RETRACTED: Survey geometry and the internal consistency of recent cosmic shear measurements (Retracted Article)

被引：70

作者：

Troxel, M. A. ^{[1
,2
]}

Krause, E. ^{[3
,4
]}

Chang, C. ^{[5
]}

Eifler, T. F. ^{[3
,4
]}

Friedrich, O. ^{[6
,7
]}

Gruen, D. ^{[8
,9
]}

MacCrann, N. ^{[1
,2
]}

Chen, A. ^{[10
]}

Davis, C. ^{[8
]}

DeRose, J. ^{[8
,11
]}

Dodelson, S. ^{[12
]}

Gatti, M. ^{[13
]}

Hoyle, B. ^{[6
,7
]}

Huterer, D. ^{[10
]}

Jarvis, M. ^{[14
]}

Lacasa, F. ^{[15
,16
,17
]}

Lemos, P. ^{[18
,19
]}

Peiris, H. V. ^{[20
]}

Prat, J. ^{[13
]}

Samuroff, S. ^{[12
]}

Sanchez, C. ^{[13
,14
]}

Sheldon, E. ^{[21
]}

Vielzeuf, P. ^{[13
]}

Wang, M. ^{[22
]}

Zuntz, J. ^{[23
]}

Lahav, O. ^{[20
]}

Abdalla, F. B. ^{[20
,24
]}

Allam, S. ^{[22
]}

Annis, J. ^{[22
]}

Avila, S. ^{[25
]}

Bertin, E. ^{[26
,27
]}

Brooks, D. ^{[20
]}

Burke, D. L. ^{[8
,9
]}

Rosell, A. Carnero ^{[17
,28
]}

Kind, M. Carrasco ^{[29
,30
]}

Carretero, J. ^{[13
]}

Crocce, M. ^{[31
,32
]}

Cunha, C. E. ^{[8
]}

D'Andrea, C. B. ^{[14
]}

da Costa, L. N. ^{[17
,28
]}

De Vicente, J. ^{[33
]}

Diehl, H. T. ^{[22
]}

Doel, P. ^{[20
]}

Evrard, A. E. ^{[10
,34
]}

Flaugher, B. ^{[22
]}

Fosalba, P. ^{[31
,32
]}

Frieman, J. ^{[5
,22
]}

Garcia-Bellido, J. ^{[35
]}

Gaztanaga, E. ^{[31
,32
]}

Gerdes, D. W. ^{[10
,34
]}

机构：

[1] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[2] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

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

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

[5] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

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

[7] Ludwig Maximilians Univ Munchen, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany

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

[9] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[10] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[11] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[12] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15312 USA

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

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

[15] Univ Geneva, Dept Phys Theor, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[16] Univ Geneva, Ctr Astroparticle Phys, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

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

[18] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[19] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

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

[21] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA

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

[23] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland

[24] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

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

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

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

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

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

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

[31] IEEC, E-08193 Barcelona, Spain

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

[33] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain

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

[35] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain

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

[37] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[38] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[39] Australian Astron Observ, N Ryde, NSW 2113, Australia

[40] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

[41] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain

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

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

[44] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[45] Brandeis Univ, Dept Phys, 415 South St, Waltham, MA 02453 USA

[46] Univ Estadual Campinas, Inst Fis Gleb Wataghin, BR-13083859 Campinas, SP, Brazil

[47] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA

[48] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 479卷 / 04期

基金：

欧洲研究理事会; 澳大利亚研究理事会; 美国国家航空航天局; 美国国家科学基金会;

关键词：

gravitational lensing: weak; methods: data analysis; methods: statistical; COSMOLOGICAL PARAMETER CONSTRAINTS; ACCURATE HALO-MODEL; 2-POINT STATISTICS; DARK ENERGY; MASSIVE NEUTRINOS; POWER SPECTRA; CFHTLENS; CATALOG;

D O I：

10.1093/mnras/sty1889

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We explore the impact of an update to the typical approximation for the shape noise term in the analytic covariance matrix for cosmic shear experiments that assumes the absence of survey boundary and mask effects. We present an exact expression for the number of galaxy pairs in this term based on the survey mask, which leads to more than a factor of three increase in the shape noise on the largest measured scales for the Kilo-Degree Survey (KiDS-450) real-space cosmic shear data. We compare the result of this analytic expression to several alternative methods for measuring the shape noise from the data and find excellent agreement. This update to the covariance resolves any internal model tension evidenced by the previously large cosmological best-fitting chi(2) for the KiDS-450 cosmic shear data. The best-fitting chi(2) is reduced from 161 to 121 for 118 degrees of freedom. We also apply a correction to how the multiplicative shear calibration uncertainty is included in the covariance. This change shifts the inferred amplitude of the correlation function to higher values. We find that this improves agreement of the KiDS-450 cosmic shear results with Dark Energy Survey Year 1 and Planck results.

引用

页码：4998 / 5004

页数：7

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