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

description: We present constraints on extensions to the $Λ$CDM 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 \textit{Planck} data. None of these model extensions significantly relax the tension between Hubble-constant, $H_0$, constraints from the CMB and from distance-ladder measurements using Cepheids and supernovae. The addition of the SPT-3G 2018 data to \textit{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 $H_0$ from combined SPT, \textit{Planck}, and ACT DR4 datasets. While individual experiments see some indications of different $H_0$ values between the $TT$, $TE$, and $EE$ spectra, the combined $H_0$ constraints are consistent between the three spectra. For the full combined datasets, we report $H_0 = 67.49 \pm 0.53\,\mathrm{km\,s^{-1}\,Mpc^{-1}}$, which is the tightest constraint on $H_0$ from CMB power spectra to date and in $4.1\,σ$ tension with the most precise distance-ladder-based measurement of $H_0$. The SPT-3G survey is planned to continue through at least 2023, with existing maps of combined 2019 and 2020 data already having $\sim3.5\times$ lower noise than the maps used in this analysis.
description: Submitted to PRD; 19 pages, 7 figures