15806 10.1140/epjc/s10052-026-15806-w 564 125 Evidence for evolving dark energy from DESI DR2 BAO and Pantheon + , DES-Dovekie, and Union3 Regular Article - Theoretical Physics Theoretical Physics 1 21 2026 5 6 2026 3 3 2026 5 2 2026 5 22 2026 5 22 The Author(s) 2026 Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/ . Funded by SCOAP3. 10052 86 86 5 5 Himanshu Chaudhary himanshu.chaudhary@ubbcluj.ro himanshuch1729@gmail.com Salvatore Capozziello capozziello@na.infn.it Vipin Kumar Sharma vipin.339122@lpu.co.in Isidro Gómez-Vargas isidro.gomezvargas@unige.ch G. Mustafa gmustafa3828@gmail.com https://ror.org/02rmd1t30 grid.7399.4 0000 0004 1937 1397 Department of Physics Babeş-Bolyai University Kogălniceanu Street Cluj-Napoca 400084 Romania https://ror.org/014te7048 grid.442897.4 0000 0001 0743 1899 Research Center of Astrophysics and Cosmology, Khazar University 41 Mehseti Street Baku AZ1096 Azerbaijan https://ror.org/05290cv24 grid.4691.a 0000 0001 0790 385X Dipartimento di Fisica “E. Pancini” Università di Napoli “Federico II”, Complesso Universitario di Monte Sant’ Angelo Edificio G, Via Cinthia Napoli 80126 Italy https://ror.org/005ta0471 grid.6045.7 0000 0004 1757 5281 Istituto Nazionale di Fisica Nucleare (INFN) sez. di Napoli, Via Cinthia 9 Napoli 80126 Italy https://ror.org/04swxte59 grid.508348.2 Scuola Superiore Meridionale Via Mezzocannone 4 Napoli 80134 Italy https://ror.org/00et6q107 grid.449005.c 0000 0004 1756 737X International Center for High Energy Physics and Applications Lovely Professional University Phagwara Punjab 144411 India https://ror.org/01swzsf04 grid.8591.5 0000 0001 2175 2154 Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix Geneva 1290 Switzerland https://ror.org/01vevwk45 grid.453534.0 0000 0001 2219 2654 Department of Physics Zhejiang Normal University Jinhua 321004 People’s Republic of China https://ror.org/04b69g067 grid.412867.e 0000 0001 0043 6347 College of Graduate Studies Walailak University Thasala Nakhon Si Thammarat 80160 Thailand Abstract Evidences for evolving dark energy are shown using baryon acoustic oscillation measurements from the recent Dark Energy Spectroscopic Instrument Data Release 2, combined with different Type Ia supernova datasets (Pantheon + , DES-Dovekie, and Union3) and the CMB compressed likelihood. We examine several dark energy parameterizations, including the Logarithmic, Exponential, CPL, BA, JBP, Thawing, Mirage, and GEDE models. Analyzing the DESI DR2 measurements alone, we find that evidence for evolving dark energy is primarily driven by the LRG1-2 tracers, as their inclusion yields a preferred value of -1$$]]> w 0 > - 1 . However, as each tracer provides only limited observables, this preference can result in an underconstrained and potentially unstable inference. Further, we find that each dark energy model predicts values in the -1$$]]> w 0 > - 1 , w a < 0 quadrant, a region characterized by the Quintom-B type dark energy scenario. The logarithmic bayes factor shows that, among all models, the Mirage model shows the inconclusive-to-moderate evidence across all dataset combinations. Consistently, the statistical significance remains modest, with N σ ∼ 1.1 -2.3, and no model showing a robust preference for dynamical dark energy using late-time datasets alone. The evolution of w(z) shows a phantom crossing around z ∼ 0.5 in most dynamical dark energy models, and the evolution of f DE ( z ) converges to f DE ( 0 ) = 1 in all dark energy models.