Abstract
We present constraints on the f(R) gravity model using a sample of 1005 galaxy clusters in the redshift range 0.25-1.78 that have been selected through the thermal Sunyaev-Zel'dovich effect from South Pole Telescope data and subjected to optical and near-infrared confirmation with the multicomponent matched filter algorithm. We employ weak gravitational lensing mass calibration from the Dark Energy Survey Year 3 data for 688 clusters at z<0.95 and from the Hubble Space Telescope for 39 clusters with 0.6<z<1.7. Our cluster sample is a powerful probe of f(R) gravity, because this model predicts a scale-dependent enhancement in the growth of structure, which impacts the halo mass function (HMF) at cluster mass scales. To account for these modified gravity effects on the HMF, our analysis employs a semianalytical approach calibrated with numerical simulations. Combining calibrated cluster counts with primary cosmic microwave background temperature and polarization anisotropy measurements from the Planck 2018 release, we derive robust constraints on the f(R) parameter fR0. Our results, log10|fR0|<-5.32 at the 95% credible level, are the tightest current constraints on f(R) gravity from cosmological scales. This upper limit rules out f(R)-like deviations from general relativity that result in more than a ∼20% enhancement of the cluster population on mass scales M200c>3×1014M⊙.
| Original language | English |
|---|---|
| Article number | 043519 |
| Journal | Physical Review D |
| Volume | 111 |
| Issue number | 4 |
| DOIs | |
| State | Published - Feb 15 2025 |
Funding
This research was supported by (1) the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC-2094-390783311, by (2) the Max Planck Society Faculty Fellowship program at MPE, and by (3) the Ludwig-Maximilians-Universität in Munich. The FORGE simulations and analyses of this project made use of the DiRAC@Durham facility managed by the Institute for Computational Cosmology (ICC) on behalf of the STFC DiRAC HPC Facility . The equipment was funded by BEIS capital funding via STFC Capital Grants No. ST/K00042X/1, No. ST/P002293/1, No. ST/R002371/1, and No. ST/S002502/1, Durham University and STFC Operations Grant No. ST/R000832/1. DiRAC is part of the National e-Infrastructure. B. L. is supported by STFC via Consolidated Grant No. ST/X001075/1. The Innsbruck authors acknowledge support provided by the Austrian Research Promotion Agency (FFG) and the Federal Ministry of the Republic of Austria for Climate Action, Environment, Mobility, Innovation and Technology (BMK) via the Austrian Space Applications Programme with Grants No. 899537, No. 900565, and No. 911971. The South Pole Telescope program is supported by the National Science Foundation (NSF) through the Grants No. OPP-1852617 and No. 2332483. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago. Work at Argonne National Lab is supported by UChicago Argonne LLC, Operator of Argonne National Laboratory (Argonne), Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians-Universität München and the associated Excellence Cluster Origins, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. F.), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (No. FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This work is based on observations made with the NASA/ESA Hubble Space Telescope, using imaging data from the SPT follow-up GO Programs No. 12246 (PI: C. S.), No. 12477 (PI: F. W. H.), No. 13412 (PI: T. S.), No. 14252 (PI: V. S.), No. 14352 (PI: J. H.-L.), and No. 14677 (PI: T. S.). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA Contract No. NAS 5-26555. It is also based on observations made with ESO Telescopes at the La Silla Paranal Observatory under Programs No. 086.A-0741 (PI: Bazin), No. 088.A-0796 (PI: Bazin), No. 088.A-0889 (PI: Mohr), No. 089.A-0824 (PI: Mohr), No. 0100.A-0204 (PI: T. S.), No. 0100.A-0217 (PI: Hernández-Martín), No. 0101.A-0694 (PI: Zohren), and No. 0102.A-0189 (PI: Zohren). It is also based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea), under Programs No. 2014B-0338 and No. 2016B-0176 (PI: B. B.). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.