Cosmological lensing ratios with DES Y1, SPT, and Planck
Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2019-07, Vol.487 (1), p.1363-1379 |
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| creator | Prat, J Baxter, E Shin, T Sánchez, C Chang, C Jain, B Miquel, R Alarcon, A Bacon, D Bernstein, G M Cawthon, R Crawford, T M Davis, C De Vicente, J Dodelson, S Eifler, T F Friedrich, O Gatti, M Gruen, D Hartley, W G Holder, G P Hoyle, B Jarvis, M Krause, E MacCrann, N Mawdsley, B Nicola, A Omori, Y Pujol, A Rau, M M Reichardt, C L Samuroff, S Sheldon, E Troxel, M A Vielzeuf, P Zuntz, J Abbott, T M C Abdalla, F B Annis, J Avila, S Aylor, K Benson, B A Bertin, E Bleem, L E Brooks, D Burke, D L Carlstrom, J E Carrasco Kind, M Carretero, J Chang, C L Cho, H-M Chown, R Crites, A T Cunha, C E da Costa, L N Desai, S Diehl, H T Dietrich, J P Dobbs, M A Doel, P Everett, W B Evrard, A E Flaugher, B Fosalba, P García-Bellido, J Gaztanaga, E George, E M Gerdes, D W Giannantonio, T Gruendl, R A Gschwend, J Gutierrez, G de Haan, T Halverson, N W Harrington, N L Holzapfel, W L Honscheid, K Hou, Z Hrubes, J D James, D J Jeltema, T Knox, L Kron, R Kuehn, K Kuropatkin, N Lahav, O Lee, A T Leitch, E M Lima, M Luong-Van, D Maia, M A G Manzotti, A Marrone, D P Marshall, J L McMahon, J J Melchior, P Menanteau, F Meyer, S S Miller, C J Mocanu, L M |
| description | Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise ratio down to small angular scales, even where directly modelling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance ΛCDM model, we find a best-fitting lensing ratio amplitude of A = 1.1 ± 0.1. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation. |
| doi_str_mv | 10.1093/mnras/stz1309 |
| format | Article |
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(ORNL), Oak Ridge, TN (United States) ; Brookhaven National Lab. (BNL), Upton, NY (United States) ; Argonne National Lab. (ANL), Argonne, IL (United States) ; Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States) ; Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><description>Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise ratio down to small angular scales, even where directly modelling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance ΛCDM model, we find a best-fitting lensing ratio amplitude of A = 1.1 ± 0.1. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stz1309</identifier><language>eng</language><publisher>United States: Oxford University Press (OUP): Policy P - Oxford Open Option A</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; Astrophysics ; cosmological parameters ; cosmology: observations ; gravitational lensing: weak ; large-scale structure of Universe ; Physics</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2019-07, Vol.487 (1), p.1363-1379</ispartof><rights>Distributed under a Creative Commons 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Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Prat, J</creatorcontrib><creatorcontrib>Baxter, E</creatorcontrib><creatorcontrib>Shin, T</creatorcontrib><creatorcontrib>Sánchez, C</creatorcontrib><creatorcontrib>Chang, C</creatorcontrib><creatorcontrib>Jain, B</creatorcontrib><creatorcontrib>Miquel, R</creatorcontrib><creatorcontrib>Alarcon, A</creatorcontrib><creatorcontrib>Bacon, D</creatorcontrib><creatorcontrib>Bernstein, G M</creatorcontrib><creatorcontrib>Cawthon, R</creatorcontrib><creatorcontrib>Crawford, T M</creatorcontrib><creatorcontrib>Davis, C</creatorcontrib><creatorcontrib>De Vicente, J</creatorcontrib><creatorcontrib>Dodelson, S</creatorcontrib><creatorcontrib>Eifler, T F</creatorcontrib><creatorcontrib>Friedrich, O</creatorcontrib><creatorcontrib>Gatti, M</creatorcontrib><creatorcontrib>Gruen, D</creatorcontrib><creatorcontrib>Hartley, W G</creatorcontrib><creatorcontrib>Holder, G P</creatorcontrib><creatorcontrib>Hoyle, 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D</creatorcontrib><creatorcontrib>Burke, D L</creatorcontrib><creatorcontrib>Carlstrom, J E</creatorcontrib><creatorcontrib>Carrasco Kind, M</creatorcontrib><creatorcontrib>Carretero, J</creatorcontrib><creatorcontrib>Chang, C L</creatorcontrib><creatorcontrib>Cho, H-M</creatorcontrib><creatorcontrib>Chown, R</creatorcontrib><creatorcontrib>Crites, A T</creatorcontrib><creatorcontrib>Cunha, C E</creatorcontrib><creatorcontrib>da Costa, L N</creatorcontrib><creatorcontrib>Desai, S</creatorcontrib><creatorcontrib>Diehl, H T</creatorcontrib><creatorcontrib>Dietrich, J P</creatorcontrib><creatorcontrib>Dobbs, M A</creatorcontrib><creatorcontrib>Doel, P</creatorcontrib><creatorcontrib>Everett, W B</creatorcontrib><creatorcontrib>Evrard, A E</creatorcontrib><creatorcontrib>Flaugher, B</creatorcontrib><creatorcontrib>Fosalba, P</creatorcontrib><creatorcontrib>García-Bellido, J</creatorcontrib><creatorcontrib>Gaztanaga, E</creatorcontrib><creatorcontrib>George, E M</creatorcontrib><creatorcontrib>Gerdes, D W</creatorcontrib><creatorcontrib>Giannantonio, T</creatorcontrib><creatorcontrib>Gruendl, R A</creatorcontrib><creatorcontrib>Gschwend, J</creatorcontrib><creatorcontrib>Gutierrez, G</creatorcontrib><creatorcontrib>de Haan, T</creatorcontrib><creatorcontrib>Halverson, N W</creatorcontrib><creatorcontrib>Harrington, N L</creatorcontrib><creatorcontrib>Holzapfel, W L</creatorcontrib><creatorcontrib>Honscheid, K</creatorcontrib><creatorcontrib>Hou, Z</creatorcontrib><creatorcontrib>Hrubes, J D</creatorcontrib><creatorcontrib>James, D J</creatorcontrib><creatorcontrib>Jeltema, T</creatorcontrib><creatorcontrib>Knox, L</creatorcontrib><creatorcontrib>Kron, R</creatorcontrib><creatorcontrib>Kuehn, K</creatorcontrib><creatorcontrib>Kuropatkin, N</creatorcontrib><creatorcontrib>Lahav, O</creatorcontrib><creatorcontrib>Lee, A T</creatorcontrib><creatorcontrib>Leitch, E M</creatorcontrib><creatorcontrib>Lima, M</creatorcontrib><creatorcontrib>Luong-Van, D</creatorcontrib><creatorcontrib>Maia, M A G</creatorcontrib><creatorcontrib>Manzotti, A</creatorcontrib><creatorcontrib>Marrone, D P</creatorcontrib><creatorcontrib>Marshall, J L</creatorcontrib><creatorcontrib>McMahon, J J</creatorcontrib><creatorcontrib>Melchior, P</creatorcontrib><creatorcontrib>Menanteau, F</creatorcontrib><creatorcontrib>Meyer, S S</creatorcontrib><creatorcontrib>Miller, C J</creatorcontrib><creatorcontrib>Mocanu, L M</creatorcontrib><creatorcontrib>The DES and SPT Collaborations</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Brookhaven National Lab. (BNL), Upton, NY (United States)</creatorcontrib><creatorcontrib>Argonne National Lab. (ANL), Argonne, IL (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><title>Cosmological lensing ratios with DES Y1, SPT, and Planck</title><title>Monthly notices of the Royal Astronomical Society</title><description>Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise ratio down to small angular scales, even where directly modelling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance ΛCDM model, we find a best-fitting lensing ratio amplitude of A = 1.1 ± 0.1. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>cosmological parameters</subject><subject>cosmology: observations</subject><subject>gravitational lensing: weak</subject><subject>large-scale structure of 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Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>1XC</scope><scope>VOOES</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-5933-5150</orcidid><orcidid>https://orcid.org/0000-0002-6389-5409</orcidid><orcidid>https://orcid.org/0000-0002-2744-4934</orcidid><orcidid>https://orcid.org/0000-0001-7039-9078</orcidid><orcidid>https://orcid.org/0000-0002-1510-5214</orcidid><orcidid>https://orcid.org/0000000259335150</orcidid><orcidid>https://orcid.org/0000000227444934</orcidid><orcidid>https://orcid.org/0000000263895409</orcidid></search><sort><creationdate>20190721</creationdate><title>Cosmological lensing ratios with DES Y1, SPT, and Planck</title><author>Prat, J ; Baxter, E ; Shin, T ; Sánchez, C ; Chang, C ; Jain, B ; Miquel, R ; Alarcon, A ; Bacon, D ; Bernstein, G M ; Cawthon, R ; Crawford, T M ; Davis, C ; De Vicente, J ; Dodelson, S ; Eifler, T F ; Friedrich, O ; Gatti, M ; Gruen, D ; Hartley, W G ; Holder, G P ; Hoyle, B ; Jarvis, M ; Krause, E ; MacCrann, N ; Mawdsley, B ; Nicola, A ; Omori, Y ; Pujol, A ; Rau, M M ; Reichardt, C L ; Samuroff, S ; Sheldon, E ; Troxel, M A ; Vielzeuf, P ; Zuntz, J ; Abbott, T M C ; Abdalla, F B ; Annis, J ; Avila, S ; Aylor, K ; Benson, B A ; Bertin, E ; Bleem, L E ; Brooks, D ; Burke, D L ; Carlstrom, J E ; Carrasco Kind, M ; Carretero, J ; Chang, C L ; Cho, H-M ; Chown, R ; Crites, A T ; Cunha, C E ; da Costa, L N ; Desai, S ; Diehl, H T ; Dietrich, J P ; Dobbs, M A ; Doel, P ; Everett, W B ; Evrard, A E ; Flaugher, B ; Fosalba, P ; García-Bellido, J ; Gaztanaga, E ; George, E M ; Gerdes, D W ; Giannantonio, T ; Gruendl, R A ; Gschwend, J ; Gutierrez, G ; de Haan, T ; Halverson, N W ; Harrington, N L ; Holzapfel, W L ; Honscheid, K ; Hou, Z ; Hrubes, J D ; James, D J ; Jeltema, T ; Knox, L ; Kron, R ; Kuehn, K ; Kuropatkin, N ; Lahav, O ; Lee, A T ; Leitch, E M ; Lima, M ; Luong-Van, D ; Maia, M A G ; Manzotti, A ; Marrone, D P ; Marshall, J L ; McMahon, J J ; Melchior, P ; Menanteau, F ; Meyer, S S ; Miller, C J ; Mocanu, L M</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c337t-35b8492fd6df49dbf5ee04887e474935b2520f3d8d24cf6f9a4e8ce65d38b5593</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Astrophysics</topic><topic>cosmological parameters</topic><topic>cosmology: observations</topic><topic>gravitational lensing: weak</topic><topic>large-scale structure of Universe</topic><topic>Physics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Prat, J</creatorcontrib><creatorcontrib>Baxter, E</creatorcontrib><creatorcontrib>Shin, T</creatorcontrib><creatorcontrib>Sánchez, C</creatorcontrib><creatorcontrib>Chang, C</creatorcontrib><creatorcontrib>Jain, B</creatorcontrib><creatorcontrib>Miquel, R</creatorcontrib><creatorcontrib>Alarcon, A</creatorcontrib><creatorcontrib>Bacon, D</creatorcontrib><creatorcontrib>Bernstein, G M</creatorcontrib><creatorcontrib>Cawthon, R</creatorcontrib><creatorcontrib>Crawford, T M</creatorcontrib><creatorcontrib>Davis, C</creatorcontrib><creatorcontrib>De Vicente, J</creatorcontrib><creatorcontrib>Dodelson, S</creatorcontrib><creatorcontrib>Eifler, T F</creatorcontrib><creatorcontrib>Friedrich, O</creatorcontrib><creatorcontrib>Gatti, M</creatorcontrib><creatorcontrib>Gruen, D</creatorcontrib><creatorcontrib>Hartley, W G</creatorcontrib><creatorcontrib>Holder, G P</creatorcontrib><creatorcontrib>Hoyle, B</creatorcontrib><creatorcontrib>Jarvis, M</creatorcontrib><creatorcontrib>Krause, E</creatorcontrib><creatorcontrib>MacCrann, N</creatorcontrib><creatorcontrib>Mawdsley, B</creatorcontrib><creatorcontrib>Nicola, A</creatorcontrib><creatorcontrib>Omori, Y</creatorcontrib><creatorcontrib>Pujol, A</creatorcontrib><creatorcontrib>Rau, M M</creatorcontrib><creatorcontrib>Reichardt, C L</creatorcontrib><creatorcontrib>Samuroff, S</creatorcontrib><creatorcontrib>Sheldon, E</creatorcontrib><creatorcontrib>Troxel, M A</creatorcontrib><creatorcontrib>Vielzeuf, P</creatorcontrib><creatorcontrib>Zuntz, J</creatorcontrib><creatorcontrib>Abbott, T M C</creatorcontrib><creatorcontrib>Abdalla, F B</creatorcontrib><creatorcontrib>Annis, J</creatorcontrib><creatorcontrib>Avila, S</creatorcontrib><creatorcontrib>Aylor, K</creatorcontrib><creatorcontrib>Benson, B A</creatorcontrib><creatorcontrib>Bertin, E</creatorcontrib><creatorcontrib>Bleem, L E</creatorcontrib><creatorcontrib>Brooks, D</creatorcontrib><creatorcontrib>Burke, D L</creatorcontrib><creatorcontrib>Carlstrom, J E</creatorcontrib><creatorcontrib>Carrasco Kind, M</creatorcontrib><creatorcontrib>Carretero, J</creatorcontrib><creatorcontrib>Chang, C L</creatorcontrib><creatorcontrib>Cho, H-M</creatorcontrib><creatorcontrib>Chown, R</creatorcontrib><creatorcontrib>Crites, A T</creatorcontrib><creatorcontrib>Cunha, C E</creatorcontrib><creatorcontrib>da Costa, L N</creatorcontrib><creatorcontrib>Desai, S</creatorcontrib><creatorcontrib>Diehl, H T</creatorcontrib><creatorcontrib>Dietrich, J P</creatorcontrib><creatorcontrib>Dobbs, M A</creatorcontrib><creatorcontrib>Doel, P</creatorcontrib><creatorcontrib>Everett, W B</creatorcontrib><creatorcontrib>Evrard, A E</creatorcontrib><creatorcontrib>Flaugher, B</creatorcontrib><creatorcontrib>Fosalba, P</creatorcontrib><creatorcontrib>García-Bellido, J</creatorcontrib><creatorcontrib>Gaztanaga, E</creatorcontrib><creatorcontrib>George, E M</creatorcontrib><creatorcontrib>Gerdes, D W</creatorcontrib><creatorcontrib>Giannantonio, T</creatorcontrib><creatorcontrib>Gruendl, R A</creatorcontrib><creatorcontrib>Gschwend, J</creatorcontrib><creatorcontrib>Gutierrez, G</creatorcontrib><creatorcontrib>de Haan, T</creatorcontrib><creatorcontrib>Halverson, N W</creatorcontrib><creatorcontrib>Harrington, N L</creatorcontrib><creatorcontrib>Holzapfel, W L</creatorcontrib><creatorcontrib>Honscheid, K</creatorcontrib><creatorcontrib>Hou, Z</creatorcontrib><creatorcontrib>Hrubes, J D</creatorcontrib><creatorcontrib>James, D J</creatorcontrib><creatorcontrib>Jeltema, T</creatorcontrib><creatorcontrib>Knox, L</creatorcontrib><creatorcontrib>Kron, R</creatorcontrib><creatorcontrib>Kuehn, K</creatorcontrib><creatorcontrib>Kuropatkin, N</creatorcontrib><creatorcontrib>Lahav, O</creatorcontrib><creatorcontrib>Lee, A T</creatorcontrib><creatorcontrib>Leitch, E M</creatorcontrib><creatorcontrib>Lima, M</creatorcontrib><creatorcontrib>Luong-Van, D</creatorcontrib><creatorcontrib>Maia, M A G</creatorcontrib><creatorcontrib>Manzotti, A</creatorcontrib><creatorcontrib>Marrone, D P</creatorcontrib><creatorcontrib>Marshall, J L</creatorcontrib><creatorcontrib>McMahon, J J</creatorcontrib><creatorcontrib>Melchior, P</creatorcontrib><creatorcontrib>Menanteau, F</creatorcontrib><creatorcontrib>Meyer, S S</creatorcontrib><creatorcontrib>Miller, C J</creatorcontrib><creatorcontrib>Mocanu, L M</creatorcontrib><creatorcontrib>The DES and SPT Collaborations</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Brookhaven National Lab. (BNL), Upton, NY (United States)</creatorcontrib><creatorcontrib>Argonne National Lab. (ANL), Argonne, IL (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><collection>OSTI.GOV</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Prat, J</au><au>Baxter, E</au><au>Shin, T</au><au>Sánchez, C</au><au>Chang, C</au><au>Jain, B</au><au>Miquel, R</au><au>Alarcon, A</au><au>Bacon, D</au><au>Bernstein, G M</au><au>Cawthon, R</au><au>Crawford, T M</au><au>Davis, C</au><au>De Vicente, J</au><au>Dodelson, S</au><au>Eifler, T F</au><au>Friedrich, O</au><au>Gatti, M</au><au>Gruen, D</au><au>Hartley, W G</au><au>Holder, G P</au><au>Hoyle, B</au><au>Jarvis, M</au><au>Krause, E</au><au>MacCrann, N</au><au>Mawdsley, B</au><au>Nicola, A</au><au>Omori, Y</au><au>Pujol, A</au><au>Rau, M M</au><au>Reichardt, C L</au><au>Samuroff, S</au><au>Sheldon, E</au><au>Troxel, M A</au><au>Vielzeuf, P</au><au>Zuntz, J</au><au>Abbott, T M C</au><au>Abdalla, F B</au><au>Annis, J</au><au>Avila, S</au><au>Aylor, K</au><au>Benson, B A</au><au>Bertin, E</au><au>Bleem, L E</au><au>Brooks, D</au><au>Burke, D L</au><au>Carlstrom, J E</au><au>Carrasco Kind, M</au><au>Carretero, J</au><au>Chang, C L</au><au>Cho, H-M</au><au>Chown, R</au><au>Crites, A T</au><au>Cunha, C E</au><au>da Costa, L N</au><au>Desai, S</au><au>Diehl, H T</au><au>Dietrich, J P</au><au>Dobbs, M A</au><au>Doel, P</au><au>Everett, W B</au><au>Evrard, A E</au><au>Flaugher, B</au><au>Fosalba, P</au><au>García-Bellido, J</au><au>Gaztanaga, E</au><au>George, E M</au><au>Gerdes, D W</au><au>Giannantonio, T</au><au>Gruendl, R A</au><au>Gschwend, J</au><au>Gutierrez, G</au><au>de Haan, T</au><au>Halverson, N W</au><au>Harrington, N L</au><au>Holzapfel, W L</au><au>Honscheid, K</au><au>Hou, Z</au><au>Hrubes, J D</au><au>James, D J</au><au>Jeltema, T</au><au>Knox, L</au><au>Kron, R</au><au>Kuehn, K</au><au>Kuropatkin, N</au><au>Lahav, O</au><au>Lee, A T</au><au>Leitch, E M</au><au>Lima, M</au><au>Luong-Van, D</au><au>Maia, M A G</au><au>Manzotti, A</au><au>Marrone, D P</au><au>Marshall, J L</au><au>McMahon, J J</au><au>Melchior, P</au><au>Menanteau, F</au><au>Meyer, S S</au><au>Miller, C J</au><au>Mocanu, L M</au><aucorp>The DES and SPT Collaborations</aucorp><aucorp>SLAC National Accelerator Lab., Menlo Park, CA (United States)</aucorp><aucorp>Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)</aucorp><aucorp>Brookhaven National Lab. (BNL), Upton, NY (United States)</aucorp><aucorp>Argonne National Lab. (ANL), Argonne, IL (United States)</aucorp><aucorp>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</aucorp><aucorp>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Cosmological lensing ratios with DES Y1, SPT, and Planck</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2019-07-21</date><risdate>2019</risdate><volume>487</volume><issue>1</issue><spage>1363</spage><epage>1379</epage><pages>1363-1379</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise ratio down to small angular scales, even where directly modelling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance ΛCDM model, we find a best-fitting lensing ratio amplitude of A = 1.1 ± 0.1. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation.</abstract><cop>United States</cop><pub>Oxford University Press (OUP): Policy P - Oxford Open Option A</pub><doi>10.1093/mnras/stz1309</doi><tpages>17</tpages><orcidid>https://orcid.org/0000-0002-5933-5150</orcidid><orcidid>https://orcid.org/0000-0002-6389-5409</orcidid><orcidid>https://orcid.org/0000-0002-2744-4934</orcidid><orcidid>https://orcid.org/0000-0001-7039-9078</orcidid><orcidid>https://orcid.org/0000-0002-1510-5214</orcidid><orcidid>https://orcid.org/0000000259335150</orcidid><orcidid>https://orcid.org/0000000227444934</orcidid><orcidid>https://orcid.org/0000000263895409</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0035-8711 |
| ispartof | Monthly notices of the Royal Astronomical Society, 2019-07, Vol.487 (1), p.1363-1379 |
| issn | 0035-8711 1365-2966 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1487407 |
| source | Oxford Journals Open Access Collection |
| subjects | ASTRONOMY AND ASTROPHYSICS Astrophysics cosmological parameters cosmology: observations gravitational lensing: weak large-scale structure of Universe Physics |
| title | Cosmological lensing ratios with DES Y1, SPT, and Planck |
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