Interacting dark sector within ETHOS: Cosmological constraints from SPT cluster abundance with DES and HST weak lensing data

We use galaxy cluster abundance measurements from the South Pole Telescope enhanced by multicomponent matched filter confirmation and complemented with mass information obtained using weak-lensing data from Dark Energy Survey Year 3 (DES Y3) and targeted Hubble Space Telescope observations for probing deviations from the cold dark matter paradigm. Concretely, we consider a class of dark sector models featuring interactions between dark matter (DM) and a dark radiation (DR) component within the framework of the effective theory of structure formation (ETHOS). We focus on scenarios that lead to power suppression over a wide range of scales, and thus can be tested with data sensitive to large scales, as realized, for example, for DM–DR interactions following from an unbroken non-Abelian <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>S</a:mi><a:mi>U</a:mi><a:mo stretchy="false">(</a:mo><a:mi>N</a:mi><a:mo stretchy="false">)</a:mo></a:math> gauge theory (interaction rate with power-law index <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>n</e:mi><e:mo>=</e:mo><e:mn>0</e:mn></e:math> within the ETHOS parametrization). Cluster abundance measurements are mostly sensitive to the amount of DR interacting with DM, parametrized by the ratio of DR temperature to the cosmic microwave background (CMB) temperature, <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:msub><g:mi>ξ</g:mi><g:mi>DR</g:mi></g:msub><g:mo>=</g:mo><g:msub><g:mi>T</g:mi><g:mi>DR</g:mi></g:msub><g:mo>/</g:mo><g:msub><g:mi>T</g:mi><g:mi>CMB</g:mi></g:msub></g:math>. We find an upper limit <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi>ξ</i:mi><i:mi>DR</i:mi></i:msub><i:mo>&lt;</i:mo><i:mn>17</i:mn><i:mo>%</i:mo></i:math> at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:msub><k:mi>ξ</k:mi><k:mi>DR</k:mi></k:msub><k:mo>&lt;</k:mo><k:mn>10</k:mn><k:mo>%</k:mo></k:math>, corresponding to a limit on the abundance of interacting DR that is around 3 times tighter than that from CMB + BAO data alone. We also discuss the complementarity of weak lensing informed cluster abundance studies with probes sensitive to smaller scales, explore the impact on our analysis of massive neutrinos, and comment on a slight preference for the presence of a nonzero interacting DR abundance, which enables a physical solution to the <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>S</m:mi><m:mn>8</m:mn></m:msub></m:math> tension.

Authors

Institutions

Publication Details

Journal
Physical review. D/Physical review. D.
Published
2025-04-24
DOI
https://doi.org/10.1103/physrevd.111.083543
Citations
1
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
1.15

Funders

Controls
|||
ALL TIME
JAN
FEB
MAR
APR
MAY
JUN
JUL
AUG
SEP
OCT
article

Interacting dark sector within ETHOS: Cosmological constraints from SPT cluster abundance with DES and HST weak lensing data

A. Pieres, S. R. Hinton, D. Brooks, J. Carretero et al.
1 citations
Physical review. D/Physical review. D.
Galaxies: Formation, Evolution, Phenomena
1.15
article

Interacting dark sector within ETHOS: Cosmological constraints from SPT cluster abundance with DES and HST weak lensing data

A. Pieres, S. R. Hinton, D. Brooks, J. Carretero, Mathias Garny, J. García-Bellido, S. Bocquet, S. Allam, S. W. Allen, C. L. Reichardt, J. L. Marshall, Guillaume Mahler, M. R. Smith, G. Giannini, M. Schubnell, J. Frieman, D. Gruen, S. Grandis, T. Schrabback, Kathy Romer, A. A. Plazas, Gregory Tarlé, E. Suchyta, A. Porredon, J. Myles, B. Flaugher, O. Alves, P. Wiseman, L. E. Bleem, N. Weaverdyck, Scott Dodelson, Gaston Gutierrez, D. Sanchez Cid, Asmaa Mazoun, Eusebio Sanchez, J. Weller, V. Vikram, A. Carnero Rosell, J. De Vicente, S. Samuroff, I. Sevilla-Noarbe, D.J James, K. Kuehn, J. García-Bellido, J. J. Mohr, T. M. Davis, R. L. C. Ogando, M. Lima, R. Miquel, M. E. S. Pereira, H. T. Diehl, F. Andrade-Oliveira, Andrius Tamosiunas, M. Aguena, M. Costanzi, D. L. Tucker, S Lee, Henrique Rubira, Raven Gassis, Matthias Klein, O. Lahav, P. Doel, M. Carrasco Kind, L. N. da Costa, M. E. C. Swanson, S Desai, S. Everett
article en
1 citations

Abstract

We use galaxy cluster abundance measurements from the South Pole Telescope enhanced by multicomponent matched filter confirmation and complemented with mass information obtained using weak-lensing data from Dark Energy Survey Year 3 (DES Y3) and targeted Hubble Space Telescope observations for probing deviations from the cold dark matter paradigm. Concretely, we consider a class of dark sector models featuring interactions between dark matter (DM) and a dark radiation (DR) component within the framework of the effective theory of structure formation (ETHOS). We focus on scenarios that lead to power suppression over a wide range of scales, and thus can be tested with data sensitive to large scales, as realized, for example, for DM–DR interactions following from an unbroken non-Abelian <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>S</a:mi><a:mi>U</a:mi><a:mo stretchy="false">(</a:mo><a:mi>N</a:mi><a:mo stretchy="false">)</a:mo></a:math> gauge theory (interaction rate with power-law index <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>n</e:mi><e:mo>=</e:mo><e:mn>0</e:mn></e:math> within the ETHOS parametrization). Cluster abundance measurements are mostly sensitive to the amount of DR interacting with DM, parametrized by the ratio of DR temperature to the cosmic microwave background (CMB) temperature, <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:msub><g:mi>ξ</g:mi><g:mi>DR</g:mi></g:msub><g:mo>=</g:mo><g:msub><g:mi>T</g:mi><g:mi>DR</g:mi></g:msub><g:mo>/</g:mo><g:msub><g:mi>T</g:mi><g:mi>CMB</g:mi></g:msub></g:math>. We find an upper limit <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi>ξ</i:mi><i:mi>DR</i:mi></i:msub><i:mo>&lt;</i:mo><i:mn>17</i:mn><i:mo>%</i:mo></i:math> at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:msub><k:mi>ξ</k:mi><k:mi>DR</k:mi></k:msub><k:mo>&lt;</k:mo><k:mn>10</k:mn><k:mo>%</k:mo></k:math>, corresponding to a limit on the abundance of interacting DR that is around 3 times tighter than that from CMB + BAO data alone. We also discuss the complementarity of weak lensing informed cluster abundance studies with probes sensitive to smaller scales, explore the impact on our analysis of massive neutrinos, and comment on a slight preference for the presence of a nonzero interacting DR abundance, which enables a physical solution to the <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>S</m:mi><m:mn>8</m:mn></m:msub></m:math> tension.

Physical review. D/Physical review. D.Vol. 111(8)
Institució Catalana de Recerca i Estudis Avançats (ES), California Institute of Technology (US), Argonne National Laboratory (US), Oak Ridge National Laboratory (US), Fermi National Accelerator Laboratory (US), Consejo Superior de Investigaciones Científicas (ES), University of Trieste (IT), Lawrence Berkeley National Laboratory (US), Universidad de La Laguna (ES), Universität Hamburg (DE), University of Sussex (GB), The University of Queensland (AU), The University of Melbourne (AU), Universidade de São Paulo (BR), Institute for High Energy Physics (ES), Durham University (GB), Universität Innsbruck (AT), Princeton University (US), University of Cambridge (GB), University of Michigan (US), Lowell Observatory (US), Trieste Astronomical Observatory (IT), Mitchell Institute (US), SLAC National Accelerator Laboratory (US), Australian Astronomical Observatory (AU), Lander Institute (IL), University of Chicago (US), Max Planck Institute for Extraterrestrial Physics (DE), Kavli Institute for Particle Astrophysics and Cosmology (US), Excellence Cluster Origins (DE), Institute of Particle Physics (CA), Center for Astrophysics Harvard & Smithsonian (US), National Observatory (BR), Instituto de Astrofísica de Canarias (ES), Laboratório Interinstitucional de e-Astronomia (BR), Institute for Fundamental Physics of the Universe (IT), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), University of Southampton (GB), University College London (GB), Case Western Reserve University (US), Technical University of Munich (DE), University of Cincinnati (US), Indian Institute of Technology Hyderabad (IN), Lancaster University (GB), Carnegie Mellon University (US), Ludwig-Maximilians-Universität München (DE), Universidad del Noreste (MX), Ruhr University Bochum (DE), Texas A&M University (US), University of California, Berkeley (US)
National Science Foundation, David and Lucile Packard Foundation, U.S. Department of Energy, National Aeronautics and Space Administration, Stanford University, University of California, Santa Cruz, University of Pennsylvania, Ohio State University, University of Chicago, University of Michigan, Texas A and M University, University of Portsmouth, National Centre for Supercomputing Applications, Higher Education Funding Council for England, Space Telescope Science Institute, Centres de Recerca de Catalunya, European Space Agency, 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, 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, Max-Planck-Gesellschaft, 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, Technische Universität München, 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, Comisión Nacional de Investigación Científica y Tecnológica, 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 20%
Galaxies: Formation, Evolution, Phenomena
1.15
DOIOpen Access PDFOpenAlex
AI Navigator

Ask Laika to Summarize, Analyze, and Connect papers live on the map.

Summarize Papers & Methodologies

Extract key findings, datasets, and comparative methods across publications.

Benchmark Rankings & Visual Analytics

Rank top research institutions, authors, funders, topics, and journals by Field-Weighted Citation Impact (FWCI) and paper volume with instant charts.

Connect Distant Disciplines

Bridge topological clusters on the map to find hidden collaborative intersections.