{"total":13,"items":[{"citing_arxiv_id":"2606.31299","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Distance duality relation in symmetric teleparallel gravity","primary_cat":"gr-qc","submitted_at":"2026-06-30T08:11:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In symmetric teleparallel f(Q) gravity with nonminimal EM-nonmetricity coupling, the distance duality relation is dynamically violated, yielding a generalized formula relating observational distances to the Hubble rate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31274","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Fragility of stealth solutions in mimetic gravity","primary_cat":"gr-qc","submitted_at":"2026-06-30T07:47:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Stealth solutions in mimetic gravity decouple from background dynamics on the lambda=0 branch but impose an infinite hierarchy of constraints on perturbations, rendering the screening limit non-uniform and pathological.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10597","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Synergy between the gravitational potential decay rate and other structure growth probes in testing gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T09:01:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Tomographic DR data added to Σ8 + fσ8 tightens phenomenological MG parameters (μ0, Σ0, η0) and EFT α coefficients by factors of 1.5–2.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.24089","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exploring the Dark Sector: Interacting Radiation in Light of Modern Cosmological Probes","primary_cat":"astro-ph.CO","submitted_at":"2026-05-22T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New constraints on dark radiation parameters from recent cosmological datasets show the model alleviates the Hubble tension with SH0ES inclusion while remaining consistent with standard expectations without it.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22801","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Another Look at the Weak-Field Limit of Generalized Hybrid Metric-Palatini Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-21T17:53:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Generalized hybrid metric-Palatini gravity propagates a massless spin-2 mode and two massive scalars in the weak field; stability requires algebraic conditions on f derivatives at flat space, and planetary data constrain the scalar masses in a hierarchical regime.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20989","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Relativistic effects in k-essence","primary_cat":"astro-ph.CO","submitted_at":"2026-04-22T18:21:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Relativistic effects dominate large-scale galaxy power spectra and grow with redshift, but are largely insensitive to k-essence microphysics in Fourier space while the angular spectrum shows clearer model distinctions, especially for the tachyon.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"essence,\" henceforth). It may be worth noting that k- essence, with LagrangianP(ϕ, X) and kinetic termX( ˙ϕ) where ˙ϕis time derivative ofϕ, was originally introduced as \"k-inflation\" in [28], as a dynamical explanation for the well known early-time cosmic inflation. The first appli- cation of k-essence to the late-time cosmic acceleration, as dark energy, was done in [29], where it was referred to as \"kinetically driven quintessence.\" It was further presented, for the first time as \"k-field\" or \"k-essence\" in [16], as a dynamical solution to the problem of a small cosmological constant and late-time cosmic acceleration. Later, its present name was settled for in [17], where its essentials (basics and dynamical analysis) were pre-"},{"citing_arxiv_id":"2603.27386","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Thermal channels of scalar and tensor waves in Jordan-frame scalar--tensor gravity","primary_cat":"gr-qc","submitted_at":"2026-03-28T19:37:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Scalar and tensor perturbations in Jordan-frame scalar-tensor gravity admit an exact linear-order Eckart effective-fluid description, with gravitational-wave damping governed by the scalar sector's transverse-traceless anisotropic stress.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.03110","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"[26] S.-J. Jin, Y.-Z. Zhang, J.-Y. Song, J.-F. Zhang, and X. Zhang, Sci. China Phys. Mech. Astron.67, 220412 (2024), arXiv:2305.19714 [astro-ph.CO]. [27] T. Clifton, P. G. Ferreira, A. Padilla, and C. Sko- rdis, Phys. Rept.513, 1 (2012), arXiv:1106.2476 [astro- ph.CO]. [28] K. Koyama, Rept. Prog. Phys.79, 046902 (2016), arXiv:1504.04623 [astro-ph.CO]. [29] M. Ishak, Living Rev. Rel.22, 1 (2019), arXiv:1806.10122 [astro-ph.CO]. [30] S. M. Carroll, V. Duvvuri, M. Trodden, and M. S. Turner, Phys. Rev. D70, 043528 (2004), arXiv:astro- ph/0306438. [31] S. Capozziello, S. Carloni, and A. Troisi, Recent Res. Dev. Astron. Astrophys.1, 625 (2003), arXiv:astro- ph/0303041. [32] W. Hu and I. Sawicki, Phys. Rev."},{"citing_arxiv_id":"2512.08972","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Degenerate higher-order scalar-tensor theories in metric-affine gravity","primary_cat":"gr-qc","submitted_at":"2025-12-02T15:03:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A metric-affine version of quadratic DHOST theories is derived and reduced to a one-function family that satisfies degeneracy conditions and light-speed gravitational wave propagation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.19770","ref_index":66,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational particle production, the cosmological tensions and fast radio bursts","primary_cat":"gr-qc","submitted_at":"2025-08-27T10:53:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Gravitational vacuum polarization explains the Hubble tension by increasing direct H0 measurements while leaving indirect ones unaffected, does not impact the sigma8 tension, and predicts FRB measurements match CMB/BAO values.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14738","ref_index":141,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"method","top_context_polarity":"use_method","context_text":"the condition w0+wa < 0 to enforce early matter domina- tion. While other justifiable choices are possible, and the values of Bayesian quantities such as the model evidence will always depend on the particular choice used, we con- sider this the minimal empirical approach. Whenever the equation of state crosses the w = −1 boundary we use the parametrized post-Friedmann (PPF) approach of [141, 142] to include dark energy perturbations when calculating CMB power spectra-however, as shown be- low, the method of accounting for dark energy perturba- tions does not play a major role, since simply applying an early-Universe CMB prior on ( θ∗, ωb, ωc) largely re- produces the same results on w0 and wa. Our primary measure of the statistical significance of"},{"citing_arxiv_id":"2411.12022","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"1017/CBO9781139175180. [14] D. Huterer, Growth of cosmic structure , Astron. Astrophys. Rev. 31 (2023) 2 [ 2212.05003]. [15] K. Koyama, Cosmological Tests of Modified Gravity, Rept. Prog. Phys. 79 (2016) 046902 [1504.04623]. [16] A. Joyce, L. Lombriser and F. Schmidt, Dark Energy Versus Modified Gravity, Ann. Rev. Nucl. Part. Sci. 66 (2016) 95 [ 1601.06133]. [17] M. Ishak, Testing General Relativity in Cosmology, Living Rev. Rel. 22 (2019) 1 [1806.10122]. [18] S. Alam, C. Arnold, A. Aviles, R. Bean, Y.-C. Cai, M. Cautun et al., Towards testing the theory of gravity with DESI: summary statistics, model predictions and future simulation requirements, J. Cosmology Astropart. Phys. 2021 (2021) 050 [ 2011.05771]."},{"citing_arxiv_id":"2404.03002","ref_index":76,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Early Data Release of the Dark Energy Spectroscopic Instrument , arXiv e-prints (2023) arXiv:2306.06308 [2306.06308]. [74] K. Koyama, Cosmological Tests of Modified Gravity, Rept. Prog. Phys. 79 (2016) 046902 [1504.04623]. [75] A. Joyce, L. Lombriser and F. Schmidt, Dark Energy Versus Modified Gravity, Ann. Rev. Nucl. Part. Sci. 66 (2016) 95 [ 1601.06133]. [76] M. Ishak, Testing General Relativity in Cosmology, Living Rev. Rel. 22 (2019) 1 [1806.10122]. [77] S. Alam, C. Arnold, A. Aviles, R. Bean, Y.-C. Cai, M. Cautun et al., Towards testing the theory of gravity with DESI: summary statistics, model predictions and future simulation requirements, J. Cosmology Astropart. Phys. 2021 (2021) 050 [ 2011.05771]."}],"limit":50,"offset":0}