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Title: 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 now report the $EE$ and $TE$ power spectra over the spherical harmonic multipole range $$50 < \ell \leq 8000$$, and detect the first nine acoustic peaks in the $EE$ spectrum with high signal-to-noise. These measurements are the most sensitive to date of the $EE$ and $TE$ angular polarization power spectra at $$\ell > 1050$$ and $$\ell > 1475$$, respectively. The observations cover $$500\, \rm{deg}^2$$ of sky, a fivefold increase in area compared to previous SPTpol power spectrum releases, leading to more than a factor of two reduction in bandpower uncertainties. The additional sky coverage increases our sensitivity to the photon-diffusion damping tail of the CMB angular power spectra, which enables tighter constraints on $$\Lambda CDM$$ model extensions such as primordial helium content $$Y_\rm{p}$$ and effective number of relativistic species $$N_\rm{eff}$$. Furthermore, after masking all sources with unpolarized flux $>50$ mJy we place a 95% confidence upper limit on residual polarized point-source power of $$D_\ell < 0.10 \mu{\rm K}^2$$ at $$\ell=3000$$. This limit is a factor of four lower than the previous best upper limit, and suggests that the $EE$ damping tail is brighter than foregrounds to at least $$\ell = 4100$$ with modest source masking. Finally, we find cosmological parameter constraints consistent with those for $Planck$ temperature when fitting SPTpol data at $$\ell < 1000$$. However, including SPTpol data at $$\ell > 1000$$ results in a preference for a higher value of the expansion rate ($$H_0 = 71.2 \pm 2.1\,\mbox{km}\,s^{-1}\mbox{Mpc}^{-1}$$) and a lower value for present-day density fluctuations ($$\sigma_8 = 0.77 \pm 0.02$$). (Abridged).
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Publication Date:
Report Number(s):
FERMILAB-PUB-17-297-AE; arXiv:1707.09353
Journal ID: ISSN 1538-4357; 1613500
Grant/Contract Number:
AC02-76SF00515; AC02-07CH11359; AC02-06CH11357; AC02-05CH11231; PLR-1248097; PHY-0114422; GBMF#947; AST-1402161; FT150100074; AST-0956135
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 852; Journal Issue: 2; Journal ID: ISSN 1538-4357
Institute of Physics (IOP)
Research Org:
Argonne National Lab. (ANL), Argonne, IL (United States); Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org:
USDOE; National Science Foundation (NSF); Univ. of Chicago, IL (United States); Australian Research Council (ARC); Science and Technologies Facilities Council (STFC) (United Kingdom); Natural Sciences and Engineering Research Council of Canada (NSERC); Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs program
Contributing Orgs:
Country of Publication:
United States
79 ASTRONOMY AND ASTROPHYSICS; cosmic background radiation; cosmological parameters; cosmology: observations; polarization
OSTI Identifier:
Alternate Identifier(s):
OSTI ID: 1375726; OSTI ID: 1436172