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T.M.D., A.C., R.C., and S.H. acknowledge the support of an Australian Research Council Australian Laureate Fellowship (FL180100168) funded by the Australian Government, and A.M. is supported by the ARC Discovery Early Career Researcher Award (DECRA) project No. DE230100055. M.S., H.Q., and J.L. are supported by DOE grant DE-FOA-0002424 and NSF grant AST-2108094. R.K. is supported by DOE grant DE-SC0009924. M.V. was partly supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51546.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. L.K. thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. L.G. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN), the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033, and the European Social Fund (ESF) "Investing in your future" under the 2019 Ramon y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOST-FLOWS project, from Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Maria de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant. R.J.F. and D.S. were supported in part by NASA grant 14-WPS14-0048. The UCSC team is supported in part by NASA grants NNG16PJ34G and NNG17PX03C issued through the Roman Science Investigation Teams Program; NSF grants AST-1518052 and AST-1815935; NASA through grant No. AR-14296 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; and fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation to R.J.F. We acknowledge the University of Chicago's Research Computing Center for their support of this work. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. Based in part on data acquired at the Anglo-Australian Telescope. We acknowledge the traditional custodians of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present. Parts of this research were supported by the Australian Research Council through project Nos. CE110001020, FL180100168, and DE230100055. Based in part on observations obtained at the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigacion y Desarrollo (Chile), Ministerio de Ciencia, Tecnologia e Innovacion (Argentina), Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This includes data from programs GN-2015B-Q-10, GN-2016B-LP-10, GN-2017B-LP-10, GS-2013B-Q-45, GS-2015B-Q-7, GS-2016B-LP-10, GS-2016B-Q-41, and GS-2017B-LP-10 (PI: Foley). Some of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 nonprofit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (PIs: Foley, Kirshner, and Nugent). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This Letter includes results based on data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile (PI: Foley), and the Southern African Large Telescope (SALT; PIs: M. Smith & E. Kasai). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/20072013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under contract No. DE-AC02-05CH11231 using NERSC award HEP-ERCAP0023923. This manuscript has been authored by Fermi Research Alliance, LLC, under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

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The Dark Energy Survey: Cosmology Results with ∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set

Publicated to:Astrophysical Journal Letters. 973 (1): L14- - 2024-09-20 973(1), DOI: 10.3847/2041-8213/ad6f9f

Authors: Abbott, 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; Rosell, A Carnero; 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; Ferte, A; Flaugher, B; Foley, R J; Fosalba, P; Friedel, D; Frieman, J; Frohmaier, C; Galbany, L; Garcia-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-Fernandez, J; Menanteau, F; Miquel, R; Mohr, J J; Mould, J; Muir, J; Moller, 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; Malagon, A A Plazas; Popovic, B; Porredon, A; Prat, J; Qu, H; Raveri, M; Rodriguez-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; Sanchez, 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

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Abstract

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 Omega(M) = 0.352 +/- 0.017 in flat Lambda CDM. SN data alone now require acceleration (q(0) < 0 in Lambda CDM) with over 5 sigma confidence. We find (Omega 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 (W) = (Omega(M), w(0), w(a)) = (0.495(-0043)(+0.033), -0.36(-0.30)(+0.36), -8.8(-4.5)(+3.7)), consistent with a constant equation of state to within similar to 2 sigma. Including Planck cosmic microwave background, Sloan Digital Sky Survey baryon acoustic oscillation, and DES 3 x 2pt data gives (Omega(M), w) = (0.321 +/- 0.007, -0.941 +/- 0.026). In all cases, dark energy is consistent with a cosmological constant to within similar to 2 sigma. Systematic errors on cosmological parameters are subdominant compared to statistical errors; these results thus pave the way for future photometrically classified SN analyses.

Keywords