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    SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G main field

    E. Camphuis1,*, W. Quan2,3,4, L. Balkenhol1,†, A. R. Khalife1, F. Ge5,6,7, F. Guidi1, N. Huang8, G. P. Lynch7, Y. Omori9,4 et al. (SPT-3G Collaboration)

    Y. Omori9,4, C. Trendafilova10, A. J. Anderson11,4,9, B. Ansarinejad12, M. Archipley9,4, P. S. Barry34, K. Benabed1, A. N. Bender2,4,9, B. A. Benson11,4,9, F. Bianchini5,6,13, L. E. Bleem2,4,9, F. R. Bouchet1, L. Bryant14, M. G. Campitiello2, J. E. Carlstrom4,14,3,2,9, C. L. Chang2,4,9, P. Chaubal12, P. M. Chichura3,4, A. Chokshi9, T.-L. Chou9,4,15, A. Coerver8, T. M. Crawford9,4, C. Daley16,17, T. de Haan18, K. R. Dibert9,4, M. A. Dobbs19,20, M. Doohan12, A. Doussot1, D. Dutcher21, W. Everett22, C. Feng23, K. R. Ferguson24,25, K. Fichman3,4, A. Foster21, S. Galli1,‡, A. E. Gambrel4, R. W. Gardner14, N. Goeckner-Wald6,5, R. Gualtieri2,26, S. Guns8, N. W. Halverson27,28, E. Hivon1, G. P. Holder23, W. L. Holzapfel8, J. C. Hood4, A. Hryciuk3,4, F. Kéruzoré2, L. Knox7, M. Korman29, K. Kornoelje9,4,2, C.-L. Kuo5,6,13, K. Levy12, A. E. Lowitz4, C. Lu23, A. Maniyar5,6,13, E. S. Martsen9,4, F. Menanteau17,10, M. Millea8, J. Montgomery19, Y. Nakato6, T. Natoli4, G. I. Noble30,31, A. Ouellette23, Z. Pan2,4,3, P. Paschos14, K. A. Phadke17,10,32, A. W. Pollak9, K. Prabhu7, S. Raghunathan10, M. Rahimi12, A. Rahlin9,4, C. L. Reichardt12, M. Rouble19, J. E. Ruhl29, E. Schiappucci12, A. Simpson9,4, J. A. Sobrin11,4, A. A. Stark33, J. Stephen14, C. Tandoi17, B. Thorne7, C. Umilta23, J. D. Vieira17,23,10, A. Vitrier1, Y. Wan17,10, N. Whitehorn25, W. L. K. Wu5,13, M. R. Young11,4, and J. A. Zebrowski4,9,11 (SPT-3G Collaboration)

    • 1Sorbonne Université, CNRS, UMR 7095, Institut d’Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, France
    • 2High-Energy Physics Division, Argonne National Laboratory, 9700 South Cass Avenue, Lemont, Illinois 60439, USA
    • 3Department of Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
    • 4Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
    • 5Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, California 94305, USA
    • 6Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, California 94305, USA
    • 7Department of Physics and Astronomy, University of California, One Shields Avenue, Davis, California 95616, USA
    • 8Department of Physics, University of California, Berkeley, California 94720, USA
    • 9Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
    • 10Center for AstroPhysical Surveys, National Center for Supercomputing Applications, Urbana, Illinois 61801, USA
    • 11Fermi National Accelerator Laboratory, MS209, P.O. Box 500, Batavia, Illinois 60510, USA
    • 12School of Physics, University of Melbourne, Parkville, VIC 3010, Australia
    • 13SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
    • 14Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
    • 15National Taiwan University, No. 1, Section 4, Roosevelt Road, Taipei 106319, Taiwan
    • 16Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191, Gif-sur-Yvette, France
    • 17Department of Astronomy, University of Illinois Urbana-Champaign, 1002 West Green Street, Urbana, Illinois 61801, USA
    • 18High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
    • 19Department of Physics and McGill Space Institute, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, Canada
    • 20Canadian Institute for Advanced Research, CIFAR Program in Gravity and the Extreme Universe, Toronto, Ontario M5G 1Z8, Canada
    • 21Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, New Jersey 08544, USA
    • 22Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
    • 23Department of Physics, University of Illinois Urbana-Champaign, 1110 West Green Street, Urbana, Illinois 61801, USA
    • 24Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
    • 25Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
    • 26Department of Physics and Astronomy, Northwestern University, 633 Clark St, Evanston, Illinois 60208, USA
    • 27CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
    • 28Department of Physics, University of Colorado, Boulder, Colorado 80309, USA
    • 29Department of Physics, Case Western Reserve University, Cleveland, Ohio 44106, USA
    • 30Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
    • 31David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
    • 32NSF-Simons AI Institute for the Sky (SkAI), 172 East Chestnut Street, Chicago, Illinois 60611, USA
    • 33Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, Massachusetts 02138, USA
    • 34School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, United Kingdom

    • *Contact author: etienne.camphuis@iap.fr
    • †Contact author: lennart.balkenhol@iap.fr
    • ‡Contact author: gallis@iap.fr
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    Phys. Rev. D 113, 083504 – Published 1 April, 2026

    DOI: https://doi.org/10.1103/7wt3-9v2y

    Abstract

    We present measurements of the temperature and E-mode polarization angular power spectra of the cosmic microwave background (CMB) from observations of 4% of the sky with SPT-3G, the current camera on the South Pole Telescope (SPT). The maps used in this analysis are the deepest used in a CMB TT/TE/EE analysis to date. The maps and resulting power spectra have been validated through blind and unblind tests. The measurements of the lensed EE and TE spectra are the most precise to date at ℓ=1800–4000 and ℓ=2200–4000, respectively. Combining our TT/TE/EE spectra with previously published SPT-3G CMB lensing results, we find parameters for the standard Λ cold dark matter (ΛCDM) model consistent with Planck and ACT DR6 with comparable constraining power. We report a Hubble constant of H0=66.66±0.60  km s−1 Mpc−1 from SPT-3G alone, 6.2σ away from local measurements from SH0ES. For the first time, combined ground-based (SPT+ACT) CMB primary and lensing data have reached Planck’s constraining power on some parameters, a milestone for CMB cosmology. The combination of these three CMB experiments yields the tightest CMB constraints to date, with H0=67.19±0.38  km s−1 Mpc−1, and the amplitude of clustering σ8=0.8137±0.0037. CMB data alone show no evidence for physics beyond ΛCDM, however, we observe a 2.8σ difference in ΛCDM between CMB and baryon acoustic oscillation (BAO) results from DESI-DR2, which is relaxed in extended models. The combination of CMB and BAO yields 2−3σ shifts from ΛCDM in the curvature of the Universe, the amplitude of CMB lensing, or the dark energy equation of state. It also drives mild preferences for models that address the Hubble tension through modified recombination or variations in the electron mass in a nonflat Universe. This work highlights the growing power of ground-based CMB experiments and lays a foundation for further cosmological analyses with SPT-3G.

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    Phys. Rev. D 113, 083504– Published 1 April, 2026
    • Received 2 July 2025
    • Accepted 5 January 2026
    Article part of CHORUS
    Accepted manuscript will be available starting 1 April, 2027.
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