The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties

Journal Article · Fri Jan 05 00:00:00 EST 2024 · TBD

OSTI ID:2282565

Vincenzi, M.  ^[1]; Brout, D. ^[2]; Armstrong, P. ^[3]; Popovic, B. ^[4]; Taylor, G. ^[3]; Acevedo, M. ^[5]; Camilleri, R. ^[6]; Chen, R. ^[1]; Davis, T. M. ^[6]; Lee, J. ^[5]; Lidman, C. ^[7]; Hinton, S. R. ^[6]; Kelsey, L. ^[8]; Kessler, R. ^[9]; Möller, A. ^[10]; Qu, H. ^[5]; Sako, M. ^[5]; Sanchez, B. ^[11]; Scolnic, D. ^[1]; Smith, M. ^[12] ; Sullivan, M. ^[12]; Wiseman, P. ^[12]; Asorey, J. ^[13]; Bassett, B. A. ^[14]; Carollo, D. ^[15]; Carr, A. ^[6]; Foley, R. J. ^[16]; Frohmaier, C. ^[12]; Galbany, L. ^[17]; Glazebrook, K. ^[10]; Kovacs, E. ^[18]; Kuehn, K. ^[19]; Malik, U. ^[3]; Nichol, R. C. ^[20]; Rose, B. ^[21]; Tucker, B. E. ^[3]; Toy, M. ^[12]; Tucker, D. L. ^[22]; Yuan, F. ^[3]; Abbott, T. M.C. ^[23]; Aguena, M. ^[24]; Alves, O. ^[25]; Andrade-Oliveira, F. ^[25]; Annis, J. ^[22]; Bacon, D. ^[8]; Bechtol, K. ^[26]; Bernstein, G. M. ^[5]; Brooks, D. ^[27]; Burke, D. L. ^[28]; Carnero Rosell, A. ^[29]; Carretero, J. ^[30]; Castander, F. J. ^[17]; Conselice, C. ^[31]; da Costa, L. N. ^[24]; Pereira, M. E.S. ^[32]; Desai, S. ^[33]; Diehl, H. T. ^[22]; Doel, P. ^[27]; Ferrero, I. ^[34]; Flaugher, B. ^[22]; Friedel, D. ^[35]; Frieman, J. ^[36]; García-Bellido, J. ^[37]; Gatti, M. ^[5]; Giannini, G. ^[38]; Gruen, D. ^[39]; Gruendl, R. A. ^[40]; Hollowood, D. L. ^[16]; Honscheid, K. ^[41]; Huterer, D. ^[25]; James, D. J. ^[42]; Kuropatkin, N. ^[22]; Lahav, O. ^[27]; Lee, S. ^[43]; Lin, H. ^[22]; Marshall, J. L. ^[44]; Mena-Fernández, J. ^[45]; Menanteau, F. ^[40]; Miquel, R. ^[46]; Palmese, A. ^[47]; Pieres, A. ^[48]; Plazas Malagón, A. A. ^[28]; Porredon, A. ^[49]; Romer, A. K. ^[50]; Roodman, A. ^[28]; Sanchez, E. ^[51]; Sanchez Cid, D. ^[51]; Schubnell, M. ^[25]; Sevilla-Noarbe, I. ^[51]; Suchyta, E. ^[52]; Swanson, M. E.C. ^[35]; Tarle, G. ^[25]; To, C. ^[53]; Walker, A. R. ^[23]; Weaverdyck, N. ^[54]; Yamamoto, M. ^[1]

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1. Duke U.
2. Boston U.; Harvard-Smithsonian Ctr. Astrophys.
3. Australian Natl. U., Canberra
4. IP2I, Lyon
5. UPenn, Philadelphia
6. Queensland U.
7. ARC, Canberra; Australian Natl. U., Canberra (main); Australian Natl. U., Canberra
8. Portsmouth U., ICG
9. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP
10. Swinburne U. Tech., Hawthorn
11. Marseille, CPPM
12. Southampton U.
13. Madrid U.
14. African Inst. Math. Sci., Cape Town; South African Astron. Observ.
15. Trieste Observ.
16. UC, Santa Cruz
17. Barcelona, IEEC
18. Argonne (main)
19. Australian Astron. Observ.; Lowell Observ.
20. U. Surrey (main)
21. Baylor U.; Duke U.
22. Fermilab
23. Cerro-Tololo InterAmerican Obs.
24. LIneA, Rio de Janeiro
25. U. Michigan, Ann Arbor
26. Wisconsin U., Madison
27. University Coll. London
28. KIPAC, Menlo Park; SLAC
29. IAC, La Laguna; LIneA, Rio de Janeiro; Laguna U., Tenerife
30. Barcelona, IFAE
31. Jodrell Bank; Nottingham U.
32. Hamburg Observ.
33. Indian Inst. Tech., Hyderabad
34. Inst. Theor. Astrophys., Oslo
35. NCSA, Urbana
36. Fermilab; Chicago U., KICP
37. Madrid, IFT
38. Barcelona, IFAE; Chicago U., KICP
39. Munich U.
40. NCSA, Urbana; Illinois U., Urbana, Astron. Dept.
41. Ohio State U., CCAPP; Ohio State U.
42. Harvard-Smithsonian Ctr. Astrophys.
43. Caltech, JPL
44. Texas A-M
45. LPSC, Grenoble
46. ICREA, Barcelona; Barcelona, Autonoma U.; Barcelona, IFAE
47. Carnegie Mellon U.
48. LIneA, Rio de Janeiro; Rio de Janeiro Observ.
49. Ruhr U., Bochum
50. Sussex U.
51. Madrid, CIEMAT
52. ORNL, Oak Ridge (main)
53. Ohio State U., CCAPP
54. U. Michigan, Ann Arbor; LBNL, Berkeley

We present the full Hubble diagram of photometrically-classified Type Ia supernovae (SNe Ia) from the Dark Energy Survey supernova program (DES-SN). DES-SN discovered more than 20,000 SN candidates and obtained spectroscopic redshifts of 7,000 host galaxies. Based on the light-curve quality, we select 1635 photometrically-identified SNe Ia with spectroscopic redshift 0.10$< z <$1.13, which is the largest sample of supernovae from any single survey and increases the number of known $z>0.5$ supernovae by a factor of five. In a companion paper, we present cosmological results of the DES-SN sample combined with 194 spectroscopically-classified SNe Ia at low redshift as an anchor for cosmological fits. Here we present extensive modeling of this combined sample and validate the entire analysis pipeline used to derive distances. We show that the statistical and systematic uncertainties on cosmological parameters are $$\sigma_{\Omega_M,{\rm stat+sys}}^{\Lambda{\rm CDM}}=$$0.017 in a flat $$\Lambda$$CDM model, and $$(\sigma_{\Omega_M},\sigma_w)_{\rm stat+sys}^{w{\rm CDM}}=$$(0.082, 0.152) in a flat $$w$$CDM model. Combining the DES SN data with the highly complementary CMB measurements by Planck Collaboration (2020) reduces uncertainties on cosmological parameters by a factor of 4. In all cases, statistical uncertainties dominate over systematics. We show that uncertainties due to photometric classification make up less than 10% of the total systematic uncertainty budget. This result sets the stage for the next generation of SN cosmology surveys such as the Vera C. Rubin Observatory's Legacy Survey of Space and Time.

• Research Organization: Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)
• Sponsoring Organization: USDOE Office of Science (SC), High Energy Physics (HEP)
• Contributing Organization: DES
• DOE Contract Number: AC02-07CH11359
• OSTI ID: 2282565
• Report Number(s): FERMILAB-PUB-23-693-PPD; arXiv:2401.02945; oai:inspirehep.net:2743703
• Journal Information: TBD, Journal Name: TBD
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS