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

(SPT and DES Collaborations)

doi:10.1103/PhysRevD.111.083543

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

(SPT and DES Collaborations)

Workflow Systems

Research output: Contribution to journal › Article › peer-review

1 Scopus 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 SU(N) gauge theory (interaction rate with power-law index n=0 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, ζDR=TDR/TCMB. We find an upper limit ζDR<17% at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find ζDR<10%, 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 S8 tension.

Original language	English
Article number	083543
Journal	Physical Review D
Volume	111
Issue number	8
DOIs	https://doi.org/10.1103/PhysRevD.111.083543
State	Published - Apr 15 2025

Funding

We acknowledge support by the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy–EXC-2094–390783311. We acknowledge support from the Max Planck Society Faculty Fellowship program at MPE, the Ludwig-Maximilians-Universität in Munich, and the Technical University of Munich. The analysis was carried out at the Computational Center for Particle and Astrophysics (C2PAP) which is a computing facility from ORIGINS. Asmaa Mazoun thanks the mentoring program of ORIGINS; especially, Amelia Bayo Aran for her valuable advice. 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. 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 Universe, the University of Michigan, NSF 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. This was based in part on observations at NSF Cerro Tololo Inter-American Observatory at NSF 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. PID2021-123012, No. PID2021-128989, No. PID2022-141079, No. SEV-2016-0588, No. CEX2020-001058-M, and No. CEX2020-001007-S, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). 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. 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. 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: Schrabback), 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.).

Access to Document

10.1103/PhysRevD.111.083543

Cite this

@article{267fd40989f94037b1d65a8598bdb94e,

title = "Interacting dark sector within ETHOS: Cosmological constraints from SPT cluster abundance with des and HST weak lensing data",

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 SU(N) gauge theory (interaction rate with power-law index n=0 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, ζDR=TDR/TCMB. We find an upper limit ζDR<17\% at 95\% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find ζDR<10\%, 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 S8 tension.",

author = "\{(SPT and DES Collaborations)\} and A. Mazoun and S. Bocquet and Mohr, \{J. J.\} and M. Garny and H. Rubira and M. Klein and Bleem, \{L. E.\} and S. Grandis and T. Schrabback and M. Aguena and S. Allam and Allen, \{S. W.\} and O. Alves and F. Andrade-Oliveira and D. Brooks and \{Carnero Rosell\}, A. and \{Carrasco Kind\}, M. and J. Carretero and M. Costanzi and \{Da Costa\}, \{L. N.\} and Davis, \{T. M.\} and S. Desai and \{De Vicente\}, J. and Diehl, \{H. T.\} and S. Dodelson and P. Doel and S. Everett and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and R. Gassis and G. Giannini and D. Gr{\"u}n and G. Gutierrez and Hinton, \{S. R.\} and Hollowood, \{D. L.\} and James, \{D. J.\} and K. Kuehn and O. Lahav and S. Lee and M. Lima and G. Mahler and Marshall, \{J. L.\} and R. Miquel and J. Myles and Ogando, \{R. L.C.\} and Pereira, \{M. E.S.\} and A. Pieres and \{Plazas Malag{\'o}n\}, \{A. A.\} and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2025 authors. Published by the American Physical Society. Published by the American Physical Society under the terms of the {"}https://creativecommons.org/licenses/by/4.0/{"}Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.",

year = "2025",

month = apr,

day = "15",

doi = "10.1103/PhysRevD.111.083543",

language = "English",

volume = "111",

journal = "Physical Review D",

issn = "2470-0010",

publisher = "American Physical Society",

number = "8",

}

TY - JOUR

T1 - Interacting dark sector within ETHOS

T2 - Cosmological constraints from SPT cluster abundance with des and HST weak lensing data

AU - (SPT and DES Collaborations)

AU - Mazoun, A.

AU - Bocquet, S.

AU - Mohr, J. J.

AU - Garny, M.

AU - Rubira, H.

AU - Klein, M.

AU - Bleem, L. E.

AU - Grandis, S.

AU - Schrabback, T.

AU - Aguena, M.

AU - Allam, S.

AU - Allen, S. W.

AU - Alves, O.

AU - Andrade-Oliveira, F.

AU - Brooks, D.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Costanzi, M.

AU - Da Costa, L. N.

AU - Davis, T. M.

AU - Desai, S.

AU - De Vicente, J.

AU - Diehl, H. T.

AU - Dodelson, S.

AU - Doel, P.

AU - Everett, S.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gassis, R.

AU - Giannini, G.

AU - Grün, D.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - James, D. J.

AU - Kuehn, K.

AU - Lahav, O.

AU - Lee, S.

AU - Lima, M.

AU - Mahler, G.

AU - Marshall, J. L.

AU - Miquel, R.

AU - Myles, J.

AU - Ogando, R. L.C.

AU - Pereira, M. E.S.

AU - Pieres, A.

AU - Plazas Malagón, A. A.

AU - Suchyta, E.

N1 - Publisher Copyright: © 2025 authors. Published by the American Physical Society. Published by the American Physical Society under the terms of the "https://creativecommons.org/licenses/by/4.0/"Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.

PY - 2025/4/15

Y1 - 2025/4/15

N2 - 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 SU(N) gauge theory (interaction rate with power-law index n=0 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, ζDR=TDR/TCMB. We find an upper limit ζDR<17% at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find ζDR<10%, 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 S8 tension.

AB - 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 SU(N) gauge theory (interaction rate with power-law index n=0 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, ζDR=TDR/TCMB. We find an upper limit ζDR<17% at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find ζDR<10%, 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 S8 tension.

UR - https://www.scopus.com/pages/publications/105003882857

U2 - 10.1103/PhysRevD.111.083543

DO - 10.1103/PhysRevD.111.083543

M3 - Article

AN - SCOPUS:105003882857

SN - 2470-0010

VL - 111

JO - Physical Review D

JF - Physical Review D

IS - 8

M1 - 083543

ER -

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

Abstract

Funding

Access to Document

Other files and links

Fingerprint

Cite this