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

被引：27

作者：

Raghunathan, S. ^{[1
,2
]}

Patil, S. ^{[1
]}

Baxter, E. ^{[3
]}

Benson, B. A. ^{[4
,5
,6
]}

Bleem, L. E. ^{[5
,7
]}

Chou, T. L. ^{[8
]}

Crawford, T. M. ^{[5
,6
]}

Holder, G. P. ^{[9
,10
]}

McClintock, T. ^{[11
]}

Reichardt, C. L. ^{[1
]}

Rozo, E. ^{[11
]}

Varga, T. N. ^{[12
,13
]}

Abbott, T. M. C. ^{[14
]}

Ade, P. A. R. ^{[15
]}

Allam, S. ^{[16
]}

Anderson, A. J. ^{[4
]}

Annis, J. ^{[16
]}

Austermann, J. E. ^{[17
]}

Avila, S. ^{[18
]}

Beall, J. A. ^{[17
]}

Bechtol, K. ^{[19
]}

Bender, A. N. ^{[5
,7
]}

Bernstein, G. ^{[3
]}

Bertin, E. ^{[20
,21
]}

Bianchini, F. ^{[1
]}

Brooks, D. ^{[22
]}

Burke, D. L. ^{[23
,24
]}

Carlstrom, J. E. ^{[5
,6
,7
,25
,26
]}

Carretero, J. ^{[27
]}

Chang, C. L. ^{[5
,6
,7
]}

Chiang, H. C. ^{[28
]}

Cho, H-M. ^{[24
]}

Citron, R. ^{[5
]}

Crites, A. T. ^{[5
,6
,29
]}

Cunha, C. E. ^{[23
]}

da Costa, L. N. ^{[30
,31
]}

Davis, C. ^{[23
]}

Desai, S. ^{[32
]}

Diehl, H. T. ^{[16
]}

Dietrich, J. P. ^{[33
,34
]}

Dobbs, M. A. ^{[9
,10
]}

Doel, P. ^{[22
]}

Eifler, T. F. ^{[35
,36
]}

Everett, W. ^{[37
]}

Evrard, A. E. ^{[38
,39
]}

Flaugher, B. ^{[16
]}

Fosalba, P. ^{[40
,41
]}

Frieman, J. ^{[5
,16
]}

Gallicchio, J. ^{[5
,42
]}

Garcia-Bellido, J. ^{[43
]}

机构：

[1] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

[2] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

[3] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[4] Fermilab Natl Accelerator Lab, MS209,POB 500, Batavia, IL 60510 USA

[5] Univ Chicago, Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA

[6] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA

[7] Argonne Natl Lab, Div High Energy Phys, 9700 S Cass Ave, Argonne, IL 60439 USA

[8] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

[9] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada

[10] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada

[11] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA

[12] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[13] LudwigMaximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany

[14] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile

[15] Cardiff Univ, Cardiff CF10 3XQ, S Glam, Wales

[16] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[17] NIST, Quantum Devices Grp, 325 Broadway Mailcode 817-03, Boulder, CO 80305 USA

[18] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[19] LSST, 933 North Cherry Ave, Tucson, AZ 85721 USA

[20] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

[21] UPMC Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[22] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[23] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[24] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA

[25] Univ Chicago, Dept Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA

[26] Univ Chicago, Enrico Fermi Inst, 5640 South Ellis Ave, Chicago, IL 60637 USA

[27] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[28] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Durban, South Africa

[29] CALTECH, MS 249-17,1216 E Calif Blvd, Pasadena, CA 91125 USA

[30] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[31] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[32] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[33] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[34] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany

[35] Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA

[36] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[37] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[38] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[39] Univ Michigan, Dept Phys, 450 Church St, Ann Arbor, MI 48109 USA

[40] IEEC, E-08193 Barcelona, Spain

[41] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[42] Harvey Mudd Coll, 301 Platt Blvd, Claremont, CA 91711 USA

[43] UAM, CSIC, Inst Fis Teor, E-28049 Madrid, Spain

[44] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[45] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[46] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[47] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[48] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA

[49] Univ Colorado, Dept Phys, Boulder, CO 80309 USA

[50] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

来源：

ASTROPHYSICAL JOURNAL | 2019年 / 872卷 / 02期

基金：

澳大利亚研究理事会; 欧洲研究理事会; 美国国家科学基金会; 英国科学技术设施理事会;

关键词：

cosmic background radiation; galaxies: clusters: general; gravitational lensing: weak; GALAXY CLUSTERS; DARK ENERGY; MODEL; CONSTRAINTS; GIANTS;

D O I：

10.3847/1538-4357/ab01ca

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 8.7 sigma(6.7 sigma) 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-200 m =(1.62(-0.25)(+0.35) [stat.] +/- 0.04 [sys.] and (1.28(-0.18)(+0.14) [stat.] +/- 0.03 [sys.] x 10(14) M-circle dot 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.

引用

页数：14

共 25 条

[1] Detection of CMB-Cluster Lensing using Polarization Data from SPTpol
Raghunathan, S.
Patil, S.
Baxter, E.
Benson, B. A.
Bleem, L. E.
Crawford, T. M.
Holder, G. P.
McClintock, T.
Reichardt, C. L.
Varga, T. N.
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Ade, P. A. R.
Allam, S.
Anderson, A. J.
Austermann, J. E.
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Chiang, H. C.
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Costanzi, M.
Crites, A. T.
da Costa, L. N.
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Dietrich, J. P.
Dobbs, M. A.
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Flaugher, B.
Fosalba, P.
Frieman, J.
Gallicchio, J.
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PHYSICAL REVIEW LETTERS, 2019, 123 (18)
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