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Constraints on ΛCDM Extensions from the SPT-3G 2018 EE and TE Power Spectra

Balkenhol, L. and Dutcher, D. and Ade, P. A. R. and Ahmed, Z. and Anderes, E. and Anderson, A. J. and Archipley, M. and Avva, J. S. and Aylor, K. and Barry, P. S. and Basu Thakur, R. and Benabed, K. and Bender, A. N. and Benson, B. A. and Bianchini, F. and Bleem, L. E. and Bouchet, F. R. and Bryant, L. and Byrum, K. and Carlstrom, J. E. and Carter, F. W. and Cecil, T. W. and Chang, C. L. and Chaubal, P. and Chen, G. and Cho, H. -M. and Chou, T. -L. and Cliche, J. -F. and Crawford, T. M. and Cukierman, A. and Daley, C. and Haan, T. de and Denison, E. V. and Dibert, K. and Ding, J. and Dobbs, M. A. and Everett, W. and Feng, C. and Ferguson, K. R. and Foster, A. and Fu, J. and Galli, S. and Gambrel, A. E. and Gardner, R. W. and Goeckner-Wald, N. and Gualtieri, R. and Guns, S. and Gupta, N. and Guyser, R. and Halverson, N. W. and Harke-Hosemann, A. H. and Harrington, N. L. and Henning, J. W. and Hilton, G. C. and Hivon, E. and Holder, G. P. and Holzapfel, W. L. and Hood, J. C. and Howe, D. and Huang, N. and Irwin, K. D. and Jeong, O. B. and Jonas, M. and Jones, A. and Khaire, T. S. and Knox, L. and Kofman, A. M. and Korman, M. and Kubik, D. L. and Kuhlmann, S. and Kuo, C. -L. and Lee, A. T. and Leitch, E. M. and Lowitz, A. E. and Lu, C. and Meyer, S. S. and Michalik, D. and Millea, M. and Montgomery, J. and Nadolski, A. and Natoli, T. and Nguyen, H. and Noble, G. I. and Novosad, V. and Omori, Y. and Padin, S. and Pan, Z. and Paschos, P. and Pearson, J. and Posada, C. M. and Prabhu, K. and Quan, W. and Rahlin, A. and Reichardt, C. L. and Riebel, D. and Riedel, B. and Rouble, M. and Ruhl, J. E. and Sayre, J. T. and Schiappucci, E. and Shirokoff, E. and Smecher, G. and Sobrin, J. A. and Stark, A. A. and Stephen, J. and Story, K. T. and Suzuki, A. and Thompson, K. L. and Thorne, B. and Tucker, C. and Umilta, C. and Vale, L. R. and Vanderlinde, K. and Vieira, J. D. and Wang, G. and Whitehorn, N. and Wu, W. L. K. and Yefremenko, V. and Yoon, K. W. and Young, M. R. (2021) Constraints on ΛCDM Extensions from the SPT-3G 2018 EE and TE Power Spectra. . (Unpublished)

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We present constraints on extensions to the ΛCDM cosmological model from measurements of the E-mode polarization auto-power spectrum and the temperature-E-mode cross-power spectrum of the cosmic microwave background (CMB) made using 2018 SPT-3G data. The extensions considered vary the primordial helium abundance, the effective number of relativistic degrees of freedom, the sum of neutrino masses, the relativistic energy density and mass of a sterile neutrino, and the mean spatial curvature. We do not find clear evidence for any of these extensions, from either the SPT-3G 2018 dataset alone or in combination with baryon acoustic oscillation and Planck data. None of these model extensions significantly relax the tension between Hubble-constant, H₀, constraints from the CMB and from distance-ladder measurements using Cepheids and supernovae. The addition of the SPT-3G 2018 data to Planck reduces the square-root of the determinants of the parameter covariance matrices by factors of 1.3−2.0 across these models, signaling a substantial reduction in the allowed parameter volume. We also explore CMB-based constraints on H₀ from combined SPT, Planck, and ACT DR4 datasets. While individual experiments see some indications of different H₀ values between the TT, TE, and EE spectra, the combined H₀ constraints are consistent between the three spectra. For the full combined datasets, we report H₀ = 67.49±0.53 kms⁻¹ Mpc⁻¹, which is the tightest constraint on H₀ from CMB power spectra to date and in 4.1σ tension with the most precise distance-ladder-based measurement of H₀. The SPT-3G survey is planned to continue through at least 2023, with existing maps of combined 2019 and 2020 data already having ∼3.5× lower noise than the maps used in this analysis.

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Basu Thakur, R.0000-0002-3351-3078
Additional Information:We thank Brian Fields for useful discussions on cosmological models modifying the primordial helium abundance and effective number of neutrino species. The South Pole Telescope program is supported by the National Science Foundation (NSF) through grants PLR-1248097 and OPP-1852617. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through grant GBMF#947 to the University of Chicago. Argonne National Laboratory's work was supported by the U.S. Department of Energy, Office of High Energy Physics, under contract DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. The Cardiff authors acknowledge support from the UK Science and Technologies Facilities Council (STFC). The CU Boulder group acknowledges support from NSF AST-0956135. The IAP authors acknowledge support from the Centre National d'Etudes Spatiales (CNES). JV acknowledges support from the Sloan Foundation. The Melbourne authors acknowledge support from the University of Melbourne and an Australian Research Council Future Fellowship (FT150100074). The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and the Fonds de recherche du Quebec Nature et technologies. NWH acknowledges support from NSF CAREER grant AST-0956135. The UCLA and MSU authors acknowledge support from NSF AST-1716965 and CSSI-1835865. This research was done using resources provided by the Open Science Grid [49, 50], which is supported by the National Science Foundation award 1148698, and the U.S. Department of Energy's Office of Science. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231. Some of the results in this paper have been derived using the healpy and HEALPix packages. The data analysis pipeline also uses the scientific python stack [51-53].
Funding AgencyGrant Number
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore Foundation947
Department of Energy (DOE)DE-AC02-06CH11357
Department of Energy (DOE)DE-AC02-07CH11359
Science and Technology Facilities Council (STFC)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
University of MelbourneUNSPECIFIED
Australian Research CouncilFT150100074
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Fonds de recherche du Québec - Nature et technologies (FRQNT)UNSPECIFIED
Department of Energy (DOE)DE-AC02-05CH11231
Record Number:CaltechAUTHORS:20210409-082753230
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108670
Deposited By: Tony Diaz
Deposited On:11 Apr 2021 23:12
Last Modified:11 Apr 2021 23:12

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