Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data

S. Raghunathan; S. Patil; E. Baxter; B. A. Benson; L. E. Bleem; T. L. Chou; T. M. Crawford; G. P. Holder; T. McClintock; C. L. Reichardt; E. Rozo; T. N. Varga; T. M.C. Abbott; P. A.R. Ade; S. Allam; A. J. Anderson; J. Annis; J. E. Austermann; S. Avila; J. A. Beall; K. Bechtol; A. N. Bender; G. Bernstein; E. Bertin; F. Bianchini; D. Brooks; D. L. Burke; J. E. Carlstrom; J. Carretero; C. L. Chang; H. C. Chiang; H. M. Cho; R. Citron; A. T. Crites; C. E. Cunha; L. N.Da Costa; C. Davis; S. Desai; H. T. Diehl; J. P. Dietrich; M. A. Dobbs; P. Doel; T. F. Eifler; W. Everett; A. E. Evrard; B. Flaugher; P. Fosalba; J. Frieman; J. Gallicchio; J. García-Bellido; E. Gaztanaga; E. M. George; A. Gilbert; D. Gruen; R. A. Gruendl; J. Gschwend; N. Gupta; G. Gutierrez; T. De Haan; N. W. Halverson; N. Harrington; W. G. Hartley; J. W. Henning; G. C. Hilton; D. L. Hollowood; W. L. Holzapfel; K. Honscheid; Z. Hou; B. Hoyle; J. D. Hrubes; N. Huang; J. Hubmayr; K. D. Irwin; D. J. James; T. Jeltema; A. G. Kim; M. Carrasco Kind; L. Knox; A. Kovacs; K. Kuehn; N. Kuropatkin; A. T. Lee; T. S. Li; M. Lima; M. A.G. Maia; J. L. Marshall; J. J. McMahon; P. Melchior; F. Menanteau; S. S. Meyer; C. J. Miller; R. Miquel; L. Mocanu; J. Montgomery; A. Nadolski; T. Natoli; J. P. Nibarger; V. Novosad; S. Padin; A. A. Plazas; C. Pryke; D. Rapetti; A. K. Romer; A. Carnero Rosell; J. E. Ruhl; B. R. Saliwanchik; E. Sanchez; J. T. Sayre; V. Scarpine; K. K. Schaffer; M. Schubnell; S. Serrano; I. Sevilla-Noarbe; G. Smecher; R. C. Smith; M. Soares-Santos; F. Sobreira; A. A. Stark; K. T. Story; E. Suchyta; M. E.C. Swanson; G. Tarle; D. Thomas; C. Tucker; K. Vanderlinde; J. De Vicente; J. D. Vieira; G. Wang; N. Whitehorn; W. L.K. Wu; Y. Zhang

doi:10.3847/1538-4357/ab01ca

Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data

S. Raghunathan, S. Patil, E. Baxter, B. A. Benson, L. E. Bleem, T. L. Chou, T. M. Crawford, G. P. Holder, T. McClintock, C. L. Reichardt, E. Rozo, T. N. Varga, T. M.C. Abbott, P. A.R. Ade, S. Allam, A. J. Anderson, J. Annis, J. E. Austermann, S. Avila, J. A. BeallK. Bechtol, A. N. Bender, G. Bernstein, E. Bertin, F. Bianchini, D. Brooks, D. L. Burke, J. E. Carlstrom, J. Carretero, C. L. Chang, H. C. Chiang, H. M. Cho, R. Citron, A. T. Crites, C. E. Cunha, L. N.Da Costa, C. Davis, S. Desai, H. T. Diehl, J. P. Dietrich, M. A. Dobbs, P. Doel, T. F. Eifler, W. Everett, A. E. Evrard, B. Flaugher, P. Fosalba, J. Frieman, J. Gallicchio, J. García-Bellido, E. Gaztanaga, E. M. George, A. Gilbert, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, T. De Haan, N. W. Halverson, N. Harrington, W. G. Hartley, J. W. Henning, G. C. Hilton, D. L. Hollowood, W. L. Holzapfel, K. Honscheid, Z. Hou, B. Hoyle, J. D. Hrubes, N. Huang, J. Hubmayr, K. D. Irwin, D. J. James, T. Jeltema, A. G. Kim, M. Carrasco Kind, L. Knox, A. Kovacs, K. Kuehn, N. Kuropatkin, A. T. Lee, T. S. Li, M. Lima, M. A.G. Maia, J. L. Marshall, J. J. McMahon, P. Melchior, F. Menanteau, S. S. Meyer, C. J. Miller, R. Miquel, L. Mocanu, J. Montgomery, A. Nadolski, T. Natoli, J. P. Nibarger, V. Novosad, S. Padin, A. A. Plazas, C. Pryke, D. Rapetti, A. K. Romer, A. Carnero Rosell, J. E. Ruhl, B. R. Saliwanchik, E. Sanchez, J. T. Sayre, V. Scarpine, K. K. Schaffer, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, G. Smecher, R. C. Smith, M. Soares-Santos, F. Sobreira, A. A. Stark, K. T. Story, E. Suchyta, M. E.C. Swanson, G. Tarle, D. Thomas, C. Tucker, K. Vanderlinde, J. De Vicente, J. D. Vieira, G. Wang, N. Whitehorn, W. L.K. Wu, Y. Zhang

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Abstract

We use cosmic microwave background (CMB) temperature maps from the 500 deg ² SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel'dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz data sets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7σ(6.7σ) with the flux (volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be M _200m = (1.62 _-0.25 ^+0.32 [stat] ± 0.04 [sys.]) and (1.28 _-0.18 ^+0.14 [stat] ± 0.03[sys.])× 10 ¹⁴ M _⊙ for the volume- and flux-limited samples, respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES.

Original language	English
Article number	170
Journal	Astrophysical Journal
Volume	872
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ab01ca
State	Published - 2019

Funding

Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungs-gemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. We thank useful conversations with Mathew Madhavacheril at the Stanford CMB-lensing meeting in 2017, which partly inspired us in building this modified QE. The Melbourne group acknowledges support from the Australian Research Council’s Discovery Projects scheme (DP150103208). S.R. also acknowledges partial support from the Laby Foundation. L.B.’s work was supported under the U.S. Department of Energy contract DE-AC02-06CH11357. We acknowledge the use of HEALPix (Górski et al. 2005) and CAMB (Lewis et al. 2000) routines. This work was performed in the context of the South Pole Telescope scientific program. SPT is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. This manuscript has been authored by Fermi Research Alliance, LLC, under Contract No. DE-AC02-07CH11359, with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The U.S. government retains—and the publisher, by accepting the article for publication, acknowledges that the U.S. government retains—a non-exclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for US government purposes. The study is based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant No. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

Funders	Funder number
Australian Research Council Centre of Excellence for All-sky Astrophysics	CE110001020
Collaborating Institutions in the Dark Energy Survey
Deutsche Forschungs-gemeinschaft
European Union’s Seventh Framework Program
FP7/2007
Fermi Research Alliance, LLC	DE-AC02-07CH11359
INCT
Kavli Institute of Cosmological Physics at the University of Chicago
Laby Foundation
Ministry of Science and Education of Spain
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
NSF Physics Frontier Center	PHY-1125897
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
U.S. National Science Foundation
National Science Foundation	PLR-1248097, 1248097, 1138766, AST-1138766, 1125897, AST-1536171
U.S. Department of Energy	DE-AC02-05CH11231, DE-AC02-06CH11357
Gordon and Betty Moore Foundation	GBMF 947
Kavli Foundation
Office of Science
High Energy Physics
Seventh Framework Programme	240672, 306478, 291329
Higher Education Funding Council for England
Center for Cosmology and Astroparticle Physics, Ohio State University
Instituto Nacional de Ciência e Tecnologia Midas
Science and Technology Facilities Council	ST/N000668/1
European Commission
European Research Council
Australian Research Council	DP150103208
Generalitat de Catalunya
Ministerio de Economía y Competitividad	SEV-2016-0588, SEV-2016-0597, ESP2015-66861, MDM-2015-0509, FPA2015-68048, AYA2015-71825
Ministério da Ciência, Tecnologia e Inovação
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
European Regional Development Fund

Keywords

cosmic background radiation
galaxies: clusters: general
gravitational lensing: weak

Access to Document

10.3847/1538-4357/ab01ca

Cite this

Raghunathan, S., Patil, S., Baxter, E., Benson, B. A., Bleem, L. E., Chou, T. L., Crawford, T. M., Holder, G. P., McClintock, T., Reichardt, C. L., Rozo, E., Varga, T. N., Abbott, T. M. C., Ade, P. A. R., Allam, S., Anderson, A. J., Annis, J., Austermann, J. E., Avila, S., ... Zhang, Y. (2019). Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data. Astrophysical Journal, 872(2), Article 170. https://doi.org/10.3847/1538-4357/ab01ca

@article{2d588c7ffbe745599be749b8efb0e27d,

title = "Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data",

abstract = " We use cosmic microwave background (CMB) temperature maps from the 500 deg 2 SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel'dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz data sets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7σ(6.7σ) with the flux (volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be M 200m = (1.62 -0.25 +0.32 [stat] ± 0.04 [sys.]) and (1.28 -0.18 +0.14 [stat] ± 0.03[sys.])× 10 14 M ⊙ for the volume- and flux-limited samples, respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES.",

keywords = "cosmic background radiation, galaxies: clusters: general, gravitational lensing: weak",

author = "S. Raghunathan and S. Patil and E. Baxter and Benson, {B. A.} and Bleem, {L. E.} and Chou, {T. L.} and Crawford, {T. M.} and Holder, {G. P.} and T. McClintock and Reichardt, {C. L.} and E. Rozo and Varga, {T. N.} and Abbott, {T. M.C.} and Ade, {P. A.R.} and S. Allam and Anderson, {A. J.} and J. Annis and Austermann, {J. E.} and S. Avila and Beall, {J. A.} and K. Bechtol and Bender, {A. N.} and G. Bernstein and E. Bertin and F. Bianchini and D. Brooks and Burke, {D. L.} and Carlstrom, {J. E.} and J. Carretero and Chang, {C. L.} and Chiang, {H. C.} and Cho, {H. M.} and R. Citron and Crites, {A. T.} and Cunha, {C. E.} and Costa, {L. N.Da} and C. Davis and S. Desai and Diehl, {H. T.} and Dietrich, {J. P.} and Dobbs, {M. A.} and P. Doel and Eifler, {T. F.} and W. Everett and Evrard, {A. E.} and B. Flaugher and P. Fosalba and J. Frieman and J. Gallicchio and J. Garc{\'i}a-Bellido and E. Gaztanaga and George, {E. M.} and A. Gilbert and D. Gruen and Gruendl, {R. A.} and J. Gschwend and N. Gupta and G. Gutierrez and Haan, {T. De} and Halverson, {N. W.} and N. Harrington and Hartley, {W. G.} and Henning, {J. W.} and Hilton, {G. C.} and Hollowood, {D. L.} and Holzapfel, {W. L.} and K. Honscheid and Z. Hou and B. Hoyle and Hrubes, {J. D.} and N. Huang and J. Hubmayr and Irwin, {K. D.} and James, {D. J.} and T. Jeltema and Kim, {A. G.} and Kind, {M. Carrasco} and L. Knox and A. Kovacs and K. Kuehn and N. Kuropatkin and Lee, {A. T.} and Li, {T. S.} and M. Lima and Maia, {M. A.G.} and Marshall, {J. L.} and McMahon, {J. J.} and P. Melchior and F. Menanteau and Meyer, {S. S.} and Miller, {C. J.} and R. Miquel and L. Mocanu and J. Montgomery and A. Nadolski and T. Natoli and Nibarger, {J. P.} and V. Novosad and S. Padin and Plazas, {A. A.} and C. Pryke and D. Rapetti and Romer, {A. K.} and Rosell, {A. Carnero} and Ruhl, {J. E.} and Saliwanchik, {B. R.} and E. Sanchez and Sayre, {J. T.} and V. Scarpine and Schaffer, {K. K.} and M. Schubnell and S. Serrano and I. Sevilla-Noarbe and G. Smecher and Smith, {R. C.} and M. Soares-Santos and F. Sobreira and Stark, {A. A.} and Story, {K. T.} and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and D. Thomas and C. Tucker and K. Vanderlinde and Vicente, {J. De} and Vieira, {J. D.} and G. Wang and N. Whitehorn and Wu, {W. L.K.} and Y. Zhang",

year = "2019",

doi = "10.3847/1538-4357/ab01ca",

language = "English",

volume = "872",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Raghunathan, S, Patil, S, Baxter, E, Benson, BA, Bleem, LE, Chou, TL, Crawford, TM, Holder, GP, McClintock, T, Reichardt, CL, Rozo, E, Varga, TN, Abbott, TMC, Ade, PAR, Allam, S, Anderson, AJ, Annis, J, Austermann, JE, Avila, S, Beall, JA, Bechtol, K, Bender, AN, Bernstein, G, Bertin, E, Bianchini, F, Brooks, D, Burke, DL, Carlstrom, JE, Carretero, J, Chang, CL, Chiang, HC, Cho, HM, Citron, R, Crites, AT, Cunha, CE, Costa, LND, Davis, C, Desai, S, Diehl, HT, Dietrich, JP, Dobbs, MA, Doel, P, Eifler, TF, Everett, W, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gallicchio, J, García-Bellido, J, Gaztanaga, E, George, EM, Gilbert, A, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, N, Gutierrez, G, Haan, TD, Halverson, NW, Harrington, N, Hartley, WG, Henning, JW, Hilton, GC, Hollowood, DL, Holzapfel, WL, Honscheid, K, Hou, Z, Hoyle, B, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, James, DJ, Jeltema, T, Kim, AG, Kind, MC, Knox, L, Kovacs, A, Kuehn, K, Kuropatkin, N, Lee, AT, Li, TS, Lima, M, Maia, MAG, Marshall, JL, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miller, CJ, Miquel, R, Mocanu, L, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Novosad, V, Padin, S, Plazas, AA, Pryke, C, Rapetti, D, Romer, AK, Rosell, AC, Ruhl, JE, Saliwanchik, BR, Sanchez, E, Sayre, JT, Scarpine, V, Schaffer, KK, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smecher, G, Smith, RC, Soares-Santos, M, Sobreira, F, Stark, AA, Story, KT, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, C, Vanderlinde, K, Vicente, JD, Vieira, JD, Wang, G, Whitehorn, N, Wu, WLK & Zhang, Y 2019, 'Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data', Astrophysical Journal, vol. 872, no. 2, 170. https://doi.org/10.3847/1538-4357/ab01ca

TY - JOUR

T1 - Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data

AU - Raghunathan, S.

AU - Patil, S.

AU - Baxter, E.

AU - Benson, B. A.

AU - Bleem, L. E.

AU - Chou, T. L.

AU - Crawford, T. M.

AU - Holder, G. P.

AU - McClintock, T.

AU - Reichardt, C. L.

AU - Rozo, E.

AU - Varga, T. N.

AU - Abbott, T. M.C.

AU - Ade, P. A.R.

AU - Allam, S.

AU - Anderson, A. J.

AU - Annis, J.

AU - Austermann, J. E.

AU - Avila, S.

AU - Beall, J. A.

AU - Bechtol, K.

AU - Bender, A. N.

AU - Bernstein, G.

AU - Bertin, E.

AU - Bianchini, F.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carlstrom, J. E.

AU - Carretero, J.

AU - Chang, C. L.

AU - Chiang, H. C.

AU - Cho, H. M.

AU - Citron, R.

AU - Crites, A. T.

AU - Cunha, C. E.

AU - Costa, L. N.Da

AU - Davis, C.

AU - Desai, S.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Dobbs, M. A.

AU - Doel, P.

AU - Eifler, T. F.

AU - Everett, W.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - Gallicchio, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - George, E. M.

AU - Gilbert, A.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gupta, N.

AU - Gutierrez, G.

AU - Haan, T. De

AU - Halverson, N. W.

AU - Harrington, N.

AU - Hartley, W. G.

AU - Henning, J. W.

AU - Hilton, G. C.

AU - Hollowood, D. L.

AU - Holzapfel, W. L.

AU - Honscheid, K.

AU - Hou, Z.

AU - Hoyle, B.

AU - Hrubes, J. D.

AU - Huang, N.

AU - Hubmayr, J.

AU - Irwin, K. D.

AU - James, D. J.

AU - Jeltema, T.

AU - Kim, A. G.

AU - Kind, M. Carrasco

AU - Knox, L.

AU - Kovacs, A.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lee, A. T.

AU - Li, T. S.

AU - Lima, M.

AU - Maia, M. A.G.

AU - Marshall, J. L.

AU - McMahon, J. J.

AU - Melchior, P.

AU - Menanteau, F.

AU - Meyer, S. S.

AU - Miller, C. J.

AU - Miquel, R.

AU - Mocanu, L.

AU - Montgomery, J.

AU - Nadolski, A.

AU - Natoli, T.

AU - Nibarger, J. P.

AU - Novosad, V.

AU - Padin, S.

AU - Plazas, A. A.

AU - Pryke, C.

AU - Rapetti, D.

AU - Romer, A. K.

AU - Rosell, A. Carnero

AU - Ruhl, J. E.

AU - Saliwanchik, B. R.

AU - Sanchez, E.

AU - Sayre, J. T.

AU - Scarpine, V.

AU - Schaffer, K. K.

AU - Schubnell, M.

AU - Serrano, S.

AU - Sevilla-Noarbe, I.

AU - Smecher, G.

AU - Smith, R. C.

AU - Soares-Santos, M.

AU - Sobreira, F.

AU - Stark, A. A.

AU - Story, K. T.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thomas, D.

AU - Tucker, C.

AU - Vanderlinde, K.

AU - Vicente, J. De

AU - Vieira, J. D.

AU - Wang, G.

AU - Whitehorn, N.

AU - Wu, W. L.K.

AU - Zhang, Y.

PY - 2019

Y1 - 2019

N2 - We use cosmic microwave background (CMB) temperature maps from the 500 deg 2 SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel'dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz data sets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7σ(6.7σ) with the flux (volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be M 200m = (1.62 -0.25 +0.32 [stat] ± 0.04 [sys.]) and (1.28 -0.18 +0.14 [stat] ± 0.03[sys.])× 10 14 M ⊙ for the volume- and flux-limited samples, respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES.

AB - We use cosmic microwave background (CMB) temperature maps from the 500 deg 2 SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel'dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz data sets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7σ(6.7σ) with the flux (volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be M 200m = (1.62 -0.25 +0.32 [stat] ± 0.04 [sys.]) and (1.28 -0.18 +0.14 [stat] ± 0.03[sys.])× 10 14 M ⊙ for the volume- and flux-limited samples, respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES.

KW - cosmic background radiation

KW - galaxies: clusters: general

KW - gravitational lensing: weak

UR - http://www.scopus.com/inward/record.url?scp=85063490554&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ab01ca

DO - 10.3847/1538-4357/ab01ca

M3 - Article

AN - SCOPUS:85063490554

SN - 0004-637X

VL - 872

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 170

ER -

Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data

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