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

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 (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mn>3</a:mn><a:mo>×</a:mo><a:mn>2</a:mn><a:mi>pt</a:mi></a:math>) 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 <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mi mathvariant="normal">Λ</c:mi></c:math> cold dark matter (<f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:mi mathvariant="normal">Λ</f:mi><f:mi>CDM</f:mi></f:math>) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi mathvariant="normal">Ω</i:mi><i:mi mathvariant="normal">m</i:mi></i:msub><i:mo>=</i:mo><i:mn>0.300</i:mn><i:mo>±</i:mo><i:mn>0.017</i:mn></i:math> and <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>σ</m:mi><m:mn>8</m:mn></m:msub><m:mo>=</m:mo><m:mn>0.797</m:mn><m:mo>±</m:mo><m:mn>0.026</m:mn></m:math>. Compared to constraints from primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (<o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:mn>1.2</o:mn><o:mi>σ</o:mi></o:math>) for the two-parameter difference. We further obtain <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:msub><q:mi>S</q:mi><q:mn>8</q:mn></q:msub><q:mo>≡</q:mo><q:msub><q:mi>σ</q:mi><q:mn>8</q:mn></q:msub><q:mo stretchy="false">(</q:mo><q:msub><q:mi mathvariant="normal">Ω</q:mi><q:mi mathvariant="normal">m</q:mi></q:msub><q:mo>/</q:mo><q:mn>0.3</q:mn><q:msup><q:mo stretchy="false">)</q:mo><q:mn>0.5</q:mn></q:msup><q:mo>=</q:mo><q:mn>0.796</q:mn><q:mo>±</q:mo><q:mn>0.013</q:mn></q:math> which is lower than the measurement at the <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mn>1.6</w:mn><w:mi>σ</w:mi></w:math> level. The combined SPT cluster, DES <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" display="inline"><y:mn>3</y:mn><y:mo>×</y:mo><y:mn>2</y:mn><y:mi>pt</y:mi></y:math>, and datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mo>∑</ab:mo><ab:msub><ab:mi>m</ab:mi><ab:mi>ν</ab:mi></ab:msub><ab:mo>&lt;</ab:mo><ab:mn>0.25</ab:mn><ab:mtext> </ab:mtext><ab:mtext> </ab:mtext><ab:mi>eV</ab:mi></ab:math> on the sum of neutrino masses. Assuming a <cb:math xmlns:cb="http://www.w3.org/1998/Math/MathML" display="inline"><cb:mi>w</cb:mi><cb:mi>CDM</cb:mi></cb:math> model, we constrain the dark energy equation of state parameter <eb:math xmlns:eb="http://www.w3.org/1998/Math/MathML" display="inline"><eb:mi>w</eb:mi><eb:mo>=</eb:mo><eb:mo>−</eb:mo><eb:mn>1.1</eb:mn><eb:msubsup><eb:mn>5</eb:mn><eb:mrow><eb:mo>−</eb:mo><eb:mn>0.17</eb:mn></eb:mrow><eb:mrow><eb:mo>+</eb:mo><eb:mn>0.23</eb:mn></eb:mrow></eb:msubsup></eb:math> and when combining with primary CMB anisotropies, we recover <gb:math xmlns:gb="http://www.w3.org/1998/Math/MathML" display="inline"><gb:mi>w</gb:mi><gb:mo>=</gb:mo><gb:mo>−</gb:mo><gb:mn>1.2</gb:mn><gb:msubsup><gb:mn>0</gb:mn><gb:mrow><gb:mo>−</gb:mo><gb:mn>0.09</gb:mn></gb:mrow><gb:mrow><gb:mo>+</gb:mo><gb:mn>0.15</gb:mn></gb:mrow></gb:msubsup></gb:math>, a <ib:math xmlns:ib="http://www.w3.org/1998/Math/MathML" display="inline"><ib:mn>1.7</ib:mn><ib:mi>σ</ib:mi></ib:math> 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.

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Physical review. D/Physical review. D.
Published
2025-03-14
DOI
https://doi.org/10.1103/physrevd.111.063533
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5
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Galaxies: Formation, Evolution, Phenomena
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article
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article

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

J. D. Hrubes, T. Natoli, O. Lahav, J. E. Carlstrom et al.
5 citations
Physical review. D/Physical review. D.
Galaxies: Formation, Evolution, Phenomena
5.77
article

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

J. D. Hrubes, T. Natoli, O. Lahav, J. E. Carlstrom, K. Eckert, A. Ferté, N. W. Halverson, E. Gaztanaga, S. Everett, J. Myles, V. Novosad, H. Camacho, M. Gatti, J. Carretero, S. Bocquet, S. Allam, S. W. Allen, F. Kéruzoré, P.-F. Leget, Guillaume Mahler, N.P. Kuropatkin, M. R. Smith, M. R. Becker, G. Giannini, A. Saro, P Fosalba, Keren Sharon, B. Yanny, C. Romero, O. Friedrich, R Chen, M. D. Gladders, P. A. R. Ade, T. M. Crawford, J. Frieman, A. J. Anderson, Gourav Khullar, D. Gruen, Francisco Javier Castander, Matthew Bayliss, Pablo Lemos, S. S. Meyer, S. Grandis, P. Paschos, J. L. Marshall, Jason E. Austermann, T. Schrabback, J. Muir, Robert P. Kraft, A. A. Plazas, T.-L. Chou, Keunho Kim, Lincoln Bryant, Gregory Tarlé, Arnab Sarkar, B. A. Benson, J. Prat, A. Amon, A. Roodman, A. Porredon, M. Brodwin, A Navarro-Alsina, B. Stalder, Eric Huff, R. Rosenfeld, Hung-Jin Huang, A. Farahi, J. Zuntz, E. M. George, C. Corbett Moran, Xiao Fang, L. E. Bleem, V. Strazzullo, A. T. Lee, F. Elsner, J. D. Vieira, O. Alves, J. J. McMahon, I. Tutusaus, G. P. Holder, James A. Beall, H. Zohren, Michael McDonald, C. Chang, J. E. Ruhl, Martin W. Sommer, C. Tucker, E. Krause, V. Yefremenko, B. Floyd, M. A. Dobbs, N. Weaverdyck, P. Chaubal, D. J. James, S. R. Hinton, Scott Dodelson, T. Shin, J. B. Stephen, J. McCullough, Todd Veach, A. Mantz, N. Gupta, Eusebio Sanchez, G. Gutierrez, A. R. Liddle, Julie Hlavacek-Larrondo, Javier Sánchez, M. Costanzi, J. Mena-Fernández, A. Campos, Eric J. Baxter, J. Cordero, M. Crocce, J. Montgomery, A. Carnero Rosell, A. T. Crites, W G Hartley, I Harrison, Behzad Ansarinejad, T. de Haan, C. Sievers, E. Sheldon, N. MacCrann, Marco Raveri, J. P. Nibarger, Y. Park, T. F. Eifler, F. Bianchini, R. H. Wechsler, C. To, W. L. Holzapfel, S. Samuroff, J. García-Bellido, J. J. Mohr, Taweewat Somboonpanyakul, Anja von der Linden, Mike Jarvis, Joseph DeRose, J. Blazek, A. Drlica-Wagner, M. Aguena, C. Sánchez, S. Lee, C. Doux, R. L. C. Ogando, K. Herner, Shivam Pandey, A. N. Bender, M. E. C. Swanson, A. Choi, Jason Gallicchio, M. Lima, R. Miquel, Y. Zhang, A. Alarcon, Christopher E. Lidman, R. P. Rollins, R. Citron, H. T. Diehl, B. Flaugher, F. Andrade-Oliveira, Dragan Huterer A, D. L. Tucker, R. A. Gruendl, A. A. Stark, J. Elvin-Poole, I. Sevilla-Noarbe, D. Li, W. L. K. Wu, T. M. Davis, S. Patil, J. A. Zebrowski, Johannes Hubmayr, Hao‐Yi Wu, Matthias Klein, B. X. Santiago, H. C. Chiang, Rebecca Canning, A. E. Lowitz, M. A. Troxel, K. K. Schaffer, K. D. Irwin, G. I. Noble, C. L. Reichardt, P. Doel, L. Salvati, E. S. Rykoff, M. Soares-Santos, M. Carrasco Kind, C. Davis, S. Padin, L. N. da Costa, Graeme Smecher, T N Varga, Nathan Whitehorn, L. F. Secco, T. M. C. Abbott, M. R. Young, W. Everett, K. Kuehn, A. K. Romer, B. Yin, C. Pryke, M. E. S. Pereira, B. R. Saliwanchik, N. Huang, D. Thomas, R. Cawthon, D. Brooks, K. Bechtol, Joseph Roberson, A. M. Flores, L. Knox, D. L. Burke, Gary Bernstein, J. K. Wuko
article en
5 citations

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 (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mn>3</a:mn><a:mo>×</a:mo><a:mn>2</a:mn><a:mi>pt</a:mi></a:math>) 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 <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mi mathvariant="normal">Λ</c:mi></c:math> cold dark matter (<f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:mi mathvariant="normal">Λ</f:mi><f:mi>CDM</f:mi></f:math>) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi mathvariant="normal">Ω</i:mi><i:mi mathvariant="normal">m</i:mi></i:msub><i:mo>=</i:mo><i:mn>0.300</i:mn><i:mo>±</i:mo><i:mn>0.017</i:mn></i:math> and <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>σ</m:mi><m:mn>8</m:mn></m:msub><m:mo>=</m:mo><m:mn>0.797</m:mn><m:mo>±</m:mo><m:mn>0.026</m:mn></m:math>. Compared to constraints from primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (<o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:mn>1.2</o:mn><o:mi>σ</o:mi></o:math>) for the two-parameter difference. We further obtain <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:msub><q:mi>S</q:mi><q:mn>8</q:mn></q:msub><q:mo>≡</q:mo><q:msub><q:mi>σ</q:mi><q:mn>8</q:mn></q:msub><q:mo stretchy="false">(</q:mo><q:msub><q:mi mathvariant="normal">Ω</q:mi><q:mi mathvariant="normal">m</q:mi></q:msub><q:mo>/</q:mo><q:mn>0.3</q:mn><q:msup><q:mo stretchy="false">)</q:mo><q:mn>0.5</q:mn></q:msup><q:mo>=</q:mo><q:mn>0.796</q:mn><q:mo>±</q:mo><q:mn>0.013</q:mn></q:math> which is lower than the measurement at the <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mn>1.6</w:mn><w:mi>σ</w:mi></w:math> level. The combined SPT cluster, DES <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" display="inline"><y:mn>3</y:mn><y:mo>×</y:mo><y:mn>2</y:mn><y:mi>pt</y:mi></y:math>, and datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mo>∑</ab:mo><ab:msub><ab:mi>m</ab:mi><ab:mi>ν</ab:mi></ab:msub><ab:mo>&lt;</ab:mo><ab:mn>0.25</ab:mn><ab:mtext> </ab:mtext><ab:mtext> </ab:mtext><ab:mi>eV</ab:mi></ab:math> on the sum of neutrino masses. Assuming a <cb:math xmlns:cb="http://www.w3.org/1998/Math/MathML" display="inline"><cb:mi>w</cb:mi><cb:mi>CDM</cb:mi></cb:math> model, we constrain the dark energy equation of state parameter <eb:math xmlns:eb="http://www.w3.org/1998/Math/MathML" display="inline"><eb:mi>w</eb:mi><eb:mo>=</eb:mo><eb:mo>−</eb:mo><eb:mn>1.1</eb:mn><eb:msubsup><eb:mn>5</eb:mn><eb:mrow><eb:mo>−</eb:mo><eb:mn>0.17</eb:mn></eb:mrow><eb:mrow><eb:mo>+</eb:mo><eb:mn>0.23</eb:mn></eb:mrow></eb:msubsup></eb:math> and when combining with primary CMB anisotropies, we recover <gb:math xmlns:gb="http://www.w3.org/1998/Math/MathML" display="inline"><gb:mi>w</gb:mi><gb:mo>=</gb:mo><gb:mo>−</gb:mo><gb:mn>1.2</gb:mn><gb:msubsup><gb:mn>0</gb:mn><gb:mrow><gb:mo>−</gb:mo><gb:mn>0.09</gb:mn></gb:mrow><gb:mrow><gb:mo>+</gb:mo><gb:mn>0.15</gb:mn></gb:mrow></gb:msubsup></gb:math>, a <ib:math xmlns:ib="http://www.w3.org/1998/Math/MathML" display="inline"><ib:mn>1.7</ib:mn><ib:mi>σ</ib:mi></ib:math> 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.

Physical review. D/Physical review. D.Vol. 111(6)
Canadian Institute for Advanced Research (CA), University of Geneva (CH), Australian National University (AU), Institució Catalana de Recerca i Estudis Avançats (ES), California Institute of Technology (US), Argonne National Laboratory (US), Oak Ridge National Laboratory (US), Southwest Research Institute (US), Northeastern University (US), Commonwealth Scientific and Industrial Research Organisation (AU), Space Telescope Science Institute (US), University of Minnesota (US), Universidade Federal do Rio Grande do Sul (BR), Goddard Space Flight Center (US), Fermi National Accelerator Laboratory (US), National Institute of Standards and Technology (US), Institute of Space Sciences (ES), University of Hawaii System (US), Jet Propulsion Laboratory (US), Harvey Mudd College (US), University of Wisconsin–Madison (US), University of Arizona (US), High Energy Accelerator Research Organization (JP), University of Lisbon (PT), University of Trieste (IT), Lawrence Berkeley National Laboratory (US), University of Waterloo (CA), University of Illinois Urbana-Champaign (US), Art Institute of Chicago (US), Universidad de La Laguna (ES), Chulalongkorn University (TH), Universität Hamburg (DE), Istituto Nazionale di Fisica Nucleare (IT), University of Sussex (GB), The University of Queensland (AU), The University of Melbourne (AU), Kavli Institute for the Physics and Mathematics of the Universe (JP), Duke University (US), Southern Methodist University (US), Université Fédérale de Toulouse Midi-Pyrénées (FR), Universidade de São Paulo (BR), Universidade Estadual de Campinas (UNICAMP) (BR), Perimeter Institute (CA), University of Toronto (CA), University of Colorado Boulder (US), Durham University (GB), Universität Innsbruck (AT), School of the Art Institute of Chicago (US), Brookhaven National Laboratory (US), Princeton University (US), Cornell University (US), University of Cambridge (GB), University of Hawaii–West Oahu (US), Université Paris-Saclay (FR), University of Michigan (US), Lowell Observatory (US), University of Minnesota System (US), Trieste Astronomical Observatory (IT), Mitchell Institute (US), SLAC National Accelerator Laboratory (US), University of Colorado System (US), Australian Astronomical Observatory (AU), University of California System (US), University of Manchester (GB), Institute for High Performance Computing and Networking (IT), CEA Grenoble (FR), Lander Institute (IL), California University of Pennsylvania (US), University of Chicago (US), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Kavli Institute for Particle Astrophysics and Cosmology (US), Excellence Cluster Origins (DE), Menlo School (US), Institute of Particle Physics (CA), Quantum Devices (United States) (US), Canadian Institute for Theoretical Astrophysics (CA), Université Bourgogne Franche-Comté (FR), Center for Astrophysics Harvard & Smithsonian (US), National Observatory (BR), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (IT), Instituto de Astrofísica de Canarias (ES), Barcelona Institute of Science and Technology (ES), National Center for Supercomputing Applications (US), Institute for Physics (US), Three-Speed Logic (Canada) (CA), Cerro Tololo Inter-American Observatory (CL), Laboratoire de Physique Subatomique et de Cosmologie (FR), NSF NOIRLab (US), Computing Center (RU), Astronomy and Space (AU), Laboratório Interinstitucional de e-Astronomia (BR), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (IT), Institute for Fundamental Physics of the Universe (IT), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), International Center for Quantum-field Measurement Systems for Studies of the Universe and Particles, Institute of Science and Technology, Institut des langues et cultures d'Europe, Amérique, Afrique, Asie et Australie (FR), University College London (GB), UK Astronomy Technology Centre (GB), McGill University (CA), The Ohio State University (US), Case Western Reserve University (US), Stony Brook University (US), William Jewell College (US), University of Portsmouth (GB), University of Cincinnati (US), Massachusetts Institute of Technology (US), Lancaster University (GB), Université de Montréal (CA), The University of Tokyo (JP), Carnegie Mellon University (US), University of Missouri–Kansas City (US), University of Missouri (US), Cardiff University (GB), University of Pennsylvania (US), Ludwig-Maximilians-Universität München (DE), University of California, Davis (US), The University of Texas at Austin (US), KTH Royal Institute of Technology (SE), Universidad del Noreste (MX), Michigan State University (US), Universidade Estadual Paulista (Unesp) (BR), Université Grenoble Alpes (FR), Ruhr University Bochum (DE), Texas A&M University (US), University of KwaZulu-Natal (ZA), University of California, Berkeley (US), Stanford University (US), University of Edinburgh (GB), Macquarie University (AU)
National Science Foundation, David and Lucile Packard Foundation, U.S. Department of Energy, 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, 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, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, Eidgenössische Technische Hochschule Zürich, Ministério da Ciência, Tecnologia e Inovação, Conselho Nacional de Desenvolvimento Científico e Tecnológico, 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, Science and Technology Facilities Council, European Research Council, European Regional Development Fund, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, High Energy Physics, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, SLAC National Accelerator Laboratory
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