Constraints on Cosmological Parameters from the 500 deg 2 SPTPOL Lensing Power Spectrum

We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg 2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spect...

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Veröffentlicht in:	The Astrophysical journal 2020-01, Vol.888 (2), p.119
Hauptverfasser:	Bianchini, F., Wu, W. L. K., Ade, P. A. R., Anderson, A. J., Austermann, J. E., Avva, J. S., Beall, J. A., Bender, A. N., Benson, B. A., Bleem, L. E., Carlstrom, J. E., Chang, C. L., Chaubal, P., Chiang, H. C., Citron, R., Moran, C. Corbett, Crawford, T. M., Crites, A. T., de Haan, T., Dobbs, M. A., Everett, W., Gallicchio, J., George, E. M., Gilbert, A., Gupta, N., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Holder, G. P., Holzapfel, W. L., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Knox, L., Lee, A. T., Li, D., Lowitz, A., Manzotti, A., McMahon, J. J., Meyer, S. S., Millea, M., Mocanu, L. M., Montgomery, J., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Omori, Y., Padin, S., Patil, S., Pryke, C., Reichardt, C. L., Ruhl, J. E., Saliwanchik, B. R., Sayre, J. T., Schaffer, K. K., Sievers, C., Simard, G., Smecher, G., Stark, A. A., Story, K. T., Tucker, C., Vanderlinde, K., Veach, T., Vieira, J. D., Wang, G., Whitehorn, N., Yefremenko, V.
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creator	Bianchini, F. Wu, W. L. K. Ade, P. A. R. Anderson, A. J. Austermann, J. E. Avva, J. S. Beall, J. A. Bender, A. N. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Chaubal, P. Chiang, H. C. Citron, R. Moran, C. Corbett Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Everett, W. Gallicchio, J. George, E. M. Gilbert, A. Gupta, N. Halverson, N. W. Harrington, N. Henning, J. W. Hilton, G. C. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Huang, N. Hubmayr, J. Irwin, K. D. Knox, L. Lee, A. T. Li, D. Lowitz, A. Manzotti, A. McMahon, J. J. Meyer, S. S. Millea, M. Mocanu, L. M. Montgomery, J. Nadolski, A. Natoli, T. Nibarger, J. P. Noble, G. Novosad, V. Omori, Y. Padin, S. Patil, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Sievers, C. Simard, G. Smecher, G. Stark, A. A. Story, K. T. Tucker, C. Vanderlinde, K. Veach, T. Vieira, J. D. Wang, G. Whitehorn, N. Yefremenko, V.
description	We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg 2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol . The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on . Jointly fitting with BAO data, we find , , and , up to away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the signal-to-noise ratio of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement.
doi_str_mv	10.3847/1538-4357/ab6082
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L. K. ; Ade, P. A. R. ; Anderson, A. J. ; Austermann, J. E. ; Avva, J. S. ; Beall, J. A. ; Bender, A. N. ; Benson, B. A. ; Bleem, L. E. ; Carlstrom, J. E. ; Chang, C. L. ; Chaubal, P. ; Chiang, H. C. ; Citron, R. ; Moran, C. Corbett ; Crawford, T. M. ; Crites, A. T. ; de Haan, T. ; Dobbs, M. A. ; Everett, W. ; Gallicchio, J. ; George, E. M. ; Gilbert, A. ; Gupta, N. ; Halverson, N. W. ; Harrington, N. ; Henning, J. W. ; Hilton, G. C. ; Holder, G. P. ; Holzapfel, W. L. ; Hrubes, J. D. ; Huang, N. ; Hubmayr, J. ; Irwin, K. D. ; Knox, L. ; Lee, A. T. ; Li, D. ; Lowitz, A. ; Manzotti, A. ; McMahon, J. J. ; Meyer, S. S. ; Millea, M. ; Mocanu, L. M. ; Montgomery, J. ; Nadolski, A. ; Natoli, T. ; Nibarger, J. P. ; Noble, G. ; Novosad, V. ; Omori, Y. ; Padin, S. ; Patil, S. ; Pryke, C. ; Reichardt, C. L. ; Ruhl, J. E. ; Saliwanchik, B. R. ; Sayre, J. T. ; Schaffer, K. K. ; Sievers, C. ; Simard, G. ; Smecher, G. ; Stark, A. A. ; Story, K. T. ; Tucker, C. ; Vanderlinde, K. ; Veach, T. ; Vieira, J. D. ; Wang, G. ; Whitehorn, N. ; Yefremenko, V.</creator><creatorcontrib>Bianchini, F. ; Wu, W. L. K. ; Ade, P. A. R. ; Anderson, A. J. ; Austermann, J. E. ; Avva, J. S. ; Beall, J. A. ; Bender, A. N. ; Benson, B. A. ; Bleem, L. E. ; Carlstrom, J. E. ; Chang, C. L. ; Chaubal, P. ; Chiang, H. C. ; Citron, R. ; Moran, C. Corbett ; Crawford, T. M. ; Crites, A. T. ; de Haan, T. ; Dobbs, M. A. ; Everett, W. ; Gallicchio, J. ; George, E. M. ; Gilbert, A. ; Gupta, N. ; Halverson, N. W. ; Harrington, N. ; Henning, J. W. ; Hilton, G. C. ; Holder, G. P. ; Holzapfel, W. L. ; Hrubes, J. D. ; Huang, N. ; Hubmayr, J. ; Irwin, K. D. ; Knox, L. ; Lee, A. T. ; Li, D. ; Lowitz, A. ; Manzotti, A. ; McMahon, J. J. ; Meyer, S. S. ; Millea, M. ; Mocanu, L. M. ; Montgomery, J. ; Nadolski, A. ; Natoli, T. ; Nibarger, J. P. ; Noble, G. ; Novosad, V. ; Omori, Y. ; Padin, S. ; Patil, S. ; Pryke, C. ; Reichardt, C. L. ; Ruhl, J. E. ; Saliwanchik, B. R. ; Sayre, J. T. ; Schaffer, K. K. ; Sievers, C. ; Simard, G. ; Smecher, G. ; Stark, A. A. ; Story, K. T. ; Tucker, C. ; Vanderlinde, K. ; Veach, T. ; Vieira, J. D. ; Wang, G. ; Whitehorn, N. ; Yefremenko, V.</creatorcontrib><description>We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg 2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol . The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on . Jointly fitting with BAO data, we find , , and , up to away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. 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M.</creatorcontrib><creatorcontrib>Montgomery, J.</creatorcontrib><creatorcontrib>Nadolski, A.</creatorcontrib><creatorcontrib>Natoli, T.</creatorcontrib><creatorcontrib>Nibarger, J. P.</creatorcontrib><creatorcontrib>Noble, G.</creatorcontrib><creatorcontrib>Novosad, V.</creatorcontrib><creatorcontrib>Omori, Y.</creatorcontrib><creatorcontrib>Padin, S.</creatorcontrib><creatorcontrib>Patil, S.</creatorcontrib><creatorcontrib>Pryke, C.</creatorcontrib><creatorcontrib>Reichardt, C. L.</creatorcontrib><creatorcontrib>Ruhl, J. E.</creatorcontrib><creatorcontrib>Saliwanchik, B. R.</creatorcontrib><creatorcontrib>Sayre, J. T.</creatorcontrib><creatorcontrib>Schaffer, K. K.</creatorcontrib><creatorcontrib>Sievers, C.</creatorcontrib><creatorcontrib>Simard, G.</creatorcontrib><creatorcontrib>Smecher, G.</creatorcontrib><creatorcontrib>Stark, A. A.</creatorcontrib><creatorcontrib>Story, K. 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The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on . Jointly fitting with BAO data, we find , , and , up to away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. 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L. K. ; Ade, P. A. R. ; Anderson, A. J. ; Austermann, J. E. ; Avva, J. S. ; Beall, J. A. ; Bender, A. N. ; Benson, B. A. ; Bleem, L. E. ; Carlstrom, J. E. ; Chang, C. L. ; Chaubal, P. ; Chiang, H. C. ; Citron, R. ; Moran, C. Corbett ; Crawford, T. M. ; Crites, A. T. ; de Haan, T. ; Dobbs, M. A. ; Everett, W. ; Gallicchio, J. ; George, E. M. ; Gilbert, A. ; Gupta, N. ; Halverson, N. W. ; Harrington, N. ; Henning, J. W. ; Hilton, G. C. ; Holder, G. P. ; Holzapfel, W. L. ; Hrubes, J. D. ; Huang, N. ; Hubmayr, J. ; Irwin, K. D. ; Knox, L. ; Lee, A. T. ; Li, D. ; Lowitz, A. ; Manzotti, A. ; McMahon, J. J. ; Meyer, S. S. ; Millea, M. ; Mocanu, L. M. ; Montgomery, J. ; Nadolski, A. ; Natoli, T. ; Nibarger, J. P. ; Noble, G. ; Novosad, V. ; Omori, Y. ; Padin, S. ; Patil, S. ; Pryke, C. ; Reichardt, C. L. ; Ruhl, J. E. ; Saliwanchik, B. R. ; Sayre, J. T. ; Schaffer, K. K. ; Sievers, C. ; Simard, G. ; Smecher, G. ; Stark, A. A. ; Story, K. T. ; Tucker, C. ; Vanderlinde, K. ; Veach, T. ; Vieira, J. D. ; Wang, G. ; Whitehorn, N. ; Yefremenko, V.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c1221-6cc92fd64e59aaff02739b13688e90f5551281f88f3e6e18f2399b58c2948173</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Astrophysics</topic><topic>Physics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bianchini, F.</creatorcontrib><creatorcontrib>Wu, W. L. K.</creatorcontrib><creatorcontrib>Ade, P. A. R.</creatorcontrib><creatorcontrib>Anderson, A. J.</creatorcontrib><creatorcontrib>Austermann, J. E.</creatorcontrib><creatorcontrib>Avva, J. S.</creatorcontrib><creatorcontrib>Beall, J. A.</creatorcontrib><creatorcontrib>Bender, A. N.</creatorcontrib><creatorcontrib>Benson, B. A.</creatorcontrib><creatorcontrib>Bleem, L. E.</creatorcontrib><creatorcontrib>Carlstrom, J. 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P.</creatorcontrib><creatorcontrib>Noble, G.</creatorcontrib><creatorcontrib>Novosad, V.</creatorcontrib><creatorcontrib>Omori, Y.</creatorcontrib><creatorcontrib>Padin, S.</creatorcontrib><creatorcontrib>Patil, S.</creatorcontrib><creatorcontrib>Pryke, C.</creatorcontrib><creatorcontrib>Reichardt, C. L.</creatorcontrib><creatorcontrib>Ruhl, J. E.</creatorcontrib><creatorcontrib>Saliwanchik, B. R.</creatorcontrib><creatorcontrib>Sayre, J. T.</creatorcontrib><creatorcontrib>Schaffer, K. K.</creatorcontrib><creatorcontrib>Sievers, C.</creatorcontrib><creatorcontrib>Simard, G.</creatorcontrib><creatorcontrib>Smecher, G.</creatorcontrib><creatorcontrib>Stark, A. A.</creatorcontrib><creatorcontrib>Story, K. T.</creatorcontrib><creatorcontrib>Tucker, C.</creatorcontrib><creatorcontrib>Vanderlinde, K.</creatorcontrib><creatorcontrib>Veach, T.</creatorcontrib><creatorcontrib>Vieira, J. D.</creatorcontrib><creatorcontrib>Wang, G.</creatorcontrib><creatorcontrib>Whitehorn, N.</creatorcontrib><creatorcontrib>Yefremenko, V.</creatorcontrib><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bianchini, F.</au><au>Wu, W. L. K.</au><au>Ade, P. A. R.</au><au>Anderson, A. J.</au><au>Austermann, J. E.</au><au>Avva, J. S.</au><au>Beall, J. A.</au><au>Bender, A. N.</au><au>Benson, B. A.</au><au>Bleem, L. E.</au><au>Carlstrom, J. E.</au><au>Chang, C. L.</au><au>Chaubal, P.</au><au>Chiang, H. C.</au><au>Citron, R.</au><au>Moran, C. Corbett</au><au>Crawford, T. M.</au><au>Crites, A. T.</au><au>de Haan, T.</au><au>Dobbs, M. A.</au><au>Everett, W.</au><au>Gallicchio, J.</au><au>George, E. M.</au><au>Gilbert, A.</au><au>Gupta, N.</au><au>Halverson, N. W.</au><au>Harrington, N.</au><au>Henning, J. W.</au><au>Hilton, G. C.</au><au>Holder, G. P.</au><au>Holzapfel, W. L.</au><au>Hrubes, J. D.</au><au>Huang, N.</au><au>Hubmayr, J.</au><au>Irwin, K. D.</au><au>Knox, L.</au><au>Lee, A. T.</au><au>Li, D.</au><au>Lowitz, A.</au><au>Manzotti, A.</au><au>McMahon, J. J.</au><au>Meyer, S. S.</au><au>Millea, M.</au><au>Mocanu, L. M.</au><au>Montgomery, J.</au><au>Nadolski, A.</au><au>Natoli, T.</au><au>Nibarger, J. P.</au><au>Noble, G.</au><au>Novosad, V.</au><au>Omori, Y.</au><au>Padin, S.</au><au>Patil, S.</au><au>Pryke, C.</au><au>Reichardt, C. L.</au><au>Ruhl, J. E.</au><au>Saliwanchik, B. R.</au><au>Sayre, J. T.</au><au>Schaffer, K. K.</au><au>Sievers, C.</au><au>Simard, G.</au><au>Smecher, G.</au><au>Stark, A. A.</au><au>Story, K. T.</au><au>Tucker, C.</au><au>Vanderlinde, K.</au><au>Veach, T.</au><au>Vieira, J. D.</au><au>Wang, G.</au><au>Whitehorn, N.</au><au>Yefremenko, V.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Constraints on Cosmological Parameters from the 500 deg 2 SPTPOL Lensing Power Spectrum</atitle><jtitle>The Astrophysical journal</jtitle><date>2020-01-10</date><risdate>2020</risdate><volume>888</volume><issue>2</issue><spage>119</spage><pages>119-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We present cosmological constraints based on the cosmic microwave background (CMB) lensing potential power spectrum measurement from the recent 500 deg 2 SPTpol survey, the most precise CMB lensing measurement from the ground to date. We fit a flat ΛCDM model to the reconstructed lensing power spectrum alone and in addition with other data sets: baryon acoustic oscillations (BAO), as well as primary CMB spectra from Planck and SPTpol . The cosmological constraints based on SPTpol and Planck lensing band powers are in good agreement when analyzed alone and in combination with Planck full-sky primary CMB data. With weak priors on the baryon density and other parameters, the SPTpol CMB lensing data alone provide a 4% constraint on . Jointly fitting with BAO data, we find , , and , up to away from the central values preferred by Planck lensing + BAO. However, we recover good agreement between SPTpol and Planck when restricting the analysis to similar scales. We also consider single-parameter extensions to the flat ΛCDM model. The SPTpol lensing spectrum constrains the spatial curvature to be and the sum of the neutrino masses to be eV at 95% C.L. (with Planck primary CMB and BAO data), in good agreement with the Planck lensing results. With the differences in the signal-to-noise ratio of the lensing modes and the angular scales covered in the lensing spectra, this analysis represents an important independent check on the full-sky Planck lensing measurement.</abstract><pub>American Astronomical Society</pub><doi>10.3847/1538-4357/ab6082</doi><orcidid>https://orcid.org/0000-0003-4847-3483</orcidid><orcidid>https://orcid.org/0000-0001-5871-7520</orcidid><orcidid>https://orcid.org/0000-0002-2718-9996</orcidid><orcidid>https://orcid.org/0000-0003-2226-9169</orcidid><orcidid>https://orcid.org/0000-0001-7665-5079</orcidid><orcidid>https://orcid.org/0000-0001-5105-9473</orcidid><orcidid>https://orcid.org/0000-0002-5108-6823</orcidid><orcidid>https://orcid.org/0000-0001-5411-6920</orcidid><orcidid>https://orcid.org/0000-0001-9000-5013</orcidid><orcidid>https://orcid.org/0000-0001-5800-3990</orcidid><orcidid>https://orcid.org/0000-0002-0463-6394</orcidid><orcidid>https://orcid.org/0000-0002-3157-0407</orcidid><orcidid>https://orcid.org/0000-0003-0057-877X</orcidid><orcidid>https://orcid.org/0000-0002-5127-0401</orcidid><orcidid>https://orcid.org/0000-0001-8599-7249</orcidid><orcidid>https://orcid.org/0000-0001-7547-4241</orcidid></addata></record>
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issn	0004-637X 1538-4357
language	eng
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subjects	Astrophysics Physics
title	Constraints on Cosmological Parameters from the 500 deg 2 SPTPOL Lensing Power Spectrum
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