| Summary: | We present measurements of the E-mode polarization angular auto-power spectrum (EE) and temperature–E-mode cross-power spectrum (TE) of the cosmic microwave background (CMB) using 150 GHz data from three seasons of SPTpol observations. We report the power spectra over the spherical harmonic multipole range 50 < ℓ ⩽ 8000 and detect nine acoustic peaks in the EE spectrum with high signal-to-noise ratio. These measurements are the most sensitive to date of the EE and TE power spectra at ℓ > 1050 and ℓ > 1475, respectively. The observations cover 500 deg^2, a fivefold increase in area compared to previous SPTpol analyses, which increases our sensitivity to the photon diffusion damping tail of the CMB power spectra enabling tighter constraints on ΛCDM model extensions. After masking all sources with unpolarized flux > 50 mJy, we place a 95% confidence upper limit on residual polarized point-source power of D_ℓ = ℓ(ℓ +1 )C_ℓ/2 π < 0.107 µK^2 at ℓ = 3000, suggesting that the EE damping tail dominates foregrounds to at least ℓ = 4050 with modest source masking. We find that the SPTpol data set is in mild tension with the ΛCDM model (2.1σ), and different data splits prefer parameter values that differ at the ~ 1 σ level. When fitting SPTpol data at ℓ < 1000, we find cosmological parameter constraints consistent with those for Planck temperature. Including SPTpol data at ℓ > 1000 results in a preference for a higher value of the expansion rate (H_0 = 71.3 ± 2.1 km s^-1 Mpc^-1) and a lower value for present-day density fluctuations (σg_8 = 0.77 ± 0.02). © 2018 The American Astronomical Society. Received 2017 July 30. Accepted 2017 December 4. Published 2018 January 11. The South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the ...
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