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arxiv: 2511.07517 · v3 · submitted 2025-11-10 · 🌌 astro-ph.CO

The Dark Energy Survey Supernova Program: A Reanalysis Of Cosmology Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration

B. Popovic , P. Shah , W. D. Kenworthy , R. Kessler , T. M. Davis , A. Goobar , D. Scolnic , M. Vincenzi
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P. Wiseman R. Chen E. Charleton M. Acevedo P. Armstrong B.M. Boyd D. Brout R. Camilleri J. Frieman L. Galbany M. Grayling L. Kelsey B. Rose B. S\'anchez J. Lee A. M\"oller M. Smith M. Sullivan N. Shiamtanis A. Alarcon S.S. Allam F. Andrade-Oliveira S. Avila D. Bacon J. Blazek S. Bocquet D. Brooks D. L. Burke A. Carnero Rosell J. Carretero R. Cawthon L. N. da Costa M. E. da Silva Pereira H. T. Diehl S. Dodelson P. Doel S. Everett C. Frohmaier J. Garc\'ia-Bellido D. Gruen G. Gutierrez K. Herner S. R. Hinton D. L. Hollowood K. Honscheid D. Huterer D. J. James N. Jeffrey K. Kuehn O. Lahav S. Lee C. Lidman J. L. Marshall J. Mena-Fern\'andez F. Menanteau R. Miquel J. Muir J. Myles R. L. C. Ogando M. Paterno A. A. Plazas Malag\'on A. Porredon J. Prat R.C. Nichol A. K. Romer A. Roodman E. Sanchez D. Sanchez Cid I. Sevilla-Noarbe E. Suchyta M. E. C. Swanson C. To D. L. Tucker A. R. Walker N. Weaverdyck
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Pith reviewed 2026-05-17 23:20 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords supernova cosmologydark energyType Ia supernovaeDESw0 wa CDMcosmological parameterscalibration
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The pith

Re-calibrated DES Type Ia supernovae data yield w0 = -0.803 and wa = -0.72, showing 3.2 sigma preference for evolving dark energy.

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

The paper reanalyzes the DES five-year Type Ia supernova sample with an improved photometric cross-calibration between surveys, white dwarf observations to link brightness scales across redshift ranges, a retrained SALT3 light curve model, and a fixed numerical approximation in the host galaxy colour law. The resulting DES-Dovekie sample contains roughly 1600 likely Type Ia events from DES plus 200 low-redshift supernovae. In a flat Lambda CDM model the inferred matter density is Omega_m = 0.330 plus or minus 0.015, lower than the prior DES-SN5YR value. When the same sample is combined with Planck, ACT, and SPT cosmic microwave background data plus DESI DR2 measurements inside a flat w0 wa CDM cosmology, the best-fit parameters are w0 = -0.803 plus or minus 0.054 and wa = -0.72 plus or minus 0.21, rejecting a cosmological constant at 3.2 sigma significance and producing only weak Bayesian model preference for evolution.

Core claim

The authors introduce the DES-Dovekie supernova sample and report that, in combination with CMB and DESI DR2 data, it prefers a time-varying dark energy equation of state at 3.2 sigma significance in flat w0 wa CDM, with the specific best-fit values w0 = -0.803 plus or minus 0.054 and wa = -0.72 plus or minus 0.21, reduced from the 4.2 sigma preference found in the original DES-SN5YR analysis.

What carries the argument

The DES-Dovekie sample, which incorporates improved photometric cross-calibration, white dwarf linking for low-redshift calibration, retraining of the SALT3 light curve model, and correction of the host galaxy colour law numerical approximation.

If this is right

  • Omega_m shifts downward by 0.022 relative to the previous DES-SN5YR result in flat Lambda CDM.
  • The statistical significance of rejecting a cosmological constant drops from 4.2 sigma to 3.2 sigma.
  • The data produce only a weak Bayesian model preference of roughly 5 to 1 in favour of the evolving dark energy model.
  • The updated calibration changes the central values of w0 and wa enough to move the result into the regime of weak rather than moderate model preference.

Where Pith is reading between the lines

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

  • Calibration details between high- and low-redshift supernova surveys remain a dominant source of uncertainty that can shift the inferred strength of dark energy evolution signals.
  • The reduction in significance suggests that next-generation surveys with larger samples and independent calibration methods could either confirm or remove the current hint of evolution.
  • The result is consistent with the possibility that apparent tensions between supernova and other cosmological probes partly reflect differences in how each dataset is anchored to absolute brightness.

Load-bearing premise

The new photometric cross-calibration, white dwarf linking, SALT3 retraining, and host galaxy colour law fix introduce no residual systematic biases capable of altering the apparent preference for evolving dark energy.

What would settle it

An independent analysis of the same or a larger supernova sample using alternative calibration anchors that recovers w0 within 0.05 of -1 and wa within 0.1 of 0 at greater than 3 sigma would falsify the reported 3.2 sigma preference.

Figures

Figures reproduced from arXiv: 2511.07517 by A. Alarcon, A. A. Plazas Malag\'on, A. Carnero Rosell, A. Goobar, A. K. Romer, A. M\"oller, A. Porredon, A. Roodman, A. R. Walker, B.M. Boyd, B. Popovic, B. Rose, B. S\'anchez, C. Frohmaier, C. Lidman, C. To, D. Bacon, D. Brooks, D. Brout, D. Gruen, D. Huterer, D. J. James, D. L. Burke, D. L. Hollowood, D. L. Tucker, D. Sanchez Cid, D. Scolnic, E. Charleton, E. Sanchez, E. Suchyta, F. Andrade-Oliveira, F. Menanteau, G. Gutierrez, H. T. Diehl, I. Sevilla-Noarbe, J. Blazek, J. Carretero, J. Frieman, J. Garc\'ia-Bellido, J. Lee, J. L. Marshall, J. Mena-Fern\'andez, J. Muir, J. Myles, J. Prat, K. Herner, K. Honscheid, K. Kuehn, L. Galbany, L. Kelsey, L. N. da Costa, M. Acevedo, M. E. C. Swanson, M. E. da Silva Pereira, M. Grayling, M. Paterno, M. Smith, M. Sullivan, M. Vincenzi, N. Jeffrey, N. Shiamtanis, N. Weaverdyck, O. Lahav, P. Armstrong, P. Doel, P. Shah, P. Wiseman, R. Camilleri, R. Cawthon, R. Chen, R.C. Nichol, R. Kessler, R. L. C. Ogando, R. Miquel, S. Avila, S. Bocquet, S. Dodelson, S. Everett, S. Lee, S. R. Hinton, S.S. Allam, T. M. Davis, W. D. Kenworthy.

Figure 1
Figure 1. Figure 1: The DES-SN5YR sample includes the DES, CfA3S, CfA3K, CSP, and Foundation; the difference in calibration offsets for each filter and each survey is plotted at the approximate median redshift of the survey. To show the improvement in precision with the new calibration, the light-blue vertical bars show the calibration uncertainties for DES without using the nominal DA WD. The mean zero point across all surve… view at source ↗
Figure 2
Figure 2. Figure 2: Distributions of 𝑧, 𝑚𝐵, 𝑥1, 𝑐 for DES-SN5YR (black) and this work (filled histogram). We split the sample into its constituent parts, DES (blue), Foundation (teal), and Low-z (light green). We see agreement between the two analyses, with the exception of the DES 𝑐 distribution. Parameter Difference Between DES-Dovekie and DES-SN5YR 𝜎 (DES) 𝜎 (Foundation) 𝜎(Low-z) 𝑧 0.0𝜎 0.0𝜎 0.0𝜎 𝑐 2.8𝜎 0.0𝜎 0.2𝜎 𝑥1 1.2𝜎 0… view at source ↗
Figure 3
Figure 3. Figure 3: The DES-Dovekie Hubble Diagram, and the change in inferred, bias-corrected 𝜇 values between DES-SN5YR and this work. 𝑧, 𝑥1, 𝑐, 𝑚𝐵, 𝑀★, 𝜇 − 𝜇model, and the redshift and host-galaxy mass evolution of 𝑥1 and 𝑐, and require a reduced 𝜒 2 between data and simulations to lay between 0.7 and 3.0. Additionally, we provide a brief summary of the consistency and improvement tests that Dovekie performed during their … view at source ↗
Figure 4
Figure 4. Figure 4: Comparison between the simulated and observed SN parameters. The data are presented in grey, and the simulations are presented in coloured histogram. 7.2 SN Ia Properties and Astrophysics The nuisance parameters 𝛼, 𝛽, 𝛾 in Equation 1 are assumed to be con￾stant in the nominal analysis. However, a redshift evolving nuisance parameter, such as 𝛼(𝑧) = 𝛼0 + 𝛼1 × 𝑧, may capture un-modelled evolution of SN Ia pa… view at source ↗
Figure 5
Figure 5. Figure 5: Systematic and statistical error budget on Ωm for a Flat ΛCDM cosmology with SNIa only. Systematics are colour coded as in [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Systematic and statistical uncertainty budget on 𝑤, both with (right) and without (left) a CMB prior. Those systematic uncertainties that are not labelled with text represent a negligible (<0.005) systematic contribution. As the last of these combinations may at first sight indicate a weak preference for non-zero spatial curvature, we comment on this further in Section 11.2. We illustrate our results in [… view at source ↗
Figure 8
Figure 8. Figure 8: Effects of different Survey modelling systematics on the inferred SN Ia distances. Left: Choosing a shallower galaxy catalogue (DES ‘SVA Gold’). Right: Varying the efficiency of obtaining a spectroscopic redshift. Green points are individual realisations, black points are binned means. 0.25 0.30 0.35 0.40 m SN BAO CMB SN + BAO + CMB [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 7
Figure 7. Figure 7: The median binned differences between the nominal distances and the 9 calibration systematics (colour coded for each systematic surface) for DES-Dovekie. Comparable to [PITH_FULL_IMAGE:figures/full_fig_p014_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Constraints on the matter density for Flat ΛCDM for DES-Dovekie (blue), Planck CMB (grey), DESI DR2 BAO (black), and the combination SN+CMB+BAO (dark blue). MNRAS 000, 1–25 (2025) [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: The Ωm, 𝑤 contours for Flat 𝑤CDM. In blue, we present SN-only, complemented by the CMB (dark grey) and BAO (light grey) constraints. The full combination of SN+BAO+CMB is in dark blue. We include a maroon dashed line for 𝑤 = −1 = ΛCDM. Parameter Significance (𝜎syst) 𝑤0 1.1𝜎 𝑤𝑎 1.2𝜎 [PITH_FULL_IMAGE:figures/full_fig_p015_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: The cosmological contours for 𝑤0𝑤𝑎CDM cosmology. We show SN-only in light blue, SN+CMB in grey, and SN+CMB+BAO in dark blue. Our combined external probes, BAO+CMB, is shown in black. We include light maroon dashed lines for 𝑤 = −1 = ΛCDM. ΛCDM), they are consistent in their message. We discuss this further in Section 11.4. It is clear from [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Model preference in terms of the log of the Bayes ratio, Δ log Z. We have also made use of the Nautilus sampler in Cosmosis rather than Cobaya MCMC sampler, but since our chains are well￾converged we expect this to be a minor effect. Therefore, our results for DES-SN5YR are consistent with DESI Collaboration et al. (2025) within the bounds of our differing choices. 11.2 The evidence for spatial flatness I… view at source ↗
read the original abstract

We present improved cosmological constraints from a re-analysis of the Dark Energy Survey (DES) 5-year sample of Type Ia supernovae (DES-SN5YR). This re-analysis includes an improved photometric cross-calibration, recent white dwarf observations to cross-calibrate between DES and low redshift surveys, retraining the SALT3 light curve model and fixing a numerical approximation in the host galaxy colour law. Our fully recalibrated sample, which we call DES-Dovekie, comprises $\sim$1600 likely Type Ia SNe from DES and $\sim$200 low-redshift SNe from other surveys. With DES-Dovekie, we obtain $\Omega_{\rm m} = 0.330 \pm 0.015$ in Flat $\Lambda$CDM which changes $\Omega_{\rm m}$ by $-0.022$ compared to DES-SN5YR. Combining DES-Dovekie with CMB data from Planck, ACT and SPT and the DESI DR2 measurements in a Flat $w_0 w_a$CDM cosmology, we find $w_0 = -0.803 \pm 0.054$, $w_a = -0.72 \pm 0.21$. Our results hold a significance of $3.2\sigma$, reduced from $4.2\sigma$ for DES-SN5YR, to reject the null hypothesis that the data are compatible with the cosmological constant. This significance is equivalent to a Bayesian model preference odds of approximately 5:1 in favour of the Flat $w_0 w_a$CDM model. Using generally accepted thresholds for model preference, our updated data exhibits only a weak preference for evolving 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 / 2 minor

Summary. The paper reanalyzes the DES 5-year Type Ia supernova sample (DES-SN5YR) with four calibration updates: improved photometric cross-calibration, white-dwarf observations to link DES to low-redshift surveys, retraining of the SALT3 light-curve model, and a fix to a numerical approximation in the host-galaxy colour law. The resulting DES-Dovekie sample (~1600 DES SNe plus ~200 low-z SNe) yields Ω_m = 0.330 ± 0.015 in flat ΛCDM, a shift of −0.022 relative to the prior analysis. Combined with Planck+ACT+SPT CMB and DESI DR2 BAO data in flat w0waCDM, the fit gives w0 = −0.803 ± 0.054, wa = −0.72 ± 0.21, corresponding to a 3.2σ preference over ΛCDM (down from 4.2σ) and a Bayesian odds ratio of ~5:1 in favor of evolving dark energy.

Significance. If the new calibrations are shown to introduce no unaccounted redshift-dependent residuals, the work supplies a valuable update to supernova cosmology constraints and quantifies how calibration choices affect the apparent evidence for wa < 0. The transparent reporting of the drop in significance and the weak model preference (5:1 odds) is a strength. The multi-probe combination with independent CMB and DESI anchors adds robustness to the central parameter values.

major comments (2)
  1. [Abstract and cosmological results section] Abstract and the section presenting the combined cosmological constraints: the headline 3.2σ preference and the reduction from 4.2σ are stated, yet the text does not isolate the contribution of each individual update (photometric cross-calibration, white-dwarf linking, SALT3 retraining, host-galaxy colour-law fix) to the final covariance matrix or to Δχ² relative to w0 = −1, wa = 0. Because each change can alter redshift-dependent colour and stretch corrections, this omission is load-bearing for the claim that the wa constraint is robust.
  2. [Systematic error budget section] Section describing the systematic error budget and covariance construction: it is not shown that the new white-dwarf cross-calibration and host-galaxy colour-law fix have been propagated such that any residual redshift-dependent biases in the light-curve parameters are fully captured by the reported covariance. An incomplete propagation would directly affect the apparent preference for wa < 0.
minor comments (2)
  1. [Abstract] The phrase 'generally accepted thresholds for model preference' is used without specifying the numerical criteria (e.g., Jeffreys scale or ΔlnZ thresholds) applied to the 5:1 odds ratio.
  2. Comparison plots or tables contrasting DES-Dovekie distance moduli and parameter shifts with the original DES-SN5YR results would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our reanalysis of the DES-SN5YR sample. We have carefully considered the two major comments and agree that additional transparency on the individual calibration updates and systematic propagation will strengthen the manuscript. We outline our responses below and the revisions we will implement.

read point-by-point responses

  1. Referee: [Abstract and cosmological results section] Abstract and the section presenting the combined cosmological constraints: the headline 3.2σ preference and the reduction from 4.2σ are stated, yet the text does not isolate the contribution of each individual update (photometric cross-calibration, white-dwarf linking, SALT3 retraining, host-galaxy colour-law fix) to the final covariance matrix or to Δχ² relative to w0 = −1, wa = 0. Because each change can alter redshift-dependent colour and stretch corrections, this omission is load-bearing for the claim that the wa constraint is robust.

    Authors: We agree that isolating the contribution of each calibration update is important for demonstrating robustness. In the revised manuscript we will add a dedicated subsection (or supplementary table) in the cosmological results section that applies the four updates sequentially. For each step we will report the resulting shifts in w0, wa, the relevant covariance-matrix elements, and the change in Δχ² relative to the w0 = −1, wa = 0 point. These intermediate results have already been computed internally and will be presented transparently so that readers can evaluate the impact of each change on the apparent preference for evolving dark energy. revision: yes

  2. Referee: [Systematic error budget section] Section describing the systematic error budget and covariance construction: it is not shown that the new white-dwarf cross-calibration and host-galaxy colour-law fix have been propagated such that any residual redshift-dependent biases in the light-curve parameters are fully captured by the reported covariance. An incomplete propagation would directly affect the apparent preference for wa < 0.

    Authors: We have incorporated both the white-dwarf cross-calibration and the host-galaxy colour-law fix into the final covariance matrix used for the cosmological fits. To make this propagation explicit, we will expand the systematic error budget section with additional text and, where appropriate, a supplementary figure that traces how these two updates enter the covariance. We will also report the results of explicit checks for residual redshift-dependent biases in the light-curve parameters (stretch and colour) after applying the corrections, and will either confirm that any such residuals are already captured or add a corresponding systematic term if needed. revision: yes

Circularity Check

0 steps flagged

No significant circularity; cosmological parameters are direct fits to recalibrated supernova data anchored by external datasets

full rationale

The paper describes a reanalysis of DES-SN5YR data with updates to photometric cross-calibration, white dwarf linking, SALT3 retraining, and host galaxy colour law, producing the DES-Dovekie sample. Cosmological constraints (Ωm in Flat ΛCDM; w0 and wa in Flat w0 wa CDM) are obtained via standard likelihood fitting that combines the supernova distance moduli with independent CMB data (Planck, ACT, SPT) and DESI DR2 BAO measurements. No equation or step in the provided derivation chain reduces the reported w0 = -0.803 ± 0.054 or wa = -0.72 ± 0.21 to a quantity defined by the fit itself. External datasets supply independent anchors, and the significance reduction from 4.2σ to 3.2σ is presented as an empirical outcome of the recalibration rather than a constructed result. Self-citations to prior DES work exist but are not load-bearing for the central claim, which rests on the new data processing and external constraints.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central results rest on the assumption that the updated supernova calibration accurately captures intrinsic brightness variations and that external CMB and BAO datasets can be combined without unaccounted tension.

free parameters (2)
  • w0 = -0.803
    Dark energy equation-of-state parameter at z=0, fitted to the combined supernova plus CMB plus DESI data.
  • wa = -0.72
    Dark energy evolution parameter, fitted to the combined supernova plus CMB plus DESI data.
axioms (2)
  • domain assumption Flat geometry in both ΛCDM and w0waCDM models.
    All quoted constraints assume zero spatial curvature.
  • domain assumption Type Ia supernovae remain standardizable candles after the applied corrections.
    Core premise enabling distance measurements from the DES-Dovekie sample.

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  26. Testing Scale-Dependent Modified Gravity with DESI DR1

    astro-ph.CO 2026-04 accept novelty 4.0

    DESI DR1 constrains the modified gravity parameter to log10 |f_R0| < -4.59 at 95% CL, implying no detectable fifth force on scales below about 18 Mpc.

  27. The open-Universe signal: A model artifact rather than genuine curvature

    astro-ph.CO 2026-04 unverdicted novelty 4.0

    The mild open-universe signal in late-Universe data is an artifact of assuming the basic ΛCDM model rather than evidence for genuine spatial curvature.

  28. 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.

  29. Cosmology-Independent Constraints on the Etherington Relation and SNeIa Absolute Magnitude Evolution from DESI-DR2

    astro-ph.CO 2026-04 accept novelty 4.0

    DESI-DR2 angular diameter distances and SNeIa luminosity distances are statistically consistent with the Etherington relation, yielding a constraint on SNeIa absolute magnitude evolution of dM/dz = 0.07 ± 0.07.

  30. Gamma-Ray Bursts as an Independent High-Redshift Probe of Dark Energy

    astro-ph.CO 2026-03 unverdicted novelty 4.0

    Forecasts show that ~66 optical GRBs can achieve σ_w ≈ 0.47 in wCDM using Dainotti relations, matching Planck precision and enabling independent high-redshift tests of dark energy.

  31. No evidence for phantom crossing: local goodness-of-fit improvements do not persist under global Bayesian model comparison

    astro-ph.CO 2026-05 unverdicted novelty 3.0

    Local goodness-of-fit gains for w0wa and phantom crossing vanish under global Bayesian evidence, showing no statistically robust evidence for dynamical dark energy across datasets.

  32. No evidence for phantom crossing: local goodness-of-fit improvements do not persist under global Bayesian model comparison

    astro-ph.CO 2026-05 unverdicted novelty 3.0

    Global Bayesian evidence shows no statistically significant support for dynamical dark energy or phantom crossing despite limited local fit improvements in the w0wa parametrization.

  33. Dark Energy After DESI DR2: Observational Status, Reconstructions, and Physical Models

    astro-ph.CO 2026-02 unverdicted novelty 3.0

    DESI DR2 data reveals a mild mismatch for flat LambdaCDM in CMB-calibrated fits, with evolving dark energy models like CPL improving the fit in a dataset-dependent manner sensitive to supernova calibration residuals a...

  34. Breaking Free from the Swampland of Impossible Universes through the DESI Portal

    astro-ph.CO 2026-05 unverdicted novelty 2.0

    DESI data indicating evolving dark energy may allow string theory to describe observed universes without violating swampland constraints on constant dark energy.

  35. Viaggiu holographic dark energy in light of DESI DR2

    gr-qc 2026-03 unverdicted novelty 2.0

    The Viaggiu holographic dark energy model fits late-time data similarly to Lambda CDM, yielding Omega_m0 around 0.24 and a model parameter of 0.27-0.33, with AIC showing statistical indistinguishability.

Reference graph

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