First cosmology results using Type Ia supernova from the Dark Energy Survey: simulations to correct supernova distance biases

被引：52

作者：

Kessler, R. ^{[1
,2
]}

Brout, D. ^{[3
]}

D'Andrea, C. B. ^{[3
]}

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

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

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

Lasker, J. ^{[1
,2
]}

Lidman, C. ^{[6
]}

Macaulay, E. ^{[7
]}

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

Sako, M. ^{[3
]}

Scolnic, D. ^{[2
]}

Smith, M. ^{[9
]}

Sullivan, M. ^{[9
]}

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

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

Asorey, J. ^{[11
]}

Avelino, A. ^{[12
]}

Calcino, J. ^{[4
]}

Carollo, D. ^{[13
]}

Challis, P. ^{[12
]}

Childress, M. ^{[9
]}

Clocchiatti, A. ^{[14
,15
]}

Crawford, S. ^{[16
,17
]}

Filippenko, A. V. ^{[18
,19
]}

Foley, R. J. ^{[20
]}

Glazebrook, K. ^{[21
]}

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

Kasai, E. ^{[16
,22
]}

Kirshner, R. P. ^{[12
,23
]}

Lewis, G. F. ^{[24
]}

Mandel, K. S. ^{[25
,26
]}

March, M. ^{[3
]}

Morganson, E. ^{[27
]}

Muthukrishna, D. ^{[6
,8
,28
]}

Nugent, P. ^{[5
]}

Pan, Y. -C. ^{[29
,30
]}

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

Swann, E. ^{[7
]}

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

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

Uddin, S. A. ^{[31
]}

Abbott, T. M. C. ^{[32
]}

Allam, S. ^{[33
]}

Annis, J. ^{[33
]}

Avila, S. ^{[7
]}

Banerji, M. ^{[28
,34
]}

Bechtol, K. ^{[35
]}

Bertin, E. ^{[36
,37
]}

Brooks, D. ^{[38
]}

机构：

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

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

[3] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 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, DK-2100 Copenhagen O, Denmark

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

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

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

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

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

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

[17] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

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

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

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

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

[22] Univ Namibia, Dept Phys, 340 Mandume Ndemufayo Ave, Pionierspark, Windhoek, Namibia

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

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

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

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

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

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

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

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

[31] Observ Carnegie Inst Sci, 813 Santa Barbara Str, Pasadena, CA 91101 USA

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

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

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

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

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

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

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

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

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

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

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

[43] Univ Illinois, Dept Astron, 1002 W Green Str, Urbana, IL 61801 USA

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

[45] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

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

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

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

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 485卷 / 01期

基金：

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

关键词：

techniques; cosmology; supernovae; (cosmology:) dark energy; LIGHT CURVES; CONSTRAINTS; POPULATIONS; COLOR;

D O I：

10.1093/mnras/stz463

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We describe catalogue-level simulations of Type Ia supernova (SN Ia) light curves in the Dark Energy Survey Supernova Program (DES-SN) and in low-redshift samples from the Center for Astrophysics (CfA) and the Carnegie Supernova Project (CSP). These simulations are used to model biases from selection effects and light-curve analysis and to determine bias corrections for SN Ia distance moduli that are used to measure cosmological parameters. To generate realistic light curves, the simulation uses a detailed SN Ia model, incorporates information from observations (point spread function, sky noise, zero-point), and uses summary information (e.g. detection efficiency versus signal-to-noise ratio) based on 10 000 fake SN light curves whose fluxes were overlaid on images and processed with our analysis pipelines. The quality of the simulation is illustrated by predicting distributions observed in the data. Averaging within redshift bins, we find distance modulus biases up to 0.05 mag over the redshift ranges of the low-z and DES-SN samples. For individual events, particularly those with extreme red or blue colour, distance biases can reach 0.4 mag. Therefore, accurately determining bias corrections is critical for precision measurements of cosmological parameters. Files used to make these corrections are available at https://des.ncsa.illinois.edu/releases/sn.

引用

页码：1171 / 1187

页数：17

共 50 条

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