Measurements of the Temperature and E-Mode Polarization of the CMB from 500 Square Degrees of SPTpol Data

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 $50<\mathrm{\ell }\le 8000$, 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 $\mathrm{\ell }>1050$ and $\ell

1475$,respectively\mathrm{.}Theobservationscover500deg$^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 \LCDM 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 $D_\ell = \ell(\ell+1)C_\ell/2\pi <0.107,\mu{\rm K}^2$at$\ell=3000$,suggestingthatthe$EE$ damping tail dominates foregrounds to at least $\mathrm{\ell }=4050$ with modest source masking. We find that the SPTpol dataset is in mild tension with the $\mathrm{\Lambda }CDM$ model ($2.1\sigma$), and different data splits prefer parameter values that differ at the $\sim 1\sigma$ level. When fitting SPTpol data at $\mathrm{\ell }<1000$ we find cosmological parameter constraints consistent with those for $Planck$ temperature. Including SPTpol data at $\mathrm{\ell }>1000$ results in a preference for a higher value of the expansion rate ($H_0 = 71.3 \pm 2.1,\mbox{km},s^{-1}\mbox{Mpc}^{-1}$ ) and a lower value for present-day density fluctuations (${\sigma }_8=0.77\pm 0.02$).