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Measurement of gravitational lensing of the cosmic microwave background using SPT-3G 2018 data

Z. Pan ^1,2,3,*, F. Bianchini ^4,5,6,†, W. L. K. Wu ^4,6, P. A. R. Ade⁷, Z. Ahmed^4,6, E. Anderes⁸, A. J. Anderson ^9,2, B. Ansarinejad¹⁰, M. Archipley ^11,12 et al.

K. Aylor¹³, L. Balkenhol ^10,14, P. S. Barry⁷, R. Basu Thakur^2,15, K. Benabed¹⁴, A. N. Bender ^1,2,16, B. A. Benson ^9,2,16, L. E. Bleem ^1,2, F. R. Bouchet ¹⁴, L. Bryant¹⁷, K. Byrum¹, E. Camphuis¹⁴, J. E. Carlstrom^2,17,3,1,16, F. W. Carter^1,2, T. W. Cecil ¹, C. L. Chang^1,2,16, P. Chaubal¹⁰, G. Chen¹⁸, P. M. Chichura ^3,2, H.-M. Cho⁶, T.-L. Chou^3,2, J.-F. Cliche¹⁹, A. Coerver²⁰, T. M. Crawford ^2,16, A. Cukierman^4,6,5, C. Daley ¹¹, T. de Haan²¹, E. V. Denison²², K. R. Dibert^16,2, J. Ding²³, M. A. Dobbs^19,24, A. Doussot¹⁴, D. Dutcher ^3,2, W. Everett²⁵, C. Feng²⁶, K. R. Ferguson ²⁷, K. Fichman^3,2, A. Foster ²⁸, J. Fu¹¹, S. Galli¹⁴, A. E. Gambrel², R. W. Gardner¹⁷, F. Ge¹³, N. Goeckner-Wald^5,4, R. Gualtieri ¹, F. Guidi¹⁴, S. Guns²⁰, N. Gupta ^10,29, N. W. Halverson^25,30, A. H. Harke-Hosemann^1,11, N. L. Harrington²⁰, J. W. Henning^1,2, G. C. Hilton²², E. Hivon¹⁴, G. P. Holder ²⁶, W. L. Holzapfel²⁰, J. C. Hood², D. Howe¹⁸, N. Huang²⁰, K. D. Irwin^4,5,6, O. Jeong²⁰, M. Jonas⁹, A. Jones¹⁸, F. Kéruzoré¹, T. S. Khaire²³, L. Knox¹³, A. M. Kofman^11,31, M. Korman²⁸, D. L. Kubik⁹, S. Kuhlmann¹, C.-L. Kuo^4,5,6, A. T. Lee^20,32, E. M. Leitch^2,16, K. Levy¹⁰, A. E. Lowitz², C. Lu²⁶, A. Maniyar^4,5,6, F. Menanteau^11,12, S. S. Meyer^2,17,3,16, D. Michalik¹⁸, M. Millea ²⁰, J. Montgomery¹⁹, A. Nadolski¹¹, Y. Nakato⁵, T. Natoli², H. Nguyen⁹, G. I. Noble ^33,34, V. Novosad²³, Y. Omori^2,16, S. Padin^2,15, P. Paschos¹⁷, J. Pearson²³, C. M. Posada²³, K. Prabhu¹³, W. Quan^3,2, S. Raghunathan ¹², M. Rahimi¹⁰, A. Rahlin ^9,2, C. L. Reichardt ¹⁰, D. Riebel¹⁸, B. Riedel¹⁷, J. E. Ruhl²⁸, J. T. Sayre²⁵, E. Schiappucci¹⁰, E. Shirokoff^2,16, G. Smecher³⁵, J. A. Sobrin ^9,2, A. A. Stark³⁶, J. Stephen¹⁷, K. T. Story^4,5, A. Suzuki³², S. Takakura^37,30, C. Tandoi¹¹, K. L. Thompson^4,5,6, B. Thorne¹³, C. Trendafilova¹², C. Tucker⁷, C. Umilta ²⁶, L. R. Vale²², K. Vanderlinde^33,34, J. D. Vieira^11,26,12, G. Wang¹, N. Whitehorn ³⁸, V. Yefremenko¹, K. W. Yoon^4,5,6, M. R. Young^9,2, and J. A. Zebrowski^2,16,9

¹High-Energy Physics Division, Argonne National Laboratory, 9700 South Cass Avenue., Lemont, Illinois 60439, USA
²Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
³Department of Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
⁴Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, California 94305, USA
⁵Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, California 94305, USA
⁶SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
⁷School of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, United Kingdom
⁸Department of Statistics, University of California, One Shields Avenue, Davis, California 95616, USA
⁹Fermi National Accelerator Laboratory, MS209, P.O. Box 500, Batavia, Illinois 60510, USA
¹⁰School of Physics, University of Melbourne, Parkville, Victoria 3010, Australia
¹¹Department of Astronomy, University of Illinois Urbana-Champaign, 1002 West Green Street, Urbana, Illinois 61801, USA
¹²Center for AstroPhysical Surveys, National Center for Supercomputing Applications, Urbana, Illinois 61801, USA
¹³Department of Physics and Astronomy, University of California, One Shields Avenue, Davis, California 95616, USA
¹⁴Institut d’Astrophysique de Paris, UMR 7095, CNRS and Sorbonne Université, 98 bis boulevard Arago, 75014 Paris, France
¹⁵California Institute of Technology, 1200 East California Boulevard., Pasadena, California 91125, USA
¹⁶Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
¹⁷Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
¹⁸University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois 60637, USA
¹⁹Department of Physics and McGill Space Institute, McGill University, 3600 Rue University, Montreal, Quebec H3A 2T8, Canada
²⁰Department of Physics, University of California, Berkeley, California 94720, USA
²¹High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
²²NIST Quantum Devices Group, 325 Broadway Mailcode 817.03, Boulder, Colorado 80305, USA
²³Materials Sciences Division, Argonne National Laboratory, 9700 South Cass Avenue, Lemont, Illinois 60439, USA
²⁴Canadian Institute for Advanced Research, CIFAR Program in Gravity and the Extreme Universe, Toronto, Ontario M5G 1Z8, Canada
²⁵CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
²⁶Department of Physics, University of Illinois Urbana-Champaign, 1110 West Green Street, Urbana, Illinois 61801, USA
²⁷Department of Physics and Astronomy, University of California, Los Angeles, California 90095, USA
²⁸Department of Physics, Case Western Reserve University, Cleveland, Ohio 44106, USA
²⁹CSIRO Space and Astronomy, PO Box 1130, Bentley, Western Australia 6102, Australia
³⁰Department of Physics, University of Colorado, Boulder, Colorado 80309, USA
³¹Department of Physics and Astronomy, University of Pennsylvania, 209 S. 33rd Street, Philadelphia, Pennsylvania 19064, USA
³²Physics Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
³³Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
³⁴David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
³⁵Three-Speed Logic, Inc., Victoria, British Columbia V8S 3Z5, Canada
³⁶Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA
³⁷Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, Colorado 80309, USA
³⁸Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA

^*panz@anl.gov
^†fbianc@slac.stanford.edu

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Phys. Rev. D 108, 122005 – Published 12 December, 2023

DOI: https://doi.org/10.1103/PhysRevD.108.122005

Abstract

We present a measurement of gravitational lensing over $1500 \deg^{2}$ of the Southern sky using SPT-3G temperature data at 95 GHz and 150 GHz taken in 2018. The lensing amplitude relative to a fiducial Planck 2018 Lambda cold dark matter ( $Λ CDM$ ) cosmology is found to be $1.020 \pm 0.060$ , excluding instrumental and astrophysical systematic uncertainties. We conduct extensive systematic and null tests to check the robustness of the lensing measurements, and report a minimum-variance combined lensing power spectrum over angular multipoles of $50 < L < 2000$ , which we use to constrain cosmological models. When analyzed alone and jointly with primary cosmic microwave background (CMB) spectra within the $Λ CDM$ model, our lensing amplitude measurements are consistent with measurements from SPT-SZ, SPTpol, ACT, and Planck. Incorporating loose priors on the baryon density and other parameters including uncertainties on a foreground bias template, we obtain a $1 σ$ constraint on $σ_{8} Ω_{m}^{0.25} = 0.595 \pm 0.026$ using the SPT-3G 2018 lensing data alone, where $σ_{8}$ is a common measure of the amplitude of structure today and $Ω_{m}$ is the matter density parameter. Combining SPT-3G 2018 lensing measurements with baryon acoustic oscillation (BAO) data, we derive parameter constraints of $σ_{8} = 0.810 \pm 0.033$ , $S_{8} \equiv σ_{8} (Ω_{m} / 0.3)^{0.5} = 0.836 \pm 0.039$ , and Hubble constant $H_{0} = {68.8}_{- 1.6}^{+ 1.3} km s^{- 1} {Mpc}^{- 1}$ . Our preferred $S_{8}$ value is higher by 1.6 to $1.8 σ$ compared to cosmic shear measurements from DES-Y3, HSC-Y3, and KiDS-1000 at lower redshift and smaller scales. We combine our lensing data with CMB anisotropy measurements from both SPT-3G and Planck to constrain extensions of $Λ CDM$ . Using CMB anisotropy and lensing measurements from SPT-3G only, we provide independent constraints on the spatial curvature of $Ω_{K} = 0.01 4_{- 0.026}^{+ 0.023}$ (95% C.L.) and the dark energy density of $Ω_{Λ} = 0.72 2_{- 0.026}^{+ 0.031}$ (68% C.L.). When combining SPT-3G lensing data with SPT-3G CMB anisotropy and BAO data, we find an upper limit on the sum of the neutrino masses of $\sum m_{ν} < 0.30 eV$ (95% C.L.). Due to the different combination of angular scales and sky area, this lensing analysis provides an independent check on lensing measurements by ACT and Planck.

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Measurement of gravitational lensing of the cosmic microwave background using SPT-3G 2018 data

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