Rates and delay times of Type Ia supernovae in the Dark Energy Survey

被引：18

作者：

Wiseman, P. ^{[1
]}

Sullivan, M. ^{[1
]}

Smith, M. ^{[1
,2
]}

Frohmaier, C. ^{[1
,3
]}

Vincenzi, M. ^{[3
]}

Graur, O. ^{[3
]}

Popovic, B. ^{[4
]}

Armstrong, P. ^{[5
]}

Brout, D. ^{[6
]}

Davis, T. M. ^{[7
]}

Galbany, L. ^{[8
]}

Hinton, S. R. ^{[7
]}

Kelsey, L. ^{[1
]}

Kessler, R. ^{[9
,10
]}

Lidman, C. ^{[5
,11
]}

Moller, A. ^{[12
]}

Nichol, R. C. ^{[3
]}

Rose, B. ^{[4
]}

Scolnic, D. ^{[4
]}

Toy, M. ^{[1
]}

Zontou, Z. ^{[1
]}

Asorey, J. ^{[13
]}

Carollo, D. ^{[14
]}

Glazebrook, K. ^{[15
]}

Lewis, G. F. ^{[16
]}

Tucker, B. E.

Abbott, T. M. C. ^{[17
]}

Aguena, M. ^{[18
]}

Allam, S. ^{[19
]}

Andrade-Oliveira, F. ^{[18
,20
]}

Annis, J. ^{[19
]}

Bacon, D. ^{[3
]}

Bertin, E. ^{[21
,22
]}

Brooks, D. ^{[23
]}

Buckley-Geer, E. ^{[9
,19
]}

Burke, D. L. ^{[24
,25
]}

Rosell, A. Carnero ^{[18
,26
,27
]}

Kind, M. Carrasco ^{[28
,29
]}

Carretero, J. ^{[30
]}

Costanzi, M. ^{[31
,32
,33
]}

da Costa, L. N. ^{[18
,34
]}

Pereira, M. E. S. ^{[35
]}

Desai, S. ^{[36
]}

Diehl, H. T. ^{[19
]}

Doel, P. ^{[23
]}

Everett, S. ^{[37
]}

Ferrero, I ^{[38
]}

Flaugher, B. ^{[19
]}

Fosalba, P. ^{[39
,40
]}

Frieman, J. ^{[10
,19
]}

机构：

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

[2] Univ Lyon, Univ Claude Bernard Lyon 1, CNRS, IP2I Lyon IN2P3,IMR 5822, F-69622 Villeurbanne, France

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

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

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

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

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

[8] CSIC, Inst Space Sci ICE, Campus UAB S-N, E-08193 Barcelona, Spain

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

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

[11] Australian Natl Univ, Coll Sci, Ctr Gravitat Astrophys, Canberra, ACT 2601, Australia

[12] Univ Clermont Auvergne, LPC, CNRS IN2P3, F-63000 Clermont Ferrand, France

[13] Ctr Invest Energet Medioambientales & Tecnol CIEM, Av Complutense 40, Madrid 28040, Spain

[14] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy

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

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

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

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

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

[20] Univ Estadual Paulista, Inst Fis Teor, Rua Pamplona 145, BR-01405900 Sao Paulo, SP, Brazil

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

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

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

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

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

[26] Inst Astrofis Canarias, E-38205 Tenerife, Spain

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

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

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

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

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

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

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

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

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

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

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

[38] Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway

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

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

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

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

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

[44] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

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

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

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

[48] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 506卷 / 03期

基金：

美国国家科学基金会; 欧洲研究理事会; 英国科学技术设施理事会;

关键词：

supernovae: general; white dwarfs; galaxies: evolution; CO WHITE-DWARFS; STAR-FORMATION; GALAXY CLUSTERS; HOST GALAXIES; PROGENITOR CONSTRAINTS; MASS; EVOLUTION; STELLAR; SEARCH; SIMULATIONS;

D O I：

10.1093/mnras/stab1943

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 <= log (M+/M-circle dot) <= 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 +/- 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index beta = -1.13 +/- 0.05 and normalization A = 2.11 +/- 0.05 x 10(-13) SNe M-circle dot(-1) yr(-1), which corresponds to an overall SN la production efficiency N-Ia/M-* = 0.9(-0.7)(+4.0) x 10(-3) SNe M-circle dot(-1). Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors.

引用

页码：3330 / 3348

页数：19

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