Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing

被引：615

作者：

Abbott, T. M. C. ^{[1
]}

Aguena, M. ^{[2
]}

Alarcon, A. ^{[3
]}

Allam, S. ^{[4
]}

Alves, O. ^{[2
,5
,6
]}

Amon, A. ^{[7
]}

Andrade-Oliveira, F. ^{[2
,6
]}

Annis, J. ^{[4
]}

Avila, S. ^{[8
]}

Bacon, D. ^{[9
]}

Baxter, E. ^{[10
]}

Bechtol, K. ^{[11
]}

Becker, M. R. ^{[3
]}

Bernstein, G. M. ^{[12
]}

Bhargava, S. ^{[13
]}

Birrer, S. ^{[14
]}

Blazek, J. ^{[15
,16
]}

Brandao-Souza, A. ^{[2
,17
]}

Bridle, S. L. ^{[18
]}

Brooks, D. ^{[19
]}

Buckley-Geer, E. ^{[4
,20
]}

Burke, D. L. ^{[7
,21
]}

Camacho, H. ^{[2
,6
]}

Campos, A. ^{[22
]}

Carnero Rosell, A. ^{[2
,23
,24
]}

Carrasco Kind, M. ^{[25
,26
]}

Carretero, J. ^{[27
]}

Castander, F. J. ^{[28
,29
]}

Cawthon, R. ^{[11
]}

Chang, C. ^{[20
,30
]}

Chen, A. ^{[5
]}

Chen, R. ^{[31
]}

Choi, A. ^{[32
]}

Conselice, C. ^{[18
,33
]}

Cordero, J. ^{[18
]}

Costanzi, M. ^{[34
,35
,36
]}

Crocce, M. ^{[28
,29
]}

da Costa, L. N. ^{[2
,37
]}

Pereira, M. E. da Silva ^{[5
]}

Davis, C. ^{[7
]}

Davis, T. M. ^{[38
]}

De Vicente, J. ^{[39
]}

DeRose, J. ^{[40
]}

Desai, S. ^{[41
]}

Di Valentino, E. ^{[18
]}

Diehl, H. T. ^{[4
]}

Dietrich, J. P. ^{[42
]}

Dodelson, S. ^{[22
,43
]}

Doel, P. ^{[19
]}

Doux, C. ^{[12
]}

机构：

[1] NSFs Natl Opt Infrared Astron Res Lab, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

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

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

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

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

[6] Univ Estadual Paulista, Inst Fis Teor, BR-01140070 Sao Paulo, Brazil

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

[8] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, Madrid 28049, Spain

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

[10] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

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

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

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

[14] Stanford Univ, Grad Sch Educ, 160,450 Serra Mall, Stanford, CA 94305 USA

[15] Northeastern Univ, Dept Phys, Boston, MA 02115 USA

[16] Ecole Polytech Fed Lausanne EPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland

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

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

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

[20] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

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

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

[23] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain

[24] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[25] Natl Ctr Supercomp Applicat, Ctr Astrophys Surveys, 1205 West Clark St, Urbana, IL 61801 USA

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

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

[28] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain

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

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

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

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

[33] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

[34] Univ Trieste, Dept Phys, Astron Unit, Via Tiepolo 11, I-34131 Trieste, Italy

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

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

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

[38] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[39] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid 28040, Spain

[40] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

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

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

[43] Carnegie Mellon Univ, NSF AI Planning Inst Phys Future, Pittsburgh, PA 15213 USA

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

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

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

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

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

[49] Univ Texas Austin, Dept Stat, Austin, TX 78757 USA

[50] Univ Texas Austin, Dept Data Sci, Austin, TX 78757 USA

来源：

PHYSICAL REVIEW D | 2022年 / 105卷 / 02期

基金：

英国科学技术设施理事会; 欧洲研究理事会; 美国国家科学基金会;

关键词：

DIGITAL SKY SURVEY; ANISOTROPIC POWER SPECTRUM; SPECTROSCOPIC SURVEY MEASUREMENT; MASS CORRELATION-FUNCTION; SUPERNOVA LEGACY SURVEY; LUMINOUS RED GALAXIES; PHOTOMETRIC DATA SET; COSMIC SHEAR; PARAMETER CONSTRAINTS; IA SUPERNOVAE;

D O I：

10.1103/PhysRevD.105.023520

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first cosmology results from large-scale structure using the full 5000 deg(2) of imaging data from the Dark Energy Survey (DES) Data Release 1. We perform an analysis of large-scale structure combining three two-point correlation functions (3 x 2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions, galaxy-galaxy lensing. To achieve the cosmological precision enabled by these measurements has required updates to nearly every part of the analysis from DES Year 1, including the use of two independent galaxy clustering samples, modeling advances, and several novel improvements in the calibration of gravitational shear and photometric redshift inference. The analysis was performed under strict conditions to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results and tests of the robustness of our results to this decision. We model the data within the flat Lambda CDM and wCDM cosmological models, marginalizing over 25 nuisance parameters. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude S-8 = 0.776(-0.017)(+0.017) and matter density Omega(m) = 0.339(-0.031)(+0.032) in Lambda CDM, mean with 68% confidence limits; S-8 = 0.775(-0.024)(+0.026), Omega(m) = 0.352(-0.041)(+0.035), and dark energy equation-of-state parameter w = -0.98(-0.02)(+0.32) in wCDM. These constraints correspond to an improvement in signal-to-noise of the DES Year 33 x 2pt data relative to DES Year 1 by a factor of 2.1, about 20% more than expected from the increase in observing area alone. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed p = 0.13-0.48. We find better agreement between DES 3 x 2pt and Planck than in DES Y1, despite the significantly improved precision of both. When combining DES 3 x 2pt data with available baryon acoustic oscillation, redshift-space distortion, and type la supernovae data, we find p = 0.34. Combining all of these datasets with Planck CMB lensing yields joint parameter constraints of S-8 = 0.812(-0.008)(+0.008), Omega(m) = 0.306(-0.005)(+0.004), h = 0.680(-0.003)(+0.004), and Sigma m(nu) < 0.13 eV (95% C.L.) in Lambda CDM; S-8 = 0.812(-0.008)(+0.008), Omega(m) = 0.302(-0.006)(+0.006), h = 0.687(-0.007)(+0.006), and w = -1.031(-0.027)(+0.030) in wCDM.

引用

页数：42

共 230 条

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共 230 条

[1] The Dark Energy Survey: more than dark energy - an overview [J].

Abbott, T. ;

Abdalla, F. B. ;

Aleksic, J. ;

Allam, S. ;

Amara, A. ;

Bacon, D. ;

Balbinot, E. ;

Banerji, M. ;

Bechtol, K. ;

Benoit-Levy, A. ;

Bernstein, G. M. ;

Bertin, E. ;

Blazek, J. ;

Bonnett, C. ;

Bridle, S. ;

Brooks, D. ;

Brunner, R. J. ;

Buckley-Geer, E. ;

Burke, D. L. ;

Caminha, G. B. ;

Capozzi, D. ;

Carlsen, J. ;

Carnero-Rosell, A. ;

Carollo, M. ;

Carrasco-Kind, M. ;

Carretero, J. ;

Castander, F. J. ;

Clerkin, L. ;

Collett, T. ;

Conselice, C. ;

Crocce, M. ;

Cunha, C. E. ;

D'Andrea, C. B. ;

da Costa, L. N. ;

Davis, T. M. ;

Desai, S. ;

Diehl, H. T. ;

Dietrich, J. P. ;

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