Modified gravity constraints from the full shape modeling of clustering measurements from DESI 2024

Abstract We present cosmological constraints on deviations from general relativity (GR) from the first-year of clustering observations from the Dark Energy Spectroscopic Instrument (DESI) in combination with other available datasets including the CMB data from Planck with CMB-lensing from Planck and ACT, BBN constraints on the physical baryon density, the galaxy weak lensing and clustering from DESY3 and supernova data from DESY5. We first consider the μ ( a,k )–Σ( a,k ) modified gravity (MG) parameterization (as well as η ( a,k )) in a ΛCDM and a w 0 w a CDM cosmological backgrounds. Using a functional form for time-only evolution gives μ 0 = 0.11 +0.44 -0.54 from DESI(FS+BAO)+BBN and a wide prior on n s . Using DESI(FS+BAO)+CMB+DESY3+DESY5-SN, we obtain μ 0 = 0.05 ± 0.22 and Σ 0 = 0.008 ± 0.045 and similarly μ 0 = 0.02 +0.19 -0.24 and η 0 = 0.09 +0.36 -0.60 , in an ΛCDM background. In w 0 w a CDM we obtain μ 0 = -0.24 +0.32 -0.28 and Σ 0 = 0.006 ± 0.043, consistent with GR, and we still find a preference of the data for a dynamical dark energy with w 0 > -1 and w a < 0. Using functional dependencies in both time and scale gives μ 0 and Σ 0 with a same level of precision as above but other scale MG parameters remain hard to constrain. We then move to binned parameterizations in a ΛCDM background starting with two bins in redshift and obtain, μ 1 = 1.02 ± 0.13, μ 2 = 1.04 ± 0.11, Σ 1 = 1.021 ± 0.029 and Σ 2 = 1.022 +0.027 -0.023 , all consistent with the unity value of GR in the binning formalism. We then extend the analysis to combine two bins in redshift and two in scale giving 8 MG parameters that we find all consistent with GR. We note that we find here that the tension reported in previous studies about Σ 0 being inconsistent with GR when using Planck PR3 data goes away when we use the recent LoLLiPoP + HiLLiPoP likelihoods. As noted in previous studies, this seems to indicate that the tension is indeed related to the CMB lensing anomaly in PR3 which is also resolved when using the recent likelihoods. We then constrain the class of Horndeski theory in the effective field theory of dark energy approach. We consider both EFT-basis and α -basis in the analysis. Assuming a power law parameterization for the EFT function Ω, which controls non-minimal coupling, we obtain Ω 0 = 0.012 +0.001 -0.012 and s 0 = 0.996 +0.54 -0.20 from the combination of DESI(FS+BAO)+DESY5SN+CMB in a ΛCDM background, which are consistent with GR. Similar results are obtained when using the α -basis and assuming no-braiding ( α B = 0) giving c M < 1.14 at 95% CL in a ΛCDM background, also in agreement with GR. However, we see a mild yet consistent indication for c B > 0 when α B is allowed to vary which will require further study to determine whether this is due to systematics or new physics.

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Journal
Journal of Cosmology and Astroparticle Physics
Published
2025-09-01
DOI
https://doi.org/10.1088/1475-7516/2025/09/053
Citations
30
Primary Topic
Geophysics and Gravity Measurements
Type
article
Field-Weighted Citation Impact
53.81

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article

Modified gravity constraints from the full shape modeling of clustering measurements from DESI 2024

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30 citations
Journal of Cosmology and Astroparticle Physics
Geophysics and Gravity Measurements
53.81
article

Modified gravity constraints from the full shape modeling of clustering measurements from DESI 2024

D. Kirkby, H. E. Noriega, C. García-Quintero, D. Brooks, Rongpu Zhou, E. Chaussidon, S. Juneau, S Ferraro, Alejandro Avilés, N. Palanque‐Delabrouille, Gregory Tarlé, Andreu Font-Ribera, Jorge L. Cervantes–Cota, Laurent Le Guillou, Christophe Yèche, Gustavo Niz, D. Bianchi, David J. Schlegel, Ignasi Pérez-Ràfols, Axel de la Macorra, Héctor Gil-Marín, Liu Chiao Yi, D Huterer, M. Landriau, Giacomo Rossi, Gong‐Bo Zhao, Chenghang Zheng, Arman Shafieloo, Anthony Kremin, Eusebio Sanchez, Alexie Leauthaud, ENRIQUE GAZTAÑAGA, R. H. Wechsler, Cullan Howlett, Arjun T. Dey, J. E. Forero-Romero, Steven P. Ahlen, Aaron Meisner, Pauline Zarrouk, R. Miquel, Theodore S. Kisner, John Moustakas, Wei Fang, Georgios Valogiannis, Claire Poppett, Jian Pan, U. Andrade, Arnaud de Mattia, Mustapha Ishak, L. Medina-Varela, Hee‐Jong Seo, M. Vargas-Magaña, R. Calderón, K. Lodha, Hu Zou, T. Claybaugh, M. Schubnell, S. Cole, Klaus Honscheid, K. Fanning, ChangHoon Hahn, Francisco Prada, E. Burtin, G. Gutiérrez, D. Sprayberry
article en
30 citations

Abstract

Abstract We present cosmological constraints on deviations from general relativity (GR) from the first-year of clustering observations from the Dark Energy Spectroscopic Instrument (DESI) in combination with other available datasets including the CMB data from Planck with CMB-lensing from Planck and ACT, BBN constraints on the physical baryon density, the galaxy weak lensing and clustering from DESY3 and supernova data from DESY5. We first consider the μ ( a,k )–Σ( a,k ) modified gravity (MG) parameterization (as well as η ( a,k )) in a ΛCDM and a w 0 w a CDM cosmological backgrounds. Using a functional form for time-only evolution gives μ 0 = 0.11 +0.44 -0.54 from DESI(FS+BAO)+BBN and a wide prior on n s . Using DESI(FS+BAO)+CMB+DESY3+DESY5-SN, we obtain μ 0 = 0.05 ± 0.22 and Σ 0 = 0.008 ± 0.045 and similarly μ 0 = 0.02 +0.19 -0.24 and η 0 = 0.09 +0.36 -0.60 , in an ΛCDM background. In w 0 w a CDM we obtain μ 0 = -0.24 +0.32 -0.28 and Σ 0 = 0.006 ± 0.043, consistent with GR, and we still find a preference of the data for a dynamical dark energy with w 0 > -1 and w a < 0. Using functional dependencies in both time and scale gives μ 0 and Σ 0 with a same level of precision as above but other scale MG parameters remain hard to constrain. We then move to binned parameterizations in a ΛCDM background starting with two bins in redshift and obtain, μ 1 = 1.02 ± 0.13, μ 2 = 1.04 ± 0.11, Σ 1 = 1.021 ± 0.029 and Σ 2 = 1.022 +0.027 -0.023 , all consistent with the unity value of GR in the binning formalism. We then extend the analysis to combine two bins in redshift and two in scale giving 8 MG parameters that we find all consistent with GR. We note that we find here that the tension reported in previous studies about Σ 0 being inconsistent with GR when using Planck PR3 data goes away when we use the recent LoLLiPoP + HiLLiPoP likelihoods. As noted in previous studies, this seems to indicate that the tension is indeed related to the CMB lensing anomaly in PR3 which is also resolved when using the recent likelihoods. We then constrain the class of Horndeski theory in the effective field theory of dark energy approach. We consider both EFT-basis and α -basis in the analysis. Assuming a power law parameterization for the EFT function Ω, which controls non-minimal coupling, we obtain Ω 0 = 0.012 +0.001 -0.012 and s 0 = 0.996 +0.54 -0.20 from the combination of DESI(FS+BAO)+DESY5SN+CMB in a ΛCDM background, which are consistent with GR. Similar results are obtained when using the α -basis and assuming no-braiding ( α B = 0) giving c M < 1.14 at 95% CL in a ΛCDM background, also in agreement with GR. However, we see a mild yet consistent indication for c B > 0 when α B is allowed to vary which will require further study to determine whether this is due to systematics or new physics.

Journal of Cosmology and Astroparticle PhysicsVol. 2025(09)
Boston University (US), Institució Catalana de Recerca i Estudis Avançats (ES), Universidad de Guanajuato (MX), Fermi National Accelerator Laboratory (US), Hiroshima Shudo University (JP), Berkeley College (US), Harvard University (US), High Energy Accelerator Research Organization (JP), Lawrence Berkeley National Laboratory (US), University of Waterloo (CA), North China Electric Power University (CN), Korea Advanced Institute of Science and Technology (KR), The University of Queensland (AU), University of Pittsburgh (US), Perimeter Institute (CA), University of California, Santa Cruz (US), Institute for High Energy Physics (ES), University of Milan (IT), University of Michigan (US), Korea Astronomy and Space Science Institute (KR), Regional Municipality of Waterloo (CA), Sejong University (KR), Hefei University (CN), National Solar Observatory (US), Institut d'Estudis Espacials de Catalunya (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), Korean Association for the Study of Intestinal Diseases (KR), Menlo School (US), Institut Català de Ciències del Clima (ES), Stanford Health Care (US), Laboratoire de Physique Nucléaire et de Hautes Énergies (FR), Lickenbrock (US), Indiana Cancer Consortium (US), Centre for Theoretical Physics and Astrophysics (UZ), Michigan United (US), Astrobiology Center (JP), Unidades Centrales Científico-Técnicas (ES), Institut Cartogràfic i Geològic de Catalunya (ES), Stanford Medicine (US), UC Irvine Health (US), Mylan (Switzerland) (CH), National Astronomical Observatories (CN), Institut de Recherche sur les Lois Fondamentales de l'Univers (FR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), State Library of Ohio (US), University College London (GB), University of Portsmouth (GB), Centro de Investigación y de Estudios Avanzados del Instituto Politécnico Nacional (MX), Universidad Intercontinental (MX), Universidad Nacional Autónoma de México (MX), Siena College (US), Netherlands Institute for Radio Astronomy (NL), Universitat Politècnica de Catalunya (ES), Stanford University (US)
National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Gordon and Betty Moore Foundation, Space Telescope Science Institute, Ministerstvo Školství, Mládeže a Tělovýchovy, Ministerio de Ciencia e Innovación, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Office of Science, Science and Technology Facilities Council, Division of Astronomical Sciences
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