{"total":12,"items":[{"citing_arxiv_id":"2605.21456","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Negative neutrino mass or negative dark energy?","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:46:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A sign-switching dark energy model (Λ_s CDM) recovers positive effective neutrino masses (0.055 ± 0.050 eV) consistent with oscillation data, unlike ΛCDM which prefers negative values (-0.075 eV), for DESI DR2 + CMB + supernova fits with z_† > 2.4.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Crosses the Line: Quantifying and Testing the Evidence for Phantom Crossing (2025), 2506.19053. [122] K. Lodhaet al.(DESI), DESI 2024: Constraints on physics-focused aspects of dark energy using DESI DR1 BAO data, Phys. Rev. D111, 023532 (2025), 2405.13588. 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Vasar, and H."},{"citing_arxiv_id":"2604.03756","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Is the $w_0w_a$CDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?","primary_cat":"astro-ph.CO","submitted_at":"2026-04-04T15:05:07+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Planck PR4 CMB data mildly favors dynamical dark energy, but this preference weakens when accounting for possible excess smoothing, indicating the signal may partly arise from data processing issues.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"CO]. [15] K. V. Berghaus, J. A. Kable, and V. Miranda, Quan- tifying scalar field dynamics with DESI 2024 Y1 BAO measurements, Phys. Rev. D110, 103524 (2024), arXiv:2404.14341 [astro-ph.CO]. [16] D. Shlivko and P. J. Steinhardt, Assessing observational constraints on dark energy, Phys. Lett. B855, 138826 39 (2024), arXiv:2405.03933 [astro-ph.CO]. [17] S. Bhattacharya, G. Borghetto, A. Malhotra, S. Parameswaran, G. Tasinato, and I. Zavala, Cos- mological constraints on curved quintessence, JCAP09, 073, arXiv:2405.17396 [astro-ph.CO]. [18] M. Van Raamsdonk and C. Waddell, Holographic mo- tivations and observational evidence for decreasing dark energy, (2024), arXiv:2406.02688 [hep-th]. [19] K. Lodhaet al."},{"citing_arxiv_id":"2603.25797","ref_index":178,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark energy from string theory: an introductory review","primary_cat":"hep-th","submitted_at":"2026-03-26T18:05:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"String theory imposes constraints on dark energy but permits various construction attempts for de Sitter vacua and single-field exponential quintessence models despite obstructions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"of a holographic boundary in some attempts of a \"dS/CFT\" correspondence. Its absence may then help understanding the difficulties encountered in those efforts (away from low dimensions). Having no event horizon would also benefit to the construction of a (quantum gravity) S-matrix, thanks to causally connected asymptotic states. These comments are in line with [177,178], discussing the TCC in a holographic context. This question of the horizon is also related to that of (eternal) cosmological acceleration; using this relation, similar criticism 16Expressed in terms of the FLRW metric (B.6), one verifies that anti-de Sitter and Minkowski spacetimes do not admit a cosmological event horizon. This agrees with the NCHC, since those are thought to be consistent"},{"citing_arxiv_id":"2603.21125","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Model-Independent Reconstruction of Quintessence Potential and Kinetic Energy from DESI DR2 and Pantheon+ Supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-03-22T08:46:57+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Quintessence potential decreases monotonically with redshift while kinetic energy crosses zero near z=1, with negative values at intermediate redshifts being statistical artifacts from derivative reconstruction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.09467","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the Hubble tension problem in the framework of holographic dark energy","primary_cat":"astro-ph.CO","submitted_at":"2025-11-12T16:39:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"HDE models with future event horizon IR cutoff partially ease the Hubble tension while Hubble-scale cutoffs do not, consistent across six models and multiple BAO/SN/CMB combinations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D110, 083528 (2024), arXiv:2408.17318 [astro-ph.CO]. [20] L. A. Anchordoqui, I. Antoniadis, and D. Lust, Phys. Lett. B868, 139632 (2025), arXiv:2503.19428 [hep-th]. [21] J.-Q. Wang, R.-G. Cai, Z.-K. Guo, and S.-J. Wang, (2025), arXiv:2508.01759 [astro-ph.CO]. [22] W. J. Wolf, P. G. Ferreira, and C. Garc' ıa-Garc' ıa, (2025), arXiv:2509.17586 [astro-ph.CO]. [23] W. Giar` e, M. A. Sabogal, R. C. Nunes, and E. Di Valentino, Phys. Rev. Lett.133, 251003 (2024), arXiv:2404.15232 [astro-ph.CO]. [24] G. Montani, N. Carlevaro, L. A. Escamilla, and E. Di Valentino, Phys. Dark Univ.48, 101848 (2025), arXiv:2404.15977 [gr-qc]. [25] T.-N. Li, P.-J. Wu, G.-H. Du, S.-J. Jin, H.-L. Li, J.- F. Zhang, and X. Zhang, Astrophys."},{"citing_arxiv_id":"2511.05653","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Dark Energy Microphysics with kSZ Tomography","primary_cat":"astro-ph.CO","submitted_at":"2025-11-07T19:00:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fisher-matrix forecasts for LSST- and CMB-S4-like surveys show kSZ tomography tightens constraints on dark energy parameters w0 and wa by 15% and 32% while assessing detectability of perturbations for different sound speeds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.03779","ref_index":25,"ref_count":1,"confidence":0.98,"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":"2505.24732","ref_index":96,"ref_count":1,"confidence":0.98,"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 Dark Energy Survey: Cosmology Results with∼1500 New High-redshift Type Ia Supernovae Using the Full 5 yr Data Set, Astrophys. J. Lett. 973 (1) (2024) L14.arXiv:2401.02929. [95] Y. Yang, Q. Wang, X. Ren, E. N. Saridakis, Y.-F. Cai, Modified Gravity Realizations of Quintom Dark Energy after DESI DR2, Astrophys. J. 988 (1) (2025) 123.arXiv:2504.06784. [96] D. Shlivko, P. J. Steinhardt, Assessing observational constraints on dark energy, Phys. Lett. B 855 (2024) 138826. arXiv:2405.03933. [97] G. Ye, M. Martinelli, B. Hu, A. Silvestri, Hints of Nonminimally Coupled Gravity in DESI 2024 Baryon Acoustic Oscillation Measurements, Phys. Rev. Lett. 134 (18) (2025) 181002.arXiv:2407.15832. [98] Y. Tada, T. Terada, Quintessential interpretation of the evolving dark energy in light of DESI observations, Phys."},{"citing_arxiv_id":"2503.14743","ref_index":186,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Extended Dark Energy analysis using DESI DR2 BAO measurements","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:17+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"for w0waCDM over algebraic-thawing model, however, cannot be straightforwardly converted into p-values or n-sigma levels because algebraic thawing and w0waCDM models are not nested. To achieve −∆χ2 comparable to w0wa with thawing models would require an exceptionally fine-tuned poten- tial V (φ) [184], precise initial field settings [185], or 'data- informed' prior choices [186], resulting in w(z ≳ 0.3) = −1 followed by a rapid increase tow(z ≲ 0.3) > −1. This suggests that a sharp increase followed by a decrease in dark energy density may be a necessary feature, since models that do not cross the phantom divide tend to underperform compared to those that do. The specific behavior of w(z) suggested by the data - a phantom"},{"citing_arxiv_id":"2503.14738","ref_index":151,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:12+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR2 BAO data exhibits 2.3 sigma tension with CMB in Lambda-CDM but prefers evolving dark energy (w0 > -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Linder, W. Sohn, A. de Mattia, J. L. Cervantes-Cota, R. Crittenden, T. M. Davis, M. Ishak, A. G. Kim, W. Matthewson, G. Niz, S. Park, J. Aguilar, and oth- ers, J. Cosmology Astropart. Phys. 2024, 048 (2024), arXiv:2405.04216 [astro-ph.CO]. [150] D. Shlivko and P. J. Steinhardt, Physics Letters B 855, 138826 (2024), arXiv:2405.03933 [astro-ph.CO]. [151] K. Lodha, A. Shafieloo, R. Calderon, E. Linder, W. Sohn, J. L. Cervantes-Cota, A. de Mattia, J. Garc' ıa- Bellido, M. Ishak, W. Matthewson, J. Aguilar, S. Ahlen, D. Brooks, T. Claybaugh, A. de la Macorra, and oth- ers, Phys. Rev. D 111, 023532 (2025), arXiv:2405.13588 [astro-ph.CO]. [152] A. Lewis and E. Chamberlain, arXiv e-prints , arXiv:2412.13894 (2024), arXiv:2412."},{"citing_arxiv_id":"2502.08876","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI Dark Secrets","primary_cat":"astro-ph.CO","submitted_at":"2025-02-13T01:21:31+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI data prefer w0wa models over LambdaCDM but scalar-field models with β fit worse individually; combined with Planck CMB and Pantheon+ SNe the data favor 0.27 < β < 1.03 at 95% credibility.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.03002","ref_index":227,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:51+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First-year DESI BAO data are consistent with flat LambdaCDM and, when combined with CMB, show a 2.5-3.9 sigma preference for evolving dark energy (w0 > -1, wa < 0) that strengthens with certain supernova datasets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Reconstructing Dark Energy using Crossing Statistics with DESI DR1 BAO data , arXiv e-prints (2024) arXiv:2405.04216 [ 2405.04216]. 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