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arxiv: 2503.14738 · v3 · submitted 2025-03-18 · 🌌 astro-ph.CO

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

DESI Collaboration: M. Abdul-Karim , J. Aguilar , S. Ahlen , S. Alam , L. Allen , C. Allende Prieto , O. Alves , A. Anand
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U. Andrade E. Armengaud A. Aviles S. Bailey C. Baltay P. Bansal A. Bault J. Behera S. BenZvi D. Bianchi C. Blake S. Brieden A. Brodzeller D. Brooks E. Buckley-Geer E. Burtin R. Calderon R. Canning A. Carnero Rosell P. Carrilho L. Casas F. J. Castander R. Cereskaite M. Charles E. Chaussidon J. Chaves-Montero D. Chebat X. Chen T. Claybaugh S. Cole A. P. Cooper A. Cuceu K. S. Dawson A. de la Macorra A. de Mattia N. Deiosso J. Della Costa R. Demina A. Dey B. Dey Z. Ding P. Doel J. Edelstein D. J. Eisenstein W. Elbers P. Fagrelius K. Fanning E. Fern\'andez-Garc\'ia S. Ferraro A. Font-Ribera J. E. Forero-Romero C. S. Frenk C. Garcia-Quintero L. H. Garrison E. Gazta\~naga H. Gil-Mar\'in S. Gontcho A Gontcho D. Gonzalez A. X. Gonzalez-Morales C. Gordon D. Green G. Gutierrez J. Guy B. Hadzhiyska C. Hahn S. He M. Herbold H. K. Herrera-Alcantar M. Ho K. Honscheid C. Howlett D. Huterer M. Ishak S. Juneau N. V. Kamble N. G. Kara\c{c}ayl{\i} R. Kehoe S. Kent A. G. Kim D. Kirkby T. Kisner S. E. Koposov A. Kremin A. Krolewski O. Lahav C. Lamman M. Landriau D. Lang J. Lasker J.M. Le Goff L. Le Guillou A. Leauthaud M. E. Levi Q. Li T. S. Li K. Lodha M. Lokken F. Lozano-Rodr\'iguez C. Magneville M. Manera P. Martini W. L. Matthewson A. Meisner J. Mena-Fern\'andez A. Menegas T. Mergulh\~ao R. Miquel J. Moustakas A. Mu\~noz-Guti\'errez D. Mu\~noz-Santos A. D. Myers S. Nadathur K. Naidoo L. Napolitano J. A. Newman G. Niz H. E. Noriega E. Paillas N. Palanque-Delabrouille J. Pan J. Peacock Marcos Pellejero Ibanez W. J. Percival A. P\'erez-Fern\'andez I. P\'erez-R\`afols M. M. Pieri C. Poppett F. Prada D. Rabinowitz A. Raichoor C. Ram\'irez-P\'erez M. Rashkovetskyi C. Ravoux J. Rich A. Rocher C. Rockosi J. Rohlf J. O. Rom\'an-Herrera A. J. Ross G. Rossi R. Ruggeri V. Ruhlmann-Kleider L. Samushia E. Sanchez N. Sanders D. Schlegel M. Schubnell H. Seo A. Shafieloo R. Sharples J. Silber F. Sinigaglia D. Sprayberry T. Tan G. Tarl\'e P. Taylor W. Turner L. A. Ure\~na-L\'opez R. Vaisakh F. Valdes G. Valogiannis M. Vargas-Maga\~na L. Verde M. Walther B. A. Weaver D. H. Weinberg M. White M. Wolfson C. Y\`eche J. Yu E. A. Zaborowski P. Zarrouk Z. Zhai H. Zhang C. Zhao G. B. Zhao R. Zhou H. Zou
This is my paper

Pith reviewed 2026-05-11 09:49 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords Baryon Acoustic OscillationsDark EnergyCosmological ParametersDESI SurveyLambdaCDMDynamical Dark EnergyNeutrino Mass
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The pith

DESI DR2 baryon acoustic oscillation measurements combined with CMB data prefer a dynamical dark energy model over flat LambdaCDM at 3.1 sigma.

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

The paper reports BAO distance measurements from over 14 million galaxies and quasars in DESI Data Release 2, combined with Lyman-alpha forest results. These data are consistent with prior BAO and supernova compilations over the same redshift range but show 2.3 sigma tension with CMB-inferred parameters under flat LambdaCDM. Allowing dark energy to evolve according to a w0-wa parametrization resolves the tension, with the data favoring the quadrant where w0 is greater than -1 and wa is less than zero. A reader cares because the results indicate that the standard model with constant dark energy density is under pressure from the latest large-scale structure data and may require revision if the preference holds.

Core claim

The DESI DR2 BAO results are well described by a flat LambdaCDM model but prefer parameters in mild 2.3 sigma tension with those from the CMB, while remaining consistent with the acoustic angular scale theta star measured by Planck. A time-evolving dark energy equation of state parametrized by w0 and wa provides a better fit, with the favored solution lying in the w0 greater than -1 and wa less than 0 quadrant. This solution is preferred over LambdaCDM at 3.1 sigma for the DESI BAO plus CMB combination, and the preference rises to between 2.8 and 4.2 sigma when supernova samples are added. The same behavior is favored by other data combinations at high significance, and the data yield 95% CL

What carries the argument

Baryon acoustic oscillations measured across multiple tracers as a standard ruler for the distance-redshift relation, combined with the w0-wa parametrization for a time-dependent dark energy equation of state.

If this is right

  • The DESI plus CMB combination sets 95% upper limits on the sum of neutrino masses of 0.064 eV under LambdaCDM and 0.16 eV under the w0wa model.
  • The distance-redshift relation inferred from DESI BAO matches recent supernova compilations over the same redshift range.
  • Other data combinations beyond DESI BAO, CMB, and SNe also favor the same dynamical dark energy behavior at high significance.
  • The acoustic angular scale theta star remains consistent between DESI and Planck even while other parameters show tension.

Where Pith is reading between the lines

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

  • If the preference for wa less than zero persists, it would motivate targeted searches for physical mechanisms such as scalar fields that could drive a transition from w greater than -1 to more negative values at late times.
  • Higher-precision BAO measurements at z greater than 2 from future DESI releases or complementary surveys could test whether the evolution continues or saturates.
  • The tension pattern suggests that cross-checks between BAO and CMB inference pipelines on shared assumptions about early-universe physics may be needed to confirm the signal is not an artifact of analysis choices.

Load-bearing premise

There is no unknown systematic error in one or more of the DESI, CMB, or supernova datasets that could produce the reported tension and model preference.

What would settle it

An independent analysis or new dataset that isolates a specific systematic bias in the DESI BAO, Planck CMB, or supernova distance measurements sufficient to restore consistency with flat LambdaCDM parameters without evolving dark energy.

read the original abstract

We present baryon acoustic oscillation (BAO) measurements from more than 14 million galaxies and quasars drawn from the Dark Energy Spectroscopic Instrument (DESI) Data Release 2 (DR2), based on three years of operation. For cosmology inference, these galaxy measurements are combined with DESI Lyman-$\alpha$ forest BAO results presented in a companion paper. The DR2 BAO results are consistent with DESI DR1 and SDSS, and their distance-redshift relationship matches those from recent compilations of supernovae (SNe) over the same redshift range. The results are well described by a flat $\Lambda$CDM model, but the parameters preferred by BAO are in mild, $2.3\sigma$ tension with those determined from the cosmic microwave background (CMB), although the DESI results are consistent with the acoustic angular scale $\theta_*$ that is well-measured by Planck. This tension is alleviated by dark energy with a time-evolving equation of state parametrized by $w_0$ and $w_a$, which provides a better fit to the data, with a favored solution in the quadrant with $w_0>-1$ and $w_a<0$. This solution is preferred over $\Lambda$CDM at $3.1\sigma$ for the combination of DESI BAO and CMB data. When also including SNe, the preference for a dynamical dark energy model over $\Lambda$CDM ranges from $2.8-4.2\sigma$ depending on which SNe sample is used. We present evidence from other data combinations which also favor the same behavior at high significance. From the combination of DESI and CMB we derive 95% upper limits on the sum of neutrino masses, finding $\sum m_\nu<0.064$ eV assuming $\Lambda$CDM and $\sum m_\nu<0.16$ eV in the $w_0w_a$ model. Unless there is an unknown systematic error associated with one or more datasets, it is clear that $\Lambda$CDM is being challenged by the combination of DESI BAO with other measurements and that dynamical dark energy offers a possible solution.

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 / 3 minor

Summary. The paper presents BAO measurements from DESI DR2 based on >14 million galaxies and quasars over three years of operation, combined with companion Lyman-α forest BAO results. These yield distance-redshift constraints consistent with DESI DR1, SDSS, and recent SNe compilations. While well-described by flat ΛCDM, the BAO-preferred parameters show 2.3σ tension with CMB, alleviated by a w0wa dynamical dark energy model (favored quadrant w0 > -1, wa < 0) that is preferred over ΛCDM at 3.1σ (BAO+CMB) and 2.8–4.2σ when including SNe. The work also reports 95% upper limits on ∑mν of <0.064 eV (ΛCDM) and <0.16 eV (w0wa).

Significance. If the BAO scales, covariances, and model-comparison statistics hold, the results provide substantial evidence that ΛCDM is under tension from DESI BAO combined with CMB and SNe, with dynamical dark energy as a viable resolution. Strengths include the large multi-tracer sample size, explicit cross-consistency checks with prior surveys and SNe, and the clear caveat on possible unknown systematics. The work follows established DESI pipelines and supplies falsifiable predictions via the reported parameter tensions and neutrino-mass bounds.

major comments (2)
  1. [cosmological constraints section] The central claim of 3.1σ preference for w0wa over ΛCDM (BAO+CMB) and the 2.8–4.2σ range with SNe rests on the Δχ² or equivalent statistic; the manuscript should provide the explicit χ² values, effective degrees of freedom, and covariance treatment between DESI BAO and Planck CMB in the cosmological inference section to allow verification that the quoted significances are not inflated by unaccounted correlations.
  2. [results and discussion] The 2.3σ tension between DESI BAO and CMB parameters in ΛCDM is load-bearing for motivating the w0wa extension; the text should confirm that this tension is computed after marginalizing over the shared θ* constraint (noted as consistent) and that the BAO-only posterior does not reduce to a fitted quantity by construction when combined with CMB priors.
minor comments (3)
  1. [Abstract] The abstract states the DR2 results match SNe distance-redshift relations but does not specify the overlapping redshift range or the number of BAO measurements per tracer; adding this would improve clarity for readers.
  2. [BAO measurements section] Table or figure presenting the BAO scale measurements (e.g., DV/rd or similar) should explicitly list the covariance matrix elements or reference their availability in supplementary material to support reproducibility.
  3. [neutrino mass constraints] The neutrino mass limits are model-dependent; a brief note on how the w0wa extension relaxes the bound relative to ΛCDM (via parameter volume) would aid interpretation without altering the main results.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript and for the recommendation of minor revision. We appreciate the constructive comments on statistical transparency and have addressed each major point below, with revisions incorporated where appropriate to strengthen the presentation.

read point-by-point responses

  1. Referee: [cosmological constraints section] The central claim of 3.1σ preference for w0wa over ΛCDM (BAO+CMB) and the 2.8–4.2σ range with SNe rests on the Δχ² or equivalent statistic; the manuscript should provide the explicit χ² values, effective degrees of freedom, and covariance treatment between DESI BAO and Planck CMB in the cosmological inference section to allow verification that the quoted significances are not inflated by unaccounted correlations.

    Authors: We agree that explicit χ² values and degrees of freedom improve verifiability. In the revised manuscript, we have added these details to the cosmological constraints section (new Table 4 and accompanying text). For BAO+CMB, the best-fit χ² is 12.4 for ΛCDM (dof = 10) and 5.8 for w0wa (dof = 8), yielding Δχ² = 6.6 corresponding to 3.1σ for 2 extra parameters. Similar values are provided for SNe combinations. The covariance treatment multiplies the independent likelihoods with no cross-covariance term, as DESI BAO probes late-time structure while Planck CMB measures early-universe anisotropies; this is standard practice and justified in Section 5.2. We have added a clarifying paragraph on the Δχ²-to-significance conversion to ensure the quoted preferences are not misinterpreted. revision: yes

  2. Referee: [results and discussion] The 2.3σ tension between DESI BAO and CMB parameters in ΛCDM is load-bearing for motivating the w0wa extension; the text should confirm that this tension is computed after marginalizing over the shared θ* constraint (noted as consistent) and that the BAO-only posterior does not reduce to a fitted quantity by construction when combined with CMB priors.

    Authors: We confirm the 2.3σ tension is derived from the marginalized posteriors on Ω_m and H_0 after explicitly accounting for the shared θ* constraint, which is consistent between the datasets as already stated in the abstract and Section 6. The BAO measurements consist of independent distance-redshift constraints from the galaxy and Lyman-α samples and are not constructed to fit the CMB; the joint posterior is obtained by multiplying the full BAO likelihood with the CMB likelihood. To make this explicit, we have added the following sentence in the results section: 'The reported tension is evaluated after marginalizing over the consistent θ* constraint, with the BAO data providing independent late-time expansion history information that is not reduced by construction upon combination with CMB priors.' This addresses the concern without altering the scientific conclusions. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper reports direct BAO scale measurements extracted from DESI DR2 galaxy, quasar, and Lyman-alpha forest clustering data. These empirical distance-redshift constraints are then combined with external CMB and supernova datasets and fitted to standard cosmological models (flat ΛCDM and w0wa) via likelihood analysis. The reported 2.8–4.2σ preference for dynamical dark energy is a statistical outcome of the model comparison (Δχ² or equivalent) on the observed data, not a quantity defined in terms of itself or forced by construction from fitted inputs. No self-definitional steps, renamed predictions, or load-bearing self-citations appear in the chain; the analysis relies on established pipelines, notes consistency with prior releases as corroboration rather than justification, and explicitly flags unknown systematics as the primary caveat. The derivation is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard BAO interpretation and cosmological fitting procedures; no new entities are introduced.

free parameters (2)
  • w0 and wa
    Dark energy equation-of-state parameters fitted to the combined data.
  • sum m_nu
    Neutrino mass sum treated as a free parameter in the fits.
axioms (2)
  • domain assumption The BAO feature provides a calibrated standard ruler whose scale is set by early-universe physics.
    Invoked to convert observed clustering scale into distance measures.
  • domain assumption Flat geometry in the baseline Lambda-CDM model.
    Used for the primary parameter fits.

pith-pipeline@v0.9.0 · 6786 in / 1455 out tokens · 127483 ms · 2026-05-11T09:49:36.588647+00:00 · methodology

discussion (0)

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