{"total":21,"items":[{"citing_arxiv_id":"2607.02017","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Boson Stars in Teleparallel Gravity with a Nonminimally Coupled Field: The Violation of Energy Conditions and Gravitational Waveforms from EMRIs","primary_cat":"gr-qc","submitted_at":"2026-07-02T10:49:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Boson stars in teleparallel gravity with nonminimal coupling show negative energy density and energy-condition violation in excited states, with EMRI waveforms potentially detectable by LISA.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31299","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.21826","ref_index":88,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"produced by an independently conserved DE fluid, but by a different way in which cosmic acceleration is encoded in the field equations (Carroll et al. 2004; Clifton et al. 2012). In non-minimally coupled scalar-field scenarios, the relation among matter, spacetime geometry, and the scalar degree of freedom differs from that in minimally coupled DE within general relativity (Gubitosi et al. 2013; Koyama 2016; Cai et al. 2016; Ishak 2019). When these theories are rewritten in an effective general-relativistic form, the additional terms can be absorbed into an effective DE density and pressure, leadingtoanapparentevolutionof𝑤(𝑎)(Chudaykin&Kunz 2024;Yangetal.2024;Yeetal.2025;Tauleetal.2025;Ishak et al. 2025; Wolf et al. 2025b; Pan & Ye 2026). Moreover, a departure fromΛCDM does not necessarily"},{"citing_arxiv_id":"2606.12521","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Matter with a Drag at Low Redshift","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"iDCDM adds two parameters to LambdaCDM so that dark matter decay produces late-time interacting radiation, yielding a distinctive low-redshift suppression of structure growth while leaving BBN and primary CMB unchanged.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10597","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.04077","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lagrangian Extensions of Newtonian Gravity constrained by Solar System tests","primary_cat":"gr-qc","submitted_at":"2026-06-02T17:11:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Derives post-Newtonian equations from a scalar-extended Newtonian Lagrangian and bounds its free parameter with Solar System observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27301","ref_index":183,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22599","ref_index":4,"ref_count":1,"confidence":0.98,"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":"2605.04154","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Master Equation for Screening in Luminal Horndeski Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-05T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A master screening equation is derived for luminal Horndeski gravity that recovers Vainshtein and Chameleon mechanisms and introduces Phaedrus screening with screening radius scaling linearly with source mass.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Results And Evidence For Evolving Dark Energy With An Updated Type Ia Supernova Calibration,\" arXiv:2511.07517 [astro-ph.CO]. [3] K. Koyama, \"Cosmological Tests of Modified Gravity,\"Rept. Prog. Phys.79(2016) no. 4, 046902,arXiv:1504.04623 [astro-ph.CO]. [4] P. G. Ferreira, \"Cosmological Tests of Gravity,\"Ann. Rev. Astron. Astrophys.57(2019) 335-374, arXiv:1902.10503 [astro-ph.CO]. [5]DESICollaboration, M. Abdul Karimet al., \"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints,\"arXiv:2503.14738 [astro-ph.CO]. [6]DESICollaboration, K. Lodhaet al., \"Extended Dark Energy analysis using DESI DR2 BAO measurements,\" arXiv:2503.14743 [astro-ph.CO]. [7]DESICollaboration, W. Elberset al., \"Constraints on"},{"citing_arxiv_id":"2604.16564","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Observational tests of \\texorpdfstring{$\\Lambda(t)$}{Lambda(t)} cosmology in light of DESI DR2","primary_cat":"physics.gen-ph","submitted_at":"2026-04-17T10:06:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"MCMC constraints on two Lambda(t) models with DESI DR2, CC, and Pantheon+ data yield H0 ~72.5-73 km/s/Mpc, Omega_m0 near standard values in joint fits, and n~0.3 indicating mild deviation from LambdaCDM.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder,\"Astrophys. J.973(2024) no. 1, 30, arXiv:2404.08038 [astro-ph.CO]. [22] K. K. Rogers and V . Poulin, \"5σtension between Planck cosmic microwave background and eBOSS Lyman-alpha forest and constraints on physics beyond ΛCDM,\"Phys. Rev. Res.7(2025) no. 1, L012018, arXiv:2311.16377 [astro-ph.CO]. [23] Ruchika, L. Perivolaropoulos, and A. Melchiorri, \"Effects of a local physics change on the SH0ES determination of H0,\"Phys. Rev. D111(2025) no. 12, 123526,arXiv:2408.03875 [astro-ph.CO]. [24] M. Lopez-Corredoira, F. Melia, J. J. Wei, and C. Y. Gao, \"Age of Massive Galaxies at Redshift 8,\"Astrophys. J. 970(2024) no. 1, 63,arXiv:2405.12665 [astro-ph."},{"citing_arxiv_id":"2603.23634","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Testing Dark Energy with Black Hole Ringdown","primary_cat":"gr-qc","submitted_at":"2026-03-24T18:20:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dynamical dark energy imprints O(1) shifts on black hole quasi-normal modes via cosmological hair, enabling constraints at 10^{-2} (LVK) to 10^{-4} (LISA) precision using the cubic Galileon as example.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"freedom with non-trivial time dependence - see [9-14] for reviews. This time dependence naturally gives rise to cos- mological hair in the context of black hole solutions, i.e. the local black hole physics is no longer controlled by just the mass, spin and charge of the black hole (as in GR/ΛCDM), but also impacted by the dynamical dark energy field, see e.g. [15, 16]. Yet, until recently, when their stability was fully investigated, all such known solutions were found to be un- stable [16-25]. This changed with the recent discovery of a stable solution in [26]. Derived in the context of the cubic Galileon [27] - an illustrative theory sharing key characteris- tics of much wider classes of scalar-tensor theories - this solu-"},{"citing_arxiv_id":"2603.22398","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Stable black hole solutions with cosmological hair","primary_cat":"gr-qc","submitted_at":"2026-03-23T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Stable black hole solutions with cosmological scalar hair are explicitly derived in the cubic Galileon theory, recovering cosmological behavior at large distances and regular short-range dynamics.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"513(2012) 1-189, arXiv:1106.2476 [astro-ph.CO]. [15] E. O. Babichev, V . I. Dokuchaev, and Y . N. Eroshenko, \"Black holes in the presence of dark energy,\"Phys. Usp.56(2013) 1155-1175,arXiv:1406.0841 [gr-qc]. [16] A. Joyce, B. Jain, J. Khoury, and M. Trodden, \"Beyond the Cosmological Standard Model,\"Phys. Rept.568(2015) 1-98, arXiv:1407.0059 [astro-ph.CO]. [17] K. Koyama, \"Cosmological Tests of Modified Gravity,\"Rept. Prog. Phys.79(2016) no. 4, 046902,arXiv:1504.04623 [astro-ph.CO]. [18] T. Kobayashi, \"Horndeski theory and beyond: a review,\"Rept. Prog. Phys.82(2019) no. 8, 086901,arXiv:1901.07183 [gr-qc]. 29 [19] T. Jacobson, \"Primordial black hole evolution in tensor scalar cosmology,\"Phys. Rev. Lett.83(1999) 2699-2702,"},{"citing_arxiv_id":"2602.03110","ref_index":28,"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":"background","top_context_polarity":"background","context_text":"-S. Xue, and X. Zhang, JCAP 07, 005 (2021), arXiv:2101.10714 [astro-ph.CO]. 11 [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."},{"citing_arxiv_id":"2601.05145","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"How deep can a cosmic void be? Voids-informed theoretical bounds in Galileon gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-01-08T17:32:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Galileon models must obey a void-depth limit tied to expansion history to avoid force breakdowns, excluding ~60% of a linear parameterization's space by z less than or equal to 10.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.03314","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"EFT of Dark Energy with Cosmic Chronometers: Reconstructing Background EFT Functions","primary_cat":"astro-ph.CO","submitted_at":"2025-12-02T23:54:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reconstruction of EFT background functions from cosmic chronometer Hubble data allows model-independent tests of dark energy evolution in scalar-tensor theories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.08972","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2508.19106","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tracing Signatures of Modified Gravity in Redshift-Space Galaxy Bispectrum Multipoles: Prospects for Euclid","primary_cat":"astro-ph.CO","submitted_at":"2025-08-26T15:10:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"In Hu-Sawicki f(R) gravity the redshift-space bispectrum monopole and quadrupole show 2-8% deviations from GR at z=0.7 and k~0.3 h/Mpc with forecasted SNR of 30 and 15 for Euclid.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"son, JCAP08, 010, arXiv:1211.7054 [astro-ph.CO]. [16] G. Gubitosi, F. Piazza, and F. Vernizzi, JCAP02, 032, arXiv:1210.0201 [hep-th]. [17] G. W. Horndeski, Int. J. Theor. Phys.10, 363 (1974). [18] M. Crisostomi, M. Hull, K. Koyama, and G. Tasinato, JCAP03, 038, arXiv:1601.04658 [hep-th]. [19] D. Langlois and K. Noui, JCAP07, 016, arXiv:1512.06820 [gr-qc]. [20] M. Crisostomi, K. Koyama, and G. Tasinato, JCAP04, 044, arXiv:1602.03119 [hep-th]. [21] T. P. Sotiriou and V. Faraoni, Rev. Mod. Phys.82, 451 (2010), arXiv:0805.1726 [gr-qc]. [22] F. S. N. Lobo, J. Phys. Conf. Ser.600, 012006 (2015), arXiv:1412.0867 [gr-qc]. [23] E. V. Linder, Phys. Rev. D81, 127301 (2010), [Erratum: Phys.Rev.D 82, 109902 (2010)], arXiv:1005."},{"citing_arxiv_id":"2411.12022","ref_index":15,"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":"A common and promising approach to testing deviations from general relativity (GR) is to add physically motivated phenomenological parameters to the perturbed Einstein's gravita- tional field equations and test the deviations of such parameters from their GR predicted values. Whilst many such modified-gravity (MG) parameterisations have been proposed in the literature (see e.g. the reviews [15, 17, 204] and references therein), we focus here on one that is based on the coupling of gravitational potentials to the source content of spacetime. In the conformal Newtonian gauge, the flat Friedmann-Lemaˆ ıtre-Robertson-Walker met- ric with scalar perturbations can be written as ds2 = a(τ)2[−(1 + 2Ψ)dτ 2 + (1 − 2Φ)δijdxidxj], (5.1) where Ψ and Φ are two gravitational potentials, τ is the conformal time, xi and xj are spatial"},{"citing_arxiv_id":"2404.03002","ref_index":74,"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":"Rashkovetskyi, C. Saulder, J.N. Aguilar, S. Ahlen et al., First detection of the BAO signal from early DESI data , MNRAS 525 (2023) 5406 [ 2304.08427]. [73] DESI Collaboration, A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, G. Aldering et al., The 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."},{"citing_arxiv_id":"2312.01406","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutron stars more compact than black holes as a probe of strong-field gravity","primary_cat":"gr-qc","submitted_at":"2023-12-03T14:09:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Stable neutron-star configurations denser than black holes exist in quasi-topological gravity and may produce detectable gravitational-wave echoes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}