Constraints on <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:mrow></mml:math> gravity from thermal-S

We present constraints on the <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>f</a:mi><a:mo stretchy="false">(</a:mo><a:mi>R</a:mi><a:mo stretchy="false">)</a:mo></a:math> 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 <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>z</e:mi><e:mo>&lt;</e:mo><e:mn>0.95</e:mn></e:math> and from the Hubble Space Telescope for 39 clusters with <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:mn>0.6</g:mn><g:mo>&lt;</g:mo><g:mi>z</g:mi><g:mo>&lt;</g:mo><g:mn>1.7</g:mn></g:math>. Our cluster sample is a powerful probe of <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:mi>f</i:mi><i:mo stretchy="false">(</i:mo><i:mi>R</i:mi><i:mo stretchy="false">)</i:mo></i:math> 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 <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:mi>f</m:mi><m:mo stretchy="false">(</m:mo><m:mi>R</m:mi><m:mo stretchy="false">)</m:mo></m:math> parameter <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:msub><q:mi>f</q:mi><q:mrow><q:mi>R</q:mi><q:mn>0</q:mn></q:mrow></q:msub></q:math>. Our results, <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"><s:msub><s:mi>log</s:mi><s:mn>10</s:mn></s:msub><s:mo stretchy="false">|</s:mo><s:msub><s:mi>f</s:mi><s:mrow><s:mi>R</s:mi><s:mn>0</s:mn></s:mrow></s:msub><s:mo stretchy="false">|</s:mo><s:mo>&lt;</s:mo><s:mo>−</s:mo><s:mn>5.32</s:mn></s:math> at the 95% credible level, are the tightest current constraints on <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mi>f</w:mi><w:mo stretchy="false">(</w:mo><w:mi>R</w:mi><w:mo stretchy="false">)</w:mo></w:math> gravity from cosmological scales. This upper limit rules out <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mi>f</ab:mi><ab:mo stretchy="false">(</ab:mo><ab:mi>R</ab:mi><ab:mo stretchy="false">)</ab:mo></ab:math>-like deviations from general relativity that result in more than a <eb:math xmlns:eb="http://www.w3.org/1998/Math/MathML" display="inline"><eb:mo>∼</eb:mo><eb:mn>20</eb:mn><eb:mo>%</eb:mo></eb:math> enhancement of the cluster population on mass scales <gb:math xmlns:gb="http://www.w3.org/1998/Math/MathML" display="inline"><gb:mrow><gb:msub><gb:mrow><gb:mi>M</gb:mi></gb:mrow><gb:mrow><gb:mn>200</gb:mn><gb:mi mathvariant="normal">c</gb:mi></gb:mrow></gb:msub><gb:mo>&gt;</gb:mo><gb:mn>3</gb:mn><gb:mo>×</gb:mo><gb:msup><gb:mrow><gb:mn>10</gb:mn></gb:mrow><gb:mrow><gb:mn>14</gb:mn></gb:mrow></gb:msup><gb:msub><gb:mrow><gb:mi>M</gb:mi></gb:mrow><gb:mrow><gb:mo stretchy="false">⊙</gb:mo></gb:mrow></gb:msub></gb:mrow></gb:math>.

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Publication Details

Journal
Physical review. D/Physical review. D.
Published
2025-02-10
DOI
https://doi.org/10.1103/physrevd.111.043519
Citations
8
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
9.24

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article

Constraints on <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:mrow></mml:math> gravity from thermal-S

M. Paterno, I. Ferrero, Cheng-Zong Ruan, M. Gatti et al.
8 citations
Physical review. D/Physical review. D.
Galaxies: Formation, Evolution, Phenomena
9.24
article

Constraints on <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>R</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:mrow></mml:math> gravity from thermal-S

M. Paterno, I. Ferrero, Cheng-Zong Ruan, M. Gatti, S. Bocquet, C. L. Reichardt, R. A. Gruendl, L. N. da Costa, G. Giannini, D. Gruen, S. Grandis, T. Schrabback, Kathy Romer, A. A. Plazas, Gregory Tarlé, Fabian Schmidt, Arnab Sarkar, J. Myles, Baojiu Li, E. Suchyta, J. Carretero, L. E. Bleem, N. Weaverdyck, E. Sanchez, D. L. Burke, A. Pieres, J. Weller, J. Mena-Fernández, Sophie M. L. Vogt, A. Carnero Rosell, I. Sevilla-Noarbe, César Hernández‐Aguayo, J. Frieman, J. García-Bellido, J. J. Mohr, M. Lima, M. E. S. Pereira, S. Everett, M. Aguena, David J. Brooks, M. Costanzi, S Lee, S. R. Hinton, S. Samuroff, Matthias Klein, C. T. Davies, V. Vikram, M E C Swanson, M. Smith, Peter Doel, J. L. Marshall, J. De Vicente, A. Campos, R. Miquel, J. García-Bellido
article en
8 citations

Abstract

We present constraints on the <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>f</a:mi><a:mo stretchy="false">(</a:mo><a:mi>R</a:mi><a:mo stretchy="false">)</a:mo></a:math> 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 <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>z</e:mi><e:mo>&lt;</e:mo><e:mn>0.95</e:mn></e:math> and from the Hubble Space Telescope for 39 clusters with <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:mn>0.6</g:mn><g:mo>&lt;</g:mo><g:mi>z</g:mi><g:mo>&lt;</g:mo><g:mn>1.7</g:mn></g:math>. Our cluster sample is a powerful probe of <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:mi>f</i:mi><i:mo stretchy="false">(</i:mo><i:mi>R</i:mi><i:mo stretchy="false">)</i:mo></i:math> 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 <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:mi>f</m:mi><m:mo stretchy="false">(</m:mo><m:mi>R</m:mi><m:mo stretchy="false">)</m:mo></m:math> parameter <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:msub><q:mi>f</q:mi><q:mrow><q:mi>R</q:mi><q:mn>0</q:mn></q:mrow></q:msub></q:math>. Our results, <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"><s:msub><s:mi>log</s:mi><s:mn>10</s:mn></s:msub><s:mo stretchy="false">|</s:mo><s:msub><s:mi>f</s:mi><s:mrow><s:mi>R</s:mi><s:mn>0</s:mn></s:mrow></s:msub><s:mo stretchy="false">|</s:mo><s:mo>&lt;</s:mo><s:mo>−</s:mo><s:mn>5.32</s:mn></s:math> at the 95% credible level, are the tightest current constraints on <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mi>f</w:mi><w:mo stretchy="false">(</w:mo><w:mi>R</w:mi><w:mo stretchy="false">)</w:mo></w:math> gravity from cosmological scales. This upper limit rules out <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mi>f</ab:mi><ab:mo stretchy="false">(</ab:mo><ab:mi>R</ab:mi><ab:mo stretchy="false">)</ab:mo></ab:math>-like deviations from general relativity that result in more than a <eb:math xmlns:eb="http://www.w3.org/1998/Math/MathML" display="inline"><eb:mo>∼</eb:mo><eb:mn>20</eb:mn><eb:mo>%</eb:mo></eb:math> enhancement of the cluster population on mass scales <gb:math xmlns:gb="http://www.w3.org/1998/Math/MathML" display="inline"><gb:mrow><gb:msub><gb:mrow><gb:mi>M</gb:mi></gb:mrow><gb:mrow><gb:mn>200</gb:mn><gb:mi mathvariant="normal">c</gb:mi></gb:mrow></gb:msub><gb:mo>&gt;</gb:mo><gb:mn>3</gb:mn><gb:mo>×</gb:mo><gb:msup><gb:mrow><gb:mn>10</gb:mn></gb:mrow><gb:mrow><gb:mn>14</gb:mn></gb:mrow></gb:msup><gb:msub><gb:mrow><gb:mi>M</gb:mi></gb:mrow><gb:mrow><gb:mo stretchy="false">⊙</gb:mo></gb:mrow></gb:msub></gb:mrow></gb:math>.

Physical review. D/Physical review. D.Vol. 111(4)
Institució Catalana de Recerca i Estudis Avançats (ES), California Institute of Technology (US), Vassar College (US), Argonne National Laboratory (US), Oak Ridge National Laboratory (US), Northeastern University (US), Fermi National Accelerator Laboratory (US), Jet Propulsion Laboratory (US), University of Trieste (IT), Lawrence Berkeley National Laboratory (US), University of Illinois Urbana-Champaign (US), Universität Hamburg (DE), University of Sussex (GB), The University of Queensland (AU), The University of Melbourne (AU), Universidade de São Paulo (BR), University of Oslo (NO), Durham University (GB), Universität Innsbruck (AT), Princeton University (US), University of Michigan (US), Trieste Astronomical Observatory (IT), Mitchell Institute (US), SLAC National Accelerator Laboratory (US), University of California System (US), California University of Pennsylvania (US), University of Chicago (US), Shanghai Institute for Science of Science (CN), Max Planck Institute for Extraterrestrial Physics (DE), Kavli Institute for Particle Astrophysics and Cosmology (US), Excellence Cluster Origins (DE), Institute of Particle Physics (CA), Max Planck Institute for Astrophysics (DE), National Observatory (BR), Instituto de Astrofísica de Canarias (ES), Barcelona Institute of Science and Technology (ES), National Center for Supercomputing Applications (US), Institute for Physics (US), Laboratoire de Physique Subatomique et de Cosmologie (FR), Laboratório Interinstitucional de e-Astronomia (BR), Institute for Fundamental Physics of the Universe (IT), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), Institute of Science and Technology, University College London (GB), Universidad Autónoma de Madrid (ES), Massachusetts Institute of Technology (US), Lancaster University (GB), Carnegie Mellon University (US), University of Pennsylvania (US), Ludwig-Maximilians-Universität München (DE), Universidad del Noreste (MX), Texas A&M University (US), University of California, Berkeley (US), Stanford University (US)
National Science Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Stanford University, University of California, Santa Cruz, Ohio State University, University of Chicago, University of Michigan, Texas A and M University, University of Portsmouth, National Centre for Supercomputing Applications, Department for Business, Energy and Industrial Strategy, UK Government, Higher Education Funding Council for England, Centres de Recerca de Catalunya, Bundesministerium für Klimaschutz, Umwelt, Energie, Mobilität, Innovation und Technologie, University of Cambridge, University College London, European Commission, University of Nottingham, University of Sussex, University of Edinburgh, Durham University, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, Eidgenössische Technische Hochschule Zürich, Ministerio de Ciencia, Tecnología e Innovación Productiva, Ministério da Ciência, Tecnologia e Inovação, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Korea Astronomy and Space Science Institute, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos, Ministerio de Ciencia e Innovación, Österreichische Forschungsförderungsgesellschaft, Ludwig-Maximilians-Universität München, Instituto Nacional de Ciência e Tecnologia: Física Nuclear e Aplicações, Institut de Física d'Altes Energies, University of Illinois at Urbana-Champaign, Office of Science, Seventh Framework Programme, Center for Cosmology and Astroparticle Physics, Ohio State University, Kavli Institute for Cosmological Physics, University of Chicago, National Research Council Canada, Science and Technology Facilities Council, European Research Council, Deutsches Elektronen-Synchrotron, Comisión Nacional de Investigación Científica y Tecnológica, Consejo Superior de Investigaciones Científicas, European Regional Development Fund, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, High Energy Physics, Integrated Electronics Engineering Center, Binghamton University, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, SLAC National Accelerator Laboratory
Openalex Percentile: Top 2%
Galaxies: Formation, Evolution, Phenomena
9.24
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