@article{fe739110d98448b98c7bdab12c9186fe,
title = "Measurements of the e -mode polarization and temperature- e -mode correlation of the CMB from SPT-3G 2018 data",
abstract = "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 deg2 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≤ℓ<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≤ℓ≤1400 for EE and 300≤ℓ≤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 data set is well fit by a ΛCDM cosmological model with parameter constraints consistent with those from Planck and SPTpol data. From SPT-3G data alone, we find H0=68.8±1.5 km s-1 Mpc-1 and σ8=0.789±0.016, with a gravitational lensing amplitude consistent with the ΛCDM prediction (AL=0.98±0.12). We combine the SPT-3G and the Planck data sets and obtain joint constraints on the ΛCDM model. The volume of the 68% confidence region in six-dimensional ΛCDM parameter space is reduced by a factor of 1.5 compared to Planck-only constraints, with no significant 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.",
author = "{(SPT-3G Collaboration)} and D. Dutcher and L. Balkenhol and Ade, {P. A.R.} and Z. Ahmed and E. Anderes and Anderson, {A. J.} and M. Archipley and Avva, {J. S.} and K. Aylor and Barry, {P. S.} and {Basu Thakur}, R. and K. Benabed and Bender, {A. N.} and Benson, {B. A.} and F. Bianchini and Bleem, {L. E.} and Bouchet, {F. R.} and L. Bryant and K. Byrum and Carlstrom, {J. E.} and Carter, {F. W.} and Cecil, {T. W.} and Chang, {C. L.} and P. Chaubal and G. Chen and Cho, {H. M.} and Chou, {T. L.} and Cliche, {J. F.} and Crawford, {T. M.} and A. Cukierman and C. Daley and {De Haan}, T. and Denison, {E. V.} and K. Dibert and J. Ding and Dobbs, {M. A.} and W. Everett and C. Feng and Ferguson, {K. R.} and A. Foster and J. Fu and S. Galli and Gambrel, {A. E.} and Gardner, {R. W.} and N. Goeckner-Wald and R. Gualtieri and S. Guns and N. Gupta and Holder, {G. P.} and Vieira, {J. D.}",
note = "Funding Information: The South Pole Telescope program is supported by the National Science Foundation (NSF) through Grants No. PLR-1248097 and No. OPP-1852617. Partial support is also provided by the NSF Physics Frontier Center Grant No. 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 No. GBMF#947 to the University of Chicago. Argonne National Laboratory{\textquoteright}s work was supported by the U.S. Department of Energy, Office of High Energy Physics, under Contract No. 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{\textquoteright}{\'E}tudes Spatiales (CNES). J. V. 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 Qu{\'e}bec Nature et technologies. N. W. H. acknowledges support from NSF CAREER Grant No. 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 , which is supported by the National Science Foundation Grant No. 1148698, and the U.S. Department of Energy{\textquoteright}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 . Publisher Copyright: {\textcopyright} 2021 American Physical Society.",
year = "2021",
month = jul,
day = "15",
doi = "10.1103/PhysRevD.104.022003",
language = "English (US)",
volume = "104",
journal = "Physical Review D",
issn = "2470-0010",
publisher = "American Physical Society",
number = "2",
}