{"total":12,"items":[{"citing_arxiv_id":"2607.01226","ref_index":144,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T17:57:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Dynamical dark energy remains preferred across extended models while curvature, neutrino mass and inflation parameters show strong model dependence, with no resolution of the H0 tension.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Lond. A383 (2025) 20240022 [2406.12106]. [142]CosmoVerse Networkcollaboration,The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics,Phys. Dark Univ.49(2025) 101965 [2504.01669]. [143] G. Efstathiou,A Lockdown Perspective on the Hubble Tension (with comments from the SH0ES team),2007.10716. [144] E. Mortsell, A. Goobar, J. Johansson and S. Dhawan,Sensitivity of the Hubble Constant Determination to Cepheid Calibration,Astrophys. J.933(2022) 212 [2105.11461]. [145] E. Mortsell, A. Goobar, J. Johansson and S. Dhawan,The Hubble Tension Revisited: Additional Local Distance Ladder Uncertainties,Astrophys. J.935(2022) 58 [2106.09400]. [146] A. Sharon, D."},{"citing_arxiv_id":"2606.31324","ref_index":93,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological Viability of Exponential Infrared $f(T)$ Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-06-30T08:27:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Exponential IR f(T) gravity Model I alleviates Hubble tension but is disfavoured by combined Planck/ACT/SPT+DESI+Pantheon+ data; Model II is ruled out because background constraints force unphysical shifts in CMB parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(2026), arXiv:2504.17859 [gr-qc]. 29 [90] H. Cheng, E. Di Valentino, L. A. Escamilla, A. A. Sen, and L. Visinelli, JCAP09, 031 (2025), arXiv:2505.02932 [astro-ph.CO]. [91] H. Cheng, E. Di Valentino, and L. Visinelli, JHEAp53, 100610 (2026), arXiv:2505.22066 [astro-ph.CO]. [92] E. ¨Oz¨ ulker, E. Di Valentino, and W. Giar` e, (2025), arXiv:2506.19053 [astro-ph.CO]. [93] T.-N. Li, G.-H. Du, S.-H. Zhou, Y.-H. Li, J.-F. Zhang, and X. Zhang, Phys. Dark Univ.52, 102254 (2026), arXiv:2511.22512 [astro-ph.CO]. [94] D. H. Lee, W. Yang, E. Di Valentino, S. Pan, and C. van de Bruck, Phys. Rev. D113, 063554 (2026), arXiv:2507.11432 [astro-ph.CO]. [95] E. Fazzari, W. Giar` e, and E. Di Valentino, Astrophys. J. Lett.996(2026), 10."},{"citing_arxiv_id":"2606.21826","ref_index":158,"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":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review of DESI evidence for dynamical dark energy, its dependence on parametrization and datasets, and alternative beyond-LambdaCDM interpretations that may address cosmological tensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20036","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evolving Dark Energy Is Vacuum Energy After All","primary_cat":"astro-ph.CO","submitted_at":"2026-06-18T10:10:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A QCD-vacuum-based model of dynamical dark energy fits Planck+ACT+SPT, DESI DR2, and supernova data while reproducing the late-time evolution favored by DESI.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19090","ref_index":94,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resolving the Hubble Tension in the Early Dark Energy Framework with JWST and DESI Data","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T13:58:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Axion EDE model fitted to Planck/ACT/SPT CMB, DESI BAO, and JWST UV luminosity function data yields H0 = 71.58 ± 1.05 km s^{-1} Mpc^{-1}, reduces H0 tension to 1.0 sigma, and improves Δχ^{2}_tot = -18.26 over Λ CDM.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"B873, 140180 (2026), arXiv:2404.18579 [astro-ph.CO]. [92] T.-N. Li, G.-H. Du, S.-H. Zhou, Y.-H. Li, J.-F. Zhang, and X. Zhang, Phys. Dark Univ.52, 102254 (2026), arXiv:2511.22512 [astro-ph.CO]. [93] E. Specogna, S. A. Adil, E. Ozulker, E. Di Valentino, R. C. Nunes, O. Akarsu, and A. A. Sen, Phys. Rev. D 113, 103549 (2026), arXiv:2504.17859 [gr-qc]. [94] 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:2511.12017 [astro- 10 ph.CO]. [95] T.-N. Li, W. Giar` e, G.-H. Du, Y.-H. Li, E. Di Valentino, J.-F. Zhang, and X. Zhang, (2026), arXiv:2601.07361 [astro-ph.CO]. [96] G.-H. Du, T.-N. Li, T. Liu, J.-F. Zhang, and X."},{"citing_arxiv_id":"2606.06495","ref_index":131,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"What it takes to solve the Hubble tension through Modifications of Cosmological Recombination II: in light of ACT DR6 and DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Perturbative modifications to the electron mass m_e(z) resolve the Hubble tension with Planck+ACT CMB data but cannot when DESI DR2 BAO data are added due to lowered Omega_m.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"Smith and N. Sch¨ oneberg, Phys. Rev. D112, 083559 (2025), arXiv:2503.20002 [astro-ph.CO]. [129] M. Scherer, M. A. Sabogal, R. C. Nunes, and A. De Fe- lice, Phys. Rev. D112, 043513 (2025), arXiv:2504.20664 [astro-ph.CO]. [130] E. Specogna, S. A. Adil, E. 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[134] N."},{"citing_arxiv_id":"2606.05853","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reconstructing dark energy with fewer assumptions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T08:27:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bin-wise uncorrelated reconstruction from DESI/SDSS BAO and Pantheon+/Union3.1/DES-Dovekie supernovae yields dark energy density peaking then declining and equation of state oscillating with phantom crossing near z~0.7, consistent across datasets at moderate significance.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the accuracy of the marginalizedf DE(z) posteriors, which is determined from performance on mock datasets, as discussed in Appendix A. There are some caveats to the binning choice for fDE(z). First, one must remain consistent with the nor- malization conditionf DE(0) = 1, which follows directly from the definition of this function. In the DESI re- constructions [68], this was achieved by fixingf DE(z) to unity over the small intervalz∈[0, z min) and using zmin ∼0.05 as the minimum redshift of the first recon- struction amplitude [110]. We adopt this strategy here, fixingf DE(z) = 1 withinz∈[0, z min) and restricting the first amplitude to [z min,0.1). Ideally, one would choosezmin ∼0.01 so that no SNe Ia measurements are omitted from the reconstruction."},{"citing_arxiv_id":"2606.05005","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T15:26:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Upper bounds on total neutrino mass in four phenomenological interacting dark energy models are derived from DESI DR2 BAO plus CMB and SNIa data, showing strong dependence on the interaction term form and statistical preference for models that tighten the bound below the oscillation lower limit.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"988, 243 (2025), arXiv:2504.21373 [astro-ph.CO]. [40] E. M. Teixeira, W. Giar` e, N. B. Hogg, T. 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N."},{"citing_arxiv_id":"2605.21456","ref_index":38,"ref_count":1,"confidence":0.9,"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":"[36] E. Di Valentino, A. Mukherjee, and A. A. Sen, Dark Energy with Phantom Crossing and theH0 Tension, Entropy23, 404 (2021), 2005.12587. [37] S. A. Adil, Ö. Akarsu, E. Di Valentino, R. C. Nunes, E. Özülker, A. A. Sen, and E. 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Rev."},{"citing_arxiv_id":"2511.09467","ref_index":48,"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":"Su, JCAP09, 053 (2024), arXiv:2405.05798 [astro- ph.CO]. [45] S. Roy Choudhury and T. Okumura, Astrophys. J. Lett. 976, L11 (2024), arXiv:2409.13022 [astro-ph.CO]. [46] Y.-H. Pang, X. Zhang, and Q.-G. Huang, JCAP04, 057 (2025), arXiv:2411.14189 [astro-ph.CO]. [47] L. Huang, R.-G. Cai, and S.-J. Wang, Sci. 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