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 (US) |
---|---|
Article number | 170 |
Journal | Astrophysical Journal |
Volume | 872 |
Issue number | 2 |
DOIs | |
State | Published - Jan 1 2019 |
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Keywords
- cosmic background radiation
- galaxies: clusters: general
- gravitational lensing: weak
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Mass Calibration of Optically Selected des Clusters Using a Measurement of CMB-cluster Lensing with SPTpol Data. / 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.; Beall, J. A.; Bechtol, K.; Bender, A. N.; Bernstein, G.; Bertin, E.; Bianchini, F.; Brooks, D.; Burke, D. L.; Carlstrom, J. E.; Carretero, J.; Chang, C. L.; Chiang, H. C.; Cho, H. M.; Citron, R.; Crites, A. T.; Cunha, C. E.; Costa, L. N.Da; Davis, C.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Dobbs, M. A.; Doel, P.; Eifler, T. F.; Everett, W.; Evrard, A. E.; Flaugher, B.; Fosalba, P.; Frieman, J.; Gallicchio, J.; García-Bellido, J.; Gaztanaga, E.; George, E. M.; Gilbert, A.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gupta, N.; Gutierrez, G.; Haan, T. De; Halverson, N. W.; Harrington, N.; Hartley, W. G.; Henning, J. W.; Hilton, G. C.; Hollowood, D. L.; Holzapfel, W. L.; Honscheid, K.; Hou, Z.; Hoyle, B.; Hrubes, J. D.; Huang, N.; Hubmayr, J.; Irwin, K. D.; James, D. J.; Jeltema, T.; Kim, A. G.; Kind, M. Carrasco; Knox, L.; Kovacs, A.; Kuehn, K.; Kuropatkin, N.; Lee, A. T.; Li, T. S.; Lima, M.; Maia, M. A.G.; Marshall, J. L.; McMahon, J. J.; Melchior, P.; Menanteau, F.; Meyer, S. S.; Miller, C. J.; Miquel, R.; Mocanu, L.; Montgomery, J.; Nadolski, A.; Natoli, T.; Nibarger, J. P.; Novosad, V.; Padin, S.; Plazas, A. A.; Pryke, C.; Rapetti, D.; Romer, A. K.; Rosell, A. Carnero; Ruhl, J. E.; Saliwanchik, B. R.; Sanchez, E.; Sayre, J. T.; Scarpine, V.; Schaffer, K. K.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I.; Smecher, G.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Stark, A. A.; Story, K. T.; Suchyta, E.; Swanson, M. E.C.; Tarle, G.; Thomas, D.; Tucker, C.; Vanderlinde, K.; Vicente, J. De; Vieira, J. D.; Wang, G.; Whitehorn, N.; Wu, W. L.K.; Zhang, Y.
In: Astrophysical Journal, Vol. 872, No. 2, 170, 01.01.2019.Research output: Contribution to journal › Article
}
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 - 2019/1/1
Y1 - 2019/1/1
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
UR - http://www.scopus.com/inward/citedby.url?scp=85063490554&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab01ca
DO - 10.3847/1538-4357/ab01ca
M3 - Article
AN - SCOPUS:85063490554
VL - 872
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 170
ER -