arxiv: 2404.03002 · v3 · submitted 2024-04-03 · 🌌 astro-ph.CO

Recognition: no theorem link

DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

DESI Collaboration: A. G. Adame , J. Aguilar , S. Ahlen , S. Alam , D. M. Alexander , M. Alvarez , O. Alves , A. Anand

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U. Andrade E. Armengaud S. Avila A. Aviles H. Awan B. Bahr-Kalus S. Bailey C. Baltay A. Bault J. Behera S. BenZvi A. Bera F. Beutler D. Bianchi C. Blake R. Blum S. Brieden A. Brodzeller D. Brooks E. Buckley-Geer E. Burtin R. Calderon R. Canning A. Carnero Rosell R. Cereskaite J. L. Cervantes-Cota S. Chabanier E. Chaussidon J. Chaves-Montero S. Chen X. Chen T. Claybaugh S. Cole A. Cuceu T. M. Davis K. Dawson A. de la Macorra A. de Mattia N. Deiosso A. Dey B. Dey Z. Ding P. Doel J. Edelstein S. Eftekharzadeh D. J. Eisenstein A. Elliott P. Fagrelius K. Fanning S. Ferraro J. Ereza N. Findlay B. Flaugher A. Font-Ribera D. Forero-S\'anchez J. E. Forero-Romero C. S. Frenk C. Garcia-Quintero E. Gazta\~naga H. Gil-Mar\'in S. Gontcho A Gontcho A. X. Gonzalez-Morales V. Gonzalez-Perez C. Gordon D. Green D. Gruen R. Gsponer G. Gutierrez J. Guy B. Hadzhiyska C. Hahn M. M. S Hanif H. K. Herrera-Alcantar K. Honscheid C. Howlett D. Huterer V. Ir\v{s}i\v{c} M. Ishak S. Juneau N. G. Kara\c{c}ayl{\i} R. Kehoe S. Kent D. Kirkby A. Kremin A. Krolewski Y. Lai T.-W. Lan M. Landriau D. Lang J. Lasker J.M. Le Goff L. Le Guillou A. Leauthaud M. E. Levi T. S. Li E. Linder K. Lodha C. Magneville M. Manera D. Margala P. Martini M. Maus P. McDonald L. Medina-Varela A. Meisner J. Mena-Fern\'andez R. Miquel J. Moon S. Moore J. Moustakas N. Mudur E. Mueller A. Mu\~noz-Guti\'errez A. D. Myers S. Nadathur L. Napolitano R. Neveux J. A. Newman N. M. Nguyen J. Nie G. Niz H. E. Noriega N. Padmanabhan E. Paillas N. Palanque-Delabrouille J. Pan S. Penmetsa W. J. Percival M. M. Pieri M. Pinon C. Poppett A. Porredon F. Prada A. P\'erez-Fern\'andez I. P\'erez-R\`afols D. Rabinowitz A. Raichoor C. Ram\'irez-P\'erez S. Ramirez-Solano C. Ravoux M. Rashkovetskyi M. Rezaie J. Rich A. Rocher C. Rockosi N.A. Roe A. Rosado-Marin A. J. Ross G. Rossi R. Ruggeri V. Ruhlmann-Kleider L. Samushia E. Sanchez C. Saulder E. F. Schlafly D. Schlegel M. Schubnell H. Seo A. Shafieloo R. Sharples J. Silber A. Slosar A. Smith D. Sprayberry T. Tan G. Tarl\'e P. Taylor S. Trusov L. A. Ure\~na-L\'opez R. Vaisakh D. Valcin F. Valdes M. Vargas-Maga\~na L. Verde M. Walther B. Wang M. S. Wang B. A. Weaver N. Weaverdyck R. H. Wechsler D. H. Weinberg M. White J. Yu Y. Yu S. Yuan C. Y\`eche E. A. Zaborowski P. Zarrouk H. Zhang C. Zhao R. Zhao R. Zhou T. Zhuang H. Zou

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Pith reviewed 2026-05-12 02:06 UTC · model grok-4.3

classification 🌌 astro-ph.CO

keywords baryon acoustic oscillationsDESI surveycosmological parametersdark energy equation of stateLambdaCDM modelneutrino mass sumHubble constant

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The pith

DESI baryon acoustic oscillation measurements from the first year are consistent with flat LambdaCDM but show a preference for evolving dark energy when combined with CMB or supernova data.

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

The paper measures baryon acoustic oscillations using data from the Dark Energy Spectroscopic Instrument's first year, covering galaxy, quasar, and Lyman-alpha forest tracers in seven redshift bins up to z=4.2. These measurements alone support the standard flat LambdaCDM cosmology with a matter density of 0.295 plus or minus 0.015. When combined with cosmic microwave background data from Planck, the constraints tighten to a matter density of 0.307 plus or minus 0.005 and Hubble constant of 67.97 plus or minus 0.38 km/s/Mpc. Extending the model to allow for a time-varying dark energy equation of state, the data show a 2.5 to 3.9 sigma preference for evolving dark energy depending on which supernova dataset is included. The analysis also provides upper limits on the sum of neutrino masses.

Core claim

DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate relative to the sound horizon in seven redshift bins from over 6 million objects, yielding cosmological constraints consistent with flat LambdaCDM for the baseline model while combinations with CMB and supernova data favor models with w0 greater than -1 and wa less than 0 at up to 3.9 sigma significance.

What carries the argument

Baryon acoustic oscillations extracted from galaxy, quasar and Lyman-alpha forest tracers as standard rulers to measure distance-redshift relations relative to the sound horizon.

Load-bearing premise

The BAO scale extraction assumes that standard models of galaxy bias, redshift-space distortions and reconstruction fully account for all relevant systematics without leaving significant residuals.

What would settle it

A reanalysis of the same DESI spectra using substantially different modeling of redshift-space distortions or reconstruction that shifts the reported BAO scales by more than the quoted uncertainties would falsify the cosmological constraints.

read the original abstract

We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$\alpha$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the sound horizon, in seven redshift bins from over 6 million extragalactic objects in the redshift range $0.1<z<4.2$. DESI BAO data alone are consistent with the standard flat $\Lambda$CDM cosmological model with a matter density $\Omega_\mathrm{m}=0.295\pm 0.015$. Paired with a BBN prior and the robustly measured acoustic angular scale from the CMB, DESI requires $H_0=(68.52\pm0.62)$ km/s/Mpc. In conjunction with CMB anisotropies from Planck and CMB lensing data from Planck and ACT, we find $\Omega_\mathrm{m}=0.307\pm 0.005$ and $H_0=(67.97\pm0.38)$ km/s/Mpc. Extending the baseline model with a constant dark energy equation of state parameter $w$, DESI BAO alone require $w=-0.99^{+0.15}_{-0.13}$. In models with a time-varying dark energy equation of state parametrized by $w_0$ and $w_a$, combinations of DESI with CMB or with SN~Ia individually prefer $w_0>-1$ and $w_a<0$. This preference is 2.6$\sigma$ for the DESI+CMB combination, and persists or grows when SN~Ia are added in, giving results discrepant with the $\Lambda$CDM model at the $2.5\sigma$, $3.5\sigma$ or $3.9\sigma$ levels for the addition of Pantheon+, Union3, or DES-SN5YR datasets respectively. For the flat $\Lambda$CDM model with the sum of neutrino mass $\sum m_\nu$ free, combining the DESI and CMB data yields an upper limit $\sum m_\nu < 0.072$ $(0.113)$ eV at 95% confidence for a $\sum m_\nu>0$ $(\sum m_\nu>0.059)$ eV prior. These neutrino-mass constraints are substantially relaxed in models beyond $\Lambda$CDM. [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.

Desk Editor's Note private letter to a colleague

DESI DR1 BAO release gives new seven-bin measurements from 6M+ objects that fit flat LCDM on their own but show 2.5-3.9 sigma pull to evolving DE with SN datasets.

read the letter

The key takeaway is that this paper puts out the first public DESI DR1 BAO scales in seven redshift bins from galaxies, quasars, and Lyman-alpha forest. Those specific D_M/r_d and D_H/r_d values are new and absent from earlier BOSS/eBOSS papers. On their own they sit right on flat LambdaCDM with Omega_m = 0.295 plus or minus 0.015, and when combined with Planck they tighten H0 to 67.97 plus or minus 0.38 km/s/Mpc while giving a neutrino mass limit below 0.072 eV at 95 percent under the usual prior. The analysis uses the standard template fit with linear bias, RSD, and reconstruction, which is the right choice for a data-release paper and produces internally consistent results across tracers. The w0-wa extension is where the numbers get interesting: DESI plus CMB alone prefers w0 greater than -1 and wa less than 0 at 2.6 sigma, and that grows when Pantheon+, Union3, or DES-SN5YR are added. The paper reports those levels plainly without overclaiming. The soft spot is exactly the one the stress-test flags. The cosmological posteriors rest on the extracted BAO scales being free of residual bias or reconstruction artifacts that the standard models miss. If any scale-dependent effect leaks through, it shifts the distances and can change the significance of the dark-energy deviation. The abstract notes consistency checks, but the full covariance matrices and systematic tests need to be examined closely to judge how much weight the 3-plus sigma hints deserve. This paper is for anyone who needs the latest BAO data points for their own fits or for testing Hubble tension and dark energy models. The data themselves are worth referee time even if the model extensions stay tentative. I would send it to peer review.

Referee Report

1 major / 2 minor

Summary. The manuscript reports cosmological constraints from baryon acoustic oscillation (BAO) measurements extracted from the first year of DESI observations (Data Release 1), using galaxy, quasar, and Lyman-alpha forest tracers across seven redshift bins spanning 0.1 < z < 4.2. DESI BAO data alone are consistent with flat LambdaCDM (Omega_m = 0.295 +/- 0.015); combined with BBN and Planck CMB data they yield Omega_m = 0.307 +/- 0.005 and H0 = 67.97 +/- 0.38 km/s/Mpc. Extensions to constant-w and w0-wa dark energy models show consistency with w = -1 from BAO alone but 2.5-3.9 sigma preferences for evolving dark energy (w0 > -1, wa < 0) when supernova datasets are added; neutrino mass limits are also derived.

Significance. If the BAO scale measurements hold, this work delivers the first major cosmological results from DESI, adding seven new high-precision distance and expansion-rate anchors that tighten constraints on Omega_m, H0, and dark energy evolution. The reported consistency with LambdaCDM from BAO alone, the H0 value from BBN+CMB+DESI, and the quantified tension levels in w0-wa extensions when SN data are included provide falsifiable tests that can be checked with future data releases. The neutrino-mass upper limits are competitive within the stated priors.

major comments (1)

[BAO measurement and fitting pipeline (sections describing template fits to galaxy, quasar, and Lyman-alpha tracers)] The central claims (flat LambdaCDM consistency, H0 value, and w0-wa tension levels) rest directly on the seven extracted BAO scales (D_M/r_d and D_H/r_d or their combination). The extraction pipeline uses standard linear bias, RSD modeling, and reconstruction; any unaccounted residual scale-dependent bias or reconstruction artifact would shift these scales and propagate into the posteriors. A dedicated section quantifying the impact of these assumptions (e.g., via mock-based residual tests or alternative modeling) is needed to confirm that the reported 2.5-3.9 sigma deviations are not driven by modeling choices.

minor comments (2)

[Abstract and Section 2] The abstract and main text should explicitly state the total number of objects and the precise redshift bin boundaries for each tracer to allow immediate reproducibility checks.
[Results and data tables] Covariance matrices between the seven BAO measurements and their combination with external datasets should be provided in a machine-readable format or clearly tabulated to support independent re-analyses.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and constructive recommendation. We address the single major comment below and have revised the manuscript to incorporate additional discussion of the BAO pipeline robustness.

read point-by-point responses

Referee: [BAO measurement and fitting pipeline (sections describing template fits to galaxy, quasar, and Lyman-alpha tracers)] The central claims (flat LambdaCDM consistency, H0 value, and w0-wa tension levels) rest directly on the seven extracted BAO scales (D_M/r_d and D_H/r_d or their combination). The extraction pipeline uses standard linear bias, RSD modeling, and reconstruction; any unaccounted residual scale-dependent bias or reconstruction artifact would shift these scales and propagate into the posteriors. A dedicated section quantifying the impact of these assumptions (e.g., via mock-based residual tests or alternative modeling) is needed to confirm that the reported 2.5-3.9 sigma deviations are not driven by modeling choices.

Authors: We agree that explicit quantification of modeling assumptions in the BAO extraction is important for supporting the central claims. The seven BAO scales are derived from template fits whose details and validation are presented in the companion measurement papers (DESI 2024 I-V). Those works include extensive mock-based tests for residual scale-dependent bias, reconstruction artifacts, and alternative RSD/bias modeling choices, showing that any such effects remain well below the statistical precision of the measurements. To directly address the referee's request, we have added a new dedicated subsection (Section 3.4 in the revised manuscript) that summarizes these validation results, reports the quantified residual biases on D_M/r_d and D_H/r_d, and confirms that they do not shift the extracted scales at a level capable of driving the reported 2.5-3.9 sigma preferences in the w0-wa extensions. We also briefly discuss consistency checks with alternative fitting pipelines. This addition ensures the robustness discussion is self-contained within the present paper. revision: yes

Circularity Check

0 steps flagged

DESI BAO cosmological constraints derived from new data fits with no reduction by construction

full rationale

The paper reports new BAO scale measurements (D_M/r_d, D_H/r_d) extracted from DESI galaxy, quasar and Lyman-alpha data in seven redshift bins, then fits these scales to cosmological models (flat LambdaCDM, wCDM, w0waCDM) using standard likelihoods plus independent external priors (BBN, Planck CMB). No equation or step equates a reported constraint to a quantity defined by the same fit; the measured scales are independent observables, and methodology citations to prior DESI papers describe standard bias/RSD/reconstruction templates that are externally falsifiable. This yields a minor self-citation score without load-bearing circularity.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The reported constraints rest on fitting standard cosmological models to new BAO scale measurements using external priors and the assumption that the BAO feature is correctly modeled in each tracer.

free parameters (2)

Omega_m
Matter density parameter fitted directly to DESI BAO data in the baseline flat LambdaCDM model.
w0 and wa
Dark-energy equation-of-state parameters introduced and fitted in the extended model; their posterior preference is the key extension result.

axioms (2)

domain assumption Flat spatial geometry (Omega_k = 0)
Baseline model assumption used when quoting Omega_m and H0 constraints.
domain assumption Standard BAO modeling and reconstruction for all tracers
Assumes galaxy bias, redshift-space distortions and reconstruction fully capture the observed clustering without unmodeled systematics.

pith-pipeline@v0.9.0 · 6939 in / 1541 out tokens · 79337 ms · 2026-05-12T02:06:52.743925+00:00 · methodology

discussion (0)

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