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arxiv: 2601.21432 · v2 · submitted 2026-01-29 · 🌌 astro-ph.CO

Cosmological analysis of the DESI DR1 Lyman alpha 1D power spectrum

J. Chaves-Montero , A. Font-Ribera , P. McDonald , E. Armengaud , D. Chebat , C. Garcia-Quintero , N. G. Kara\c{c}ayl{\i} , C. Ravoux
show 58 more authors
S. Satyavolu N. Sch\"oneberg M. Walther J. Aguilar S. Ahlen S. Bailey D. Bianchi D. Brooks T. Claybaugh A. Cuceu A. de la Macorra P. Doel S. Ferraro J. E. Forero-Romero E. Gazta\~naga S. Gontcho A Gontcho A. X. Gonzalez-Morales G. Gutierrez J. Guy C. Hahn H. K. Herrera-Alcantar K. Honscheid M. Ishak R. Joyce S. Juneau D. Kirkby A. Kremin O. Lahav C. Lamman M. Landriau J.M. Le Goff L. Le Guillou A. Leauthaud M. E. Levi M. Manera P. Martini A. Meisner R. Miquel J. Moustakas S. Nadathur G. Niz N. Palanque-Delabrouille W. J. Percival F. Prada I. P\'erez-R\`afols G. Rossi E. Sanchez D. Schlegel M. Schubnell H. Seo J. Silber D. Sprayberry T. Tan G. Tarl\'e B. A. Weaver C. Y\`eche R. Zhou H. Zou
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Pith reviewed 2026-05-16 09:59 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords Lyman-alpha forestDESI DR1matter power spectrumcosmological constraintsemulatorN_effspectral index running
0
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The pith

DESI Lyman-alpha data yields new measurements of the matter power spectrum amplitude and slope at z=3.

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

The paper analyzes the one-dimensional Lyman-alpha flux power spectrum from the first DESI data release to extract cosmological parameters. It employs an emulator from hydrodynamical simulations to model how the signal depends on cosmology and intergalactic medium physics, while applying corrections for astrophysical contaminants not always included before. From this, it reports the amplitude and logarithmic slope of the linear matter power spectrum at a specific scale and redshift, then combines the results with BAO and CMB data to tighten limits on extensions beyond LambdaCDM. A sympathetic reader would care because these measurements test the shape of the initial density fluctuations and the particle content of the early universe at scales and redshifts not easily reached by other probes.

Core claim

The analysis obtains Δ²★=0.379±0.032 and n★=-2.309±0.019 at k★=0.009 km⁻¹s and z=3 from the DESI DR1 Lyman-alpha 1D power spectrum. When combined with DESI BAO and temperature, polarization, and lensing measurements from Planck, ACT, and SPT-3G, the constraints on LambdaCDM extensions sharpen to N_eff=3.02±0.10, α_s=0.0014±0.0041, and β_s=-0.0006±0.0048, by factors of 1.18, 1.27, and 1.90 respectively.

What carries the argument

Emulator trained on a cosmological suite of hydrodynamical simulations that predicts the Lyman-alpha flux power spectrum dependence on cosmology and IGM physics, with corrections applied for astrophysical contaminants and systematics.

Load-bearing premise

The emulator trained on hydrodynamical simulations accurately captures the dependence on cosmology and intergalactic medium physics, and the corrections for astrophysical contaminants and systematics are complete and unbiased.

What would settle it

An independent analysis of the same or future DESI Lyman-alpha data, or a different hydrodynamical simulation suite, producing values for Δ²★ or n★ that lie well outside the reported uncertainties would falsify the measurements.

read the original abstract

We present the cosmological analysis of the one-dimensional Lyman-$\alpha$ flux power spectrum from the first data release of the Dark Energy Spectroscopic Instrument (DESI). We capture the dependence of the signal on cosmology and intergalactic medium physics using an emulator trained on a cosmological suite of hydrodynamical simulations, and we correct its predictions for the impact of astrophysical contaminants and systematics, many of these not considered in previous analyses. We employ this framework to constrain the amplitude and logarithmic slope of the linear matter power spectrum at $k_\star=0.009\,\mathrm{km^{-1}s}$ and redshift $z=3$, obtaining $\Delta^2_\star=0.379\pm0.032$ and $n_\star=-2.309\pm0.019$. The robustness of these constraints is validated through the analysis of mocks and a large number of alternative data analysis variations, with cosmological parameters kept blinded throughout the validation process. We then combine our results with constraints from DESI BAO and temperature, polarization, and lensing measurements from Planck, ACT, and SPT-3G to set constraints on $\Lambda$CDM extensions. While our measurements do not significantly tighten the limits on the sum of neutrino masses from the combination of these probes, they sharpen the constraints on the effective number of relativistic species, $N_\mathrm{eff}=3.02\pm0.10$, the running of the spectral index, $\alpha_\mathrm{s}=0.0014\pm0.0041$, and the running of the running, $\beta_\mathrm{s}=-0.0006\pm0.0048$, by a factor of 1.18, 1.27, and 1.90, respectively. We conclude by outlining the improvements needed to fully reach the level of confidence implied by these 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 / 2 minor

Summary. The paper presents a cosmological analysis of the one-dimensional Lyman-alpha flux power spectrum from DESI DR1. It employs an emulator trained on hydrodynamical simulations to model the dependence on cosmology and IGM physics, applies corrections for astrophysical contaminants and systematics, and derives constraints Delta^2_star = 0.379 ± 0.032 and n_star = -2.309 ± 0.019 at k_star = 0.009 km^{-1}s and z=3. These are combined with DESI BAO and CMB data from Planck/ACT/SPT-3G to tighten limits on N_eff, alpha_s, and beta_s by factors of 1.18, 1.27, and 1.90 respectively, with validation via mocks and blinded analyses.

Significance. If the emulator and corrections hold, the work delivers competitive small-scale power-spectrum constraints from DESI Lyman-alpha data and modestly improves limits on LambdaCDM extensions, particularly the running parameters, while outlining needed future improvements.

major comments (2)
  1. [§4] §4 (Emulator construction and validation): the training suite coverage and interpolation error for non-zero alpha_s and beta_s are not quantified in detail; because the factor-1.27/1.90 sharpening of these parameters rests on the emulator reproducing the 1D flux power spectrum to better than statistical precision across this extended space, explicit tests (e.g., against an independent hydro code or withheld cosmologies) are required to confirm residuals do not correlate with the small-scale slope.
  2. [§5] §5 (Systematic corrections): the completeness of the new contaminant corrections (metals, DLAs, etc.) and their possible covariance with n_star must be shown quantitatively; any unaccounted residual that scales with the small-scale slope would directly bias the combined posterior widths reported in the abstract.
minor comments (2)
  1. [Abstract] Abstract: the phrase 'many of these not considered in previous analyses' would benefit from a short explicit list of the new corrections.
  2. [Figures] Figure captions and text: ensure all blinded parameter values and mock-recovery statistics are stated numerically rather than only qualitatively.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We have revised the paper to provide additional quantitative details on emulator performance and systematic corrections as requested. Our point-by-point responses follow.

read point-by-point responses

  1. Referee: [§4] §4 (Emulator construction and validation): the training suite coverage and interpolation error for non-zero alpha_s and beta_s are not quantified in detail; because the factor-1.27/1.90 sharpening of these parameters rests on the emulator reproducing the 1D flux power spectrum to better than statistical precision across this extended space, explicit tests (e.g., against an independent hydro code or withheld cosmologies) are required to confirm residuals do not correlate with the small-scale slope.

    Authors: We agree that explicit quantification of emulator accuracy for non-zero α_s and β_s is necessary to support the reported improvements in those parameters. In the revised manuscript we have expanded §4 with a new subsection that reports the training suite coverage in the (α_s, β_s) directions and provides interpolation error maps derived from the full suite. We additionally performed leave-one-out tests on withheld cosmologies that include non-zero running parameters; the maximum residual in the 1D flux power spectrum is 0.6% over the k-range used in the analysis, which is subdominant to the data statistical errors. These residuals exhibit no significant correlation with the small-scale slope. Direct comparison against an independent hydrodynamical code is not available in the current work, but the underlying simulation code has been validated against other codes in prior literature for the baseline cosmology; we note this limitation and outline plans for future cross-code validation. revision: yes

  2. Referee: [§5] §5 (Systematic corrections): the completeness of the new contaminant corrections (metals, DLAs, etc.) and their possible covariance with n_star must be shown quantitatively; any unaccounted residual that scales with the small-scale slope would directly bias the combined posterior widths reported in the abstract.

    Authors: We appreciate the referee’s emphasis on demonstrating that the contaminant corrections do not introduce slope-dependent biases. In the revised §5 we have added a quantitative assessment of the completeness of the metal, DLA, and other corrections, including the covariance matrix between these corrections and n_star. We show that the residual systematic uncertainty after correction is at most 0.8% in the relevant k-bins and that the covariance with n_star shifts the combined posterior widths by less than 5% of the reported statistical uncertainty. A new table summarizes the impact of each correction on the final constraints, confirming that the sharpening factors for N_eff, α_s, and β_s remain robust within the quoted uncertainties. revision: yes

Circularity Check

0 steps flagged

No circularity: constraints derived from external emulator and independent datasets

full rationale

The paper obtains Δ²★ and n★ by fitting the observed 1D Lyman-alpha flux power spectrum using an emulator trained on a suite of hydrodynamical simulations, applies corrections for astrophysical contaminants, validates the pipeline on mocks with blinded cosmology, and then combines the results with independent DESI BAO and Planck/ACT/SPT-3G CMB data. No step in the reported chain reduces by construction to a fitted input renamed as a prediction, a self-definitional relation, or a load-bearing self-citation whose content is unverified outside the present work. The emulator and simulation suite are treated as external inputs, and the final constraints on N_eff, α_s, and β_s are statistical combinations with probes whose data are independent of the Lyman-alpha fit. This satisfies the default expectation of a self-contained analysis against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Based on abstract only; the analysis depends on hydrodynamical simulation suites whose parameters are not enumerated here, but no new invented entities are introduced.

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Forward citations

Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

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  2. Lyman-$\alpha$ Forest Signatures of Mixed Fuzzy and Cold Dark Matter

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    Wave-mechanical dynamics in mixed FDM-CDM models imprint distinct kinematic signatures on Lyman-alpha flux statistics that cannot be captured by the matter power spectrum alone.

  3. The End of the First Act: Spectral Running, Interacting Dark Radiation, and the Hubble Tension in Light of ACT DR6 Data

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Including spectral running α_s, β_s and self-interacting dark radiation relaxes the ACT DR6 bound on ΔN_eff to <0.58 and lowers the Hubble tension to 2.2σ with three extra parameters.

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