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

Henning, J. W. and Moran, C. Corbett and Crites, A. T. and Padin, S. (2018) Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data. Astrophysical Journal, 852 (2). Art. No. 97. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20180116-071347175

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Abstract

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).


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa9ff4DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa9ff4/metaPublisherArticle
https://arxiv.org/abs/1707.09353arXivDiscussion Paper
Additional Information:© 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 Gordon and Betty Moore Foundation through grant GBMF#947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. J.W.H. is supported by the National Science Foundation under award no. AST-1402161. C.R. acknowledges support from an Australian Research Council Future Fellowship (FT150100074). B.B. is supported by the Fermi Research Alliance LLC under contract no. De-AC02-07CH11359 with the U.S. Department of Energy. 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 McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. Work at Argonne National Lab is supported by UChicago Argonne LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under contract no. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. This work used resources made available on the Jupiter cluster, a joint data-intensive computing project between the High Energy Physics Division and the Computing, Environment, and Life Sciences (CELS) Directorate at Argonne National Laboratory. The data analysis pipeline also uses the scientific python stack (Hunter 2007; Jones et al. 2001; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFPLR-1248097
NSFPHY-0114422
Gordon and Betty Moore Foundation947
Department of Energy (DOE)UNSPECIFIED
NSFAST-1402161
Australian Research CouncilFT150100074
Department of Energy (DOE)DE-AC02-07CH11359
Science and Technology Facilities Council (STFC)UNSPECIFIED
NSFAST-0956135
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Canada Research Chairs ProgramUNSPECIFIED
Department of Energy (DOE)DE-AC02-06CH11357
Argonne Center for Nanoscale MaterialsUNSPECIFIED
Subject Keywords:cosmic background radiation; cosmological parameters; cosmology: observations; polarization
Record Number:CaltechAUTHORS:20180116-071347175
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180116-071347175
Official Citation:J. W. Henning et al 2018 ApJ 852 97
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:84324
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:17 Jan 2018 18:35
Last Modified:17 Jan 2018 18:35

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