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arxiv: 2604.14504 · v1 · submitted 2026-04-16 · 🌌 astro-ph.CO

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Forecasting neutrino mass constraints from the Nancy Grace Roman Space Telescope

Francesco Spezzati , Yun Wang , Andrew Hearin
Authors on Pith no claims yet

Pith reviewed 2026-05-10 10:41 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords neutrino massRoman Space Telescopegalaxy power spectrumcosmological forecastslarge-scale structureH-alpha galaxiesEFT of LSSmodel-independent analysis
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The pith

Roman Space Telescope forecasts limit neutrino mass sum below 0.28 eV from galaxy clustering.

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

The paper forecasts the ability of the Nancy Grace Roman Space Telescope to measure the total mass of neutrinos by analyzing the clustering of galaxies it will observe across a wide sky area. Simulated catalogs of hydrogen emission-line galaxies are used to test two approaches: one that assumes the standard Lambda CDM cosmology and incorporates priors from other data, and another that remains independent of any specific background model. These methods extract information from the full shape of the galaxy power spectrum multipoles to derive upper bounds on neutrino mass while also recovering expansion and growth parameters. The results indicate that Roman observations can deliver constraints competitive with other major surveys and help test how neutrinos influence the large-scale structure of the universe.

Core claim

Using full-shape analyses of the galaxy power spectrum multipoles from simulated lightcone mock catalogs of H-alpha emission-line galaxies over 2400 square degrees and 0.5 < z < 2, the Lambda CDM analysis yields m_nu < 0.380 eV (0.162 eV) at 95% (68%) C.L. with BBN prior and broad n_s prior, tightening to m_nu < 0.276 eV (0.121 eV) with added Planck priors on omega_b, omega_cdm, and n_s; the same data also constrain H0 to 1.3%, Omega_m to 4.3%, and sigma_8 to 2.9%. The model-independent phenomenological approach recovers unbiased measurements of angular diameter distance, Hubble parameter, and growth of structure across redshift bins and produces m_nu < 0.63 eV (0.36 eV) at 95% (68%) C.L. in

What carries the argument

Full-shape analysis of galaxy power spectrum multipoles from simulated H-alpha galaxy lightcone mocks, performed via Effective Field Theory of Large-Scale Structure within Lambda CDM and via a model-independent phenomenological framework that fits angular diameter distance, Hubble parameter, and growth without assuming a background cosmology.

If this is right

  • Roman data will constrain the Hubble constant to 1.3 percent precision, matter density to 4.3 percent, and sigma_8 to 2.9 percent.
  • The sum of neutrino masses will be bounded at the level of 0.12 eV at 68 percent C.L. in the standard model when external priors are included.
  • Unbiased measurements of angular diameter distance, Hubble parameter, and structure growth can be obtained across multiple redshift bins without assuming Lambda CDM.
  • The resulting neutrino mass limits are comparable in strength to those expected from other Stage IV galaxy surveys.

Where Pith is reading between the lines

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

  • These forecasts suggest that Roman measurements could be combined with CMB data to further tighten neutrino mass bounds and help address existing tensions in Hubble constant or sigma_8 values.
  • The model-independent method opens a route to detect possible deviations from standard cosmology directly in the clustering statistics.
  • Tighter neutrino mass limits from such surveys would narrow the allowed range for extensions of particle physics models involving massive neutrinos.

Load-bearing premise

The simulated lightcone mock catalogs must accurately reproduce the real properties, selection effects, and clustering of H-alpha galaxies in the actual Roman High Latitude Wide Area Spectroscopic Survey.

What would settle it

Analysis of real Roman telescope data yielding neutrino mass upper limits that differ substantially from the forecasted values of 0.276 eV or 0.63 eV at 68 percent C.L., or showing biased recovery of distance and growth parameters.

Figures

Figures reproduced from arXiv: 2604.14504 by Andrew Hearin, Francesco Spezzati, Yun Wang.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Measurements of the monopoles and quadrupoles of the galaxy power spectrum for the Roman mock, for the [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Posteriors of cosmological parameters obtained [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Posteriors means and 1 [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: Cosmological parameters posteriors for the [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
read the original abstract

We present realistic forecasts for the constraining power of the Nancy Grace Roman Space Telescope on fundamental cosmological parameters, with particular emphasis on the absolute neutrino mass scale, using full-shape analyzes of the galaxy power spectrum. We analyze simulated lightcone mock catalogs of H$\alpha$ emission-line galaxies spanning the redshift range $0.5 < z < 2$ over $2400\ \mathrm{deg}^2$, designed to reproduce the expected properties of the Roman High Latitude Wide Area Spectroscopic Survey. We perform parameter inference on the galaxy power spectrum multipoles using two complementary theoretical frameworks: a model-dependent approach based on the Effective Field Theory of Large-Scale Structure (EFT of LSS) within $\Lambda$CDM, and a model-independent phenomenological approach that makes no assumptions about the background cosmological model. In the $\Lambda$CDM analysis, we find $m_\nu < 0.380(0.162)\ \mathrm{eV}$ at $95(68)\%$ C.L. using Big Bang Nucleosynthesis (BBN) prior and a broad prior on $n_s$, which tightens to $m_\nu < 0.276(0.121)\ \mathrm{eV}$ when Planck priors on $\omega_b$, $\omega_\mathrm{cdm}$, and $n_s$ are added. Our forecasts show that Roman can additionally constrain $H_0$, $\Omega_m$, and $\sigma_8$ with precisions of $1.3\%$, $4.3\%$, and $2.9\%$ in line with Stage IV galaxy survey measurements and forecasts. In the model-independent analysis, we demonstrate that the phenomenological model can robustly recover unbiased measurements of the angular diameter distance, the Hubble parameter, and the growth of structure across all redshift bins, in the same range of scales as the EFT model, and obtain $m_\nu < 0.63(0.36)\ \mathrm{eV}$ at $95(68)\%$ C.L. when Planck priors are included.

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 manuscript presents forecasts for neutrino mass constraints from the Nancy Grace Roman Space Telescope's High Latitude Wide Area Spectroscopic Survey, using full-shape power spectrum multipole analysis of simulated Hα emission-line galaxy lightcone mocks spanning 0.5 < z < 2 over 2400 deg². It applies both an EFT-of-LSS model within ΛCDM (reporting m_ν < 0.380(0.162) eV at 95(68)% CL with BBN prior on ω_b and broad n_s prior, tightening to < 0.276(0.121) eV with added Planck priors) and a model-independent phenomenological approach (recovering unbiased DA(z), H(z), fσ8 and yielding m_ν < 0.63(0.36) eV with Planck priors), while also forecasting 1.3%, 4.3%, and 2.9% precision on H0, Ωm, and σ8.

Significance. If the mocks faithfully reproduce the survey's selection, redshift distribution, and clustering, the results would offer useful benchmarks for Roman's expected contribution to neutrino mass constraints alongside other Stage IV surveys, with the model-independent recovery providing a valuable cross-check on robustness without background cosmology assumptions.

major comments (2)
  1. [Mock catalog construction and validation] The central m_ν forecasts and parameter precisions are load-bearing on the fidelity of the simulated lightcone mock catalogs in reproducing the expected Hα luminosity function, completeness, redshift errors, scale-dependent bias, and clustering over 0.5 < z < 2. The manuscript should include quantitative validation (e.g., comparisons of monopole/quadrupole amplitudes or power spectrum residuals) to confirm the mocks match the Roman survey properties; without this, the reported limits such as m_ν < 0.380 eV cannot be considered fully reliable.
  2. [Power spectrum analysis and covariance estimation] The analysis applies specific scale cuts to the power spectrum multipoles and estimates the covariance from the mocks, but details on the exact k-range, justification for EFT validity, and covariance construction (including shot noise and fiber-collision effects) are insufficiently specified. These choices directly affect the posterior widths on m_ν, H0, Ωm, and σ8, and require explicit tests for robustness.
minor comments (2)
  1. [Abstract] The abstract could more clearly state the number of redshift bins used and the precise survey footprint to aid quick assessment of the forecast scope.
  2. [Notation and priors] Notation for parameters (e.g., ω_b, ω_cdm, n_s) and priors should be consistently defined and cross-referenced between text, tables, and figures.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their detailed and constructive feedback on our manuscript forecasting neutrino mass constraints from the Roman Space Telescope. We address each of the major comments below and have revised the manuscript accordingly to enhance its clarity and robustness.

read point-by-point responses

  1. Referee: [Mock catalog construction and validation] The central m_ν forecasts and parameter precisions are load-bearing on the fidelity of the simulated lightcone mock catalogs in reproducing the expected Hα luminosity function, completeness, redshift errors, scale-dependent bias, and clustering over 0.5 < z < 2. The manuscript should include quantitative validation (e.g., comparisons of monopole/quadrupole amplitudes or power spectrum residuals) to confirm the mocks match the Roman survey properties; without this, the reported limits such as m_ν < 0.380 eV cannot be considered fully reliable.

    Authors: We acknowledge the importance of providing explicit validation for the mock catalogs to support the reliability of our forecasts. While the mocks were designed to reproduce the survey's Hα luminosity function, completeness, and clustering properties as detailed in the methods, we agree that quantitative comparisons were not sufficiently highlighted. In the revised manuscript, we will add a dedicated subsection presenting comparisons of the mock power spectrum multipoles (monopole and quadrupole) to theoretical expectations or survey requirements, including residuals and agreement metrics over the relevant scales and redshifts. This addition will directly address the concern and bolster confidence in the reported neutrino mass limits. revision: yes

  2. Referee: [Power spectrum analysis and covariance estimation] The analysis applies specific scale cuts to the power spectrum multipoles and estimates the covariance from the mocks, but details on the exact k-range, justification for EFT validity, and covariance construction (including shot noise and fiber-collision effects) are insufficiently specified. These choices directly affect the posterior widths on m_ν, H0, Ωm, and σ8, and require explicit tests for robustness.

    Authors: We appreciate this comment on the need for greater specificity in our analysis methodology. The scale cuts were set to k_max = 0.2 h Mpc^{-1} to remain within the regime where the EFT of LSS is valid, based on convergence tests from prior literature. The covariance matrix is computed directly from the ensemble of mock realizations, which inherently includes shot noise contributions, and fiber collisions are accounted for in the mock generation pipeline. To improve the manuscript, we will expand the 'Analysis' section with explicit statements of the k-range used (0.01 < k < 0.2 h/Mpc), additional justification for the EFT validity including references to perturbation theory scales, and a more detailed description of the covariance estimation procedure. We will also include a robustness test by varying the scale cuts and showing the impact on parameter constraints. revision: yes

Circularity Check

0 steps flagged

No significant circularity: forecasts are derived outputs from mock fitting, not inputs by construction

full rationale

The paper generates simulated lightcone mocks to match expected Roman Hα survey properties, measures power spectrum multipoles, and fits them with EFT-of-LSS (within ΛCDM) or a model-independent phenomenological framework to obtain neutrino mass upper limits and other parameter constraints. These bounds (e.g., m_ν < 0.380 eV at 95% CL) are statistical outputs of the inference step rather than equivalent to any input by definition or renaming. The model-independent recovery of DA(z), H(z), and fσ8 is presented as validation of unbiased recovery on the same mocks, but does not reduce the central claims to self-definition or fitted inputs called predictions. No self-citation chains, uniqueness theorems, or ansatzes are invoked in a load-bearing way that collapses the derivation. The analysis remains self-contained against external benchmarks of mock fidelity and survey expectations.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The forecasts rest on standard cosmological modeling assumptions and mock generation techniques drawn from prior literature, without introducing new free parameters beyond the usual cosmological ones or new entities.

free parameters (2)
  • BBN prior on ω_b
    Used as a prior in the ΛCDM analysis to help constrain neutrino mass.
  • Planck priors on ω_b, ω_cdm, n_s
    Added in tighter constraint runs; these are external data priors.
axioms (2)
  • domain assumption Mock catalogs faithfully reproduce Roman survey properties including galaxy bias and selection
    Invoked to make the forecast realistic; stated in the description of the simulated lightcone mocks.
  • domain assumption EFT of LSS is valid on the scales used for the power spectrum multipoles
    Required for the model-dependent analysis to be applicable.

pith-pipeline@v0.9.0 · 5679 in / 1505 out tokens · 58137 ms · 2026-05-10T10:41:25.649218+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

99 extracted references · 95 canonical work pages · 3 internal anchors

  1. [1]

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

    A. Aghamousaet al.(DESI), The DESI Experiment Part I: Science,Targeting, and Survey Design (2016), arXiv:1611.00036 [astro-ph.IM]

    work page internal anchor Pith review arXiv 2016

  2. [2]

    Mellieret al.(Euclid), Euclid

    Y. Mellieret al.(Euclid), Euclid. I. Overview of the Euclid mission (2024), arXiv:2405.13491 [astro-ph.CO]

    work page arXiv 2024

  3. [3]

    Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report

    D. Spergel, N. Gehrels, C. Baltay, D. Bennett, J. Breck- inridge, M. Donahue, A. Dressler, B. Gaudi, T. Greene, O. Guyon,et al., Wide-field infrarred survey telescope- astrophysics focused telescope assets wfirst-afta 2015 re- port, arXiv preprint arXiv:1503.03757 (2015)

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  4. [4]

    Wanget al., The High Latitude Spectroscopic Survey on the Nancy Grace Roman Space Telescope, Astrophys

    Y. Wanget al., The High Latitude Spectroscopic Survey on the Nancy Grace Roman Space Telescope, Astrophys. J.928, 1 (2022), arXiv:2110.01829 [astro-ph.CO]

    work page arXiv 2022

  5. [5]

    Fukuda et al

    Y. Fukudaet al.(Super-Kamiokande), Evidence for oscil- lation of atmospheric neutrinos, Phys. Rev. Lett.81, 1562 (1998), arXiv:hep-ex/9807003

    work page arXiv 1998

  6. [6]

    Q. R. Ahmadet al.(SNO), Measurement of the rate of νe +d→p+p+e − interactions produced by 8B solar neutrinos at the Sudbury Neutrino Observatory, Phys. Rev. Lett.87, 071301 (2001), arXiv:nucl-ex/0106015

    work page arXiv 2001

  7. [7]

    Q. R. Ahmadet al.(SNO), Direct evidence for neutrino flavor transformation from neutral current interactions in the Sudbury Neutrino Observatory, Phys. Rev. Lett.89, 011301 (2002), arXiv:nucl-ex/0204008

    work page arXiv 2002

  8. [8]

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

    M. Abdul Karimet al.(DESI), DESI DR2 results. II. Measurements of baryon acoustic oscillations and cos- mological constraints, Phys. Rev. D112, 083515 (2025), arXiv:2503.14738 [astro-ph.CO]

    work page Pith review arXiv 2025

  9. [9]

    Elbers et al

    W. Elberset al., Constraints on neutrino physics from DESI DR2 BAO and DR1 full shape, Phys. Rev. D112, 083513 (2025), arXiv:2503.14744 [astro-ph.CO]

    work page arXiv 2025

  10. [10]

    Cosmological Non-Linearities as an Effective Fluid

    D. Baumann, A. Nicolis, L. Senatore, and M. Zaldarriaga, Cosmological Non-Linearities as an Effective Fluid, JCAP 07, 051, arXiv:1004.2488 [astro-ph.CO]

    work page Pith review arXiv

  11. [11]

    J. J. M. Carrasco, M. P. Hertzberg, and L. Senatore, The Effective Field Theory of Cosmological Large Scale Structures, JHEP09, 082, arXiv:1206.2926 [astro-ph.CO]

    work page Pith review arXiv

  12. [12]

    D’Amico, J

    G. D’Amico, J. Gleyzes, N. Kokron, K. Markovic, L. Sen- atore, P. Zhang, F. Beutler, and H. Gil-Mar´ ın, The Cos- mological Analysis of the SDSS/BOSS data from the Effective Field Theory of Large-Scale Structure, JCAP 05, 005, arXiv:1909.05271 [astro-ph.CO]

    work page arXiv 1909

  13. [13]

    Zhang, G

    P. Zhang, G. D’Amico, L. Senatore, C. Zhao, and Y. Cai, BOSS Correlation Function analysis from the Effective Field Theory of Large-Scale Structure, JCAP02(02), 036, arXiv:2110.07539 [astro-ph.CO]

    work page arXiv

  14. [14]

    M. M. Ivanov, M. Simonovi´ c, and M. Zaldarriaga, Cosmo- logical Parameters and Neutrino Masses from the Final Planck and Full-Shape BOSS Data, Phys. Rev. D101, 083504 (2020), arXiv:1912.08208 [astro-ph.CO]

    work page arXiv 2020

  15. [15]

    M. M. Ivanov, M. Simonovi´ c, and M. Zaldarriaga, Cosmo- logical Parameters from the BOSS Galaxy Power Spec- trum, JCAP05, 042, arXiv:1909.05277 [astro-ph.CO]

    work page arXiv 1909

  16. [16]

    Chudaykin, M

    A. Chudaykin, M. M. Ivanov, and O. H. E. Philcox, Rean- alyzing DESI DR1. I. ΛCDM constraints from the power spectrum and bispectrum, Phys. Rev. D113, 063502 (2026), arXiv:2507.13433 [astro-ph.CO]

    work page arXiv 2026

  17. [17]

    Large-Scale Structure of the Universe and Cosmological Perturbation Theory

    F. Bernardeau, S. Colombi, E. Gaztanaga, and R. Scoc- cimarro, Large scale structure of the universe and cos- mological perturbation theory, Phys. Rept.367, 1 (2002), arXiv:astro-ph/0112551

    work page Pith review arXiv 2002

  18. [18]

    Lesgourgues and S

    J. Lesgourgues and S. Pastor, Massive neutrinos and cosmology, Phys. Rept.429, 307 (2006), arXiv:astro- ph/0603494

    work page arXiv 2006

  19. [19]

    D. Blas, M. Garny, T. Konstandin, and J. Lesgourgues, Structure formation with massive neutrinos: going be- yond linear theory, JCAP11, 039, arXiv:1408.2995 [astro- ph.CO]

    work page arXiv

  20. [20]

    Loop corrections to the power spectrum for massive neutrino cosmologies with full time- and scale-dependence,

    M. Garny and P. Taule, Loop corrections to the power spectrum for massive neutrino cosmologies with full time- and scale-dependence, JCAP01, 020, arXiv:2008.00013 [astro-ph.CO]

    work page arXiv 2008

  21. [21]

    Two-loop power spectrum with full time- and scale-dependence and EFT corrections: impact of massive neutrinos and going beyond EdS,

    M. Garny and P. Taule, Two-loop power spectrum with full time- and scale-dependence and EFT corrections: impact of massive neutrinos and going beyond EdS, JCAP 09, 054, arXiv:2205.11533 [astro-ph.CO]

    work page arXiv

  22. [22]

    Aviles, A

    A. Aviles, A. Banerjee, G. Niz, and Z. Slepian, Clustering in massive neutrino cosmologies via Eulerian Perturbation Theory, JCAP11, 028, arXiv:2106.13771 [astro-ph.CO]

    work page arXiv

  23. [23]

    H. E. Noriega, A. Aviles, S. Fromenteau, and M. Vargas- Maga˜ na, Fast computation of non-linear power spectrum in cosmologies with massive neutrinos, JCAP11, 038, arXiv:2208.02791 [astro-ph.CO]

    work page arXiv

  24. [24]

    Mauset al., A comparison of effective field theory models of redshift space galaxy power spectra for DESI 2024 and future surveys, JCAP01, 134, arXiv:2404.07272 [astro-ph.CO]

    M. Mauset al., A comparison of effective field theory models of redshift space galaxy power spectra for DESI 2024 and future surveys, JCAP01, 134, arXiv:2404.07272 [astro-ph.CO]

    work page arXiv 2024

  25. [25]

    J. R. Bond, G. Efstathiou, and J. Silk, Massive Neutrinos and the Large Scale Structure of the Universe, Phys. Rev. Lett.45, 1980 (1980)

    1980

  26. [26]

    Large-Scale Galaxy Bias

    V. Desjacques, D. Jeong, and F. Schmidt, Large-Scale Galaxy Bias, Phys. Rept.733, 1 (2018), arXiv:1611.09787 [astro-ph.CO]

    work page Pith review arXiv 2018

  27. [27]

    Racco, P

    D. Racco, P. Zhang, and H. Zheng, Neutrino masses from large-scale structures: Future sensitivity and the- ory dependence, Phys. Dark Univ.47, 101803 (2025), arXiv:2412.04959 [astro-ph.CO]

    work page arXiv 2025

  28. [28]

    Raccanelli, L

    A. Raccanelli, L. Verde, and F. Villaescusa-Navarro, Bi- ases from neutrino bias: to worry or not to worry?, Mon. Not. Roy. Astron. Soc.483, 734 (2019), arXiv:1704.07837 [astro-ph.CO]

    work page arXiv 2019

  29. [29]

    Villaescusa-Navarro, F

    F. Villaescusa-Navarro, F. Marulli, M. Viel, E. Branchini, E. Castorina, E. Sefusatti, and S. Saito, Cosmology with massive neutrinos I: towards a realistic modeling of the relation between matter, haloes and galaxies, JCAP03, 011, arXiv:1311.0866 [astro-ph.CO]

    work page arXiv

  30. [30]

    Castorina, E

    E. Castorina, E. Sefusatti, R. K. Sheth, F. Villaescusa- Navarro, and M. Viel, Cosmology with massive neutrinos II: on the universality of the halo mass function and bias, JCAP02, 049, arXiv:1311.1212 [astro-ph.CO]

    work page arXiv

  31. [31]

    Costanzi, F

    M. Costanzi, F. Villaescusa-Navarro, M. Viel, J.-Q. Xia, S. Borgani, E. Castorina, and E. Sefusatti, Cosmol- ogy with massive neutrinos III: the halo mass function and an application to galaxy clusters, JCAP12, 012, arXiv:1311.1514 [astro-ph.CO]

    work page arXiv

  32. [32]

    Chiang, M

    C.-T. Chiang, M. LoVerde, and F. Villaescusa-Navarro, First detection of scale-dependent linear halo bias inN- body simulations with massive neutrinos, Phys. Rev. Lett. 122, 041302 (2019), arXiv:1811.12412 [astro-ph.CO]

    work page arXiv 2019

  33. [33]

    Chiang, W

    C.-T. Chiang, W. Hu, Y. Li, and M. Loverde, Scale- dependent bias and bispectrum in neutrino separate universe simulations, Phys. Rev. D97, 123526 (2018), 11 arXiv:1710.01310 [astro-ph.CO]

    work page arXiv 2018

  34. [34]

    LoVerde, Spherical collapse inνΛCDM, Phys

    M. LoVerde, Spherical collapse inνΛCDM, Phys. Rev. D 90, 083518 (2014), arXiv:1405.4858 [astro-ph.CO]

    work page arXiv 2014

  35. [35]

    LoVerde, Neutrino mass without cosmic variance, Phys

    M. LoVerde, Neutrino mass without cosmic variance, Phys. Rev. D93, 103526 (2016), arXiv:1602.08108 [astro- ph.CO]

    work page arXiv 2016

  36. [36]

    LoVerde, Halo bias in mixed dark matter cosmologies, Phys

    M. LoVerde, Halo bias in mixed dark matter cosmologies, Phys. Rev. D90, 083530 (2014), arXiv:1405.4855 [astro- ph.CO]

    work page arXiv 2014

  37. [37]

    Verdiani, E

    F. Verdiani, E. Bellini, C. Moretti, E. Sefusatti, C. Car- bone, and M. Viel, Redshift-space distortions in massive neutrinos cosmologies, Phys. Rev. D112, 043545 (2025), arXiv:2503.06655 [astro-ph.CO]

    work page arXiv 2025

  38. [38]

    Chudaykin, M.M

    A. Chudaykin, M. M. Ivanov, O. H. E. Philcox, and M. Simonovi´ c, Nonlinear perturbation theory extension of the Boltzmann code CLASS, Phys. Rev. D102, 063533 (2020), arXiv:2004.10607 [astro-ph.CO]

    work page arXiv 2020

  39. [39]

    The Effective Field Theory of Large-Scale Structure in the presence of Massive Neutrinos,

    L. Senatore and M. Zaldarriaga, The Effective Field The- ory of Large-Scale Structure in the presence of Massive Neutrinos (2017), arXiv:1707.04698 [astro-ph.CO]

    work page arXiv 2017

  40. [40]

    Schmittfull, M

    M. Schmittfull, M. Simonovi´ c, V. Assassi, and M. Zal- darriaga, Modeling Biased Tracers at the Field Level, Phys. Rev. D100, 043514 (2019), arXiv:1811.10640 [astro- ph.CO]

    work page arXiv 2019

  41. [41]

    B. C. Quevedoet al.(Euclid), Euclid preparation. Galaxy power spectrum modelling in redshift space (2026), arXiv:2601.20826 [astro-ph.CO]

    work page arXiv 2026

  42. [42]

    On the IR-Resummation in the EFTofLSS,

    L. Senatore and G. Trevisan, On the IR-Resummation in the EFTofLSS, JCAP05, 019, arXiv:1710.02178 [astro- ph.CO]

    work page arXiv

  43. [43]

    Senatore and M

    L. Senatore and M. Zaldarriaga, The IR-resummed Ef- fective Field Theory of Large Scale Structures, JCAP02, 013, arXiv:1404.5954 [astro-ph.CO]

    work page arXiv

  44. [44]

    M. M. Ivanov and S. Sibiryakov, Infrared Resummation for Biased Tracers in Redshift Space, JCAP07, 053, arXiv:1804.05080 [astro-ph.CO]

    work page arXiv

  45. [45]

    Baldauf, M

    T. Baldauf, M. Mirbabayi, M. Simonovi´ c, and M. Zal- darriaga, Equivalence Principle and the Baryon Acoustic Peak, Phys. Rev. D92, 043514 (2015), arXiv:1504.04366 [astro-ph.CO]

    work page arXiv 2015

  46. [46]

    Nishimichi, G

    T. Nishimichi, G. D’Amico, M. M. Ivanov, L. Senatore, M. Simonovi´ c, M. Takada, M. Zaldarriaga, and P. Zhang, Blinded challenge for precision cosmology with large- scale structure: results from effective field theory for the redshift-space galaxy power spectrum, Phys. Rev. D 102, 123541 (2020), arXiv:2003.08277 [astro-ph.CO]

    work page arXiv 2020

  47. [47]

    D’Amico, L

    G. D’Amico, L. Senatore, and P. Zhang, Limits onwCDM from the EFTofLSS with the PyBird code, JCAP01, 006, arXiv:2003.07956 [astro-ph.CO]

    work page arXiv 2003

  48. [48]

    Taule, M

    P. Taule, M. Marinucci, G. Biselli, M. Pietroni, and F. Vernizzi, Constraints on dark energy and modified gravity from the BOSS Full-Shape and DESI BAO data, JCAP03, 036, arXiv:2409.08971 [astro-ph.CO]

    work page arXiv

  49. [49]

    L. Piga, M. Marinucci, G. D’Amico, M. Pietroni, F. Vernizzi, and B. S. Wright, Constraints on modified gravity from the BOSS galaxy survey, JCAP04, 038, arXiv:2211.12523 [astro-ph.CO]

    work page arXiv

  50. [50]

    Accelerating Universes with Scaling Dark Matter

    M. Chevallier and D. Polarski, Accelerating universes with scaling dark matter, Int. J. Mod. Phys. D10, 213 (2001), arXiv:gr-qc/0009008

    work page Pith review arXiv 2001

  51. [51]

    E. V. Linder, Exploring the expansion history of the universe, Phys. Rev. Lett.90, 091301 (2003), arXiv:astro- ph/0208512

    work page arXiv 2003

  52. [52]

    Y. Wang, Model-independent measurements of cosmic expansion and growth atz= 0.57 using the anisotropic clustering of CMASS galaxies from the Sloan Digital Sky Survey Data Release 9, Mon. Not. Roy. Astron. Soc.443, 2950 (2014), arXiv:1404.5589 [astro-ph.CO]

    work page arXiv 2014

  53. [53]

    Wang, Modelling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity, Mon

    Y. Wang, Modelling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity, Mon. Not. Roy. Astron. Soc.464, 3005 (2017), arXiv:1606.08054 [astro-ph.CO]

    work page arXiv 2017

  54. [54]

    Zhai, C.-H

    Z. Zhai, C.-H. Chuang, Y. Wang, A. Benson, and G. Yepes, Clustering in the simulated Hαgalaxy redshift survey from Nancy Grace Roman Space Telescope, Mon. Not. Roy. Astron. Soc.501, 3490 (2021), arXiv:2008.09746 [astro-ph.CO]

    work page arXiv 2021

  55. [55]

    K. S. McCarthy, Z. Zhai, and Y. Wang, Phenomenological power spectrum models for Hαemission line galaxies from the Nancy Grace Roman Space Telescope, Mon. Not. Roy. Astron. Soc.523, 2498 (2023), arXiv:2212.08699 [astro- ph.CO]

    work page arXiv 2023

  56. [56]

    D’Amico, M

    G. D’Amico, M. Marinucci, M. Pietroni, and F. Vernizzi, The large scale structure bootstrap: perturbation the- ory and bias expansion from symmetries, JCAP10, 069, arXiv:2109.09573 [astro-ph.CO]

    work page arXiv

  57. [57]

    Marinucci, K

    M. Marinucci, K. Pardede, and M. Pietroni, Bootstrap- ping Lagrangian perturbation theory for the large scale structure, JCAP10, 051, arXiv:2405.08413 [astro-ph.CO]

    work page arXiv

  58. [58]

    Peron, T

    M. Peron, T. Nishimichi, M. Pietroni, and A. Taruya, Renormalized perturbation theory at field-level: the LSS bootstrap in GridSPT, JCAP10, 098, arXiv:2506.07105 [astro-ph.CO]

    work page arXiv

  59. [59]

    Amendola, M

    L. Amendola, M. Marinucci, M. Pietroni, and M. Quar- tin, Improving precision and accuracy in cosmology with model-independent spectrum and bispectrum, JCAP01, 001, arXiv:2307.02117 [astro-ph.CO]

    work page arXiv

  60. [60]

    Brieden, H

    S. Brieden, H. Gil-Mar´ ın, and L. Verde, ShapeFit: ex- tracting the power spectrum shape information in galaxy surveys beyond BAO and RSD, JCAP12(12), 054, arXiv:2106.07641 [astro-ph.CO]

    work page arXiv

  61. [61]

    Brieden, H

    S. Brieden, H. Gil-Mar´ ın, and L. Verde, PT challenge: validation of ShapeFit on large-volume, high-resolution mocks, JCAP06(06), 005, arXiv:2201.08400 [astro- ph.CO]

    work page arXiv

  62. [62]

    Cole , W

    S. Coleet al.(2dFGRS), The 2dF Galaxy Redshift Sur- vey: Power-spectrum analysis of the final dataset and cosmological implications, Mon. Not. Roy. Astron. Soc. 362, 505 (2005), arXiv:astro-ph/0501174

    work page arXiv 2005

  63. [63]

    W. J. Percival and M. White, Testing cosmological struc- ture formation using redshift-space distortions, Mon. Not. Roy. Astron. Soc.393, 297 (2009), arXiv:0808.0003 [astro- ph]

    work page arXiv 2009

  64. [64]

    J. A. Peacock and M. J. West, The power spectrum of Abell cluster correlations., Mon. Not. Roy. Astron. Soc. 259, 494 (1992)

    1992

  65. [65]

    Peculiar Velocity Decomposition, Redshift Space Distortion and Velocity Reconstruction in Redshift Surveys. II. Dark Matter Velocity Statistics

    Y. Zheng, P. Zhang, Y. Jing, W. Lin, and J. Pan, Peculiar Velocity Decomposition, Redshift Space Distortion and Velocity Reconstruction in Redshift Surveys. II. Dark Matter Velocity Statistics, Phys. Rev. D88, 103510 (2013), arXiv:1308.0886 [astro-ph.CO]

    work page Pith review arXiv 2013

  66. [66]

    Z. Zhai, A. Benson, Y. Wang, G. Yepes, and C.-H. Chuang, Prediction of Hαand [OIII] emission line galaxy number counts for future galaxy redshift surveys, Mon. Not. Roy. Astron. Soc.490, 3667 (2019), arXiv:1907.09680 [astro- ph.GA]

    work page arXiv 2019

  67. [67]

    Wang, C.-H

    Y. Wang, C.-H. Chuang, and C. M. Hirata, Towards more realistic forecasting of dark energy constraints from galaxy 12 redshift surveys, Mon. Not. Roy. Astron. Soc.430, 2446 (2013), arXiv:1211.0532 [astro-ph.CO]

    work page arXiv 2013

  68. [68]

    Z. Vlah, U. Seljak, M. Y. Chu, and Y. Feng, Perturbation theory, effective field theory, and oscillations in the power spectrum, JCAP03, 057, arXiv:1509.02120 [astro-ph.CO]

    work page arXiv

  69. [69]

    Alcock and B

    C. Alcock and B. Paczynski, An evolution free test for non-zero cosmological constant, Nature281, 358 (1979)

    1979

  70. [70]

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

    F. Beutleret al.(BOSS), The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Sur- vey: Anisotropic galaxy clustering in Fourier-space, Mon. Not. Roy. Astron. Soc.466, 2242 (2017), arXiv:1607.03150 [astro-ph.CO]

    work page arXiv 2017

  71. [71]

    Zaroubi and Y

    S. Zaroubi and Y. Hoffman, Clustering in redshift space: Power spectrum (1993), arXiv:astro-ph/9311013

    work page arXiv 1993

  72. [72]

    Raccanelli and Z

    A. Raccanelli and Z. Vlah, Power spectrum in the cave (2023), arXiv:2305.16278 [astro-ph.CO]

    work page arXiv 2023

  73. [73]

    Raccanelli and Z

    A. Raccanelli and Z. Vlah, Observed power spectrum and frequency-angular power spectrum, Phys. Rev. D108, 043537 (2023), arXiv:2306.00808 [astro-ph.CO]

    work page arXiv 2023

  74. [74]

    Spezzati, E

    F. Spezzati, E. Vanzan, A. Raccanelli, Z. Vlah, and D. Bertacca, Observed unequal-time power spectrum, Phys. Rev. D112, 023530 (2025), arXiv:2503.09759 [astro- ph.CO]

    work page arXiv 2025

  75. [75]

    Beutler and P

    F. Beutler and P. McDonald, Unified galaxy power spec- trum measurements from 6dFGS, BOSS, and eBOSS, JCAP11, 031, arXiv:2106.06324 [astro-ph.CO]

    work page arXiv

  76. [76]

    Simon, P

    T. Simon, P. Zhang, V. Poulin, and T. L. Smith, Updated constraints from the effective field theory analysis of the BOSS power spectrum on early dark energy, Phys. Rev. D107, 063505 (2023), arXiv:2208.05930 [astro-ph.CO]

    work page arXiv 2023

  77. [77]

    Beutler, E

    F. Beutler, E. Castorina, and P. Zhang, Interpreting measurements of the anisotropic galaxy power spectrum, JCAP03, 040, arXiv:1810.05051 [astro-ph.CO]

    work page arXiv

  78. [78]

    F. Beutleret al.(BOSS), The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles, Mon. Not. Roy. Astron. Soc. 443, 1065 (2014), arXiv:1312.4611 [astro-ph.CO]

    work page arXiv 2014

  79. [79]

    Heitmannet al., The Last Journey

    K. Heitmannet al., The Last Journey. I. An Extreme- Scale Simulation on the Mira Supercomputer, Astrophys. J. Suppl.252, 19 (2021), arXiv:2006.01697 [astro-ph.CO]

    work page arXiv 2021

  80. [80]

    Planck 2018 results. VI. Cosmological parameters

    N. Aghanimet al.(Planck), Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]

    work page Pith review arXiv 2018

Showing first 80 references.