{"total":10,"items":[{"citing_arxiv_id":"2605.13546","ref_index":30,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"No evidence for phantom crossing: local goodness-of-fit improvements do not persist under global Bayesian model comparison","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T13:54:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Global Bayesian evidence shows no statistically significant support for dynamical dark energy or phantom crossing despite limited local fit improvements in the w0wa parametrization.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"06618 [astro-ph.CO] . [27] B. R. Dinda, R. Maartens, S. Saito, and C. Clarkson, JCAP08, 018 (2025), arXiv:2504.09681 [astro-ph.CO] . [28] ¨O. Akarsu, M. Caruana, K. F. Dialektopoulos, L. A. Escamilla, E. O. Kahya, and J. Levi Said, (2026), arXiv:2604.12987 [astro-ph.CO] . [29] G. Montefalcone and R. Stiskalek, (2026), arXiv:2603.25735 [astro-ph.CO] . [30] S. Nesseris, Y. Akrami, and G. D. Starkman, (2025), arXiv:2503.22529 [astro-ph.CO] . [31] T. Xu, S. Kumar, Y. Chen, A. J. S. Capistrano, and ¨O. Akarsu, (2026), arXiv:2602.11936 [astro-ph.CO] . [32] D. D. Y. Ong, D. Yallup, and W. Handley, (2026), arXiv:2603.05472 [astro-ph.CO] . [33] L. T. Hergt, S. Henrot-Versill' e, M. Tristram, and D. Scott, (2026), arXiv:2602."},{"citing_arxiv_id":"2604.03167","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Mapping the redshift drift at various redshifts through cosmography","primary_cat":"astro-ph.CO","submitted_at":"2026-04-03T16:44:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Cosmographic Taylor and Padé models fitted to Pantheon+SH0ES+GRB+DESI BAO data yield redshift drift predictions compatible with ΛCDM and ω0ω1CDM at 1-2σ, with mock drift data tightening q0 and j0 bounds.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Sapone and S. Nesseris, Phys. Rev. D112, 063523 (2025), 2412.01740. [26] S. Nesseris, Y. Akrami, and G. D. Starkman, arXiv e- prints arXiv:2503.22529 (2025), 2503.22529. [27] W. Giar` e, Phys. Rev. D112, 023508 (2025), 2409.17074. [28] E. Silva, M. A. Sabogal, M. Scherer, R. C. Nunes, E. Di Valentino, and S. Kumar, Phys. Rev. D111, 123511 (2025), 2503.23225. [29] E. 'O Colg' ain and M. M. Sheikh-Jabbari, MNRAS542, L24 (2025), 2412.12905. [30] G. Rodrigues, R. de Souza, and J. Alcaniz, Phys. Rev. D112, 103519 (2025), 2506.22373. [31] E. 'O Colg' ain, M. G. Dainotti, S. Capozziello, S. Pouro- jaghi, M. M. Sheikh-Jabbari, and D. Stojkovic, Jour- nal of High Energy Astrophysics49, 100428 (2026), 2404.08633. [32] I."},{"citing_arxiv_id":"2603.26560","ref_index":153,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Exploring the interplay of late-time dynamical dark energy and new physics before recombination","primary_cat":"astro-ph.CO","submitted_at":"2026-03-27T16:25:41+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"To ensure a consistent treatment, in Secs. 4.1 and 4.2 we also marginalize over M. In section 4.3, where we do not assume standard pre-recombination physics, we employ CMB/BBN information in a more compressed form, in terms of the following Gaussian priors on the CMB acoustic scale and the baryon energy density: 100θ ∗ = 1.04223±0.00055 [132] andω b = 0.02196±0.00063 [153]. The former is extracted from an analysis ofPlanckbaseline TT,TE,EE likelihoods assuming a ΛCDM+N eff cosmology and one massive neutrino with mν = 0.06 eV, whereas the latter has been obtained from a BBN analysis also allowing for a - 12 - CMB+DESI DR2+PantheonPlus CMB+DESI DR2+DES Dovekie χ2 min(ΛCDM) 1422.69 1652.03 χ2 min(CPL) 1414.43 1640.41"},{"citing_arxiv_id":"2603.11377","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A class of decelerating inhomogeneous cosmological models giving rise to accelerating FLRW universes at large scales","primary_cat":"gr-qc","submitted_at":"2026-03-11T23:38:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Inhomogeneous decelerating models generate effective accelerating FLRW universes at large scales through backreaction that mimics a running dark-energy term.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.07398","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Study of the cosmological tensions and DESI-DR2 in the framework of the Little Rip model","primary_cat":"astro-ph.CO","submitted_at":"2026-03-08T01:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"The Little Rip model reduces the Hubble tension below 3σ with CMB plus BAO data but only improves the statistical fit to CMB data alone per Bayes factors, and shifts toward quintessence behavior when DESI-DR2 is included.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.20757","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses","primary_cat":"astro-ph.CO","submitted_at":"2025-11-25T19:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reanalysis of DESI full-shape clustering data tightens constraints on neutrino mass, spatial curvature, and dark energy equation-of-state parameters relative to BAO-only results.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Fifth, the CPL parametrization has also been extensively interrogated: though it is capable of describing a variety of dark energy models [24], it is important to note that the parameters are purely effective values, and do not fully encapsulate the dark energy expansion history [ 25]. Sixth, the role of higher-order terms in the w(a) expansion is debated [ 26], though [3] found that adding such terms does not significantly improve the fit to the combined data and would thus be disfavored from a model comparison perspective. Finally, the evidence for dynamical dark energy weakens significantly in some analysis variants, e.g. [14, 27]. From a theoretical perspective, the best-fit dark energy model is puzzling."},{"citing_arxiv_id":"2511.18657","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"How Complex is Dark Energy? A Bayesian Analysis of CPL Extensions with Recent DESI BAO Measurements","primary_cat":"astro-ph.CO","submitted_at":"2025-11-23T23:56:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian evidence from DESI BAO plus CMB and SN data favors the standard CPL evolving dark energy model over both simpler constant-w and more complex higher-order extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.03779","ref_index":90,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Beyond CPL: Evidence for dynamical dark energy in three-parameter models","primary_cat":"astro-ph.CO","submitted_at":"2025-10-04T11:08:41+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Two three-parameter extensions of the mAH dark energy parametrization are compared to LambdaCDM, wCDM, CPL and others using CMB, DESI BAO, H(z), RSD and three SNIa samples, yielding Delta chi-squared improvements of 6-38 and 2-5 sigma tensions with LambdaCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.13302","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Comparing Minimal and Non-Minimal Quintessence Models to 2025 DESI Data","primary_cat":"astro-ph.CO","submitted_at":"2025-09-16T17:55:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Quintessence models with standard potentials give only modest improvements over Lambda to DESI data on evolving dark energy, while non-minimal couplings allow temporary phantom behavior but face tight gravity constraints except for carefully selected narrow ranges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.24732","ref_index":121,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The Quintom theory of dark energy after DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2025-05-30T15:54:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"This review traces the history of dynamical dark energy, presents the no-go theorem against single-field crossing of w = -1, and surveys viable Quintom constructions including multi-field models and modified gravity in light of DESI DR2 hints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The CPL parametrization fixed the higher-order terms of Taylor expansion. This kind of parameterization is just an effective low-redshift parameterization, does not introduce any extra information from the higher order terms. To examine the possible higher order effects and avoid such a bias, one could extend the parametrization to include higher-order terms or adopt data-driven approaches [121]. Thus, non-parametric approaches are very important and necessary. One widely used non-parametric method is the Gaussian process regression [138-141]. The Gaussian-process regression allows one to reconstruct the function and its derivatives in a model-independent manner from observational data points, utilizing a chosen kernel covariance function."}],"limit":50,"offset":0}