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Dynamical dark energy in light of the DESI DR2 baryonic acoustic oscillations measurements

Gan GuBeijing ObservXiaoma WangBeijing, Inst. High Energy PhysYuting WangInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing, People's Republic of ChinaGong‐Bo ZhaoBeijing, Inst. High Energy PhysLevon PogosianDepartment of Physics, Simon Fraser University, Burnaby, British Columbia CanadaK. KoyamaKavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, JapanJ. A. PeacockInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, UKZheng CaiDepartment of Astronomy, Tsinghua University, Beijing, People's Republic of ChinaJorge L. Cervantes–CotaMexico, ININMustapha IshakDepartment of Physics, The University of Texas at Dallas, Richardson, TX USAArman ShafielooTaejon, Elect. Telecomm. Res. InstRuiyang ZhaoUniversity of Chinese Academy of Sciences, Beijing, People's Republic of ChinaS. AhlenPhysics Department, Boston University, Boston, MA, USADavide BianchiDipartimento di Fisica 'Aldo Pontremoli', Università degli Studi di Milano, Milan, ItalyDavid BrooksDepartment of Physics & Astronomy, University College London, London, UKT. ClaybaughLawrence Berkeley National Laboratory, Berkeley, CA USAShaun ColeDurham U., ICCAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Circuito de la Investigación Científica, Ciudad Universitaria, Mexico City, MexicoArnaud de MattiaIRFU, SaclayP. DoelDepartment of Physics & Astronomy, University College London, London, UKS. FerraroUC, Berkeley, Math. DeptJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Bogotá, ColombiaE. GaztañagaInstitute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, UKSatya Gontcho A GontchoLawrence Berkeley National Laboratory, Berkeley, CA USAG. GutiérrezFermi National Accelerator Laboratory, Batavia, IL USAChang Hoon HahnArizona U., Astron. Dept. - Steward ObservCullan HowlettSchool of Mathematics and Physics, University of Queensland, Brisbane, Queensland AustraliaR. KehoeDepartment of Physics, Southern Methodist University, Dallas, TX USAD. KirkbyDepartment of Physics and Astronomy, University of California, Irvine, CA USAJean‐Paul KneibInstitute of Physics, Laboratory of Astrophysics, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, Versoix, SwitzerlandAnthony KreminLawrence Berkeley National Laboratory, Berkeley, CA USAO. LahavDepartment of Physics & Astronomy, University College London, London, UKMartin LandriauLawrence Berkeley National Laboratory, Berkeley, CA USAL. Le GuillouSorbonne UniversitéAlexie LeauthaudDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA USAM. E. LeviLawrence Berkeley National Laboratory, Berkeley, CA USAMarc ManeraDepartament de Física, Serra Húnter, Universitat Autònoma de Barcelona, Barcelona, SpainAaron MeisnerNatl. Solar Observ., TucsonR. MiquelInstitut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Barcelona, SpainJohn MoustakasDepartment of Physics and Astronomy, Siena College, Loudonville, NY USAA. Muñoz-GutiérrezUniversidad Nacional Autónoma de MéxicoS. NadathurInstitute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, UKJeffrey A. NewmanDepartment of Physics & Astronomy and Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, Pittsburgh, PA USAN. Palanque‐DelabrouilleLawrence Berkeley National Laboratory, Berkeley, CA USAWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, Waterloo, Ontario CanadaFrancisco PradaInstituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, Granada, SpainIgnasi Pérez-RàfolsDepartament de Física, EEBE, Universitat Politècnica de Catalunya, Barcelona, SpainGraziano RossiDepartment of Physics and Astronomy, Sejong University, Seoul, Republic of KoreaLado SamushiaFaculty of Natural Sciences and Medicine, Ilia State University, Tbilisi, GeorgiaE. SánchezCentro de Investigaciones Energéticas, Medioambientales y TecnológicasDavid J. SchlegelLawrence Berkeley National Laboratory, Berkeley, CA USAHee‐Jong SeoDepartment of Physics & Astronomy, Ohio University, Athens, OH USADavid SprayberryNSF NOIRLab, Tucson, AZ, USAG. TarléMichigan UMichael WaltherLudwig-Maximilians-Universität MünchenBenjamin A. WeaverNatl. Solar Observ., TucsonPauline ZarroukLaboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), Sorbonne Université, CNRS/IN2P3, Paris, FranceCheng ZhaoDepartment of Astronomy, Tsinghua University, Beijing, People's Republic of ChinaRongpu ZhouLawrence Berkeley National Laboratory, Berkeley, CA USAH. ZouNational Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China

Nature Astronomyjournal2025en

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Litsenziya: cc-by-nc-nd

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Annotatsiya

Understanding whether cosmic acceleration arises from a cosmological constant or a dynamical component is a central goal of cosmology, and the Dark Energy Spectroscopic Instrument (DESI) enables stringent tests with high-precision distance measurements. Here we analyse measurements of baryon acoustic oscillations in DESI Data Release 1 and Data Release 2 and consider type Ia supernovae and a distance prior for the cosmic microwave background. With the larger statistical power and wider redshift coverage of Data Release 2, the preference for dynamical dark energy does not diminish relative to Data Release 1. Using both a shape-function reconstruction and non-parametric approaches with a Horndeski-motivated correlation prior, we find that the equation of state for dark energy w(z) varies with redshift. Baryon acoustic oscillation data alone yield modest constraints, but in combination with independent supernova compilations and the prior for the cosmic microwave background, they strengthen the evidence for dynamics. A Bayesian comparison of models shows moderate support for departures from Λ cold dark matter (ΛCDM) when several degrees of freedom in w(z) are allowed, corresponding to ~3σ tension with ΛCDM (and higher for some datasets). Despite methodological differences, our results are consistent with companion DESI papers, underscoring the complementarity of the approaches. Possible systematics remain under study; forthcoming DESI, Euclid and next-generation cosmic microwave background data will provide decisive tests. A complementary analysis of DESI DR2 distance measurements along with supernova and CMB data shows consistent, moderate evidence that dark energy changes over time rather than behaving as a simple cosmological constant.

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Cosmology and Gravitation Theories Galaxies: Formation, Evolution, Phenomena Dark Matter and Cosmic Phenomena

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DOI: 10.1038/s41550-025-02669-6

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