First Cosmology Results Using SNe Ia from the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

被引：83

作者：

Brout, D. ^{[1
]}

Scolnic, D. ^{[2
]}

Kessler, R. ^{[2
,3
]}

D'Andrea, C. B. ^{[1
]}

Davis, T. M. ^{[4
]}

Gupta, R. R. ^{[5
]}

Hinton, S. R. ^{[4
]}

Kim, A. G. ^{[5
]}

Lasker, J. ^{[2
,3
]}

Lidman, C. ^{[6
]}

Macaulay, E. ^{[7
]}

Moller, A. ^{[6
,8
]}

Nichol, R. C. ^{[7
]}

Sako, M. ^{[1
]}

Smith, M. ^{[9
]}

Sullivan, M. ^{[9
]}

Zhang, B. ^{[6
,8
]}

Andersen, P. ^{[4
,10
]}

Asorey, J. ^{[11
]}

Avelino, A. ^{[12
]}

Bassett, B. A. ^{[13
,14
]}

Brown, P. ^{[15
,16
]}

Calcino, J. ^{[4
]}

Carollo, D. ^{[17
]}

Challis, P. ^{[12
]}

Childress, M. ^{[9
]}

Clocchiatti, A. ^{[18
,19
]}

Filippenko, A., V ^{[20
,21
]}

Foley, R. J. ^{[22
]}

Galbany, L. ^{[23
]}

Glazebrook, K. ^{[24
]}

Hoormann, J. K. ^{[4
]}

Kasai, E. ^{[14
,25
]}

Kirshner, R. P. ^{[12
,26
]}

Kuehn, K. ^{[27
]}

Kuhlmann, S. ^{[28
]}

Lewis, G. F. ^{[29
]}

Mandel, K. S. ^{[30
,31
]}

March, M. ^{[1
]}

Miranda, V ^{[32
]}

Morganson, E. ^{[33
]}

Muthukrishna, D. ^{[6
,8
,34
]}

Nugent, P. ^{[5
]}

Palmese, A. ^{[35
]}

Pan, Y-C ^{[36
,37
]}

Sharp, R. ^{[6
]}

Sommer, N. E. ^{[6
,8
]}

Swann, E. ^{[7
]}

Thomas, R. C. ^{[5
]}

Tucker, B. E. ^{[6
,8
]}

机构：

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

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

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

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

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

[6] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

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

[8] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia

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

[10] Univ Copenhagen, Dark Cosmol Ctr, Juliane Maries Vej 30, Copenhagen, Denmark

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

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

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

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

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

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

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

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

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

[20] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[21] Univ Calif Berkeley, Miller Senior Fellow Miller Inst Basic Res Sci, Berkeley, CA 94720 USA

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

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

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

[25] Univ Namibia, Dept Phys, 340 Mandume Ndemufayo Ave,Pionierspk, Windhoek, Namibia

[26] Gordon & Betty Moore Fdn, 1661 Page Mill Rd, Palo Alto, CA 94304 USA

[27] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

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

[29] Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia

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

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

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

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

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

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

[36] Natl Astron Observ Japan, Div Theoret Astron, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[37] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan

[38] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[39] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile

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

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

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

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

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

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

[46] CIEMAT, Madrid, Spain

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

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

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

[50] IEEC, E-08034 Barcelona, Spain

来源：

ASTROPHYSICAL JOURNAL | 2019年 / 874卷 / 02期

基金：

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

关键词：

cosmological parameters; dark energy; supernovae: general; SUPERNOVA LEGACY SURVEY; LIGHT CURVES; HOST GALAXIES; REDSHIFT; CONSTRAINTS; PARAMETERS; AGE; SPECTROSCOPY; PHOTOMETRY; SELECTION;

D O I：

10.3847/1538-4357/ab08a0

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017 < z < 0.849. We combine the DES-SN sample with an external sample of 122 low-redshift (z < 0.1) SNe. Ia, resulting in a "DES-SN3YR" sample of 329 SNe Ia. Our cosmological analyses are blinded: after combining our DES-SN3YR distances with constraints from the Cosmic Microwave Background, our uncertainties in the measurement of the dark energy equation-of-state parameter, w, are 0.042. (stat) and 0.059 (stat+syst) at 68% confidence. We provide a detailed systematic uncertainty budget, which has nearly equal contributions from photometric calibration, astrophysical bias corrections, and instrumental bias corrections. We also include several new sources of systematic uncertainty. While our sample is less than one-third the size of the Pantheon sample, our constraints on w are only larger by 1.4x, showing the impact of the DES-SN. Ia light-curve quality. We find that the traditional stretch and color standardization parameters of the DES-SNe. Ia are in agreement with earlier SN. Ia samples such as Pan-STARRS1 and the Supernova Legacy Survey. However, we find smaller intrinsic scatter about the Hubble diagram (0.077 mag). Interestingly, we find no evidence for a Hubble residual step (0.007 +/- 0.018 mag) as a function of host-galaxy mass for the DES subset, in 2.4 sigma tension with previous measurements. We also present novel validation methods of our sample using simulated SNe. Ia inserted in DECam images and using large catalog-level simulations to test for biases in our analysis pipelines.

引用

页数：29

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