A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg2 of SPTpol Temperature and Polarization Data

W. L.K. Wu; L. M. Mocanu; P. A.R. Ade; A. J. Anderson; J. E. Austermann; J. S. Avva; J. A. Beall; A. N. Bender; B. A. Benson; F. Bianchini; L. E. Bleem; J. E. Carlstrom; C. L. Chang; H. C. Chiang; R. Citron; C. Corbett Moran; T. M. Crawford; A. T. Crites; T. D. De Haan; M. A. Dobbs; W. Everett; J. Gallicchio; E. M. George; A. Gilbert; N. Gupta; N. W. Halverson; N. Harrington; J. W. Henning; G. C. Hilton; G. P. Holder; W. L. Holzapfel; Z. Hou; J. D. Hrubes; N. Huang; J. Hubmayr; K. D. Irwin; L. Knox; A. T. Lee; D. Li; A. Lowitz; A. Manzotti; J. J. McMahon; S. S. Meyer; M. Millea; J. Montgomery; A. Nadolski; T. Natoli; J. P. Nibarger; G. I. Noble; V. Novosad; Y. Omori; S. Padin; S. Patil; C. Pryke; C. L. Reichardt; J. E. Ruhl; B. R. Saliwanchik; J. T. Sayre; K. K. Schaffer; C. Sievers; G. Simard; G. Smecher; A. A. Stark; K. T. Story; C. Tucker; K. Vanderlinde; T. Veach; J. D. Vieira; G. Wang; N. Whitehorn; V. Yefremenko

doi:10.3847/1538-4357/ab4186

A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg² of SPTpol Temperature and Polarization Data

W. L.K. Wu, L. M. Mocanu, P. A.R. Ade, A. J. Anderson, J. E. Austermann, J. S. Avva, J. A. Beall, A. N. Bender, B. A. Benson, F. Bianchini, L. E. Bleem, J. E. Carlstrom, C. L. Chang, H. C. Chiang, R. Citron, C. Corbett Moran, T. M. Crawford, A. T. Crites, T. D. De Haan, M. A. DobbsW. Everett, J. Gallicchio, E. M. George, A. Gilbert, N. Gupta, N. W. Halverson, N. Harrington, J. W. Henning, G. C. Hilton, G. P. Holder, W. L. Holzapfel, Z. Hou, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, L. Knox, A. T. Lee, D. Li, A. Lowitz, A. Manzotti, J. J. McMahon, S. S. Meyer, M. Millea, J. Montgomery, A. Nadolski, T. Natoli, J. P. Nibarger, G. I. Noble, V. Novosad, Y. Omori, S. Padin, S. Patil, C. Pryke, C. L. Reichardt, J. E. Ruhl, B. R. Saliwanchik, J. T. Sayre, K. K. Schaffer, C. Sievers, G. Simard, G. Smecher, A. A. Stark, K. T. Story, C. Tucker, K. Vanderlinde, T. Veach, J. D. Vieira, G. Wang, N. Whitehorn, V. Yefremenko

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

52 Scopus citations

Abstract

We present a measurement of the cosmic microwave background lensing potential using 500 deg² 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 ≲ 250, using a quadratic estimator on a combination of cosmic microwave background 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 (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find =0.944 0.025 (Sys.) SRC=restricting to only polarization data, we find POL=0.906\pm 0.090 0.040. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

Original language	English (US)
Article number	70
Journal	Astrophysical Journal
Volume	884
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ab4186
State	Published - Oct 10 2019

Bibliographical note

Funding Information:
2019-10-10 2019-10-14 13:11:00 cgi/release: Article released bin/incoming: New from .zip NSF PLR-1248097 NSF-PFC PHY- 0114422 Gordan and Betty Moore Foundation GBMF#947 NSF PHY-1125897 NSF AST-1402161 Australian Research Council Future Fellowship FT150100074 Fermi Research Alliance De-AC02-07CH11359 NSF AST-0956135 NSF AST-1716965 NSF CSSI-1835865 yes

Funding Information:
The authors would like to acknowledge helpful comments from Chang Feng and Srinivasan Raghunathan on the manuscript. 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 No. 947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. W.L.K.W. is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. 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 the Fonds de Recherche du Qu?bec - Nature et technologies. The UCLA authors acknowledge support from NSF AST-1716965 and CSSI-1835865. 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 research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC02-05CH11231. The data analysis pipeline also uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). G. Longhi's color scheme suggestions are gratefully acknowledged.

Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.

Keywords

cosmology: cosmic background radiation
large-scale structure of the universe

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10.3847/1538-4357/ab4186

https://authors.library.caltech.edu/99251/1/Wu_2019_ApJ_884_70.pdf

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Wu, W. L. K., Mocanu, L. M., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bianchini, F., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chiang, H. C., Citron, R., Moran, C. C., Crawford, T. M., Crites, A. T., De Haan, T. D., ... Yefremenko, V. (2019). A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg² of SPTpol Temperature and Polarization Data. Astrophysical Journal, 884(1), [70]. https://doi.org/10.3847/1538-4357/ab4186

Wu, WLK, Mocanu, LM, Ade, PAR, Anderson, AJ, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, CC, Crawford, TM, Crites, AT, De Haan, TD, Dobbs, MA, Everett, W, Gallicchio, J, George, EM, Gilbert, A, Gupta, N, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Manzotti, A, McMahon, JJ, Meyer, SS, Millea, M, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Omori, Y, Padin, S, Patil, S, Pryke, C, Reichardt, CL, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Sievers, C, Simard, G, Smecher, G, Stark, AA, Story, KT, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N & Yefremenko, V 2019, 'A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg² of SPTpol Temperature and Polarization Data', Astrophysical Journal, vol. 884, no. 1, 70. https://doi.org/10.3847/1538-4357/ab4186

@article{272f184be136499887ff918bd73d4109,

title = "A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg2 of SPTpol Temperature and Polarization Data",

abstract = "We present a measurement of the cosmic microwave background lensing potential using 500 deg2 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 ≲ 250, using a quadratic estimator on a combination of cosmic microwave background 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 (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find =0.944 0.025 (Sys.) SRC=restricting to only polarization data, we find POL=0.906\pm 0.090 0.040. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.",

keywords = "cosmology: cosmic background radiation, large-scale structure of the universe",

author = "Wu, {W. L.K.} and Mocanu, {L. M.} and Ade, {P. A.R.} and Anderson, {A. J.} and Austermann, {J. E.} and Avva, {J. S.} and Beall, {J. A.} and Bender, {A. N.} and Benson, {B. A.} and F. Bianchini and Bleem, {L. E.} and Carlstrom, {J. E.} and Chang, {C. L.} and Chiang, {H. C.} and R. Citron and Moran, {C. Corbett} and Crawford, {T. M.} and Crites, {A. T.} and {De Haan}, {T. D.} and Dobbs, {M. A.} and W. Everett and J. Gallicchio and George, {E. M.} and A. Gilbert and N. Gupta and Halverson, {N. W.} and N. Harrington and Henning, {J. W.} and Hilton, {G. C.} and Holder, {G. P.} and Holzapfel, {W. L.} and Z. Hou and Hrubes, {J. D.} and N. Huang and J. Hubmayr and Irwin, {K. D.} and L. Knox and Lee, {A. T.} and D. Li and A. Lowitz and A. Manzotti and McMahon, {J. J.} and Meyer, {S. S.} and M. Millea and J. Montgomery and A. Nadolski and T. Natoli and Nibarger, {J. P.} and Noble, {G. I.} and V. Novosad and Y. Omori and S. Padin and S. Patil and C. Pryke and Reichardt, {C. L.} and Ruhl, {J. E.} and Saliwanchik, {B. R.} and Sayre, {J. T.} and Schaffer, {K. K.} and C. Sievers and G. Simard and G. Smecher and Stark, {A. A.} and Story, {K. T.} and C. Tucker and K. Vanderlinde and T. Veach and Vieira, {J. D.} and G. Wang and N. Whitehorn and V. Yefremenko",

note = "Funding Information: 2019-10-10 2019-10-14 13:11:00 cgi/release: Article released bin/incoming: New from .zip NSF PLR-1248097 NSF-PFC PHY- 0114422 Gordan and Betty Moore Foundation GBMF#947 NSF PHY-1125897 NSF AST-1402161 Australian Research Council Future Fellowship FT150100074 Fermi Research Alliance De-AC02-07CH11359 NSF AST-0956135 NSF AST-1716965 NSF CSSI-1835865 yes Funding Information: The authors would like to acknowledge helpful comments from Chang Feng and Srinivasan Raghunathan on the manuscript. 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 No. 947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. W.L.K.W. is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. 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 the Fonds de Recherche du Qu?bec - Nature et technologies. The UCLA authors acknowledge support from NSF AST-1716965 and CSSI-1835865. 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 research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC02-05CH11231. The data analysis pipeline also uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). G. Longhi's color scheme suggestions are gratefully acknowledged. Publisher Copyright: {\textcopyright} 2019. The American Astronomical Society. All rights reserved.",

year = "2019",

month = oct,

day = "10",

doi = "10.3847/1538-4357/ab4186",

language = "English (US)",

volume = "884",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "1",

}

TY - JOUR

T1 - A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg2 of SPTpol Temperature and Polarization Data

AU - Wu, W. L.K.

AU - Mocanu, L. M.

AU - Ade, P. A.R.

AU - Anderson, A. J.

AU - Austermann, J. E.

AU - Avva, J. S.

AU - Beall, J. A.

AU - Bender, A. N.

AU - Benson, B. A.

AU - Bianchini, F.

AU - Bleem, L. E.

AU - Carlstrom, J. E.

AU - Chang, C. L.

AU - Chiang, H. C.

AU - Citron, R.

AU - Moran, C. Corbett

AU - Crawford, T. M.

AU - Crites, A. T.

AU - De Haan, T. D.

AU - Dobbs, M. A.

AU - Everett, W.

AU - Gallicchio, J.

AU - George, E. M.

AU - Gilbert, A.

AU - Gupta, N.

AU - Halverson, N. W.

AU - Harrington, N.

AU - Henning, J. W.

AU - Hilton, G. C.

AU - Holder, G. P.

AU - Holzapfel, W. L.

AU - Hou, Z.

AU - Hrubes, J. D.

AU - Huang, N.

AU - Hubmayr, J.

AU - Irwin, K. D.

AU - Knox, L.

AU - Lee, A. T.

AU - Li, D.

AU - Lowitz, A.

AU - Manzotti, A.

AU - McMahon, J. J.

AU - Meyer, S. S.

AU - Millea, M.

AU - Montgomery, J.

AU - Nadolski, A.

AU - Natoli, T.

AU - Nibarger, J. P.

AU - Noble, G. I.

AU - Novosad, V.

AU - Omori, Y.

AU - Padin, S.

AU - Patil, S.

AU - Pryke, C.

AU - Reichardt, C. L.

AU - Ruhl, J. E.

AU - Saliwanchik, B. R.

AU - Sayre, J. T.

AU - Schaffer, K. K.

AU - Sievers, C.

AU - Simard, G.

AU - Smecher, G.

AU - Stark, A. A.

AU - Story, K. T.

AU - Tucker, C.

AU - Vanderlinde, K.

AU - Veach, T.

AU - Vieira, J. D.

AU - Wang, G.

AU - Whitehorn, N.

AU - Yefremenko, V.

N1 - Funding Information: 2019-10-10 2019-10-14 13:11:00 cgi/release: Article released bin/incoming: New from .zip NSF PLR-1248097 NSF-PFC PHY- 0114422 Gordan and Betty Moore Foundation GBMF#947 NSF PHY-1125897 NSF AST-1402161 Australian Research Council Future Fellowship FT150100074 Fermi Research Alliance De-AC02-07CH11359 NSF AST-0956135 NSF AST-1716965 NSF CSSI-1835865 yes Funding Information: The authors would like to acknowledge helpful comments from Chang Feng and Srinivasan Raghunathan on the manuscript. 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 No. 947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. W.L.K.W. is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. 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 the Fonds de Recherche du Qu?bec - Nature et technologies. The UCLA authors acknowledge support from NSF AST-1716965 and CSSI-1835865. 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 research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC02-05CH11231. The data analysis pipeline also uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). G. Longhi's color scheme suggestions are gratefully acknowledged. Publisher Copyright: © 2019. The American Astronomical Society. All rights reserved.

PY - 2019/10/10

Y1 - 2019/10/10

N2 - We present a measurement of the cosmic microwave background lensing potential using 500 deg2 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 ≲ 250, using a quadratic estimator on a combination of cosmic microwave background 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 (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find =0.944 0.025 (Sys.) SRC=restricting to only polarization data, we find POL=0.906\pm 0.090 0.040. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

AB - We present a measurement of the cosmic microwave background lensing potential using 500 deg2 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 ≲ 250, using a quadratic estimator on a combination of cosmic microwave background 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 (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find =0.944 0.025 (Sys.) SRC=restricting to only polarization data, we find POL=0.906\pm 0.090 0.040. Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

KW - cosmology: cosmic background radiation

KW - large-scale structure of the universe

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