{"total":12,"items":[{"citing_arxiv_id":"2607.00133","ref_index":90,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modified Cosmology from Mass-to-Horizon Relation: Background Evolution","primary_cat":"gr-qc","submitted_at":"2026-06-30T20:12:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Viable generalized horizon entropies from the mass-to-horizon relation are restricted to a narrow neighborhood around the Bekenstein-Hawking law, yielding only Lambda-CDM-like background evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26576","ref_index":235,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detectors for CLASS-W2: The second 90 GHz telescope of the Cosmology Large Angular Scale Surveyor","primary_cat":"astro-ph.IM","submitted_at":"2026-06-25T03:52:30+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A new 296-detector 90 GHz TES bolometer array for CLASS achieves uniform properties, 16 μK√s NET, 0.37 optical efficiency, and a 41% mapping speed boost after addressing blue-leak radiation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Paine, \"The am atmospheric model,\" Sept. 2024. 32 D. H. Martin and E. Puplett, \"Polarised interferometric spectrometry for the millimeter and submillimeter spectrum.,\"Infrared Physics10, pp. 105-109, 1970. 33 Planck Collaboration, P. A. R. Ade, N. Aghanim, M. Ashdown, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, N. Bartolo, E. Battaner, and et al., \"Planck 2015 results. IV . Low Frequency Instrument beams and window functions,\"Astronomy & Astrophysics594, p. A4, Sept. 2016. 34 J. L. Weiland, N. Odegard, R. S. Hill, E. Wollack, G. Hinshaw, M. R. Greason, N. Jarosik, L. Page, C. L. Bennett, J. Dunkley, B. Gold, M. Halpern, A. Kogut, E. Komatsu, D. Larson, M. Limon, S. S. Meyer, M. R. Nolta, K. M. Smith, D."},{"citing_arxiv_id":"2606.22431","ref_index":217,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"An Interplay Between Fractional Calculus and Holographic Dark Energy","primary_cat":"gr-qc","submitted_at":"2026-06-21T10:44:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Introduces Fractional Holographic Dark Energy (FHDE) via fractionally corrected entropy from a modified Wheeler-DeWitt equation and studies its late-time cosmology, field reconstructions, and extensions to modified gravity theories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00411","ref_index":87,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The sound of dynamical dark energy and modified gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-05-29T23:05:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Using CMB, SN, BAO and shear data, the work shows dynamical dark energy in MG models correlates with deviations from GR below z=2 at >95% CL, a link that holds for varying sound speed but vanishes for a cosmological constant.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18659","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Faster CMB lensing with control variates","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T17:05:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A control variate technique using differenced estimates from realistic masked and isotropic simulations reduces the computational cost of CMB lensing bias calculations by a factor of three to five.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.08449","ref_index":80,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Coupled Dark Energy and Dark Matter for DESI: An Effective Guide to the Phantom Divide","primary_cat":"astro-ph.CO","submitted_at":"2026-04-09T16:45:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Coupled quintessence-dark matter models can produce an apparent phantom-crossing effective equation of state matching DESI preferences if the scalar field begins frozen in the radiation era.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"We require that the cumulative DM mass drift prior to recombination does not exceed approximately 1%, i.e. |∆ lnm|rec ≲10 −2. Then an upper boundbβrec ≲O(0.1) can be derived. Finally, the scalar field must provide a subdominant contributiontothetotalenergydensityatrecombination. As a benchmark, we adopt the Planck 2015 upper bound on a constant early-DE fraction [80], according to which theenergyfractionΩ ϕ ofthescalarfieldatrecombination should satisfy Ωϕ(zrec)<0.0036 (95% C.L.).(53) We note that as for the two constraints discussed above, also the value used here should be considered as a conser- vative necessary proxy only. Since the potential energy is negligible at that epoch,Ωϕ reduces to the kinetic es-"},{"citing_arxiv_id":"2603.21125","ref_index":5,"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":"2602.03110","ref_index":118,"ref_count":1,"confidence":0.98,"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":"method","top_context_polarity":"use_method","context_text":"cific forms to perform a likelihood analysis. We focus on the \"late-time\" modification scenario, motivated by the coincidence of cosmic acceleration and the onset of DE dominance. For modifications that are scale-independent on sub-horizon scales (valid for the quasi-static regime of many scalar-tensor theories), we adopt a parameter- ization proportional to the DE density Ω DE(a), given by [118] µ(a) = 1 +µ 0 ΩDE(a) ΩΛ ,(6) Σ(a) = 1 + Σ0 ΩDE(a) ΩΛ ,(7) where Ω Λ is the DE density parameter atz= 0. The free parametersµ 0 and Σ0 quantify the amplitude of the deviation today. In GR,µ 0 = Σ0 = 0. For the background evolution, we perform our analysis in two background expansion scenarios: •ΛCDM: The equation of state (EoS) of DE is fixed tow=−1."},{"citing_arxiv_id":"2505.24732","ref_index":75,"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":"dataset","top_context_polarity":"use_dataset","context_text":"Astrophys. 571 (2014) A16.arXiv: 1303.5076. [73] M. Betoule, et al., Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples, Astron. Astrophys. 568 (2014) A22.arXiv:1401.4064. 20 [74] P. A. R. Ade, et al., Planck 2015 results. XIII. Cosmological parameters, Astron. Astrophys. 594 (2016) A13.arXiv: 1502.01589. [75] P. A. R. Ade, et al., Planck 2015 results. XIV. Dark energy and modified gravity, Astron. Astrophys. 594 (2016) A14. arXiv:1502.01590. [76] M. A. Troxel, et al., Dark Energy Survey Year 1 results: Cosmological constraints from cosmic shear, Phys. Rev. D 98 (4) (2018) 043528.arXiv:1708.01538. [77] T. M. C. Abbott, et al., Dark Energy Survey year 1 results: Cosmological constraints from galaxy clustering and weak"},{"citing_arxiv_id":"2503.14743","ref_index":128,"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":"Pogosian, and G.-B. Zhao, JCAP 12, 025, arXiv:astro-ph/0510293. [125] F. Simpson and S. Bridle, Phys. Rev. D 73, 083001 (2006), arXiv:astro-ph/0602213. [126] C. Garcia-Quintero, M. Ishak, and O. Ning, JCAP 12, 018, arXiv:2010.12519 [astro-ph.CO]. [127] P. A. R. Ade and others (Planck), Astron. Astrophys. 594, A14 (2016), arXiv:1502.01590 [astro-ph.CO]. [128] G.-B. Zhao and others, Nature Astron. 1, 627 (2017), arXiv:1701.08165 [astro-ph.CO]. [129] M. Raveri, L. Pogosian, K. Koyama, M. Martinelli, and others, A joint reconstruction of dark energy and modified growth evolution (2021), arXiv:2107.12990 [astro-ph.CO]. [130] L. Pogosian, M. Raveri, K. Koyama, M. Mar- tinelli, and others, Nature Astron. 6, 1484 (2022),"},{"citing_arxiv_id":"2411.12022","ref_index":207,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:35+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape clustering yields Ω_m = 0.2962 ± 0.0095 and σ_8 = 0.842 ± 0.034 in flat ΛCDM, tightening to H_0 = 68.40 ± 0.27 km/s/Mpc with CMB and DESY3, while favoring w_0 > -1, w_a < 0 and limiting neutrino mass sum to < 0.071 eV.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"This is not expected to affect our results from DESI full-shape clustering and BAO, as the scale cuts in our full-shape analysis, 0 .02 < k/ h Mpc−1 < 0.20, ensure that nonlinearities (that is, the one-loop terms in the effective field theory expansion) are small. The velocileptors prescription used for our full-shape analysis has been tested against the MG non-linear code fkpt [207], showing a good agreement in loop corrections for small deviations from GR. The external data that we use also rely on linear - 30 - model/dataset Ω m σ8 H0 µ0 Σ0[km/s/Mpc] Flatµ0Σ0ΛCDM DESI (FS+BAO)+ BBN+ns10 0.2957±0.0097 0 .839±0.034 68 .53±0.75 0 .11+0.45 −0.54 no constraint CMB-nl 0 .3041±0.0093 0 .742+0.13 −0.092 68.21±0.71 −0.66+1.5 −0.83 0."},{"citing_arxiv_id":"1807.06209","ref_index":285,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. VI. Cosmological parameters","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Final Planck CMB data confirms the flat 6-parameter ΛCDM model with Ω_c h² = 0.120 ± 0.001, Ω_b h² = 0.0224 ± 0.0001, n_s = 0.965 ± 0.004, τ = 0.054 ± 0.007, H_0 = 67.4 ± 0.5 km/s/Mpc, and no strong evidence for extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}