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

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