Measurements of the E-Mode Polarization and Temperature-E-Mode Correlation of the CMB from SPT-3G 2018 Data
Creators: name: Dutcher, D.
name: Balkenhol, L.
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: Raghunathan, S.
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 measurements of the $E$-mode ($EE$) polarization power spectrum and temperature-$E$-mode ($TE$) cross-power spectrum of the cosmic microwave background using data collected by SPT-3G, the latest instrument installed on the South Pole Telescope. This analysis uses observations of a 1500 deg$^2$ region at 95, 150, and 220 GHz taken over a four month period in 2018. We report binned values of the $EE$ and $TE$ power spectra over the angular multipole range $300 \le \ell &lt; 3000$, using the multifrequency data to construct six semi-independent estimates of each power spectrum and their minimum-variance combination. These measurements improve upon the previous results of SPTpol across the multipole ranges $300 \le \ell \le 1400$ for $EE$ and $300 \le \ell \le 1700$ for $TE$, resulting in constraints on cosmological parameters comparable to those from other current leading ground-based experiments. We find that the SPT-3G dataset is well-fit by a $Λ$CDM cosmological model with parameter constraints consistent with those from Planck and SPTpol data. From SPT-3G data alone, we find $H_0 = 68.8 \pm 1.5 \mathrm{km\,s^{-1}\,Mpc^{-1}}$ and $σ_8 = 0.789 \pm 0.016$, with a gravitational lensing amplitude consistent with the $Λ$CDM prediction ($A_L = 0.98 \pm 0.12$). We combine the SPT-3G and the Planck datasets and obtain joint constraints on the $Λ$CDM model. The volume of the 68% confidence region in six-dimensional $Λ$CDM parameter space is reduced by a factor of 1.5 compared to Planck-only constraints, with only slight shifts in central values. We note that the results presented here are obtained from data collected during just half of a typical observing season with only part of the focal plane operable, and that the active detector count has since nearly doubled for observations made with SPT-3G after 2018.