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arxiv: 2606.23936 · v1 · pith:U45SJALFnew · submitted 2026-06-22 · 🌌 astro-ph.CO

Cosmological constraints from the DESI DR1 Bispectrum Full-Shape and DR2 BAO

D. Forero-S\'anchez , S. Novell-Masot , H. Gil-Mar\'in , L. Verde , J. Aguilar , S. Ahlen , D. Bianchi , A. Brodzeller
show 43 more authors
D. Brooks F. J. Castander S. Cole A. de la Macorra J. Della Costa Biprateep Dey P. Doel S. Ferraro A. Font-Ribera J. E. Forero-Romero Satya Gontcho A Gontcho G. Gutierrez C. Hahn H. K. Herrera-Alcantar K. Honscheid D. Huterer M. Ishak D. Kirkby A. Kremin O. Lahav C. Lamman M. Landriau L. Le Guillou M. E. Levi M. Manera A. Meisner R. Miquel J. Moustakas S. Nadathur J. A. Newman G. Niz N. Palanque-Delabrouille W. J. Percival F. Prada I. P\'erez-R\`afols G. Rossi L. Samushia E. Sanchez D. Schlegel M. Schubnell J. Silber G. Tarl\'e B. A. Weaver (DESI Collaboration)
This is my paper

Pith reviewed 2026-06-26 07:08 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords DESIbispectrumBAOneutrino massdark energymodified gravityfull-shape analysis
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The pith

Bispectrum data from DESI shifts the neutrino mass sum posterior to a positive 0.26 eV mean in DESI-only fits.

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

The paper combines DESI DR1 full-shape measurements that include the galaxy bispectrum with DR2 baryon acoustic oscillation data. It accounts for the statistical overlap between these probes by using mock catalogs and compresses the data with ShapeFit to reduce prior-volume artifacts. In flat LambdaCDM the bispectrum raises the inferred amplitude of structure growth and shrinks its uncertainty. Most strikingly, the neutrino mass sum moves from a posterior consistent with zero when only the power spectrum is used to a clearly positive value once the bispectrum is added. The same data combination pulls dark-energy parameters closer to a cosmological constant and leaves modified-gravity parameters consistent with general relativity.

Core claim

In the DESI-only analysis the power-spectrum-only posterior for the sum of neutrino masses is consistent with zero, whereas adding the bispectrum yields a mean of 0.26 plus or minus 0.17 eV and a 95 percent upper limit of 0.57 eV. In LambdaCDM the bispectrum raises sigma_8 by 1.1 sigma and S_8 by 1.2 sigma while cutting their uncertainties by 26 percent and 28 percent. For w0-wa dark energy the bispectrum moves the parameters toward LambdaCDM values; when CMB data are added the combination still deviates from LambdaCDM at 2.8 sigma, but the bispectrum itself weakens that deviation relative to power-spectrum-only fits. Modified-gravity parameter mu_0 is constrained to 0.12 plus or minus 0.49,

What carries the argument

Joint full-shape analysis of the power spectrum plus bispectrum from DESI LRG galaxies, cross-covariance estimated from mocks, and ShapeFit compression applied to the combined data vector.

If this is right

  • In LambdaCDM the bispectrum raises sigma_8 by 1.1 sigma and reduces its uncertainty by 26 percent.
  • The neutrino-mass sum gains a positive mean of 0.26 plus or minus 0.17 eV with a 95 percent upper limit of 0.57 eV.
  • Evidence for time-varying dark energy is weakened relative to power-spectrum-only analyses.
  • The modified-gravity parameter mu_0 remains consistent with general relativity at 0.12 plus or minus 0.49.

Where Pith is reading between the lines

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

  • If the positive neutrino-mass shift survives in future data releases, it would tighten the tension between cosmological upper limits and oscillation lower bounds.
  • The same bispectrum inclusion could be applied to other redshift surveys to test whether the amplitude-parameter shift is universal.
  • Improved covariance modeling from larger mock suites would directly test whether the reported neutrino posterior is robust.

Load-bearing premise

The mocks used to estimate the cross-covariance between power spectrum, bispectrum and BAO must faithfully represent the true covariance of the DESI data, and ShapeFit compression must not bias the posteriors away from LambdaCDM.

What would settle it

Re-running the identical analysis with a covariance matrix measured directly from the data instead of from mocks would falsify the reported neutrino-mass shift if the posterior returns to consistency with zero.

read the original abstract

We present cosmological constraints from the combination of DESI DR1 full-shape measurements, including for the LRG bispectrum, and DESI DR2 BAO data. The joint analysis accounts for cross-covariance using mocks, while ShapeFit compression mitigates prior volume effects that hinder beyond-$\Lambda$CDM analyses. In $\Lambda$CDM, the bispectrum (P+B) shifts $\sigma_8$ up by $1.1\sigma$ and $S_8$ by $1.2\sigma$, reducing their uncertainties by $26\%$ and $28\%$, respectively. For $w_0w_a$CDM, DESI-only analyses with the bispectrum shift dark energy parameters toward $\Lambda$CDM, staying consistent with a cosmological constant within $1\sigma$. Adding CMB creates a preference for evolving dark energy: DESI+CMB (P+B) shows a $2.8\sigma$ deviation from $\Lambda$CDM. Including DES-Dovekie supernovae alone reduces this to $1.6\sigma$, while the full combination DESI+CMB+DES-Dovekie gives $3.1\sigma$, driven primarily by the CMB. The bispectrum consistently weakens evidence for time-varying dark energy relative to power-spectrum-only analyses. The bispectrum also enhances sensitivity to massive neutrinos: in DESI-only analysis, the power-spectrum-only posterior for $\sum m_\nu$ is consistent with zero, whereas adding the bispectrum yields a mean of $0.26\pm0.17$~eV and a $95\%$ upper limit of $0.57$~eV, shifting the peak into the positive region and agreeing with oscillation lower bounds. For modified gravity, the bispectrum further constrains $\mu_0 = 0.12\pm0.49$ from DESI-only data, consistent with general relativity. Our analysis shows that accounting for cross-dataset covariances and avoiding prior volume effects yields robust constraints, with the bispectrum raising amplitude parameters and tightening their uncertainties.

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 presents cosmological constraints from DESI DR1 full-shape measurements (including LRG power spectrum and bispectrum) combined with DR2 BAO data. Cross-covariance between datasets is estimated from mocks, and ShapeFit compression is applied to reduce prior-volume effects in beyond-ΛCDM extensions. In ΛCDM the bispectrum raises σ8 and S8 by ~1.1–1.2σ while tightening uncertainties; in w0waCDM it shifts dark-energy parameters toward ΛCDM; for massive neutrinos the DESI-only P+B analysis yields ∑mν = 0.26 ± 0.17 eV (95 % upper limit 0.57 eV) versus a posterior consistent with zero from power spectrum alone; modified-gravity parameter μ0 is constrained to 0.12 ± 0.49, consistent with GR.

Significance. If the mock-derived joint covariance and ShapeFit compression are shown to be unbiased for the neutrino sector, the work demonstrates that the bispectrum measurably increases sensitivity to ∑mν and amplitude parameters, producing a DESI-only posterior whose peak lies above the oscillation lower bound. The explicit treatment of cross-covariances and prior-volume mitigation also supplies a template for future full-shape analyses of Stage-IV surveys.

major comments (2)
  1. [abstract / joint-analysis paragraph] Abstract and the paragraph describing the joint analysis: the reported shift in the ∑mν posterior (from consistent with zero in P-only to 0.26 ± 0.17 eV in P+B) rests on the assumption that the mock-estimated cross-covariance matrix between power spectrum, bispectrum and BAO is an unbiased estimator of the true data covariance; no quantitative validation (e.g., comparison of mock vs. analytic covariance diagonals/off-diagonals or recovery tests on simulated data with known ∑mν) is referenced, leaving the 0.57 eV upper limit vulnerable to possible under-estimation of cross-terms.
  2. [abstract / ShapeFit paragraph] Abstract and ShapeFit description: the claim that ShapeFit compression removes prior-volume effects without biasing beyond-ΛCDM posteriors is stated without a dedicated test (e.g., comparison of compressed vs. uncompressed chains for a fiducial massive-neutrino cosmology or assessment of residual bias in the compressed likelihood for ∑mν); this assumption is load-bearing for the neutrino result.
minor comments (1)
  1. Figure captions and text should explicitly state the number of mocks used for the covariance matrix and the precise definition of the ShapeFit compression parameters.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and insightful comments, which help improve the clarity and robustness of our analysis. We address each major comment below and will incorporate revisions as noted.

read point-by-point responses

  1. Referee: [abstract / joint-analysis paragraph] Abstract and the paragraph describing the joint analysis: the reported shift in the ∑mν posterior (from consistent with zero in P-only to 0.26 ± 0.17 eV in P+B) rests on the assumption that the mock-estimated cross-covariance matrix between power spectrum, bispectrum and BAO is an unbiased estimator of the true data covariance; no quantitative validation (e.g., comparison of mock vs. analytic covariance diagonals/off-diagonals or recovery tests on simulated data with known ∑mν) is referenced, leaving the 0.57 eV upper limit vulnerable to possible under-estimation of cross-terms.

    Authors: We agree that explicit validation of the mock-derived cross-covariance would strengthen the neutrino-mass result. While the use of mocks for joint covariances follows standard practice in DESI analyses and the mocks were validated for the power spectrum and bispectrum individually, we did not include a dedicated cross-term comparison or recovery test for ∑mν in the current manuscript. In the revised version we will add a short subsection presenting (i) diagonal and off-diagonal comparisons between the mock covariance and an analytic estimate, and (ii) a recovery test on simulated data with known ∑mν, thereby confirming that the reported 0.26 ± 0.17 eV posterior is not driven by under-estimated cross-terms. revision: yes

  2. Referee: [abstract / ShapeFit paragraph] Abstract and ShapeFit description: the claim that ShapeFit compression removes prior-volume effects without biasing beyond-ΛCDM posteriors is stated without a dedicated test (e.g., comparison of compressed vs. uncompressed chains for a fiducial massive-neutrino cosmology or assessment of residual bias in the compressed likelihood for ∑mν); this assumption is load-bearing for the neutrino result.

    Authors: The manuscript relies on the ShapeFit compression as implemented and validated in the original ShapeFit papers and in prior DESI full-shape analyses. However, we acknowledge that a specific test for the massive-neutrino extension was not shown. In revision we will include a direct comparison of compressed versus uncompressed posterior contours for a fiducial ∑mν = 0.3 eV cosmology, together with a quantitative assessment of any residual bias in the compressed likelihood for ∑mν, to demonstrate that the reported shift remains robust. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper's central results are posterior constraints obtained by fitting a parametric cosmological model to external DESI DR1 full-shape (P+B) and DR2 BAO data, with cross-covariance estimated from mocks and prior-volume mitigation via ShapeFit. This does not reduce any claimed posterior shift (e.g., in ∑mν or σ8) to the inputs by construction; the likelihood is driven by the observed data vectors rather than being tautological or self-referential. No self-definitional steps, fitted parameters renamed as predictions, load-bearing self-citations, or ansatz smuggling appear in the abstract or described analysis. The derivation is therefore self-contained against external benchmarks and receives the default non-circularity finding.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claims rest on the accuracy of the full-shape modeling pipeline, the fidelity of the mock catalogs for covariance estimation, and the assumption that ShapeFit compression does not introduce bias in extended models; these are domain assumptions rather than new free parameters or invented entities.

free parameters (1)
  • cosmological parameters (Ωm, σ8, w0, wa, ∑mν, μ0)
    These are fitted to the combined DESI data; their posterior values constitute the reported constraints.
axioms (2)
  • domain assumption Mocks generated under a fiducial cosmology accurately capture the cross-covariance between power spectrum, bispectrum and BAO measurements.
    Invoked when the abstract states that the joint analysis accounts for cross-covariance using mocks.
  • domain assumption ShapeFit compression removes prior-volume effects without biasing beyond-ΛCDM parameter inference.
    Stated as the method used to mitigate prior volume effects that hinder beyond-ΛCDM analyses.

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discussion (0)

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Reference graph

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