Blinding multiprobe cosmological experiments

被引：24

作者：

Muir, J. ^{[1
,2
]}

Bernstein, G. M. ^{[3
]}

Huterer, D. ^{[2
]}

Elsner, F. ^{[4
,5
]}

Krause, E. ^{[6
]}

Roodman, A. ^{[1
,7
]}

Allam, S. ^{[8
]}

Annis, J. ^{[8
]}

Avila, S. ^{[9
]}

Bechtol, K. ^{[10
,11
]}

Bertin, E. ^{[12
,13
]}

Brooks, D. ^{[4
]}

Buckley-Geer, E. ^{[8
]}

Burke, D. L. ^{[1
,7
]}

Rosell, A. Carnero ^{[14
,15
]}

Kind, M. Carrasco ^{[16
,17
]}

Carretero, J. ^{[18
]}

Cawthon, R. ^{[11
]}

Costanzi, M. ^{[19
,20
]}

da Costa, L. N. ^{[15
,21
]}

De Vicente, J. ^{[14
]}

Desai, S. ^{[22
]}

Dietrich, J. P. ^{[23
,24
]}

Doel, P. ^{[4
]}

Eifler, T. F. ^{[6
,25
]}

Everett, S. ^{[26
]}

Fosalba, P. ^{[27
,28
]}

Frieman, J. ^{[8
,29
]}

Garcia-Bellido, J. ^{[9
]}

Gerdes, D. W. ^{[2
,30
]}

Gruen, D. ^{[17
,31
]}

Gruendl, R. A. ^{[16
,17
]}

Gschwend, J. ^{[15
,21
]}

Hartley, W. G. ^{[4
,32
]}

Hollowood, D. L. ^{[26
]}

James, D. J. ^{[33
]}

Jarvis, M. ^{[3
]}

Kuehn, K. ^{[34
,35
]}

Kuropatkin, N. ^{[8
]}

Lahav, O. ^{[4
]}

March, M. ^{[3
]}

Marshall, J. L. ^{[36
]}

Melchior, P. ^{[37
]}

Menanteau, F. ^{[16
,17
]}

Miquel, R. ^{[18
,38
]}

Ogando, R. L. C. ^{[15
,21
]}

Palmese, A. ^{[8
,29
]}

Paz-Chinchon, F. ^{[16
,17
]}

Plazas, A. A. ^{[37
]}

Romer, A. K. ^{[39
]}

机构：

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

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

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

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

[5] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany

[6] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

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

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

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

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

[11] Univ Wisconsin, Phys Dept, 2320 Chamberlin Hall,1150 Univ Ave, Madison, WI 53706 USA

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

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

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

[15] Lab Interinst eAstron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

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

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

[18] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[19] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[20] Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

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

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

[23] Excellence Cluster Origins, Boltzmannstr 2, D-85748 Garching, Germany

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

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

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

[27] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

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

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

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

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

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

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

[34] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

[35] Lowell Observ, 1400 Mars Hill Rd, Flagstaff, AZ 86001 USA

[36] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA

[37] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

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

[39] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England

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

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

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

[43] Duke Univ, Dept Phys, Durham, NC 27708 USA

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

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

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 494卷 / 03期

基金：

美国国家科学基金会; 英国科学技术设施理事会;

关键词：

methods: data analysis; methods: numerical; methods: statistical; cosmology: observations; large-scale structure of Universe; IA SUPERNOVAE; COSMIC SHEAR; CONSTRAINTS; EFFICIENT; COVARIANCES; INFERENCE; H-0;

D O I：

10.1093/mnras/staa965

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The goal of blinding is to hide an experiment's critical results - here the inferred cosmological parameters - until all decisions affecting its analysis have been finalized. This is especially important in the current era of precision cosmology, when the results of any new experiment are closely scrutinized for consistency or tension with previous results. In analyses that combine multiple observational probes, like the combination of galaxy clustering and weak lensing in the Dark Energy Survey (DES), it is challenging to blind the results while retaining the ability to check for (in)consistency between different parts of the data. We propose a simple new blinding transformation, which works by modifying the summary statistics that are input to parameter estimation, such as two-point correlation functions. The transformation shifts the measured statistics to new values that are consistent with (blindly) shifted cosmological parameters while preserving internal (in)consistency. We apply the blinding transformation to simulated data for the projected DES Year 3 galaxy clustering and weak lensing analysis, demonstrating that practical blinding is achieved without significant perturbation of internal-consistency checks, as measured here by degradation of the chi(2) between the data and best-fitting model. Our blinding method's performance is expected to improve as experiments evolve to higher precision and accuracy.

引用

页码：4454 / 4470

页数：17

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