Dark energy survey year 3 results: cosmological constraints from the analysis of cosmic shear in harmonic space

被引:34
作者
Doux, C. [1 ]
Jain, B. [1 ]
Zeurcher, D. [2 ]
Lee, J. [1 ]
Fang, X. [3 ,4 ]
Rosenfeld, R. [5 ,6 ]
Amon, A. [7 ]
Camacho, H. [6 ,8 ]
Choi, A. [9 ]
Secco, L. F. [10 ]
Blazek, J. [11 ,12 ]
Chang, C. [10 ,13 ]
Gatti, M. [1 ]
Gaztanaga, E. [14 ,15 ]
Jeffrey, N. [16 ,17 ]
Raveri, M. [1 ]
Samuroff, S. [18 ]
Alarcon, A. [19 ]
Alves, O. [6 ,20 ]
Andrade-Oliveira, F. [20 ]
Baxter, E. [21 ]
Bechtol, K. [22 ]
Becker, M. R. [19 ]
Bernstein, G. M. [1 ]
Campos, A. [18 ]
Carnero Rosell, A. [6 ,23 ,24 ]
Kind, M. Carrasco [25 ,26 ]
Cawthon, R. [27 ]
Chen, R. [28 ]
Cordero, J. [29 ]
Crocce, M. [14 ,15 ]
Davis, C. [7 ]
DeRose, J. [30 ]
Dodelson, S. [18 ,31 ]
Drlica-Wagner, A. [10 ,13 ,32 ]
Eckert, K. [1 ]
Eifler, T. F. [4 ,33 ]
Elsner, F. [16 ]
Elvin-Poole, J. [34 ,35 ]
Everett, S. [36 ]
Ferte, A. [33 ]
Fosalba, P. [14 ,15 ]
Friedrich, O. [37 ]
Giannini, G. [38 ]
Gruen, D. [39 ]
Gruendl, R. A. [25 ,26 ]
Harrison, I [29 ,40 ,41 ]
Hartley, W. G. [42 ]
Herner, K. [32 ]
Huang, H. [4 ,43 ]
机构
[1] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA
[2] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland
[3] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA
[4] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA
[5] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, Sao Paulo, Brazil
[6] Lab Interinst W Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil
[7] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA
[8] Univ Estadual Paulista, Inst Fis Teor, Sao Paulo, Brazil
[9] CALTECH, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA
[10] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[11] Northeastern Univ, Dept Phys, Boston, MA 02115 USA
[12] Ecole Polytech Fed Lausanne EPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland
[13] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA
[14] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain
[15] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain
[16] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England
[17] Univ Paris, Sorbonne Univ, Univ PSL, Lab Phys,Ecole Normale Super,ENS,CNRS, Paris, France
[18] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15312 USA
[19] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA
[20] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA
[21] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
[22] Univ Wisconsin, Phys Dept, 2320 Chamberlin Hall,1150 Univ Ave, Madison, WI 53706 USA
[23] Inst Astrofis Canarias, E-38205 Tenerife, Spain
[24] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
[25] Natl Ctr Super Comp 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] William Jewell Coll, Phys Dept, Liberty, MO 64068 USA
[28] Duke Univ, Dept Phys, Durham, NC 27708 USA
[29] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Oxford Rd, Manchester M13 9PL, Lancs, England
[30] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
[31] Carnegie Mellon Univ, NSF AI Planning Inst Phys Future, Pittsburgh, PA 15213 USA
[32] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA
[33] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
[34] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA
[35] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA
[36] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA
[37] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England
[38] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Barcelona, Spain
[39] Ludwig Maximilians Univ Munchen, Fac Phys, Univ Observ, D-81679 Munich, Germany
[40] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England
[41] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales
[42] Univ Geneva, Dept Astron, Ch Ecogia 16, CH-1290 Versoix, Switzerland
[43] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA
[44] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England
[45] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, P-1769016 Lisbon, Portugal
[46] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England
[47] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada
[48] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA
[49] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA
[50] Univ Estadual Campinas, Inst Fis Gleb Wataghin, BR-13083859 Campinas, SP, Brazil
基金
欧洲研究理事会; 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; MATTER POWER SPECTRUM; LARGE-SCALE STRUCTURE; REDSHIFT DISTRIBUTIONS; PARAMETER-ESTIMATION; BARYONIC PHYSICS; LENSING ANALYSIS; IMAGE-ANALYSIS; HALO MODEL; WEAK; IMPACT;
D O I
10.1093/mnras/stac1826
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present cosmological constraints from the analysis of angular power spectra of cosmic shear maps based on data from the first three years of observations by the Dark Energy Survey (DES Y3). Our measurements are based on the pseudo-Ct method and complement the analysis of the two-point correlation functions in real space, as the two estimators are known to compress and select Gaussian information in different ways, due to scale cuts. They may also be differently affected by systematic effects and theoretical uncertainties, making this analysis an important cross-check. Using the same fiducial Lambda cold dark matter model as in the DES Y3 real-space analysis, we find S-8 = sigma(s root)Omega m/0.3 = 0.7931(-0.025)(+0.038), which further improves to S-8 = 0.784 +/- 0.026 when including shear ratios. This result is within expected statistical fluctuations from the real-space constraint, and in agreement with DES Y3 analyses of non-Gaussian statistics, but favours a slightly higher value of S-8, which reduces the tension with the Planck 2018 constraints from 2.3 sigma in the real space analysis to 1.5 sigma here. We explore less conservative intrinsic alignments models than the one adopted in our fiducial analysis, finding no clear preference for a more complex model. We also include small scales, using an increased Fourier mode cut-off up to k(max) = 5 h Mpc(-1), which allows to constrain baryonic feedback while leaving cosmological constraints essentially unchanged. Finally, we present an approximate reconstruction of the linear matter power spectrum at present time, found to be about 20 per cent lower than predicted by Planck 2018, as reflected by the lower S-8 value.
引用
收藏
页码:1942 / 1972
页数:31
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