First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey: Constraints on Cosmological Parameters

被引：198

作者：

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

Allam, S. ^{[2
]}

Andersen, P. ^{[3
,4
]}

Angus, C. ^{[5
]}

Asorey, J. ^{[6
]}

Avelino, A. ^{[7
]}

Avila, S. ^{[8
]}

Bassett, B. A. ^{[9
,10
]}

Bechtol, K. ^{[11
]}

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

Bertin, E. ^{[13
,14
]}

Brooks, D. ^{[15
]}

Brout, D. ^{[12
]}

Brown, P. ^{[16
,17
]}

Burke, D. L. ^{[18
,19
]}

Calcino, J. ^{[3
]}

Carnero Rosell, A. ^{[20
,21
]}

Carollo, D. ^{[22
]}

Kind, M. Carrasco ^{[23
,24
]}

Carretero, J. ^{[25
]}

Casas, R. ^{[26
,27
]}

Castander, F. J. ^{[26
,27
]}

Cawthon, R. ^{[28
]}

Challis, P. ^{[7
]}

Childress, M. ^{[5
]}

Clocchiatti, A. ^{[29
,30
]}

Cunha, C. E. ^{[18
]}

D'Andrea, C. B. ^{[12
]}

da Costa, L. N. ^{[21
,31
]}

Davis, C. ^{[18
]}

Davis, T. M. ^{[3
]}

De Vicente, J. ^{[20
]}

DePoy, D. L. ^{[16
,17
]}

Desai, S. ^{[32
]}

Diehl, H. T. ^{[2
]}

Doel, P. ^{[15
]}

Drlica-Wagner, A. ^{[2
,33
]}

Eifler, T. F. ^{[34
,35
]}

Evrard, A. E. ^{[36
,37
]}

Fernandez, E. ^{[25
]}

Filippenko, A., V ^{[38
,39
]}

Finley, D. A. ^{[2
]}

Flaugher, B. ^{[2
]}

Foley, R. J. ^{[40
]}

Fosalba, P. ^{[26
,27
]}

Frieman, J. ^{[2
,33
]}

Galbany, L. ^{[41
]}

Garcia-Bellido, J. ^{[42
]}

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

Giannantonio, T. ^{[43
,44
,45
]}

机构：

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

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

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

[4] Univ Copenhagen, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark

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

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

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

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

[9] African Inst Math Sci, 6 Melrose Rd, ZA-7945 Muizenberg, South Africa

[10] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa

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

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

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

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

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

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

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

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

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

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

[21] Lab Intinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[22] INAF, Astrophys Observ Turin, I-10025 Pino Torinese, Italy

[23] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA

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

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

[26] IEEC, E-08034 Barcelona, Spain

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

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

[29] Univ Catolica Chile, Millennium Inst Astrophys, Santiago, Chile

[30] Univ Catolica Chile, Dept Phys & Astron, Santiago, Chile

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

[32] ITT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

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

[34] Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA

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

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

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

[38] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA

[39] Univ Calif Berkeley, Miller Inst Basic Res Sci, Berkeley, CA 94720 USA

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

[41] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA

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

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

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

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

[46] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[47] CALTECH, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA

[48] Univ Lisbon, Inst Super Tecn, CENTRA, Av Rovisco Pais 1, P-1049001 Lisbon, Portugal

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2019年 / 872卷 / 02期

基金：

美国国家科学基金会; 英国科学技术设施理事会; 澳大利亚研究理事会; 欧洲研究理事会;

关键词：

dark energy; dark matter; LIGHT CURVES; LEGACY SURVEY; REDSHIFT; GALAXIES; SPECTROSCOPY; PHOTOMETRY; PEGASE; AGE;

D O I：

10.3847/2041-8213/ab04fa

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first cosmological parameter constraints using measurements of type Ia supernovae (SNe Ia) from the Dark Energy Survey Supernova Program (DES-SN). The analysis uses a subsample of 207 spectroscopically confirmed SNe. Ia from the first three years of DES-SN, combined with a low-redshift sample of 122 SNe from the literature. Our "DES-SN3YR" result from these 329 SNe. Ia is based on a series of companion analyses and improvements covering SN. Ia discovery, spectroscopic selection, photometry, calibration, distance bias corrections, and evaluation of systematic uncertainties. For a flat Lambda CDM model we find a matter density Omega(m) = 0.331 +/- 0.038. For a flat wCDM model, and combining our SN. Ia constraints with those from the cosmic microwave background (CMB), we find a dark energy equation of state w = -0.978 +/- 0.059, and Omega(m) = 0.321 +/- 0.018. For a flat w(0)w(a)CDM model, and combining probes from SN. Ia, CMB and baryon acoustic oscillations, we find w(0) = -0.885 +/- 0.114 and w(a) = -0.387 +/- 0.430. These results are in agreement with a cosmological constant and with previous constraints using SNe. Ia (Pantheon, JLA).

引用

页数：9

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