A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg$^2$ of SPTpol Temperature and Polarization Data. (arXiv:1905.05777v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wu_W/0/1/0/all/0/1">W. L. K. Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mocanu_L/0/1/0/all/0/1">L. M. Mocanu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ade_P/0/1/0/all/0/1">P. A. R. Ade</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_A/0/1/0/all/0/1">A. J. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austermann_J/0/1/0/all/0/1">J. E. Austermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avva_J/0/1/0/all/0/1">J. S. Avva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beall_J/0/1/0/all/0/1">J. A. Beall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_A/0/1/0/all/0/1">A. N. Bender</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benson_B/0/1/0/all/0/1">B. A. Benson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchini_F/0/1/0/all/0/1">F. Bianchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bleem_L/0/1/0/all/0/1">L. E. Bleem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlstrom_J/0/1/0/all/0/1">J. E. Carlstrom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_C/0/1/0/all/0/1">C. L. Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiang_H/0/1/0/all/0/1">H. C. Chiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Citron_R/0/1/0/all/0/1">R. Citron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moran_C/0/1/0/all/0/1">C. Corbett Moran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crawford_T/0/1/0/all/0/1">T. M. Crawford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">A. T. Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haan_T/0/1/0/all/0/1">T. de Haan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobbs_M/0/1/0/all/0/1">M. A. Dobbs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Everett_W/0/1/0/all/0/1">W. Everett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallicchio_J/0/1/0/all/0/1">J. Gallicchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+George_E/0/1/0/all/0/1">E. M. George</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilbert_A/0/1/0/all/0/1">A. Gilbert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_N/0/1/0/all/0/1">N. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halverson_N/0/1/0/all/0/1">N. W. Halverson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harrington_N/0/1/0/all/0/1">N. Harrington</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_J/0/1/0/all/0/1">J. W. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_G/0/1/0/all/0/1">G. C. Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holder_G/0/1/0/all/0/1">G. P. Holder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holzapfel_W/0/1/0/all/0/1">W. L. Holzapfel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hou_Z/0/1/0/all/0/1">Z. Hou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hrubes_J/0/1/0/all/0/1">J. D. Hrubes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_N/0/1/0/all/0/1">N. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hubmayr_J/0/1/0/all/0/1">J. Hubmayr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Irwin_K/0/1/0/all/0/1">K. D. Irwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knox_L/0/1/0/all/0/1">L. Knox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_A/0/1/0/all/0/1">A. T. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_D/0/1/0/all/0/1">D. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lowitz_A/0/1/0/all/0/1">A. Lowitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manzotti_A/0/1/0/all/0/1">A. Manzotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">J. J. McMahon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_S/0/1/0/all/0/1">S. S. Meyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millea_M/0/1/0/all/0/1">M. Millea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montgomery_J/0/1/0/all/0/1">J. Montgomery</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nadolski_A/0/1/0/all/0/1">A. Nadolski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Natoli_T/0/1/0/all/0/1">T. Natoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nibarger_J/0/1/0/all/0/1">J. P. Nibarger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noble_G/0/1/0/all/0/1">G. I. Noble</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novosad_V/0/1/0/all/0/1">V. Novosad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omori_Y/0/1/0/all/0/1">Y. Omori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padin_S/0/1/0/all/0/1">S. Padin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patil_S/0/1/0/all/0/1">S. Patil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pryke_C/0/1/0/all/0/1">C. Pryke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichardt_C/0/1/0/all/0/1">C. L. Reichardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruhl_J/0/1/0/all/0/1">J. E. Ruhl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saliwanchik_B/0/1/0/all/0/1">B. R. Saliwanchik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sayre_J/0/1/0/all/0/1">J.T. Sayre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaffer_K/0/1/0/all/0/1">K. K. Schaffer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sievers_C/0/1/0/all/0/1">C. Sievers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simard_G/0/1/0/all/0/1">G. Simard</a>, et al. (10 additional authors not shown)

We present a measurement of the cosmic microwave background (CMB) lensing
potential using 500 deg$^2$ of 150 GHz data from the SPTpol receiver on the
South Pole Telescope. The lensing potential is reconstructed with
signal-to-noise per mode greater than unity at lensing multipoles $L lesssim
250$, using a quadratic estimator on a combination of CMB temperature and
polarization maps. We report measurements of the lensing potential power
spectrum in the multipole range of $100< L < 2000$ from sets of temperature-only, polarization-only, and minimum-variance estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit $Lambda$CDM model to the $textit{Planck}$ 2015 TT+lowP+lensing dataset. For the minimum-variance estimator, we find $A_{rm{MV}} = 0.944 pm 0.058{rm (Stat.)}pm0.025{rm (Sys.)}$; restricting to only polarization data, we find $A_{rm{POL}} = 0.906 pm 0.090 {rm (Stat.)} pm 0.040 {rm (Sys.)}$. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1 $sigma$), and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

We present a measurement of the cosmic microwave background (CMB) lensing
potential using 500 deg$^2$ of 150 GHz data from the SPTpol receiver on the
South Pole Telescope. The lensing potential is reconstructed with
signal-to-noise per mode greater than unity at lensing multipoles $L lesssim
250$, using a quadratic estimator on a combination of CMB temperature and
polarization maps. We report measurements of the lensing potential power
spectrum in the multipole range of $100< L < 2000$ from sets of
temperature-only, polarization-only, and minimum-variance estimators. We
measure the lensing amplitude by taking the ratio of the measured spectrum to
the expected spectrum from the best-fit $Lambda$CDM model to the
$textit{Planck}$ 2015 TT+lowP+lensing dataset. For the minimum-variance
estimator, we find $A_{rm{MV}} = 0.944 pm 0.058{rm (Stat.)}pm0.025{rm
(Sys.)}$; restricting to only polarization data, we find $A_{rm{POL}} = 0.906
pm 0.090 {rm (Stat.)} pm 0.040 {rm (Sys.)}$. Considering statistical
uncertainties alone, this is the most precise polarization-only lensing
amplitude constraint to date (10.1 $sigma$), and is more precise than our
temperature-only constraint. We perform null tests and consistency checks and
find no evidence for significant contamination.

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