal letters 934 (1) (2022) L7.doi:10.3847/2041-8213/ac5c5b

    work page doi:10.3847/2041-8213/ac5c5b 2022

  5. [5]

    Aghanim, Y

    N. Aghanim, Y. Akrami, M. Ashdown, et al., Planck 2018 results-VI. Cosmo- logical parameters, Astronomy & Astrophysics 641 (2020) A6

    2018

  6. [6]

    Dainotti, B

    M. Dainotti, B. De Simone, G. Montani, et al., The hubble constant ten- sion: current status and future perspectives through new cosmological probes, arXiv e-prints (2023) arXiv:2301.10572arXiv:2301.10572,doi:10.48550/ arXiv.2301.10572. URLhttps://ui.adsabs.harvard.edu/abs/2023arXiv230110572D

    work page arXiv 2023

  7. [7]

    M. G. Dainotti, G. Bargiacchi, A. Ł. Lenart, et al., Quasar standardization: Overcoming selection biases and redshift evolution, The Astrophysical Jour- nal931 (2) (2022) 106.arXiv:2203.12914,doi:10.3847/1538-4357/ac6593. URLhttps://ui.adsabs.harvard.edu/abs/2022ApJ...931..106D

    work page doi:10.3847/1538-4357/ac6593 2022

  8. [8]

    M. G. Dainotti, A. Ł. Lenart, M. G. Yengejeh, et al., A new binning method to choose a standard set of Quasars, Physics of the Dark Universe 44 (2024) 101428.arXiv:2401.12847,doi:10.1016/j.dark.2024.101428

    work page doi:10.1016/j.dark.2024.101428 2024

  9. [9]

    URLhttps://ui.adsabs.harvard.edu/abs/2025PhRvD.112f3520M

    S.Mukherjee, S.S.Pandey, A.S.Majumdar, Constrainingthehubbleparameter withthe21-cmbrightnesstemperaturesignalinauniversewithinhomogeneities, Physical Review D112 (6) (2025) 063520.arXiv:2505.22219,doi:10.1103/ w1wp-tqz2. URLhttps://ui.adsabs.harvard.edu/abs/2025PhRvD.112f3520M

    work page arXiv 2025

  10. [10]

    M. G. Dainotti, G. Bargiacchi, A. Ł. Lenart, et al., The Scavenger Hunt for Quasar Samples to Be Used as Cosmological Tools, Galaxies 12 (1) (2024) 4. arXiv:2401.11998,doi:10.3390/galaxies12010004

    work page doi:10.3390/galaxies12010004 2024

  11. [11]

    M. G. Dainotti, A. Ł. Lenart, A. Chraya, et al., The gamma-ray bursts fun- damental plane correlation as a cosmological tool, Monthly Notices of the Royal Astronomical Society518 (2) (2023) 2201–2240.arXiv:2209.08675, doi:10.1093/mnras/stac2752. URLhttps://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2201D

    work page doi:10.1093/mnras/stac2752 2023

  12. [12]

    M. G. Dainotti, G. Sarracino, S. Capozziello, Gamma-ray bursts, supernovae ia, andbaryonacousticoscillations: Abinnedcosmologicalanalysis, Publicationsof 18 the Astronomical Society of Japan74 (5) (2022) 1095–1113.arXiv:2206.07479, doi:10.1093/pasj/psac057. URLhttps://ui.adsabs.harvard.edu/abs/2022PASJ...74.1095D

    work page doi:10.1093/pasj/psac057 2022

  13. [13]

    Bargiacchi, M

    G. Bargiacchi, M. G. Dainotti, S. Capozziello, High-redshift cosmology by gamma-ray bursts: An overview, New Astronomy Reviews100 (2025) 101712. arXiv:2408.10707,doi:10.1016/j.newar.2024.101712. URLhttps://ui.adsabs.harvard.edu/abs/2025NewAR.10001712B

    work page doi:10.1016/j.newar.2024.101712 2025

  14. [14]

    S. A. Adil, M. G. Dainotti, A. A. Sen, Revisiting the concordanceΛcdm model using gamma-ray bursts together with supernovae ia and planck data, Journal of Cosmology and Astroparticle Physics2024 (8) (2024) 015.arXiv:2405.01452, doi:10.1088/1475-7516/2024/08/015. URLhttps://ui.adsabs.harvard.edu/abs/2024JCAP...08..015A

    work page doi:10.1088/1475-7516/2024/08/015 2024

  15. [15]

    B. P. Abbott, R. Abbott, T. D. Abbott, et al., Gw170817: Observation of gravitational waves from a binary neutron star inspiral, Physical Review Let- ters119 (16) (2017) 161101.arXiv:1710.05832,doi:10.1103/PhysRevLett. 119.161101. URLhttps://ui.adsabs.harvard.edu/abs/2017PhRvL.119p1101A

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett 2017

  16. [16]

    Kalita, A

    S. Kalita, A. Uniyal, T. Bulik, et al., Revealing limitation in the standard cosmological model: A redshift-dependent hubble constant from fast radio bursts, The Astrophysical Journal996 (1) (2026) 50.arXiv:2506.14947,doi: 10.3847/1538-4357/ae261b. URLhttps://ui.adsabs.harvard.edu/abs/2026ApJ...996...50K

    work page doi:10.3847/1538-4357/ae261b 2026

  17. [17]

    Laurikainen, H

    A. Faucher, D. Benisty, D. F. Mota, Hubble-constant and -mass determination of centaurus a and m83 from tip-of-red-giant-branch distances, Astronomy & Astrophysics705 (2026) A112.arXiv:2510.09190,doi:10.1051/0004-6361/ 202556283. URLhttps://ui.adsabs.harvard.edu/abs/2026A&A...705A.112F

    work page doi:10.1051/0004-6361/ 2026

  18. [18]

    G. N. Gadbail, K. Bamba, A model-independent measurement of the hub- ble constant from gravitational-wave standard sirens and electromagnetic ob- servations, arXiv e-prints (2026) arXiv:2602.04497arXiv:2602.04497,doi: 10.48550/arXiv.2602.04497. URLhttps://ui.adsabs.harvard.edu/abs/2026arXiv260204497G

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2602.04497 2026

  19. [19]

    Y. Zhan, D. Wang, S.-X. Yi, et al., Hubble constant measurement from quasiperiodic eruptions as electromagnetic counterparts to extreme mass ra- 19 tio inspirals, The Astrophysical Journal997 (2) (2026) 134.arXiv:2506.14150, doi:10.3847/1538-4357/ae2600. URLhttps://ui.adsabs.harvard.edu/abs/2026ApJ...997..134Z

    work page doi:10.3847/1538-4357/ae2600 2026

  20. [20]

    Chevallier, D

    M. Chevallier, D. Polarski, Accelerating universes with scaling dark matter, International Journal of Modern Physics D 10 (02) (2001) 213–223

    2001

  21. [21]

    E. V. Linder, Exploring the expansion history of the universe, Physical review letters 90 (9) (2003) 091301

    2003

  22. [22]

    Extended Dark Energy analysis using DESI DR2 BAO measurements

    K. Lodha, et al., Extended Dark Energy analysis using DESI DR2 BAO mea- surements (3 2025).arXiv:2503.14743

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  23. [23]

    D. D. Y. Ong, D. Yallup, W. Handley, The bayesian view of desi dr2 with unim- peded: Evidence and tension in a combined analysis with cmb and supernovae across cosmological models (2026).arXiv:2603.05472. URLhttps://arxiv.org/abs/2603.05472

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  24. [24]

    Efstathiou, Mon

    G. Efstathiou, Evolving dark energy or supernovae systematics? (2025).arXiv: 2408.07175. URLhttps://arxiv.org/abs/2408.07175

    work page arXiv 2025

  25. [25]

    Capozziello, H

    S. Capozziello, H. Chaudhary, G. Mustafa, et al., Evidence of dynamical dark energy found via the desi dr2 lymanÎś forest, Astronomy &amp; Astrophysics (Apr. 2026).doi:10.1051/0004-6361/202557820. URLhttp://dx.doi.org/10.1051/0004-6361/202557820

    work page doi:10.1051/0004-6361/202557820 2026

  26. [26]

    Chaudhary, S

    H. Chaudhary, S. Capozziello, S. Praharaj, et al., Is the ÎŻcdm model in crisis?, Journal of High Energy Astrophysics 50 (2026) 100507.doi:10.1016/j.jheap. 2025.100507. URLhttp://dx.doi.org/10.1016/j.jheap.2025.100507

    work page doi:10.1016/j.jheap 2026

  27. [27]

    Chaudhary, V

    H. Chaudhary, V. K. Sharma, S. Capozziello, et al., Probing departures from ÎŻcdm by late-time datasets, The Astrophysical Journal Supplement Series 283 (2) (2026) 73.doi:10.3847/1538-4365/ae4b3f. URLhttp://dx.doi.org/10.3847/1538-4365/ae4b3f

    work page doi:10.3847/1538-4365/ae4b3f 2026

  28. [28]

    Evidence for evolving dark energy from DESI DR2 BAO and Pantheon$^+$, DES-Dovekie, and Union3

    H. Chaudhary, S. Capozziello, V. K. Sharma, et al., Evidence for evolving dark energy from desi dr2 bao and pantheon+, des-dovekie, and union3 (2026). arXiv:2508.10514. URLhttps://arxiv.org/abs/2508.10514 20

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  29. [29]

    Chaudhary, S

    H. Chaudhary, S. Capozziello, V. K. Sharma, et al., Does desi dr2 challenge ÎŻcdm paradigm?, The Astrophysical Journal 992 (2) (2025) 194.doi:10. 3847/1538-4357/ae0458. URLhttp://dx.doi.org/10.3847/1538-4357/ae0458

    work page doi:10.3847/1538-4357/ae0458 2025

  30. [30]

    Modeling nonlinear scales for dynamical dark energy cosmologies with COLA

    J. RebouÃğas, V. Lloyd, J. Gordon, et al., Modeling nonlinear scales for dy- namical dark energy cosmologies with cola (2026).arXiv:2510.14888. URLhttps://arxiv.org/abs/2510.14888

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  31. [31]

    Ishak and L

    M.Ishak, L.Medina-Varela, Persistentandseriouschallengetotheλcdmthrone: Evidence for dynamical dark energy rising from combinations of different types of datasets (2025).arXiv:2507.22856. URLhttps://arxiv.org/abs/2507.22856

    work page arXiv 2025

  32. [32]

    C.-G. Park, B. Ratra, Updated observational constraints onϕcdm dynamical dark energy cosmological models (2025).arXiv:2509.25812. URLhttps://arxiv.org/abs/2509.25812

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  33. [33]

    A. C. Alfano, O. Luongo, Cosmic distance duality after desi 2024 data release and dark energy evolution (2025).arXiv:2501.15233. URLhttps://arxiv.org/abs/2501.15233

    work page arXiv 2024

  34. [35]

    CortÃłs, A

    M. CortÃłs, A. R. Liddle, Interpreting desiâĂŹs evidence for evolving dark energy, Journal of Cosmology and Astroparticle Physics 2024 (12) (2024) 007. doi:10.1088/1475-7516/2024/12/007. URLhttp://dx.doi.org/10.1088/1475-7516/2024/12/007

    work page doi:10.1088/1475-7516/2024/12/007 2024

  35. [36]

    Calderonet al.(DESI), DESI 2024: reconstructing dark energy using crossing statistics with DESI DR1 BAO data, JCAP10, 048, arXiv:2405.04216 [astro- ph.CO]

    R. Calderon, K. Lodha, A. Shafieloo, et al., DESI 2024: reconstructing dark energyusingcrossingstatisticswithDESIDR1BAOdata, JournalofCosmology and Astroparticle Physics2024 (10) (2024) 048.arXiv:2405.04216,doi:10. 1088/1475-7516/2024/10/048

    work page arXiv 2024

  36. [37]

    Tsujikawa, Quintessence: a review, Classical and Quantum Gravity 30 (21) (2013) 214003.doi:10.1088/0264-9381/30/21/214003

    S. Tsujikawa, Quintessence: a review, Classical and Quantum Gravity 30 (21) (2013) 214003.doi:10.1088/0264-9381/30/21/214003. URLhttp://dx.doi.org/10.1088/0264-9381/30/21/214003 21

    work page doi:10.1088/0264-9381/30/21/214003 2013

  37. [38]

    R. Caldwell, A phantom menace? cosmological consequences of a dark energy component with super-negative equation of state, Physics Letters B 545 (1âĂŞ2) (2002) 23âĂŞ29.doi:10.1016/s0370-2693(02)02589-3. URLhttp://dx.doi.org/10.1016/S0370-2693(02)02589-3

    work page doi:10.1016/s0370-2693(02)02589-3 2002

  38. [39]

    S. M. Carroll, M. Hoffman, M. Trodden, Can the dark energy equation-of-state parameter w be less than−1?, Phys. Rev. D 68 (2003) 023509.doi:10.1103/ PhysRevD.68.023509. URLhttps://link.aps.org/doi/10.1103/PhysRevD.68.023509

    work page doi:10.1103/physrevd.68.023509 2003

  39. [40]

    Schiavone, G

    T. Schiavone, G. Montani, Evolution of an effective Hubble constant in f (R) modified gravity, Nuovo Cim. C 48 (3) (2025) 105.arXiv:2408.01410,doi: 10.1393/ncc/i2025-25105-3

    work page doi:10.1393/ncc/i2025-25105-3 2025

  40. [41]

    M. G. Dainotti, B. De Simone, T. Schiavone, et al., On the Hubble constant tension in the SNe Ia Pantheon sample, The Astrophysical Journal 912 (2) (2021) 150

    2021

  41. [42]

    Fazzari, M

    E. Fazzari, M. G. Dainotti, G. Montani, et al., The effective running Hubble constant in SNe Ia as a marker for the dark energy nature, JHEAp 49 (2026) 100459.arXiv:2506.04162,doi:10.1016/j.jheap.2025.100459

    work page doi:10.1016/j.jheap.2025.100459 2026

  42. [43]

    M. G. Dainotti, B. De Simone, T. Schiavone, et al., On the evolution of the Hubble constant with the SNe Ia pantheon sample and baryon acoustic oscil- lations: a feasibility study for GRB-cosmology in 2030, Galaxies 10 (1) (2022) 24

    2030

  43. [44]

    Physical Review D , keywords =

    C. Krishnan, E. Ó. Colgáin, M. M. Sheikh-Jabbari, et al., Running Hubble Tension and a H0 Diagnostic, Phys. Rev. D 103 (10) (2021) 103509.arXiv: 2011.02858,doi:10.1103/PhysRevD.103.103509

    work page doi:10.1103/physrevd.103.103509 2021

  44. [45]

    E. Ó. Colgáin, M. G. Dainotti, S. Capozziello, et al., Does DESI 2024 Confirm ΛCDM?, arXiv preprint arXiv:2404.08633 (2024)

    work page arXiv 2024

  45. [46]

    Di Valentino, O

    E. Di Valentino, O. Mena, S. Pan, et al., In the realm of the Hubble tensionâĂŤa review of solutions, Classical and Quantum Gravity 38 (15) (2021) 153001.doi: 10.1088/1361-6382/ac086d

    work page doi:10.1088/1361-6382/ac086d 2021

  46. [48]

    Montani, E

    G. Montani, E. Fazzari, N. Carlevaro, et al., Two Dynamical Scenarios for Binned Master Sample Interpretation, Entropy 27 (2025) 895.arXiv:2507. 14048,doi:10.3390/e27090895

    work page doi:10.3390/e27090895 2025

  47. [49]

    Montani, N

    G. Montani, N. Carlevaro, M. G. Dainotti, Running Hubble constant: Evolu- tionary Dark Energy, Phys. Dark Univ. 48 (2025) 101847.arXiv:2411.07060, doi:10.1016/j.dark.2025.101847

    work page doi:10.1016/j.dark.2025.101847 2025

  48. [51]

    Montani, N

    G. Montani, N. Carlevaro, L. A. Escamilla, et al., Kinetic model for dark en- ergy—dark matter interaction: Scenario for the hubble tension, Phys. Dark Univ. 48 (2025) 101848.arXiv:2404.15977,doi:10.1016/j.dark.2025. 101848

    work page doi:10.1016/j.dark.2025 2025

  49. [52]

    Efstathiou, ToH0 or not toH0?, Monthly Notices of the Royal Astronomical Society 505 (3) (2021) 3866–3872

    G. Efstathiou, ToH0 or not toH0?, Monthly Notices of the Royal Astronomical Society 505 (3) (2021) 3866–3872

    2021

  50. [53]

    Elizalde, M

    E. Elizalde, M. Khurshudyan, S. D. Odintsov, Can we learn from matter creation to solve theH 0 tension problem?, The European Physical Journal C 84 (8) (2024) 782

    2024

  51. [54]

    M. G. Dainotti, V. Petrosian, J. Singal, et al., Determination of the intrinsic luminosity time correlation in the x-ray afterglows of gamma-ray bursts, The AstrophysicalJournal774(2)(2013)157.doi:10.1088/0004-637X/774/2/157. URLhttps://doi.org/10.1088/0004-637X/774/2/157

    work page doi:10.1088/0004-637x/774/2/157 2013

  52. [55]

    B. D. Simone, M. H. P. M. van Putten, M. G. Dainotti, et al., A doublet of cosmological models to challenge the h0 tension in the pantheon supernovae ia catalog (2024).arXiv:2411.05744. URLhttps://arxiv.org/abs/2411.05744

    work page arXiv 2024

  53. [56]

    Schiavone, G

    T. Schiavone, G. Montani, F. Bombacigno, f(R) gravity in the Jordan frame as a paradigm for the Hubble tension, Monthly Notices of the Royal Astronomical Society: Letters 522 (1) (2023) L72âĂŞL77.doi:10.1093/mnrasl/slad041

    work page doi:10.1093/mnrasl/slad041 2023

  54. [57]

    M. G. Dainotti, A. Banerjee, A. LeClair, et al., Parameterizations of the hubble constant: Logarithmic vs power-law expansion from the binned master sample of sne ia (2026).arXiv:2603.00497. 23

    work page arXiv 2026

  55. [58]

    LeClair, Quantum vacuum energy as the origin of gravity (2025).arXiv: 2509.02636

    A. LeClair, Quantum vacuum energy as the origin of gravity (2025).arXiv: 2509.02636. URLhttps://arxiv.org/abs/2509.02636

    work page arXiv 2025

  56. [59]

    Weinberg, Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity, John Wiley and Sons, New York, 1972

    S. Weinberg, Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity, John Wiley and Sons, New York, 1972

    1972

  57. [60]

    Montani, M

    G. Montani, M. V. Battisti, R. Benini, et al., Primordial cosmology, World Scientific, Singapore, 2009

    2009

  58. [61]

    V. A. Belinskii, I. M. Khalatnikov, Influence of viscosity on the character of cosmological evolution, Soviet JETT 42 (1975) 205

    1975

  59. [62]

    V. A. Belinskii, I. M. Khalatnikov, Viscosity effects in isotropic cosmologies, Soviet JETT 45 (1977) 19

    1977

  60. [63]

    V. A. Belinskii, E. S. Nikomarov, I. M. Khalatnikov, Investigation of the cos- mological evolution of viscoelastic matter with causal thermodynamics, Soviet JETT 50 (2) (1979) 21

    1979

  61. [65]

    Montani, M

    G. Montani, M. Venanzi, Bianchi i cosmology in the presence of a causally regularized viscous fluid, The European Physical Journal C 77 (7) (Jul. 2017). doi:10.1140/epjc/s10052-017-5042-z. URLhttp://dx.doi.org/10.1140/epjc/s10052-017-5042-z

    work page doi:10.1140/epjc/s10052-017-5042-z 2017

  62. [66]

    Carlevaro, G

    N. Carlevaro, G. Montani, Bulk viscosity effects on the early Universe stability, Mod. Phys. Lett. A 20 (2005) 1729–1739.doi:10.1142/S0217732305017998

    work page doi:10.1142/s0217732305017998 2005

  63. [67]

    Weinberg, Cosmology, 2008

    S. Weinberg, Cosmology, 2008

    2008

  64. [68]

    E. W. Kolb, M. S. Turner, The Early Universe, Vol. 69, 1990

    1990

  65. [69]

    J. A. Peacock, Cosmological Physics, Cambridge University Press, 1999

    1999

  66. [70]

    M. E. Peskin, D. V. Schroeder, An Introduction to Quantum Field Theory, Addison-Wesley, 1995. 24

    1995

  67. [71]

    Efstathiou, S

    G. Efstathiou, S. Gratton, The evidence for a spatially flat universe, Monthly Notices of the Royal Astronomical Society: Letters 496 (1) (2020) L91–L95

    2020

  68. [72]

    Navone, M

    I. Navone, M. G. Dainotti, E. Fazzari, et al., Creation of viscous dark energy by the hubble flow: Comparison with sne ia master sample binned data (2025). arXiv:2511.16130. URLhttps://arxiv.org/abs/2511.16130

    work page arXiv 2025

  69. [73]

    C.Krishnan, E.ÓColgáin, M.M.Sheikh-Jabbari, etal., Runninghubbletension and a h0 diagnostic, Phys. Rev. D 103 (2021) 103509.doi:10.1103/PhysRevD. 103.103509. URLhttps://link.aps.org/doi/10.1103/PhysRevD.103.103509

    work page doi:10.1103/physrevd 2021

  70. [74]

    Krishnan, R

    C. Krishnan, R. Mondol,h0 as a universal flrw diagnostic (2022).arXiv:2201. 13384. URLhttps://arxiv.org/abs/2201.13384

    work page arXiv 2022

  71. [75]

    D. C. T. M. C. Abbott, M. Acevedo, M. Aguena, et al., The dark energy survey: Cosmology results with 1500 new high-redshift type ia supernovae using the full 5-year dataset (2025).arXiv:2401.02929. URLhttps://arxiv.org/abs/2401.02929

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  72. [76]

    Scolnic, D

    D. Scolnic, D. Brout, A. Carr, et al., The Pantheon+ Analysis: The Full Data Set and Light-curve Release, The Astrophysical Journal 938 (2) (2022) 113. doi:10.3847/1538-4357/ac8b7a

    work page doi:10.3847/1538-4357/ac8b7a 2022

  73. [77]

    Brout, D

    D. Brout, D. Scolnic, B. Popovic, et al., The Pantheon+ Analysis: Cos- mological Constraints, The Astrophysical Journal 938 (2) (2022) 110.doi: 10.3847/1538-4357/ac8e04

    work page doi:10.3847/1538-4357/ac8e04 2022

  74. [78]

    D. M. Scolnic, D. Jones, A. Rest, et al., The complete light-curve sample of spectroscopically confirmed SNe Ia from Pan-STARRS1 and cosmological con- straints from the combined pantheon sample, The Astrophysical Journal 859 (2) (2018) 101

    2018

  75. [79]

    Betoule, R

    M. Betoule, R. Kessler, J. Guy, et al., Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples, Astronomy & Astrophysics 568 (2014) A22

    2014

  76. [80]

    Dainotti, G

    M. Dainotti, G. Bargiacchi, M. Bogdan, et al., On the statistical assumption on the distance moduli of supernovae ia and its impact on the determination 25 of cosmological parameters, Journal of High Energy Astrophysics 41 (2024) 30–41.doi:https://doi.org/10.1016/j.jheap.2024.01.001. URLhttps://www.sciencedirect.com/science/article/pii/ S2214404824000016

    work page doi:10.1016/j.jheap.2024.01.001 2024

  77. [81]

    M. G. Dainotti, G. Bargiacchi, M. Bogdan, et al., Reducing the uncertainty on the hubble constant up to 35% with an improved statistical analysis: Different best-fit likelihoods for type ia supernovae, baryon acoustic oscillations, quasars, and gamma-ray bursts, The Astrophysical Journal 951 (1) (2023) 63.doi: 10.3847/1538-4357/acd63f. URLhttp://dx.doi.or...

    work page doi:10.3847/1538-4357/acd63f 2023

  78. [82]

    Bargiacchi, M

    G. Bargiacchi, M. G. Dainotti, S. Nagataki, et al., Gamma-ray bursts, quasars, baryonic acoustic oscillations, and supernovae ia: new statistical insights and cosmological constraints, Monthly Notices of the Royal Astronomical Society 521 (3) (2023) 3909–3924.doi:10.1093/mnras/stad763. URLhttp://dx.doi.org/10.1093/mnras/stad763

    work page doi:10.1093/mnras/stad763 2023

  79. [83]

    Gelman, D

    A. Gelman, D. B. Rubin, Inference from iterative simulation using multiple sequences, Statistical science 7 (4) (1992) 457–472

    1992

  80. [84]

    GetDist: a Python package for analysing Monte Carlo samples

    A. Lewis, GetDist: a Python package for analysing Monte Carlo samples, JCAP 08 (2025) 025.arXiv:1910.13970,doi:10.1088/1475-7516/2025/08/025

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2025/08/025 2025

Showing first 80 references.