{"total":19,"items":[{"citing_arxiv_id":"2607.07777","ref_index":34,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Status of Single Scalar Field Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2026-07-08T17:38:46+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":4.5,"formal_verification":"none","one_line_summary":"Cosmological data can constrain only a handful of EFT parameters for single-scalar dark energy; extended models show modest preference over Λ but remain underdetermined and challenged by fifth forces and screening.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21826","ref_index":136,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Energy in the DESI Era: A Brief Review of Evidence, Beyond-$\\Lambda$CDM Interpretations, and Tensions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-20T01:29:51+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":3.0,"formal_verification":"none","one_line_summary":"DESI data hint that dark energy evolves (w0>−1, wa<0, phantom crossing) at 2.5–4.2σ, but the same expansion history can also be produced by interacting dark sectors, modified gravity, or non-cold dark matter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20794","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Horndeski Gravity with Phantom Crossing","primary_cat":"astro-ph.CO","submitted_at":"2026-06-18T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.5,"formal_verification":"none","one_line_summary":"Asymptotic Cubic Galileon models can fit Planck+DESI+DES expansion history with phantom crossing and are tightly constrained by galaxy-ISW and void-force observables.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27301","ref_index":144,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effective Phantom Dark Energy: What Cosmological Reconstruction Does and Does Not Imply","primary_cat":"astro-ph.CO","submitted_at":"2026-05-26T17:11:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Effective phantom dark energy is a background-level reconstruction that does not imply fundamental pathologies such as ghost instabilities or null energy condition violation by the underlying stress tensor.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"mological Parameters\". In:Astrophys. J.887 (Apr. 2019), p. 153.doi:10 . 3847 / 1538 - 4357/ab535d. arXiv:1904.03790 [astro-ph.CO]. [143] W. J. Wolf, P. G. Ferreira, and C. García-García. \"Cosmological constraints on Galileon dark energy with broken shift symmetry\". In:Phys. Rev. D113.2 (2026), p. 023551.doi: 10.1103/bxvj-bsv1. arXiv:2509.17586 [astro-ph.CO]. [144] S. Nojiri, S. D. Odintsov, and V. K. Oikonomou. \"Is Phantom Divide Crossing in General Relativity Completely Impossible? Shortcomings and Possible Solutions\". In: (Jan. 2026). arXiv:2601.21356 [gr-qc]. [145] Z. C. Santana Júnior et al. \"Interaction in the dark sector: A phenomenological approach\". In:Phys. Rev. D109.12 (2024), p. 123542.doi:10.1103/PhysRevD."},{"citing_arxiv_id":"2605.27221","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Dynamical Dark Energy from Multiple Probes in the Full Dark Energy Survey","primary_cat":"astro-ph.CO","submitted_at":"2026-05-26T16:08:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Full DES data from SN+BAO+3x2pt yields w0=-0.84, wa=-0.44 with 2.2σ deviation from ΛCDM; adding DESI+CMB reaches 3.0σ while 3x2pt improves figure of merit by ~10%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.26259","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Charging Across the Phantom Divide with Modified Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-25T18:38:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Horndeski gravity with shift symmetry and linear potential permits three mechanisms for crossing the phantom divide but none fit current data well without a cosmological constant.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22599","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The impact of evolving dark energy on the Weyl potential measured from the Dark Energy Survey Year 3 data","primary_cat":"astro-ph.CO","submitted_at":"2026-05-21T15:14:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Evolving dark energy models lower the tension in DES Y3 Weyl potential measurements with GR+ΛCDM predictions to 1.6-2.2σ by changing the theoretical background evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22309","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Signatures of Modified Gravity on Linear Scales in a Dynamical Dark Energy Background","primary_cat":"astro-ph.CO","submitted_at":"2026-05-21T10:55:25+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Using Planck, DESI, supernovae, and redshift-space distortions, the authors infer that modified gravity, if present, must act only below ~30 Mpc and cannot modify the large scales previously considered.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Tsujikawa, Crossing the phantom divide in scalar- tensor and vector-tensor theories, Phys. Rev. D113, L041301 (2026), arXiv:2508.17231 [astro-ph.CO]. [56] W. J. Wolf, P. G. Ferreira, and C. Garc' ıa-Garc' ıa, Cos- mological constraints on Galileon dark energy with bro- ken shift symmetry, Phys. Rev. D113, 023551 (2026), arXiv:2509.17586 [astro-ph.CO]. [57] T. Adi, Lowering the horizon on Dark Energy: A late- time response to early solutions for the Hubble tension, JCAP03, 015, arXiv:2509.12331 [astro-ph.CO]. [58] G. Alestas, M. Caldarola, I. Ocampo, S. Nesseris, and S. Tsujikawa, DESI constraints on two- field quintessence with exponential potentials, arXiv:2510.21627 (2025), arXiv:2510.21627 [astro-"},{"citing_arxiv_id":"2605.12415","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Late-time reconstruction of non-minimally coupled gravity with a smoothness prior","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T17:12:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Non-parametric reconstruction of non-minimally coupled gravity with a smoothness prior on CMB, DESI BAO, supernovae, and DES data yields a 2.8σ hint for coupling and a preference for phantom divide crossing stabilized by the coupling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Garc' ıa-Garc' ıa, T. Anton, and P. G. Ferreira, Phys. Rev. Lett.135, 081001 (2025), arXiv:2504.07679 [astro-ph.CO]. [21] J.-Q. Wang, R.-G. Cai, Z.-K. Guo, and S.-J. Wang, Phys. Rev. D113, 083534 (2026), arXiv:2508.01759 [astro- ph.CO]. [22] J.-Q. Wang, R.-G. Cai, Z.-K. Guo, Y.-H. Li, S.-J. Wang, and X. Zhang, (2026), arXiv:2604.02204 [astro-ph.CO]. [23] Z. Yao, G. Ye, and A. Silvestri, JCAP10, 078 (2025), arXiv:2508.01378 [gr-qc]. [24] G. Ye and Y. Cai, Phys. Rev. D112, L121301 (2025), arXiv:2503.22515 [gr-qc]. [25] G. Ye, (2024), arXiv:2411.11743 [astro-ph.CO]. [26] G. Gubitosi, F. Piazza, and F. Vernizzi, JCAP02, 032 (2013), arXiv:1210.0201 [hep-th]. 15 [27] J. Espejo, S. Peirone, M. Raveri, K."},{"citing_arxiv_id":"2604.08530","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Disentangling cosmic distance tensions with early and late dark energy","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T17:58:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Rev. Lett.135, 081001 (2025), arXiv:2504.07679 [astro-ph.CO]. [28] W. J. Wolf, P. G. Ferreira, and C. Garc' ıa-Garc' ıa, (2025), arXiv:2509.17586 [astro-ph.CO]. [29] A. Pourtsidou, (2025), arXiv:2509.15091 [astro-ph.CO]. [30] S. Tsujikawa, (2025), arXiv:2508.17231 [astro-ph.CO]. [31] Z. Yao, G. Ye, and A. Silvestri, (2025), arXiv:2508.01378 [gr-qc]. [32] S. L. Guedezounme, B. R. Dinda, and R. Maartens, (2025), arXiv:2507.18274 [astro-ph.CO]. [33] M. H¨ og˚ as and E. M¨ ortsell, (2025), arXiv:2507.03743 [astro-ph.CO]. [34] A. Paliathanasis, Phys. Dark Univ.49, 101993 (2025), arXiv:2504.11132 [gr-qc]. [35] D. Andriot, Phys. Dark Univ.49, 102000 (2025), arXiv:2505.10410 [hep-th]. [36] C. You, D. Wang, and T."},{"citing_arxiv_id":"2603.26560","ref_index":58,"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":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.5,"formal_verification":"none","one_line_summary":"Under standard recombination, phantom-crossing dynamical dark energy is preferred at ~97–98.5% probability; early-time fixes to the Hubble tension erase that preference while creating severe ω_m tension with CMB.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Oikonomou,Phantom crossing and oscillating dark energy with F(R) gravity,Phys. Rev. D112(2025) 104035 [2506.21010]. [56] S.S. Mishra, W.L. Matthewson, V. Sahni, A. Shafieloo and Y. Shtanov,Braneworld dark energy in light of DESI DR2,JCAP11(2025) 018 [2507.07193]. [57] M. Braglia, X. Chen and A. Loeb,Exotic dark matter and the DESI anomaly,JCAP11 (2025) 064 [2507.13925]. [58] A. G' omez-Valent and A. Gonz' alez-Fuentes,Effective phantom divide crossing with standard and negative quintessence,Phys. Lett. B872(2026) 140096 [2508.00621]. [59] S. Roy Choudhury, T. Okumura and K. Umetsu,Cosmological Constraints on Nonphantom Dynamical Dark Energy with DESI Data Release 2 Baryon Acoustic Oscillations: A 3σ+ Lensing Anomaly,Astrophys."},{"citing_arxiv_id":"2603.25999","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cosmological constraints on the big bang quantum cosmology model","primary_cat":"astro-ph.CO","submitted_at":"2026-03-27T01:31:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The JCDM model yields H0 of 66.95 plus or minus 0.51 km/s/Mpc and Omega_m of 0.3419 plus or minus 0.0065 in a flat universe, rising to H0 of 69.13 plus or minus 0.56 with slight positive curvature, fitting late-time data but struggling with full early-universe consistency.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[51] P.-J. Wu, T.-N. Li, G.-H. Du, and X. Zhang, (2025), arXiv:2509.02945 [astro-ph.CO]. [52] L. Perivolaropoulos and F. Skara, New Astron. Rev. 95, 101659 (2022), arXiv:2105.05208 [astro-ph.CO]. [53] K. W. K. Wong, M. Isi, and T. D. P. Edwards, \"Fast gravitational wave parameter estimation without com- promises,\" (2023), arXiv:2302.05333 [astro-ph.IM]. [54] W. J. Wolf, P. G. Ferreira, and C. Garc' ıa-Garc' ıa, (2025), arXiv:2509.17586 [astro-ph.CO]. [55] S.-H. Zhou, T.-N. Li, G.-H. Du, J.-Q. Jiang, J.-F. Zhang, and X. Zhang, (2025), arXiv:2509.10836 [astro-ph.CO]. [56] M. H. van Putten, Journal of High Energy Astrophysics 45, 194-199 (2025). [57] M. H. P. M. van Putten, \"The hubble parameter of the local distance ladder from dynamical dark energy with"},{"citing_arxiv_id":"2602.11936","ref_index":205,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Probing dynamical dark energy with late-time data: Evidence, tensions, and the limits of the $w_0w_a$CDM framework","primary_cat":"astro-ph.CO","submitted_at":"2026-02-12T13:35:54+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Polarski, Int. J. Mod. Phys. D10, 213 (2001), arXiv:gr-qc/0009008. [202] E. V. Linder, Phys. Rev. Lett.90, 091301 (2003), arXiv:astro-ph/0208512. [203] H. K. Jassal, J. S. Bagla, and T. Padmanabhan, Phys. Rev. D72, 103503 (2005), arXiv:astro-ph/0506748. [204] E. M. Barboza, Jr. and J. S. Alcaniz, Phys. Lett. B666, 415 (2008), arXiv:0805.1713 [astro-ph]. [205] G. Efstathiou, Mon. Not. Roy. Astron. Soc.310, 842 (1999), arXiv:astro-ph/9904356. [206] N. Dimakis, A. Paliathanasis, and T. Christodoulakis, Phys. Rev. D109, 024031 (2024), arXiv:2308.08759 [gr- qc]. [207] R. C. Nunes, S. K. Yadav, J. F. Jesus, and A. Bernui, Mon. Not. Roy. Astron. Soc.497, 2133 (2020), arXiv:2002.09293 [astro-ph.CO]. [208] P. A."},{"citing_arxiv_id":"2602.03110","ref_index":78,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Evidence for deviation in gravitational light deflection from general relativity at cosmological scales with KiDS-Legacy and CMB lensing","primary_cat":"astro-ph.CO","submitted_at":"2026-02-03T05:11:50+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"KiDS-Legacy weak lensing plus CMB data yields a 3 sigma deviation in light deflection from GR in a Lambda CDM background, with the signal driven by large-scale CMB lensing amplitudes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"00478 [astro-ph.CO]. 12 [75] P.-J. Wu, M. Zhang, and S.-J. Jin, (2025), 10.1103/zg3k-k6g1, arXiv:2512.05548 [astro-ph.CO]. [76] Y.-H. Yao, Y.-H. Shen, T.-N. Li, G.-H. Du, and Y. Gong, (2025), arXiv:2510.13436 [astro-ph.CO]. [77] W. J. Wolf, C. Garc' ıa-Garc' ıa, T. Anton, and P. G. Ferreira, Phys. Rev. Lett.135, 081001 (2025), arXiv:2504.07679 [astro-ph.CO]. [78] W. J. Wolf, P. G. Ferreira, and C. Garc' ıa-Garc' ıa, Phys. Rev. D113, 023551 (2026), arXiv:2509.17586 [astro- ph.CO]. [79] C. Li, X. Ren, Y. Yang, E. N. Saridakis, and Y.-F. Cai, (2025), arXiv:2512.16551 [astro-ph.CO]. [80] J.-Y. Song, G.-H. Du, T.-N. Li, L.-F. Wang, J.-Z. Qi, J.-F. Zhang, and X. Zhang, Sci. China Phys. Mech. Astron.69, 240413 (2026), arXiv:2511."},{"citing_arxiv_id":"2601.02077","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Joint Constraints on Neutrinos and Dynamical Dark Energy in Minimally Modified Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-01-05T12:58:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The w†VCDM model shows a statistically significant preference for late-time quintessence-phantom crossing dark energy, raises the Hubble constant, and satisfies neutrino mass and Neff constraints from current cosmological datasets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cosmological Rips and Their Observational Signatures (2025), arXiv:2512.20383 [astro-ph.CO]. [28] M. Artola, I. Ayuso, R. Lazkoz, and V. Salzano, Is CPL dark energy a mirage? (2025), arXiv:2510.04191 [astro- ph.CO]. [29] W. J. Wolf, P. G. Ferreira, and C. Garc' ıa-Garc' ıa, Cos- mological constraints on Galileon dark energy with bro- ken shift symmetry (2025), arXiv:2509.17586 [astro- ph.CO]. [30] H. Adam, M. P. Hertzberg, D. Jim' enez-Aguilar, and I. Khan, Comparing Minimal and Non-Minimal Quintessence Models to 2025 DESI Data (2025), arXiv:2509.13302 [astro-ph.CO]. [31] P.-J. Wu, T.-N. Li, G.-H. Du, and X. Zhang, Observa- tional challenges to holographic and Ricci dark energy paradigms: Insights from ACT DR6 and DESI DR2 (2025), arXiv:2509."},{"citing_arxiv_id":"2512.20832","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Thawing Quintessence: Priors, evidence, and likely trajectories","primary_cat":"astro-ph.CO","submitted_at":"2025-12-23T23:14:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian evidence from DESI DR2 BAO, Planck+ACT CMB, and multiple supernova samples favors thawing quintessence over a cosmological constant.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.09467","ref_index":29,"ref_count":1,"confidence":0.9,"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":"14934 [astro-ph.CO]. [26] T.-N. Li, G.-H. Du, Y.-H. Li, P.-J. Wu, S.-J. Jin, J.-F. Zhang, and X. Zhang, Sci. China Phys. Mech. Astron. 69, 210413 (2026), arXiv:2501.07361 [astro-ph.CO]. [27] Y.-H. Li and X. Zhang, (2025), arXiv:2506.18477 [astro- ph.CO]. [28] Y. Yang, Y. Wang, and X. Dai, Eur. Phys. J. C85, 224 (2025), arXiv:2502.17792 [astro-ph.CO]. [29] E. Silva, M. A. Sabogal, M. Scherer, R. C. Nunes, E. Di Valentino, and S. Kumar, Phys. Rev. D111, 123511 (2025), arXiv:2503.23225 [astro-ph.CO]. [30] Y. Zhai, M. de Cesare, C. van de Bruck, E. Di Valentino, and E. Wilson-Ewing, (2025), arXiv:2503.15659 [astro- ph.CO]. [31] L. Feng, T.-N. Li, G.-H. Du, J.-F. Zhang, and X. Zhang, Phys. Dark Univ.48, 101935 (2025), arXiv:2503."},{"citing_arxiv_id":"2510.04179","ref_index":24,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Crosschecking Cosmic Distances from DESI BAO and DES SNe","primary_cat":"astro-ph.CO","submitted_at":"2025-10-05T12:41:23+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"For DESI DR2 BAO versus DES SNe, the comoving-distance ratio is flat but the inverse-Hubble-distance ratio falls with redshift at 2.3–2.5σ, which the authors attribute to systematics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.03779","ref_index":68,"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}],"limit":50,"offset":0}