The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set
Authors: Abbott DES Collaboration: T. M. C. , Acevedo M. , Aguena M. , Alarcon A. , Allam S. , Alves O. , Amon A. , Andrade-Oliveira F. , Annis J. , Armstrong P. , Asorey J. , Avila S. , Bacon D. , Bassett B. A. , Bechtol K. , Bernardinelli P. H. , Bernstein G. M. , Bertin E. , Blazek J. , Bocquet S. , Brooks D. , Brout D. , Buckley-Geer E. , Burke D. L. , Camacho H. , Camilleri R. , Campos A. , Carnero Rosell A. , Carollo D. , Carr A. , Carretero J. , Castander F. J. , Cawthon R. , Chang C. , Chen R. , Choi A. , Conselice C. , Costanzi M. , da Costa L. N. , Crocce M. , Davis T. M. , DePoy D. L. , Desai S. , Diehl H. T. , Dixon M. , Dodelson S. , Doel P. , Doux C. , Drlica-Wagner A. , Elvin-Poole J. , Everett S. , Ferrero I. , Ferté A. , Flaugher B. , Foley R. J. , Fosalba P. , Friedel D. , Frieman J. , Frohmaier C. , Galbany L. , García-Bellido J. , Gatti M. , Gaztanaga E. , Giannini G. , Glazebrook K. , Graur O. , Gruen D. , Gruendl R. A. , Gutierrez G. , Hartley W. G. , Herner K. , Hinton S. R. , Hollowood D. L. , Honscheid K. , Huterer D. , Jain B. , James D. J. , Jeffrey N. , Kasai E. , Kelsey L. , Kent S. , Kessler R. , Kim A. G. , Kirshner R. P. , Kovacs E. , Kuehn K. , Lahav O. , Lee J. , Lee S. , Lewis G. F. , Li T. S. , Lidman C. , Lin H. , Malik U. , Marshall J. L. , Martini P. , Mena-Fernández J. , Menanteau F. , Miquel R. , Mohr J. J. , Mould J. , Muir J. , Möller A. , Neilsen E. , Nichol R. C. , Nugent P. , Ogando R. L. C. , Palmese A. , Pan Y.-C. , Paterno M. , Percival W. J. , Pereira M. E. S. , Pieres A. , Plazas Malagón A. A. , Popovic B. , Porredon A. , Prat J. , Qu H. , Raveri M. , Rodríguez-Monroy M. , Romer A. K. , Roodman A. , Rose B. , Sako M. , Sanchez E. , Sanchez Cid D. , Schubnell M. , Scolnic D. , Sevilla-Noarbe I. , Shah P. , Smith J. Allyn. , Smith M. , Soares-Santos M. , Suchyta E. , Sullivan M. , Suntzeff N. , Swanson M. E. C. , Sánchez B. O. , Tarle G. , Taylor G. , Thomas D. , To C. , Toy M. , Troxel M. A. , Tucker B. E. , Tucker D. L. , Uddin S. A. , Vincenzi M. , Walker A. R. , Weaverdyck N. , Wechsler R. H. , Weller J. , Wester W. , Wiseman P. , Yamamoto M. , Yuan F. , Zhang B. , Zhang Y. 
Published: October 2024

We present cosmological constraints from the sample of Type Ia supernovae (SNe Ia) discovered and measured during the full 5 yr of the Dark Energy Survey (DES) SN program. In contrast to most previous cosmological samples, in which SNe are classified based on their spectra, we classify the DES SNe using a machine learning algorithm applied to their light curves in four photometric bands. Spectroscopic redshifts are acquired from a dedicated follow-up survey of the host galaxies. After accounting for the likelihood of each SN being an SN Ia, we find 1635 DES SNe in the redshift range 0.10 < z < 1.13 that pass quality selection criteria sufficient to constrain cosmological parameters. This quintuples the number of high-quality z > 0.5 SNe compared to the previous leading compilation of Pantheon+ and results in the tightest cosmological constraints achieved by any SN data set to date. To derive cosmological constraints, we combine the DES SN data with a high-quality external low-redshift sample consisting of 194 SNe Ia spanning 0.025 < z < 0.10. Using SN data alone and including systematic uncertainties, we find ΩM = 0.352 ± 0.017 in flat ΛCDM. SN data alone now require acceleration (q
0 < 0 in ΛCDM) with over 5σ confidence. We find

(

Ω

M

,
w
)
=
(

0.264

−
0.096

+
0.074

,
−

0.80

−
0.16

+
0.14

)

in flat wCDM. For flat w
0
w

a
CDM, we find

(

Ω

M

,

w

0

,

w

a

)
=
(

0.495

−
0.043

+
0.033

,
−

0.36

−
0.30

+
0.36

,
−

8.8

−
4.5

+
3.7

)

, consistent with a constant equation of state to within ∼2σ. Including Planck cosmic microwave background, Sloan Digital Sky Survey baryon acoustic oscillation, and DES 3 × 2pt data gives (ΩM, w) = (0.321 ± 0.007, −0.941 ± 0.026). In all cases, dark energy is consistent with a cosmological constant to within ∼2σ. Systematic errors on cosmological parameters are subdominant compared to statistical errors; these results thus pave the way for future photometrically classified SN analyses.