A 2500 deg2 CMB Lensing Map from Combined South Pole Telescope and Planck Data

Y. Omori; R. Chown; G. Simard; K. T. Story; K. Aylor; E. J. Baxter; B. A. Benson; L. E. Bleem; J. E. Carlstrom; C. L. Chang; H. M. Cho; T. M. Crawford; A. T. Crites; T. De Haan; M. A. Dobbs; W. B. Everett; E. M. George; N. W. Halverson; N. L. Harrington; G. P. Holder; Z. Hou; W. L. Holzapfel; J. D. Hrubes; L. Knox; A. T. Lee; E. M. Leitch; D. Luong-Van; A. Manzotti; D. P. Marrone; J. J. McMahon; S. S. Meyer; L. M. Mocanu; J. J. Mohr; T. Natoli; S. Padin; C. Pryke; C. L. Reichardt; J. E. Ruhl; J. T. Sayre; K. K. Schaffer; E. Shirokoff; Z. Staniszewski; A. A. Stark; K. Vanderlinde; J. D. Vieira; R. Williamson; O. Zahn

doi:10.3847/1538-4357/aa8d1d

A 2500 deg² CMB Lensing Map from Combined South Pole Telescope and Planck Data

Y. Omori, R. Chown, G. Simard, K. T. Story, K. Aylor, E. J. Baxter, B. A. Benson, L. E. Bleem, J. E. Carlstrom, C. L. Chang, H. M. Cho, T. M. Crawford, A. T. Crites, T. De Haan, M. A. Dobbs, W. B. Everett, E. M. George, N. W. Halverson, N. L. Harrington, G. P. HolderZ. Hou, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, E. M. Leitch, D. Luong-Van, A. Manzotti, D. P. Marrone, J. J. McMahon, S. S. Meyer, L. M. Mocanu, J. J. Mohr, T. Natoli, S. Padin, C. Pryke, C. L. Reichardt, J. E. Ruhl, J. T. Sayre, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, K. Vanderlinde, J. D. Vieira, R. Williamson, O. Zahn

Physics and Astronomy (Twin Cities)

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

43 Scopus citations

Abstract

We present a cosmic microwave background (CMB) lensing map produced from a linear combination of South Pole Telescope (SPT) and Planck temperature data. The 150 GHz temperature data from the 2500 deg² SPT-SZ survey is combined with the Planck 143 GHz data in harmonic space to obtain a temperature map that has a broader ℓ coverage and less noise than either individual map. Using a quadratic estimator technique on this combined temperature map, we produce a map of the gravitational lensing potential projected along the line of sight. We measure the auto-spectrum of the lensing potential C_L^φφ, and compare it to the theoretical prediction for a ΛCDM cosmology consistent with the Planck 2015 data set, finding a best-fit amplitude of 0.95_-0.06^+0.06(stat.)_0.01^+0.01(sys.). The null hypothesis of no lensing is rejected at a significance of 24σ. One important use of such a lensing potential map is in cross-correlations with other dark matter tracers. We demonstrate this cross-correlation in practice by calculating the cross-spectrum, C_L^φG, between the SPT+Planck lensing map and Wide-field Infrared Survey Explorer (WISE) galaxies. We fit C_L^φG to a power law of the form P_L = a(L/L₀)^-b with a, L ₀, and b fixed, and find η^φG = C_L^φG/P_L = 0.94_-0.04^+0.04, which is marginally lower, but in good agreement with η^φG = 1.00_-0.01^+0.02, the best-fit amplitude for the cross-correlation of Planck-2015 CMB lensing and WISE galaxies over ∼67% of the sky. The lensing potential map presented here will be used for cross-correlation studies with the Dark Energy Survey, whose footprint nearly completely covers the SPT 2500 deg² field.

Original language	English (US)
Article number	124
Journal	Astrophysical Journal
Volume	849
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/aa8d1d
State	Published - Nov 10 2017

Bibliographical note

Funding Information:
We thank Hao-Yi Wu and Olivier Doré for the theoretical prediction for the cross-correlation between CIB and CMB lensing. 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. 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. C.R. acknowledges support from a Australian Research Council Future Fellowship (FT150100074). B.B. is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Argonne National Laboratorys work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. Computations were made on the supercomputer Guillimin from McGill University, managed by Calcul Québec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), the ministère de l’Économie, de la science et de l’innovation du Québec (MESI) and the Fonds de recherche du Québec—Nature et technologies (FRQ-NT). This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. 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 results in this paper have been derived using the following packages: ASTROPY, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), CAMB (Lewis et al. 2000; Howlett et al. 2012), CMOCEAN,49 HEALPIX (Górski et al. 2005), IPYTHON (Pérez & Granger 2007), LENSPIX (Lewis 2005), MATPLOTLIB (Hunter 2007), NUMPY and SCIPY (van der Walt et al. 2011), POLSPICE (Chon et al. 2004), and QUICKLENS (see footnote 39).

Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.

Keywords

cosmic background radiation
gravitational lensing: weak
large-scale structure of universe

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10.3847/1538-4357/aa8d1d

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Omori, Y., Chown, R., Simard, G., Story, K. T., Aylor, K., Baxter, E. J., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Cho, H. M., Crawford, T. M., Crites, A. T., Haan, T. D., Dobbs, M. A., Everett, W. B., George, E. M., Halverson, N. W., Harrington, N. L., ... Zahn, O. (2017). A 2500 deg² CMB Lensing Map from Combined South Pole Telescope and Planck Data. Astrophysical Journal, 849(2), Article 124. https://doi.org/10.3847/1538-4357/aa8d1d

Omori, Y, Chown, R, Simard, G, Story, KT, Aylor, K, Baxter, EJ, Benson, BA, Bleem, LE, Carlstrom, JE, Chang, CL, Cho, HM, Crawford, TM, Crites, AT, Haan, TD, Dobbs, MA, Everett, WB, George, EM, Halverson, NW, Harrington, NL, Holder, GP, Hou, Z, Holzapfel, WL, Hrubes, JD, Knox, L, Lee, AT, Leitch, EM, Luong-Van, D, Manzotti, A, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Natoli, T, Padin, S, Pryke, C, Reichardt, CL, Ruhl, JE, Sayre, JT, Schaffer, KK, Shirokoff, E, Staniszewski, Z, Stark, AA, Vanderlinde, K, Vieira, JD, Williamson, R & Zahn, O 2017, 'A 2500 deg² CMB Lensing Map from Combined South Pole Telescope and Planck Data', Astrophysical Journal, vol. 849, no. 2, 124. https://doi.org/10.3847/1538-4357/aa8d1d

@article{d520d54aff2b46dc88dbbce565f13fe3,

title = "A 2500 deg2 CMB Lensing Map from Combined South Pole Telescope and Planck Data",

abstract = "We present a cosmic microwave background (CMB) lensing map produced from a linear combination of South Pole Telescope (SPT) and Planck temperature data. The 150 GHz temperature data from the 2500 deg2 SPT-SZ survey is combined with the Planck 143 GHz data in harmonic space to obtain a temperature map that has a broader ℓ coverage and less noise than either individual map. Using a quadratic estimator technique on this combined temperature map, we produce a map of the gravitational lensing potential projected along the line of sight. We measure the auto-spectrum of the lensing potential CLφφ, and compare it to the theoretical prediction for a ΛCDM cosmology consistent with the Planck 2015 data set, finding a best-fit amplitude of 0.95-0.06+0.06(stat.)0.01+0.01(sys.). The null hypothesis of no lensing is rejected at a significance of 24σ. One important use of such a lensing potential map is in cross-correlations with other dark matter tracers. We demonstrate this cross-correlation in practice by calculating the cross-spectrum, CLφG, between the SPT+Planck lensing map and Wide-field Infrared Survey Explorer (WISE) galaxies. We fit CLφG to a power law of the form PL = a(L/L0)-b with a, L 0, and b fixed, and find ηφG = CLφG/PL = 0.94-0.04+0.04, which is marginally lower, but in good agreement with ηφG = 1.00-0.01+0.02, the best-fit amplitude for the cross-correlation of Planck-2015 CMB lensing and WISE galaxies over ∼67% of the sky. The lensing potential map presented here will be used for cross-correlation studies with the Dark Energy Survey, whose footprint nearly completely covers the SPT 2500 deg2 field.",

keywords = "cosmic background radiation, gravitational lensing: weak, large-scale structure of universe",

author = "Y. Omori and R. Chown and G. Simard and Story, {K. T.} and K. Aylor and Baxter, {E. J.} and Benson, {B. A.} and Bleem, {L. E.} and Carlstrom, {J. E.} and Chang, {C. L.} and Cho, {H. M.} and Crawford, {T. M.} and Crites, {A. T.} and Haan, {T. De} and Dobbs, {M. A.} and Everett, {W. B.} and George, {E. M.} and Halverson, {N. W.} and Harrington, {N. L.} and Holder, {G. P.} and Z. Hou and Holzapfel, {W. L.} and Hrubes, {J. D.} and L. Knox and Lee, {A. T.} and Leitch, {E. M.} and D. Luong-Van and A. Manzotti and Marrone, {D. P.} and McMahon, {J. J.} and Meyer, {S. S.} and Mocanu, {L. M.} and Mohr, {J. J.} and T. Natoli and S. Padin and C. Pryke and Reichardt, {C. L.} and Ruhl, {J. E.} and Sayre, {J. T.} and Schaffer, {K. K.} and E. Shirokoff and Z. Staniszewski and Stark, {A. A.} and K. Vanderlinde and Vieira, {J. D.} and R. Williamson and O. Zahn",

note = "Funding Information: We thank Hao-Yi Wu and Olivier Dor{\'e} for the theoretical prediction for the cross-correlation between CIB and CMB lensing. 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. 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. C.R. acknowledges support from a Australian Research Council Future Fellowship (FT150100074). B.B. is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Argonne National Laboratorys work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. Computations were made on the supercomputer Guillimin from McGill University, managed by Calcul Qu{\'e}bec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), the minist{\`e}re de l{\textquoteright}{\'E}conomie, de la science et de l{\textquoteright}innovation du Qu{\'e}bec (MESI) and the Fonds de recherche du Qu{\'e}bec—Nature et technologies (FRQ-NT). This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. 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 results in this paper have been derived using the following packages: ASTROPY, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), CAMB (Lewis et al. 2000; Howlett et al. 2012), CMOCEAN,49 HEALPIX (G{\'o}rski et al. 2005), IPYTHON (P{\'e}rez & Granger 2007), LENSPIX (Lewis 2005), MATPLOTLIB (Hunter 2007), NUMPY and SCIPY (van der Walt et al. 2011), POLSPICE (Chon et al. 2004), and QUICKLENS (see footnote 39). Publisher Copyright: {\textcopyright} 2017. The American Astronomical Society. All rights reserved.",

year = "2017",

month = nov,

day = "10",

doi = "10.3847/1538-4357/aa8d1d",

language = "English (US)",

volume = "849",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "2",

}

TY - JOUR

T1 - A 2500 deg2 CMB Lensing Map from Combined South Pole Telescope and Planck Data

AU - Omori, Y.

AU - Chown, R.

AU - Simard, G.

AU - Story, K. T.

AU - Aylor, K.

AU - Baxter, E. J.

AU - Benson, B. A.

AU - Bleem, L. E.

AU - Carlstrom, J. E.

AU - Chang, C. L.

AU - Cho, H. M.

AU - Crawford, T. M.

AU - Crites, A. T.

AU - Haan, T. De

AU - Dobbs, M. A.

AU - Everett, W. B.

AU - George, E. M.

AU - Halverson, N. W.

AU - Harrington, N. L.

AU - Holder, G. P.

AU - Hou, Z.

AU - Holzapfel, W. L.

AU - Hrubes, J. D.

AU - Knox, L.

AU - Lee, A. T.

AU - Leitch, E. M.

AU - Luong-Van, D.

AU - Manzotti, A.

AU - Marrone, D. P.

AU - McMahon, J. J.

AU - Meyer, S. S.

AU - Mocanu, L. M.

AU - Mohr, J. J.

AU - Natoli, T.

AU - Padin, S.

AU - Pryke, C.

AU - Reichardt, C. L.

AU - Ruhl, J. E.

AU - Sayre, J. T.

AU - Schaffer, K. K.

AU - Shirokoff, E.

AU - Staniszewski, Z.

AU - Stark, A. A.

AU - Vanderlinde, K.

AU - Vieira, J. D.

AU - Williamson, R.

AU - Zahn, O.

N1 - Funding Information: We thank Hao-Yi Wu and Olivier Doré for the theoretical prediction for the cross-correlation between CIB and CMB lensing. 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. 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. C.R. acknowledges support from a Australian Research Council Future Fellowship (FT150100074). B.B. is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Argonne National Laboratorys work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. Computations were made on the supercomputer Guillimin from McGill University, managed by Calcul Québec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), the ministère de l’Économie, de la science et de l’innovation du Québec (MESI) and the Fonds de recherche du Québec—Nature et technologies (FRQ-NT). This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. 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 results in this paper have been derived using the following packages: ASTROPY, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), CAMB (Lewis et al. 2000; Howlett et al. 2012), CMOCEAN,49 HEALPIX (Górski et al. 2005), IPYTHON (Pérez & Granger 2007), LENSPIX (Lewis 2005), MATPLOTLIB (Hunter 2007), NUMPY and SCIPY (van der Walt et al. 2011), POLSPICE (Chon et al. 2004), and QUICKLENS (see footnote 39). Publisher Copyright: © 2017. The American Astronomical Society. All rights reserved.

PY - 2017/11/10

Y1 - 2017/11/10

N2 - We present a cosmic microwave background (CMB) lensing map produced from a linear combination of South Pole Telescope (SPT) and Planck temperature data. The 150 GHz temperature data from the 2500 deg2 SPT-SZ survey is combined with the Planck 143 GHz data in harmonic space to obtain a temperature map that has a broader ℓ coverage and less noise than either individual map. Using a quadratic estimator technique on this combined temperature map, we produce a map of the gravitational lensing potential projected along the line of sight. We measure the auto-spectrum of the lensing potential CLφφ, and compare it to the theoretical prediction for a ΛCDM cosmology consistent with the Planck 2015 data set, finding a best-fit amplitude of 0.95-0.06+0.06(stat.)0.01+0.01(sys.). The null hypothesis of no lensing is rejected at a significance of 24σ. One important use of such a lensing potential map is in cross-correlations with other dark matter tracers. We demonstrate this cross-correlation in practice by calculating the cross-spectrum, CLφG, between the SPT+Planck lensing map and Wide-field Infrared Survey Explorer (WISE) galaxies. We fit CLφG to a power law of the form PL = a(L/L0)-b with a, L 0, and b fixed, and find ηφG = CLφG/PL = 0.94-0.04+0.04, which is marginally lower, but in good agreement with ηφG = 1.00-0.01+0.02, the best-fit amplitude for the cross-correlation of Planck-2015 CMB lensing and WISE galaxies over ∼67% of the sky. The lensing potential map presented here will be used for cross-correlation studies with the Dark Energy Survey, whose footprint nearly completely covers the SPT 2500 deg2 field.

AB - We present a cosmic microwave background (CMB) lensing map produced from a linear combination of South Pole Telescope (SPT) and Planck temperature data. The 150 GHz temperature data from the 2500 deg2 SPT-SZ survey is combined with the Planck 143 GHz data in harmonic space to obtain a temperature map that has a broader ℓ coverage and less noise than either individual map. Using a quadratic estimator technique on this combined temperature map, we produce a map of the gravitational lensing potential projected along the line of sight. We measure the auto-spectrum of the lensing potential CLφφ, and compare it to the theoretical prediction for a ΛCDM cosmology consistent with the Planck 2015 data set, finding a best-fit amplitude of 0.95-0.06+0.06(stat.)0.01+0.01(sys.). The null hypothesis of no lensing is rejected at a significance of 24σ. One important use of such a lensing potential map is in cross-correlations with other dark matter tracers. We demonstrate this cross-correlation in practice by calculating the cross-spectrum, CLφG, between the SPT+Planck lensing map and Wide-field Infrared Survey Explorer (WISE) galaxies. We fit CLφG to a power law of the form PL = a(L/L0)-b with a, L 0, and b fixed, and find ηφG = CLφG/PL = 0.94-0.04+0.04, which is marginally lower, but in good agreement with ηφG = 1.00-0.01+0.02, the best-fit amplitude for the cross-correlation of Planck-2015 CMB lensing and WISE galaxies over ∼67% of the sky. The lensing potential map presented here will be used for cross-correlation studies with the Dark Energy Survey, whose footprint nearly completely covers the SPT 2500 deg2 field.

KW - cosmic background radiation

KW - gravitational lensing: weak

KW - large-scale structure of universe

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