The DESI DR1 peculiar velocity survey: Growth rate measurements from the galaxy power spectrum

The large-scale structure of the Universe and its evolution encapsulate a wealth of cosmological information. A powerful means of unlocking this knowledge lies in measuring the auto-power spectrum and/or the cross-power spectrum of the galaxy density and momentum fields, followed by the estimation of cosmological parameters based on these spectrum measurements. In this study, we generalize the cross-power spectrum model to accommodate scenarios in which the density and momentum fields are derived from distinct galaxy surveys. The growth rate of the large-scale structures of the Universe, commonly represented as fσ8, was extracted by jointly fitting the monopole and quadrupole moments of the auto-density power spectrum, the monopole of the auto-momentum power spectrum, and the dipole of the cross-power spectrum. Our estimators, theoretical models, and parameter-fitting framework were tested using mocks, confirming their robustness and accuracy in retrieving the fiducial growth rate from simulation. These techniques were then applied to analyse the power spectrum of the DESI Bright Galaxy Survey and Peculiar Velocity Survey. The fit result of the growth rate is fσ8 = 0.440+0.080−0.096 f σ 8 = 0 . 440 − 0.096 + 0.080 $ f\sigma_8 = 0.440^{+0.080}_{-0.096} $ at effective redshift zeff = 0.07. By synthesizing the fitting outcomes from correlation functions, maximum likelihood estimation, and the power spectrum, a consensus value is yielded of fσ8(zeff = 0.07) = 0.450+0.055−0.055 f σ 8 ( z eff = 0.07 ) = 0 . 450 − 0.055 + 0.055 $ f\sigma_8(z_\mathrm{{eff}} = 0.07) = 0.450 ^{+0.055}_{-0.055} $ , and correspondingly we obtain γ = 0.580+0.110−0.110 γ = 0 . 580 − 0.110 + 0.110 $ \gamma = 0.580^{+0.110}_{-0.110} $ , Ωm = 0.301+0.011−0.011 Ω m = 0 . 301 − 0.011 + 0.011 $ \Omega_{\mathrm{m}} = 0.301^{+0.011}_{-0.011} $ , and σ8 = 0.834+0.032−0.032 σ 8 = 0 . 834 − 0.032 + 0.032 $ \sigma_8 = 0.834^{+0.032}_{-0.032} $ . The measured fσ8 and γ are consistent with the prediction of the Λ cold dark matter model and general relativity.

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DOAJ (DOAJ: Directory of Open Access Journals)
Published
2026-04-01
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https://doi.org/10.1051/0004-6361/202558368
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Galaxies: Formation, Evolution, Phenomena
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article

The DESI DR1 peculiar velocity survey: Growth rate measurements from the galaxy power spectrum

Qin F., Levi Maulana Nim. E, J. A. R., Brooks Cash D et al.
DOAJ (DOAJ: Directory of Open Access Journals)
Galaxies: Formation, Evolution, Phenomena
article

The DESI DR1 peculiar velocity survey: Growth rate measurements from the galaxy power spectrum

Qin F., Levi Maulana Nim. E, J. A. R., Brooks Cash D, Blake Gilks C, Lei Chen, Kim G, C. Baccigalupi, M. A., Ross Andrew C., Kisner T, Palanque-Delabrouille N, Claybaugh T, Chaussidon E, Gutierrez G, Lahav O, Munoz-Gutierrez A, de la Macorra A, Doel P, Bianchi D, Rossi G, Tarle G, Ishak M, Font-Ribera A, Aguilar J, Zhou R, Ferraro S, Schubnell M, Seo H, Perez-Rafols I, Sanchez E, Nadathur S, Gaztanaga E, Miquel R, Kremin A, Honscheid K, Sprayberry D, Silber J, Manera M, Turner J, Moustakas J, Poppett C, Schlegel D, Gontcho A Gontcho S, Prada F, Ahlen S, Kirkby D, Zou H, Landriau M, Le Guillou L., Weaver B. A., Percival W. J., Herrera-Alcantar H. K., Lai Y., Douglass K., Bautista J., Amsellem A. J., Zarrouk P., Said K., Lodha K., BenZvi S., Forero-Romero J. E., Huterer D., Guy J., Howlett C.
article en

Abstract

The large-scale structure of the Universe and its evolution encapsulate a wealth of cosmological information. A powerful means of unlocking this knowledge lies in measuring the auto-power spectrum and/or the cross-power spectrum of the galaxy density and momentum fields, followed by the estimation of cosmological parameters based on these spectrum measurements. In this study, we generalize the cross-power spectrum model to accommodate scenarios in which the density and momentum fields are derived from distinct galaxy surveys. The growth rate of the large-scale structures of the Universe, commonly represented as fσ8, was extracted by jointly fitting the monopole and quadrupole moments of the auto-density power spectrum, the monopole of the auto-momentum power spectrum, and the dipole of the cross-power spectrum. Our estimators, theoretical models, and parameter-fitting framework were tested using mocks, confirming their robustness and accuracy in retrieving the fiducial growth rate from simulation. These techniques were then applied to analyse the power spectrum of the DESI Bright Galaxy Survey and Peculiar Velocity Survey. The fit result of the growth rate is fσ8 = 0.440+0.080−0.096 f σ 8 = 0 . 440 − 0.096 + 0.080 $ f\sigma_8 = 0.440^{+0.080}_{-0.096} $ at effective redshift zeff = 0.07. By synthesizing the fitting outcomes from correlation functions, maximum likelihood estimation, and the power spectrum, a consensus value is yielded of fσ8(zeff = 0.07) = 0.450+0.055−0.055 f σ 8 ( z eff = 0.07 ) = 0 . 450 − 0.055 + 0.055 $ f\sigma_8(z_\mathrm{{eff}} = 0.07) = 0.450 ^{+0.055}_{-0.055} $ , and correspondingly we obtain γ = 0.580+0.110−0.110 γ = 0 . 580 − 0.110 + 0.110 $ \gamma = 0.580^{+0.110}_{-0.110} $ , Ωm = 0.301+0.011−0.011 Ω m = 0 . 301 − 0.011 + 0.011 $ \Omega_{\mathrm{m}} = 0.301^{+0.011}_{-0.011} $ , and σ8 = 0.834+0.032−0.032 σ 8 = 0 . 834 − 0.032 + 0.032 $ \sigma_8 = 0.834^{+0.032}_{-0.032} $ . The measured fσ8 and γ are consistent with the prediction of the Λ cold dark matter model and general relativity.

DOAJ (DOAJ: Directory of Open Access Journals)
University of Siena (IT), Boston University (US), Institució Catalana de Recerca i Estudis Avançats (ES), Universitat Autònoma de Barcelona (ES), Centre National de la Recherche Scientifique (FR), Fermi National Accelerator Laboratory (US), Lawrence Berkeley National Laboratory (US), University of Waterloo (CA), The University of Texas at Dallas (US), The University of Queensland (AU), Institute for High Energy Physics (ES), University of Milan (IT), Chinese Academy of Sciences (CN), Aix-Marseille Université (FR), Commissariat à l'Énergie Atomique et aux Énergies Alternatives (FR), Université Paris-Saclay (FR), University of Michigan (US), Korea Astronomy and Space Science Institute (KR), Institut d'Astrophysique de Paris (FR), Laboratoire AstroParticule et Cosmologie (FR), Sejong University (KR), Sorbonne Université (FR), Institut d'Estudis Espacials de Catalunya (ES), Bausch & Lomb (France) (FR), Laboratoire de Physique Nucléaire et de Hautes Énergies (FR), Ohio University (US), CEA Paris-Saclay (FR), Universidad de Los Andes (BO), Astronomy and Space (AU), Instituto de Astrofísica de Andalucía (ES), National Astronomical Observatories (CN), Institut de Recherche sur les Lois Fondamentales de l'Univers (FR), University College London (GB), The Ohio State University (US), Swinburne University of Technology (AU), University of Portsmouth (GB), Carnegie Mellon University (US), Universidad Nacional Autónoma de México (MX), Universitat Politècnica de Catalunya (ES)
Openalex Percentile: Top 26%
Galaxies: Formation, Evolution, Phenomena
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