Multiprobe cosmology from the abundance of SPT clusters and des galaxy clustering and weak lensing

(DES and SPT Collaborations)

doi:10.1103/PhysRevD.111.063533

Multiprobe cosmology from the abundance of SPT clusters and des galaxy clustering and weak lensing

(DES and SPT Collaborations)

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Abstract

Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the Universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (3×2pt) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining Λ cold dark matter (ΛCDM) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure ωm=0.300±0.017 and σ8=0.797±0.026. Compared to constraints from Planck primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (1.2σ) for the two-parameter difference. We further obtain S8σ8(ωm/0.3)0.5=0.796±0.013 which is lower than the Planck measurement at the 1.6σ level. The combined SPT cluster, DES 3×2pt, and Planck datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit mν<0.25 eV on the sum of neutrino masses. Assuming a wCDM model, we constrain the dark energy equation of state parameter w=-1.15-0.17+0.23 and when combining with Planck primary CMB anisotropies, we recover w=-1.20-0.09+0.15, a 1.7σ difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology and our analysis paves the way for upcoming joint analyses of next-generation datasets.

Original language	English
Article number	063533
Journal	Physical Review D
Volume	111
Issue number	6
DOIs	https://doi.org/10.1103/PhysRevD.111.063533
State	Published - Mar 15 2025

Funding

This research was supported by the Ludwig-Maximilians-Universität München, the MPG Faculty Fellowship program, and the Excellence Cluster ORIGINS, which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC-2094-390783311. The Innsbruck authors acknowledge support from 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 Grants No. 899537 and No. 900565, and No. 911971. E. K. is supported in part by Department of Energy Grant No. DE-SC0020247 and the David and Lucile Packard Foundation. C. T. is supported by the Eric and Wendy Schmidt AI in Science Postdoctoral Fellowship, a Schmidt Futures program. Work at Argonne National Laboratory was supported by the U.S. Department of Energy, Office of High Energy Physics, under Contract No. DE-AC02-06CH11357. The South Pole Telescope program is supported by the National Science Foundation (NSF) through Awards No. OPP-1852617 and No. OPP-2332483. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago. 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. Frieman), 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 (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 manuscript has been authored by employees of 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.

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10.1103/PhysRevD.111.063533

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@article{6fcad26c0f4b41849ad7a39aecc011d5,

title = "Multiprobe cosmology from the abundance of SPT clusters and des galaxy clustering and weak lensing",

abstract = "Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the Universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (3×2pt) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining Λ cold dark matter (ΛCDM) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure ωm=0.300±0.017 and σ8=0.797±0.026. Compared to constraints from Planck primary cosmic microwave background (CMB) anisotropies, our constraints are only 15\% wider with a probability to exceed of 0.22 (1.2σ) for the two-parameter difference. We further obtain S8σ8(ωm/0.3)0.5=0.796±0.013 which is lower than the Planck measurement at the 1.6σ level. The combined SPT cluster, DES 3×2pt, and Planck datasets mildly prefer a nonzero positive neutrino mass, with a 95\% upper limit mν<0.25 eV on the sum of neutrino masses. Assuming a wCDM model, we constrain the dark energy equation of state parameter w=-1.15-0.17+0.23 and when combining with Planck primary CMB anisotropies, we recover w=-1.20-0.09+0.15, a 1.7σ difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology and our analysis paves the way for upcoming joint analyses of next-generation datasets.",

author = "\{(DES and SPT Collaborations)\} and S. Bocquet and S. Grandis and E. Krause and C. To and Bleem, \{L. E.\} and M. Klein and Mohr, \{J. J.\} and T. Schrabback and A. Alarcon and O. Alves and A. Amon and F. Andrade-Oliveira and Baxter, \{E. J.\} and K. Bechtol and Becker, \{M. R.\} and Bernstein, \{G. M.\} and J. Blazek and H. Camacho and A. Campos and \{Carnero Rosell\}, A. and \{Carrasco Kind\}, M. and R. Cawthon and C. Chang and R. Chen and A. Choi and J. Cordero and M. Crocce and C. Davis and J. Derose and Diehl, \{H. T.\} and S. Dodelson and C. Doux and A. Drlica-Wagner and K. Eckert and Eifler, \{T. F.\} and F. Elsner and J. Elvin-Poole and S. Everett and X. Fang and A. Fert{\'e} and P. Fosalba and O. Friedrich and J. Frieman and M. Gatti and G. Giannini and D. Gruen and Gruendl, \{R. A.\} and I. Harrison and Hartley, \{W. G.\} and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2025 authors. Published by the American Physical Society.",

year = "2025",

month = mar,

day = "15",

doi = "10.1103/PhysRevD.111.063533",

language = "English",

volume = "111",

journal = "Physical Review D",

issn = "2470-0010",

publisher = "American Physical Society",

number = "6",

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TY - JOUR

T1 - Multiprobe cosmology from the abundance of SPT clusters and des galaxy clustering and weak lensing

AU - (DES and SPT Collaborations)

AU - Bocquet, S.

AU - Grandis, S.

AU - Krause, E.

AU - To, C.

AU - Bleem, L. E.

AU - Klein, M.

AU - Mohr, J. J.

AU - Schrabback, T.

AU - Alarcon, A.

AU - Alves, O.

AU - Amon, A.

AU - Andrade-Oliveira, F.

AU - Baxter, E. J.

AU - Bechtol, K.

AU - Becker, M. R.

AU - Bernstein, G. M.

AU - Blazek, J.

AU - Camacho, H.

AU - Campos, A.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Cawthon, R.

AU - Chang, C.

AU - Chen, R.

AU - Choi, A.

AU - Cordero, J.

AU - Crocce, M.

AU - Davis, C.

AU - Derose, J.

AU - Diehl, H. T.

AU - Dodelson, S.

AU - Doux, C.

AU - Drlica-Wagner, A.

AU - Eckert, K.

AU - Eifler, T. F.

AU - Elsner, F.

AU - Elvin-Poole, J.

AU - Everett, S.

AU - Fang, X.

AU - Ferté, A.

AU - Fosalba, P.

AU - Friedrich, O.

AU - Frieman, J.

AU - Gatti, M.

AU - Giannini, G.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Harrison, I.

AU - Hartley, W. G.

AU - Suchyta, E.

PY - 2025/3/15

Y1 - 2025/3/15

N2 - Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the Universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (3×2pt) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining Λ cold dark matter (ΛCDM) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure ωm=0.300±0.017 and σ8=0.797±0.026. Compared to constraints from Planck primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (1.2σ) for the two-parameter difference. We further obtain S8σ8(ωm/0.3)0.5=0.796±0.013 which is lower than the Planck measurement at the 1.6σ level. The combined SPT cluster, DES 3×2pt, and Planck datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit mν<0.25 eV on the sum of neutrino masses. Assuming a wCDM model, we constrain the dark energy equation of state parameter w=-1.15-0.17+0.23 and when combining with Planck primary CMB anisotropies, we recover w=-1.20-0.09+0.15, a 1.7σ difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology and our analysis paves the way for upcoming joint analyses of next-generation datasets.

AB - Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the Universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (3×2pt) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining Λ cold dark matter (ΛCDM) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure ωm=0.300±0.017 and σ8=0.797±0.026. Compared to constraints from Planck primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (1.2σ) for the two-parameter difference. We further obtain S8σ8(ωm/0.3)0.5=0.796±0.013 which is lower than the Planck measurement at the 1.6σ level. The combined SPT cluster, DES 3×2pt, and Planck datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit mν<0.25 eV on the sum of neutrino masses. Assuming a wCDM model, we constrain the dark energy equation of state parameter w=-1.15-0.17+0.23 and when combining with Planck primary CMB anisotropies, we recover w=-1.20-0.09+0.15, a 1.7σ difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology and our analysis paves the way for upcoming joint analyses of next-generation datasets.

UR - https://www.scopus.com/pages/publications/105001188817

U2 - 10.1103/PhysRevD.111.063533

DO - 10.1103/PhysRevD.111.063533

M3 - Article

AN - SCOPUS:105001188817

SN - 2470-0010

VL - 111

JO - Physical Review D

JF - Physical Review D

IS - 6

M1 - 063533

ER -

Multiprobe cosmology from the abundance of SPT clusters and des galaxy clustering and weak lensing

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