Cosmic shear measurements with Dark Energy Survey Science Verification data

被引：84

作者：

Becker, M. R. ^{[1
,2
]}

Troxel, M. A. ^{[3
]}

MacCrann, N. ^{[3
]}

Krause, E. ^{[2
]}

Eifler, T. F. ^{[4
,5
]}

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

Nicola, A. ^{[8
]}

Refregier, A. ^{[8
]}

Amara, A. ^{[8
]}

Bacon, D. ^{[9
]}

Bernstein, G. M. ^{[4
]}

Bonnett, C. ^{[10
]}

Bridle, S. L. ^{[3
]}

Busha, M. T. ^{[1
,2
]}

Chang, C. ^{[8
]}

Dodelson, S. ^{[11
,12
]}

Erickson, B. ^{[13
]}

Evrard, A. E. ^{[13
,14
]}

Frieman, J. ^{[11
,12
]}

Gaztanaga, E. ^{[15
]}

Gruen, D. ^{[6
,7
]}

Hartley, W. ^{[8
]}

Jain, B. ^{[4
]}

Jarvis, M. ^{[4
]}

Kacprzak, T. ^{[8
]}

Kirk, D. ^{[16
]}

Kravtsov, A. ^{[12
]}

Leistedt, B. ^{[16
]}

Peiris, H. V. ^{[16
]}

Rykoff, E. S. ^{[2
,17
]}

Sabiu, C. ^{[18
]}

Sanchez, C. ^{[10
]}

Seo, H. ^{[19
]}

Sheldon, E. ^{[20
]}

Wechsler, R. H. ^{[1
,2
,17
]}

Zuntz, J. ^{[3
]}

Abbott, T. ^{[21
]}

Abdalla, F. B. ^{[16
,22
]}

Allam, S. ^{[11
]}

Armstrong, R. ^{[23
]}

Banerji, M. ^{[24
,25
]}

Bauer, A. H. ^{[15
]}

Benoit-Levy, A. ^{[16
]}

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

Brooks, D. ^{[16
]}

Buckley-Geer, E. ^{[11
]}

Burke, D. L. ^{[2
,17
]}

Capozzi, D. ^{[9
]}

Carnero Rosell, A. ^{[28
,29
]}

Kind, M. Carrasco ^{[30
,31
]}

机构：

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

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

[3] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs, England

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

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

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

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

[8] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

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

[10] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain

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

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

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

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

[15] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain

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

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

[18] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[33] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[34] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

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

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

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

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

[39] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

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

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

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

[43] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain

[44] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA

[45] Www Sepnet Ac Uk, South East Phys Network, SEPnet, Southampton, Hants, England

[46] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA

来源：

PHYSICAL REVIEW D | 2016年 / 94卷 / 02期

基金：

英国科学技术设施理事会; 巴西圣保罗研究基金会; 美国国家科学基金会; 欧洲研究理事会;

关键词：

POLARIZATION POWER SPECTRA; GALAXY SHAPE MEASUREMENT; WEAK LENSING SURVEYS; NOISE BIAS; COVARIANCE; IMPACT; STATISTICS; MATTER; MODEL; SIMULATIONS;

D O I：

10.1103/PhysRevD.94.022002

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present measurements of weak gravitational lensing cosmic shear two-point statistics using Dark Energy Survey Science Verification data. We demonstrate that our results are robust to the choice of shear measurement pipeline, either NGMIX or IM3SHAPE, and robust to the choice of two-point statistic, including both real and Fourier-space statistics. Our results pass a suite of null tests including tests for B-mode contamination and direct tests for any dependence of the two-point functions on a set of 16 observing conditions and galaxy properties, such as seeing, airmass, galaxy color, galaxy magnitude, etc. We furthermore use a large suite of simulations to compute the covariance matrix of the cosmic shear measurements and assign statistical significance to our null tests. We find that our covariance matrix is consistent with the halo model prediction, indicating that it has the appropriate level of halo sample variance. We compare the same jackknife procedure applied to the data and the simulations in order to search for additional sources of noise not captured by the simulations. We find no statistically significant extra sources of noise in the data. The overall detection significance with tomography for our highest source density catalog is 9.7 sigma. Cosmological constraints from the measurements in this work are presented in a companion paper.

引用

页数：24

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