Cosmology from large-scale galaxy clustering and galaxy-galaxy lensing with Dark Energy Survey Science Verification data

被引：51

作者：

Kwan, J. ^{[1
]}

Sanchez, C. ^{[2
]}

Clampitt, J. ^{[1
]}

Blazek, J. ^{[3
]}

Crocce, M. ^{[4
]}

Jain, B. ^{[1
]}

Zuntz, J. ^{[5
]}

Amara, A. ^{[6
]}

Becker, M. R. ^{[7
,8
]}

Bernstein, G. M. ^{[1
]}

Bonnett, C.

DeRose, J. ^{[7
,8
]}

Dodelson, S. ^{[9
,10
,11
]}

Eifler, T. F. ^{[12
]}

Gaztanaga, E. ^{[4
]}

Giannantonio, T. ^{[13
,14
]}

Gruen, D. ^{[8
,15
]}

Hartley, W. G. ^{[6
]}

Kacprzak, T. ^{[6
]}

Kirk, D. ^{[16
]}

Krause, E. ^{[8
]}

MacCrann, N. ^{[5
]}

Miquel, R. ^{[2
,17
]}

Park, Y. ^{[18
]}

Ross, A. J. ^{[3
]}

Rozo, E. ^{[18
]}

Rykoff, E. S. ^{[8
,15
]}

Sheldon, E. ^{[19
]}

Troxel, M. A. ^{[5
]}

Wechsler, R. H. ^{[7
,8
,15
]}

Abbott, T. M. C. ^{[20
]}

Abdalla, F. B. ^{[16
,21
]}

Allam, S. ^{[9
]}

Benoit-Levy, A. ^{[16
,22
,23
]}

Brooks, D. ^{[16
]}

Burke, D. L. ^{[15
]}

Rosell, A. Carnero ^{[24
,25
]}

Kind, M. Carrasco ^{[26
,27
]}

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

D'Andrea, C. B. ^{[28
,29
]}

da Costa, L. N. ^{[24
,25
]}

Desai, S. ^{[30
,31
]}

Diehl, H. T. ^{[9
]}

Dietrich, J. P. ^{[30
,31
]}

Doel, P. ^{[16
]}

Evrard, A. E. ^{[32
,33
]}

Fernandez, E. ^{[2
]}

Finley, D. A. ^{[9
]}

Flaugher, B. ^{[9
]}

Fosalba, P. ^{[2
]}

机构：

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[34] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

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

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

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

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

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

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

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

[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 Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2017年 / 464卷 / 04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：

gravitational lensing: weak; cosmological parameters; large-scale structure of Universe; BARYON ACOUSTIC-OSCILLATIONS; 100 SQUARE DEGREES; PARAMETER CONSTRAINTS; WEAK; CFHTLENS; PRECISION; MODEL; DEPENDENCE; EFFICIENT; I;

D O I：

10.1093/mnras/stw2464

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present cosmological constraints from the Dark Energy Survey (DES) using a combined analysis of angular clustering of red galaxies and their cross-correlation with weak gravitational lensing of background galaxies. We use a 139 deg(2) contiguous patch of DES data from the Science Verification (SV) period of observations. Using large-scale measurements, we constrain the matter density of the Universe as Omega(m) = 0.31 +/- 0.09 and the clustering amplitude of the matter power spectrum as sigma(8) = 0.74 +/- 0.13 after marginalizing over seven nuisance parameters and three additional cosmological parameters. This translates into S-8 = sigma(8)(Omega(m)/0.3)(0.16) = 0.74 +/- 0.12 for our fiducial lens redshift bin at 0.35 < z < 0.5, while S-8 = 0.78 +/- 0.09 using two bins over the range 0.2 < z < 0.5. We study the robustness of the results under changes in the data vectors, modelling and systematics treatment, including photometric redshift and shear calibration uncertainties, and find consistency in the derived cosmological parameters. We show that our results are consistent with previous cosmological analyses from DES and other data sets and conclude with a joint analysis of DES angular clustering and galaxy-galaxy lensing with Planck Cosmic Microwave Background data, baryon accoustic oscillations and Supernova Type Ia measurements.

引用

页码：4045 / 4062

页数：18

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