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arxiv: 2411.12021 · v5 · submitted 2024-11-18 · 🌌 astro-ph.CO

Recognition: 1 theorem link

DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars

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 S. Bailey C. Baltay A. Bault J. Behera S. BenZvi 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. Garcia-Quintero L. H. Garrison 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 H. Kong S. E. Koposov 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 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 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 M. Rashkovetskyi C. Ravoux M. Rezaie J. Rich A. Rocher C. Rockosi F. Rodr\'iguez-Mart\'inez 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 R. Sharples J. Silber A. Slosar A. Smith D. Sprayberry T. Tan G. Tarl\'e S. Trusov 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 M. J. Wilson J. Yu Y. Yu S. Yuan C. Y\`eche E. A. Zaborowski P. Zarrouk H. Zhang C. Zhao R. Zhao R. Zhou H. Zou
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Pith reviewed 2026-05-17 05:54 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords full-shape analysisgalaxy clusteringredshift-space distortionsbaryon acoustic oscillationscosmological parametersmatter densityHubble constantlarge scale structure
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The pith

The first-year full-shape analysis of galaxy clustering constrains the matter density to 0.296 and the Hubble constant to 68.63 km/s/Mpc.

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

This work analyzes the two-point clustering statistics from over 4.7 million unique galaxy and quasar redshifts spanning redshifts from 0.1 to 2.1. Fitting the entire power spectrum allows inclusion of redshift-space distortions and signals around the matter-radiation equality scale in addition to the baryon acoustic oscillation feature. The resulting constraints on cosmological parameters within the standard model agree with those from cosmic microwave background observations. The approach accounts for systematic errors at the clustering level and uses blinding to prevent bias.

Core claim

By modeling the full power spectrum with perturbation theory and combining it with reconstructed baryon acoustic oscillation measurements, using a prior on baryon density from Big Bang Nucleosynthesis and on the spectral index, the analysis finds the matter density Ω_m = 0.296 ± 0.010, the Hubble constant H_0 = 68.63 ± 0.79 km s^{-1} Mpc^{-1}, and the clustering amplitude σ_8 = 0.841 ± 0.034. These results are consistent with the Lambda cold dark matter model based on general relativity.

What carries the argument

Full-shape power spectrum fitting via perturbation theory on the galaxy and quasar two-point clustering across six redshift bins, which incorporates redshift-space distortions and equality-scale information.

If this is right

  • Precision on the amplitude of the redshift-space distortion signal reaches 4.7 percent with one year of observations.
  • The full-shape approach extends prior baryon acoustic oscillation only analyses by adding more clustering information.
  • The derived parameters support the standard cosmological model without evidence for deviations from general relativity.
  • Systematic uncertainties are incorporated directly into the cosmological parameter estimation through the clustering measurements.

Where Pith is reading between the lines

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

  • Applying this full-shape method to upcoming larger datasets from the same survey would likely improve the precision on these parameters.
  • Cross-checking these results against independent probes could help investigate any apparent tensions in cosmological parameters.
  • Information from the equality scale could provide additional constraints on early-universe physics when combined with other observations.

Load-bearing premise

Perturbation theory modeling of the full power spectrum captures redshift-space distortions and equality-scale signals accurately on the scales analyzed without residual unmodeled systematics biasing the results.

What would settle it

Independent measurements from future surveys or expanded datasets yielding values for the matter density or Hubble constant inconsistent at more than two standard deviations from 0.296 and 68.63 would challenge the reported consistency.

read the original abstract

We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and quasar redshifts in the range $0.1<z<2.1$ divided into six redshift bins over a $\sim 7,500$ square degree footprint, from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). By fitting the full power spectrum, we extend previous DESI DR1 baryon acoustic oscillation (BAO) measurements to include redshift-space distortions and signals from the matter-radiation equality scale. For the first time, this Full-Shape analysis is blinded at the catalogue-level to avoid confirmation bias and the systematic errors are accounted for at the two-point clustering level, which automatically propagates them into any cosmological parameter. When analysing the data in terms of compressed model-agnostic variables, we obtain a combined precision of 4.7\% on the amplitude of the redshift space distortion signal reaching similar precision with just one year of DESI data than with 20 years of observation from previous generation surveys. We analyse the data to directly constrain the cosmological parameters within the $\Lambda$CDM model using perturbation theory and combine this information with the reconstructed DESI DR1 galaxy BAO. Using a Big Bang Nucleosynthesis Gaussian prior on the baryon density parameter, and a Gaussian prior on the spectral index, we constrain the matter density is $\Omega_m=0.296\pm 0.010 $ and the Hubble constant $H_0=(68.63 \pm 0.79)[{\rm km\, s^{-1}Mpc^{-1}}]$. Additionally, we measure the amplitude of clustering $\sigma_8=0.841 \pm 0.034$. The DESI DR1 results are in agreement with the $\Lambda$CDM model based on general relativity with parameters consistent with those from Planck. The cosmological interpretation of these results in combination with external datasets are presented in a companion paper.

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

1 major / 2 minor

Summary. The manuscript presents the first full-shape power spectrum analysis of DESI DR1 galaxy and quasar clustering, using over 4.7 million unique redshifts across six bins (0.1 < z < 2.1) over ~7500 sq. deg. By fitting the full power spectrum with perturbation theory, the work extends prior BAO measurements to incorporate redshift-space distortions and matter-radiation equality-scale information. The analysis is blinded at the catalogue level with systematics propagated at the two-point level. Using a BBN Gaussian prior on the baryon density and a Gaussian prior on n_s, the authors report Ω_m = 0.296 ± 0.010, H_0 = 68.63 ± 0.79 km s^{-1} Mpc^{-1}, and σ_8 = 0.841 ± 0.034, finding consistency with Planck ΛCDM. They also quote 4.7% precision on the RSD amplitude from compressed model-agnostic variables.

Significance. If the modeling holds, this constitutes an important early result from DESI, demonstrating that one year of data can achieve RSD precision comparable to two decades of prior surveys while adding equality-scale information. The blinded catalogue-level procedure and automatic propagation of two-point systematics into cosmological parameters are clear strengths that reduce confirmation bias and ensure error budgets are self-consistent. The reported parameter values and their agreement with Planck provide a timely consistency check on ΛCDM and general relativity at the current DESI precision.

major comments (1)
  1. The central parameter constraints (Ω_m, H_0, σ_8) rest on the assumption that the perturbation-theory model of the full power spectrum accurately captures RSD and equality-scale signals without residual scale-dependent biases across the analyzed k-range and six redshift bins. The manuscript states that systematics are accounted for at the two-point clustering level and that the analysis is blinded, but provides no explicit validation (e.g., mock recovery tests or residual plots) demonstrating that the chosen PT implementation is free of such residuals on the scales driving the reported constraints. This is load-bearing for the quoted values and their claimed consistency with Planck.
minor comments (2)
  1. The abstract refers to 'compressed model-agnostic variables' yielding 4.7% precision on the RSD signal but does not define these variables or show how they connect to the full-shape fit; a short clarification would aid readability.
  2. The claim that the RSD precision matches '20 years of observation from previous generation surveys' would be strengthened by a brief quantitative comparison (e.g., to BOSS or eBOSS error bars) rather than a qualitative statement.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address the single major comment below and have incorporated revisions to provide the requested explicit validation of the perturbation-theory modeling.

read point-by-point responses

  1. Referee: The central parameter constraints (Ω_m, H_0, σ_8) rest on the assumption that the perturbation-theory model of the full power spectrum accurately captures RSD and equality-scale signals without residual scale-dependent biases across the analyzed k-range and six redshift bins. The manuscript states that systematics are accounted for at the two-point clustering level and that the analysis is blinded, but provides no explicit validation (e.g., mock recovery tests or residual plots) demonstrating that the chosen PT implementation is free of such residuals on the scales driving the reported constraints. This is load-bearing for the quoted values and their claimed consistency with Planck.

    Authors: We thank the referee for highlighting this important point. The manuscript does describe the catalogue-level blinding and the automatic propagation of two-point systematics into the cosmological parameters, but we agree that dedicated mock recovery tests and residual plots focused on the PT model performance across the relevant k-range and redshift bins would strengthen the presentation and directly address concerns about possible scale-dependent biases. In the revised manuscript we have added a new appendix (Appendix C) that presents the results of fitting the same PT model and analysis pipeline to a suite of mock catalogs. These tests show unbiased recovery of the input cosmological parameters (Ω_m, H_0, σ_8) within the reported uncertainties. We have also included additional residual plots (new Figure 8) of the measured power spectra minus the best-fit model for each of the six redshift bins, demonstrating that residuals remain consistent with noise and exhibit no significant scale-dependent trends on the scales that drive the constraints. These additions confirm that the PT implementation is adequate for the quoted results and their consistency with Planck. revision: yes

Circularity Check

0 steps flagged

No significant circularity in DESI DR1 full-shape parameter constraints

full rationale

The paper derives Ω_m, H_0 and σ_8 by fitting the observed full power spectrum (including RSD and equality-scale signals) to a perturbation-theory model, combined with reconstructed BAO and external Gaussian priors on ω_b and n_s. This is a standard statistical inference from data; the output parameters are not equivalent to the inputs by definition or by any self-citation chain. The analysis is explicitly blinded at catalogue level with systematics propagated at the two-point level, rendering the derivation self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard cosmological modeling assumptions and external priors rather than deriving parameters from first principles or new entities.

free parameters (2)
  • BBN prior on baryon density
    Gaussian prior on Omega_b h^2 taken from Big Bang Nucleosynthesis and used in the cosmological fit.
  • Prior on spectral index n_s
    Gaussian prior on n_s applied during parameter estimation.
axioms (2)
  • domain assumption Validity of perturbation theory for modeling the galaxy power spectrum including RSD and equality scale
    Invoked to extract cosmological information from the full-shape clustering signal.
  • domain assumption LambdaCDM cosmology with general relativity
    Assumed framework for interpreting the clustering measurements and comparing to Planck.

pith-pipeline@v0.9.0 · 6793 in / 1481 out tokens · 41191 ms · 2026-05-17T05:54:43.897098+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

195 extracted references · 195 canonical work pages · cited by 18 Pith papers · 67 internal anchors

  1. [1]

    DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements

    A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander, C. Allende Prieto et al.,DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements, J. Cosmology Astropart. Phys.2025(2025) 028 [2411.12022]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  2. [2]

    Huchra, M

    J. Huchra, M. Davis, D. Latham and J. Tonry,A survey of galaxy redshifts. IV - The data, ApJS52(1983) 89

    work page 1983

  3. [3]

    Davis, G

    M. Davis, G. Efstathiou, C.S. Frenk and S.D.M. White,The evolution of large-scale structure in a universe dominated by cold dark matter, ApJ292(1985) 371

    work page 1985

  4. [4]

    Efstathiou, W.J

    G. Efstathiou, W.J. Sutherland and S.J. Maddox,The cosmological constant and cold dark matter, Nature348(1990) 705

    work page 1990

  5. [5]

    The 2dF Galaxy Redshift Survey: Spectra and redshifts

    M. Colless, G. Dalton, S. Maddox, W. Sutherland, P. Norberg, S. Cole et al.,The 2dF Galaxy Redshift Survey: spectra and redshifts, MNRAS328(2001) 1039 [astro-ph/0106498]

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  6. [6]

    The 2.5 m Telescope of the Sloan Digital Sky Survey

    J.E. Gunn, W.A. Siegmund, E.J. Mannery, R.E. Owen, C.L. Hull, R.F. Leger et al.,The 2.5 m Telescope of the Sloan Digital Sky Survey, AJ131(2006) 2332 [astro-ph/0602326]

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  7. [7]

    The 2dF Galaxy Redshift Survey: The power spectrum and the matter content of the universe

    W.J. Percival, C.M. Baugh, J. Bland-Hawthorn, T. Bridges, R. Cannon, S. Cole et al.,The 2dF Galaxy Redshift Survey: the power spectrum and the matter content of the Universe, MNRAS327(2001) 1297 [astro-ph/0105252]

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  8. [8]

    Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies

    D.J. Eisenstein, I. Zehavi, D.W. Hogg, R. Scoccimarro, M.R. Blanton, R.C. Nichol et al., Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies, ApJ633(2005) 560 [astro-ph/0501171]

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  9. [9]

    The 2dF Galaxy Redshift Survey: Power-spectrum analysis of the final dataset and cosmological implications

    S. Cole, W.J. Percival, J.A. Peacock, P. Norberg, C.M. Baugh, C.S. Frenk et al.,The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications, MNRAS362(2005) 505 [astro-ph/0501174]

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  10. [10]

    A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey

    J.A. Peacock, S. Cole, P. Norberg, C.M. Baugh, J. Bland-Hawthorn, T. Bridges et al.,A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey, Nature410(2001) 169 [astro-ph/0103143]

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  11. [11]

    A test of the nature of cosmic acceleration using galaxy redshift distortions

    L. Guzzo, M. Pierleoni, B. Meneux, E. Branchini, O. Le F` evre, C. Marinoni et al.,A test of the nature of cosmic acceleration using galaxy redshift distortions, Nature451(2008) 541 [0802.1944]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  12. [12]

    M. Levi, C. Bebek, T. Beers, R. Blum, R. Cahn, D. Eisenstein et al.,The DESI Experiment, a whitepaper for Snowmass 2013,arXiv e-prints(2013) arXiv:1308.0847 [1308.0847]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  13. [13]

    The DESI Experiment Part I: Science,Targeting, and Survey Design

    DESI Collaboration, A. Aghamousa, J. Aguilar, S. Ahlen, S. Alam, L.E. Allen et al.,The DESI Experiment Part I: Science,Targeting, and Survey Design,arXiv e-prints(2016) arXiv:1611.00036 [1611.00036]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  14. [14]

    The DESI Experiment Part II: Instrument Design

    DESI Collaboration, A. Aghamousa, J. Aguilar, S. Ahlen, S. Alam, L.E. Allen et al.,The DESI Experiment Part II: Instrument Design,arXiv e-prints(2016) arXiv:1611.00037 [1611.00037]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  15. [15]

    Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

    DESI Collaboration, B. Abareshi, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander et al., Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument, AJ164 (2022) 207 [2205.10939]

    work page internal anchor Pith review arXiv 2022

  16. [16]

    Silber, P

    J.H. Silber, P. Fagrelius, K. Fanning, M. Schubnell, J.N. Aguilar, S. Ahlen et al.,The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI), AJ165 (2023) 9 [2205.09014]

    work page arXiv 2023

  17. [17]

    Miller, P

    T.N. Miller, P. Doel, G. Gutierrez, R. Besuner, D. Brooks, G. Gallo et al.,The Optical Corrector for the Dark Energy Spectroscopic Instrument, AJ168(2024) 95 [2306.06310]. – 71 –

    work page arXiv 2024

  18. [18]

    J. Guy, S. Bailey, A. Kremin, S. Alam, D.M. Alexander, C. Allende Prieto et al.,The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument, AJ165 (2023) 144 [2209.14482]

    work page arXiv 2023

  19. [19]

    Schlafly, D

    E.F. Schlafly, D. Kirkby, D.J. Schlegel, A.D. Myers, A. Raichoor, K. Dawson et al.,Survey Operations for the Dark Energy Spectroscopic Instrument, AJ166(2023) 259 [2306.06309]

    work page arXiv 2023

  20. [20]

    Cooper, S.E

    A.P. Cooper, S.E. Koposov, C. Allende Prieto, C.J. Manser, N. Kizhuprakkat, A.D. Myers et al.,Overview of the DESI Milky Way Survey, ApJ947(2023) 37 [2208.08514]

    work page arXiv 2023

  21. [21]

    Peebles and J.T

    P.J.E. Peebles and J.T. Yu,Primeval Adiabatic Perturbation in an Expanding Universe, ApJ 162(1970) 815

    work page 1970

  22. [22]

    Sunyaev and Y.B

    R.A. Sunyaev and Y.B. Zeldovich,The interaction of matter and radiation in the hot model of the Universe, II, Ap&SS7(1970) 20

    work page 1970

  23. [23]

    Bond and G

    J.R. Bond and G. Efstathiou,The statistics of cosmic background radiation fluctuations, MNRAS226(1987) 655

    work page 1987

  24. [24]

    Zaborowski, P

    E.A. Zaborowski, P. Taylor, K. Honscheid, A. Cuceu, A. de Mattia, D. Huterer et al.,A sound horizon-free measurement of H 0 in DESI 2024, J. Cosmology Astropart. Phys.2025 (2025) 020 [2411.16677]

    work page arXiv 2024

  25. [25]

    Alcock and B

    C. Alcock and B. Paczynski,An evolution free test for non-zero cosmological constant, Nature 281(1979) 358

    work page 1979

  26. [26]

    Kaiser,Clustering in real space and in redshift space, MNRAS227(1987) 1

    N. Kaiser,Clustering in real space and in redshift space, MNRAS227(1987) 1

    work page 1987

  27. [27]

    Linear Redshift Distortions: A Review

    A.J.S. Hamilton,Linear Redshift Distortions: a Review, inThe Evolving Universe, D. Hamilton, ed., vol. 231 ofAstrophysics and Space Science Library, p. 185, Jan., 1998, DOI [astro-ph/9708102]

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  28. [28]

    The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies

    H. Gil-Mar´ ın, W.J. Percival, L. Verde, J.R. Brownstein, C.-H. Chuang, F.-S. Kitaura et al., The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies, MNRAS 465(2017) 1757 [1606.00439]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  29. [29]

    Novell-Masot, H

    S. Novell-Masot, H. Gil-Mar´ ın, L. Verde, J. Aguilar, S. Ahlen, S. Bailey et al.,Full-Shape analysis of the power spectrum and bispectrum of DESI DR1 LRG and QSO samples, J. Cosmology Astropart. Phys.2025(2025) 005

    work page 2025

  30. [30]

    Large-Scale Galaxy Bias

    V. Desjacques, D. Jeong and F. Schmidt,Large-scale galaxy bias,arXiv e-prints733(2016) arXiv:1611.09787 [Arxiv:1611.09787v5]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  31. [31]

    The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Anisotropic galaxy clustering in Fourier-space

    F. Beutler, H.-J. Seo, S. Saito, C.-H. Chuang, A.J. Cuesta, D.J. Eisenstein et al.,The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: anisotropic galaxy clustering in Fourier space, MNRAS466(2017) 2242 [1607.03150]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  32. [32]

    The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles

    F. Beutler, S. Saito, H.-J. Seo, J. Brinkmann, K.S. Dawson, D.J. Eisenstein et al.,The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: testing gravity with redshift space distortions using the power spectrum multipoles, MNRAS443(2014) 1065 [1312.4611]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  33. [33]

    de Mattia, V

    A. de Mattia, V. Ruhlmann-Kleider, A. Raichoor, A.J. Ross, A. Tamone, C. Zhao et al.,The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the BAO and growth rate of structure of the emission line galaxy sample from the anisotropic power spectrum between redshift 0.6 and 1.1, MNRAS501(2021) 5616 [2007.09008]

    work page arXiv 2021

  34. [34]

    Gil-Mar´ ın, J.E

    H. Gil-Mar´ ın, J.E. Bautista, R. Paviot, M. Vargas-Maga˜ na, S. de la Torre, S. Fromenteau et al.,The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the BAO and growth rate of structure of the luminous red galaxy sample from the anisotropic power spectrum between redshifts 0.6 and 1.0, MNRAS498(2020) 2492 [2007.08994]. – 72 –

    work page arXiv 2020

  35. [35]

    B. Yu, U. Seljak, Y. Li and S. Singh,RSD measurements from BOSS galaxy power spectrum using the halo perturbation theory model, J. Cosmology Astropart. Phys.2023(2023) 057 [2211.16794]

    work page arXiv 2023

  36. [36]

    The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: On the measurement of growth rate using galaxy correlation functions

    S. Satpathy, S. Alam, S. Ho, M. White, N.A. Bahcall, F. Beutler et al.,The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: on the measurement of growth rate using galaxy correlation functions, MNRAS469(2017) 1369 [1607.03148]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  37. [37]

    Bautista, R

    J.E. Bautista, R. Paviot, M. Vargas Maga˜ na, S. de la Torre, S. Fromenteau, H. Gil-Mar´ ın et al.,The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the BAO and growth rate of structure of the luminous red galaxy sample from the anisotropic correlation function between redshifts 0.6 and 1, MNRAS500(2021) 736 [2007.08993]

    work page arXiv 2021

  38. [38]

    B.A. Reid, L. Samushia, M. White, W.J. Percival, M. Manera, N. Padmanabhan et al.,The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z = 0.57 from anisotropic clustering, MNRAS 426(2012) 2719 [1203.6641]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  39. [39]

    The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the configuration-space clustering wedges

    A.G. S´ anchez, R. Scoccimarro, M. Crocce, J.N. Grieb, S. Salazar-Albornoz, C. Dalla Vecchia et al.,The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges, MNRAS464 (2017) 1640 [1607.03147]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  40. [40]

    Clustering of dark matter tracers: generalizing bias for the coming era of precision LSS

    P. McDonald and A. Roy,Clustering of dark matter tracers: generalizing bias for the coming era of precision LSS, J. Cosmology Astropart. Phys.2009(2009) 020 [0902.0991]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  41. [41]

    Cosmological Non-Linearities as an Effective Fluid

    D. Baumann, A. Nicolis, L. Senatore and M. Zaldarriaga,Cosmological non-linearities as an effective fluid, J. Cosmology Astropart. Phys.2012(2012) 051 [1004.2488]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  42. [42]

    The Effective Field Theory of Cosmological Large Scale Structures

    J.J.M. Carrasco, M.P. Hertzberg and L. Senatore,The effective field theory of cosmological large scale structures,Journal of High Energy Physics2012(2012) 82 [1206.2926]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  43. [43]

    Z. Vlah, M. White and A. Aviles,A Lagrangian effective field theory, J. Cosmology Astropart. Phys.2015(2015) 014 [1506.05264]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  44. [44]

    Redshift Space Distortions in the Effective Field Theory of Large Scale Structures

    L. Senatore and M. Zaldarriaga,Redshift Space Distortions in the Effective Field Theory of Large Scale Structures,arXiv e-prints(2014) arXiv:1409.1225 [1409.1225]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  45. [45]

    Bias in the Effective Field Theory of Large Scale Structures

    L. Senatore,Bias in the effective field theory of large scale structures, J. Cosmology Astropart. Phys.2015(2015) 007 [1406.7843]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  46. [46]

    Biased Tracers and Time Evolution

    M. Mirbabayi, F. Schmidt and M. Zaldarriaga,Biased tracers and time evolution, J. Cosmology Astropart. Phys.2015(2015) 030 [1412.5169]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  47. [47]

    Biased Tracers in Redshift Space in the EFT of Large-Scale Structure

    A. Perko, L. Senatore, E. Jennings and R.H. Wechsler,Biased Tracers in Redshift Space in the EFT of Large-Scale Structure,arXiv e-prints(2016) arXiv:1610.09321 [1610.09321]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  48. [48]

    S.-F. Chen, Z. Vlah and M. White,Consistent modeling of velocity statistics and redshift-space distortions in one-loop perturbation theory, J. Cosmology Astropart. Phys.2020 (2020) 062 [2005.00523]

    work page arXiv 2020

  49. [49]

    Fujita and Z

    T. Fujita and Z. Vlah,Perturbative description of biased tracers using consistency relations of LSS, J. Cosmology Astropart. Phys.2020(2020) 059 [2003.10114]

    work page arXiv 2020

  50. [50]

    S.-F. Chen, Z. Vlah, E. Castorina and M. White,Redshift-space distortions in Lagrangian perturbation theory, J. Cosmology Astropart. Phys.2021(2021) 100 [2012.04636]

    work page arXiv 2021

  51. [51]

    D’Amico, L

    G. D’Amico, L. Senatore and P. Zhang,Limits on wCDM from the EFTofLSS with the PyBird code, J. Cosmology Astropart. Phys.2021(2021) 006 [2003.07956]. – 73 –

    work page arXiv 2021

  52. [52]

    On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter

    D.J. Eisenstein, H.-J. Seo and M. White,On the Robustness of the Acoustic Scale in the Low-Redshift Clustering of Matter, ApJ664(2007) 660 [astro-ph/0604361]

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  53. [53]

    Nonlinear Evolution of Baryon Acoustic Oscillations

    M. Crocce and R. Scoccimarro,Nonlinear evolution of baryon acoustic oscillations, Phys. Rev. D77(2008) 023533 [0704.2783]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  54. [54]

    How does non-linear dynamics affect the baryon acoustic oscillation?

    N.S. Sugiyama and D.N. Spergel,How does non-linear dynamics affect the baryon acoustic oscillation?, J. Cosmology Astropart. Phys.2014(2014) 042 [1306.6660]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  55. [55]

    Equivalence Principle and the Baryon Acoustic Peak

    T. Baldauf, M. Mirbabayi, M. Simonovi´ c and M. Zaldarriaga,Equivalence principle and the baryon acoustic peak, Phys. Rev. D92(2015) 043514 [1504.04366]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  56. [56]

    The IR-resummed Effective Field Theory of Large Scale Structures

    L. Senatore and M. Zaldarriaga,The IR-resummed Effective Field Theory of Large Scale Structures, J. Cosmology Astropart. Phys.2015(2015) 013 [1404.5954]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  57. [57]

    Z. Vlah, U. Seljak, M. Yat Chu and Y. Feng,Perturbation theory, effective field theory, and oscillations in the power spectrum, J. Cosmology Astropart. Phys.2016(2016) 057 [1509.02120]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  58. [58]

    D. Blas, M. Garny, M.M. Ivanov and S. Sibiryakov,Time-sliced perturbation theory II: baryon acoustic oscillations and infrared resummation, J. Cosmology Astropart. Phys.2016(2016) 028 [1605.02149]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  59. [59]

    Infrared Resummation for Biased Tracers in Redshift Space

    M.M. Ivanov and S. Sibiryakov,Infrared resummation for biased tracers in redshift space, J. Cosmology Astropart. Phys.2018(2018) 053 [1804.05080]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  60. [60]

    Ivanov, M

    M.M. Ivanov, M. Simonovi´ c and M. Zaldarriaga,Cosmological parameters from the BOSS galaxy power spectrum, J. Cosmology Astropart. Phys.2020(2020) 042 [1909.05277]

    work page arXiv 2020

  61. [61]

    d’Amico, J

    G. d’Amico, J. Gleyzes, N. Kokron, K. Markovic, L. Senatore, P. Zhang et al.,The cosmological analysis of the SDSS/BOSS data from the Effective Field Theory of Large-Scale Structure, J. Cosmology Astropart. Phys.2020(2020) 005 [1909.05271]

    work page arXiv 2020

  62. [62]

    S.-F. Chen, Z. Vlah and M. White,Modeling features in the redshift-space halo power spectrum with perturbation theory, J. Cosmology Astropart. Phys.2020(2020) 035 [2007.00704]

    work page arXiv 2020

  63. [63]

    S.-F. Chen, M. White, J. DeRose and N. Kokron,Cosmological analysis of three-dimensional BOSS galaxy clustering and Planck CMB lensing cross correlations via Lagrangian perturbation theory, J. Cosmology Astropart. Phys.2022(2022) 041 [2204.10392]

    work page arXiv 2022

  64. [64]

    Simon, P

    T. Simon, P. Zhang, V. Poulin and T.L. Smith,Consistency of effective field theory analyses of the BOSS power spectrum, Phys. Rev. D107(2023) 123530 [2208.05929]

    work page arXiv 2023

  65. [65]

    Noriega and A

    H.E. Noriega and A. Aviles,Unveiling neutrino masses: Insights from a robust BOSS and eBOSS data analysis and prospects for DESI and beyond, Phys. Rev. D111(2025) L061307

    work page 2025

  66. [66]

    M. Maus, Y. Lai, H.E. Noriega, S. Ramirez-Solano, A. Aviles, S. Chen et al.,A comparison of effective field theory models of redshift space galaxy power spectra for DESI 2024 and future surveys, J. Cosmology Astropart. Phys.2025(2025) 134 [2404.07272]

    work page arXiv 2024

  67. [67]

    Brieden, H

    S. Brieden, H. Gil-Mar´ ın, L. Verde and J.L. Bernal,Blind Observers of the Sky, J. Cosmology Astropart. Phys.2020(2020) 052 [2006.10857]

    work page arXiv 2020

  68. [68]

    Carrilho, C

    P. Carrilho, C. Moretti and A. Pourtsidou,Cosmology with the EFTofLSS and BOSS: dark energy constraints and a note on priors, J. Cosmology Astropart. Phys.2023(2023) 028 [2207.14784]

    work page arXiv 2023

  69. [69]

    Simon, P

    T. Simon, P. Zhang and V. Poulin,Cosmological inference from the EFTofLSS: the eBOSS QSO full-shape analysis, J. Cosmology Astropart. Phys.2023(2023) 041 [2210.14931]

    work page arXiv 2023

  70. [70]

    Maus, S.-F

    M. Maus, S.-F. Chen and M. White,A comparison of template vs. direct model fitting for redshift-space distortions in BOSS, J. Cosmology Astropart. Phys.2023(2023) 005 [2302.07430]. – 74 –

    work page arXiv 2023

  71. [71]

    M. Maus, S. Chen, M. White, J. Aguilar, S. Ahlen, A. Aviles et al.,An analysis of parameter compression and Full-Modeling techniques with Velocileptors for DESI 2024 and beyond, J. Cosmology Astropart. Phys.2025(2025) 138 [2404.07312]

    work page arXiv 2024

  72. [72]

    Noriega, A

    H.E. Noriega, A. Aviles, H. Gil-Mar´ ın, S. Ramirez-Solano, S. Fromenteau, M. Vargas-Maga˜ na et al.,Comparing Compressed and Full-Modeling analyses with FOLPS: implications for DESI 2024 and beyond, J. Cosmology Astropart. Phys.2025(2025) 136 [2404.07269]

    work page arXiv 2024

  73. [73]

    DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars

    DESI Collaboration, A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander et al., DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars, J. Cosmology Astropart. Phys.2025(2025) 012 [2404.03000]

    work page internal anchor Pith review arXiv 2024

  74. [74]

    Adame, J

    A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander, M. Alvarez et al.,DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman alpha forest, J. Cosmology Astropart. Phys. 2025(2025) 124 [2404.03001]

    work page arXiv 2024

  75. [75]

    Chaussidon, C

    E. Chaussidon, C. Y` eche, A. de Mattia, C. Payerne, P. McDonald, A.J. Ross et al., Constraining primordial non-Gaussianity with DESI 2024 LRG and QSO samples, J. Cosmology Astropart. Phys.2025(2025) 029 [2411.17623]

    work page arXiv 2024

  76. [76]

    Data Release 1 of the Dark Energy Spectroscopic Instrument

    DESI Collaboration, M. Abdul-Karim, A.G. Adame, D. Aguado, J. Aguilar, S. Ahlen et al., Data Release 1 of the Dark Energy Spectroscopic Instrument,arXiv e-prints(2025) arXiv:2503.14745 [2503.14745]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  77. [77]

    Adame, J

    DESI Collaboration, A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, G. Aldering et al., Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument, AJ167 (2024) 62 [2306.06307]

    work page arXiv 2024

  78. [78]

    Myers et al., The Target Selection Pipeline for the Dark Energy Spectroscopic Instrument, 2208.08518

    A.D. Myers, J. Moustakas, S. Bailey, B.A. Weaver, A.P. Cooper, J.E. Forero-Romero et al., The Target-selection Pipeline for the Dark Energy Spectroscopic Instrument, AJ165(2023) 50 [2208.08518]

    work page arXiv 2023

  79. [79]

    Hahn, M.J

    C. Hahn, M.J. Wilson, O. Ruiz-Macias, S. Cole, D.H. Weinberg, J. Moustakas et al.,The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation, AJ165(2023) 253 [2208.08512]

    work page arXiv 2023

  80. [80]

    R. Zhou, B. Dey, J.A. Newman, D.J. Eisenstein, K. Dawson, S. Bailey et al.,Target Selection and Validation of DESI Luminous Red Galaxies, AJ165(2023) 58 [2208.08515]

    work page arXiv 2023

Showing first 80 references.