{"total":15,"items":[{"citing_arxiv_id":"2606.20794","ref_index":4,"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":6.0,"formal_verification":"none","one_line_summary":"ACG models embed the observationally preferred phantom-crossing dark energy behavior inside a consistent Horndeski Lagrangian and achieve data fits of similar quality to w0waCDM while being narrowed by perturbative probes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27727","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reconstructing ACT-compatible and GW170817-compatible Einstein-Gauss-Bonnet Inflation from the Observational Indices","primary_cat":"gr-qc","submitted_at":"2026-05-26T22:02:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Four Einstein-Gauss-Bonnet inflationary models are reconstructed from a chosen tensor-to-scalar ratio and shown to satisfy ACT and GW170817 constraints including scalar perturbation amplitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16132","ref_index":185,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nucleosynthesis in the fast ejecta of a neutron star merger","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T16:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13036","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inspiral gravitational waveforms from charged compact binaries with scalar hair","primary_cat":"gr-qc","submitted_at":"2026-05-13T05:44:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In Einstein-scalar-Maxwell theories, charged compact binaries produce gravitational waveforms containing a leading -1 post-Newtonian dipole correction controlled by one deviation parameter b.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"extremely close to that of light, thereby placing tight restrictions on dark energy models [7-11]. Subsequent GW detections, such as the BH-NS merger GW200115 [ 12], have further enriched both the observational and theoretical landscape. At the same time, some events have exhibited features that may hint at the presence of exotic compact objects (ECOs) beyond standard BHs and NSs. For instance, the event GW190521 [ 13], characterized by its short duration and unusual waveform morphology, has been interpreted as a possible merger involving nonstandard compact objects such as boson stars. In addition, events like GW190814 [ 14] and GW230529 [ 15], which involve compact objects with masses in the so-called mass gap between NSs and BHs, may also point toward the existence"},{"citing_arxiv_id":"2605.04154","ref_index":77,"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":"54 (2022) no. 10, 133,arXiv:2207.10096 [gr-qc]. [75] T. Bakeret al., \"Measuring the propagation speed of gravitational waves with LISA,\"arXiv:2203.00566 [gr-qc]. [76] T. Baker, E. Barausse, A. Chen, C. de Rham, M. Pieroni, and G. Tasinato, \"Testing gravitational wave propagation with multiband detections,\"JCAP03(2022) 044, arXiv:2209.14398 [gr-qc]. [77] S. Sirera and J. Noller, \"Testing the speed of gravity with black hole ringdowns,\"Phys. Rev. D107(2023) no. 12, 124054,arXiv:2301.10272 [gr-qc]. [78] B. Atkins, A. Malhotra, and G. Tasinato, \"Novel probe of graviton dispersion relations at nanohertz frequencies,\"Phys. Rev. D110(2024) no. 12, 124018,arXiv:2408.10122 [gr-qc]. [79] P. Creminelli and F."},{"citing_arxiv_id":"2604.16531","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"AI--Assisted Exploration: DHOST Theories without Quantum Ghosts","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T18:15:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"In DHOST theories with Gauss-Bonnet and Weyl operators, gauge symmetry invariance conditions are identical to Hamiltonian constraints eliminating ghosts.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Jimenez,The parameter space of cubic Galileon models for cosmic acceleration,Physics of the Dark Universe2(2013) 179 [1306.1262]. [9] E. Bellini, R. Jimenez and L. Verde,Signatures of Horndeski gravity on the dark matter bispectrum,JCAP2015(2015) 057 [1504.04341]. [10] E. Bellini, A.J. Cuesta, R. Jimenez and L. Verde,Constraints on deviations fromΛCDM within Horndeski gravity,JCAP2016(2016) 053 [1509.07816]. [11] T. Baker, E. Bellini, P.G. Ferreira, M. Lagos, J. Noller and I. Sawicki,Strong Constraints on Cosmological Gravity from GW170817 and GRB 170817A,PRL119(2017) 251301 [1710.06394]. [12] G.W. Horndeski,Second-order scalar-tensor field equations in a four-dimensional space,Int. J. Theor. Phys.10(1974) 363. [13] C. Deffayet and D.A. Steer,A formal introduction to Horndeski and Galileon theories and their"},{"citing_arxiv_id":"2602.00422","ref_index":66,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Jacobson's thermodynamic approach to classical gravity applied to non-Riemannian geometries: remarks on the simplicity of Nature","primary_cat":"gr-qc","submitted_at":"2026-01-31T00:19:38+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.05145","ref_index":50,"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":"2512.20553","ref_index":88,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eckart heat-flux applicability in $F(\\Phi,X)R$ theories and the existence of temperature gradients","primary_cat":"gr-qc","submitted_at":"2025-12-23T17:51:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Eckart heat flux holds for all timelike scalar configurations in F(Φ,X)R + G theories if and only if F_X ≡ 0, reducing the theory to a Jordan-like subclass of Horndeski.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.08972","ref_index":51,"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":"2412.20664","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Enhancing Early Detection and Localization of Gravitational Waves via Eccentricity-Induced Higher Harmonic Modes with 2G Detector Networks","primary_cat":"gr-qc","submitted_at":"2024-12-30T02:47:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Eccentricity-induced higher harmonics allow binary neutron star gravitational wave signals to reach detection thresholds and achieve useful localization several minutes earlier in 2G detector networks than circular signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2112.06861","ref_index":81,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Tests of General Relativity with GWTC-3","primary_cat":"gr-qc","submitted_at":"2021-12-13T18:19:04+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"No evidence for physics beyond general relativity is found in the analysis of 15 GW events from GWTC-3, with consistency in residuals, PN parameters, and remnant properties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"This joint detection also has been used to constrain the number of space-time dimensions [ 9, 80]. Results on the measure- ment of the properties of the merger remnant from ringdown, bounds on spin-induced quadrupole moment of compact bi- nary constituents and the outcome of the search for echoes have implications for models of black hole mimickers [81]. This paper analyzes events reported during the second half of the third observing run of LIGO and Virgo (O3b) [82], ex- tending our previous analysis [11] which reported the status of the bounds up to and including the first half of the third observing run (O3a). This paper also provides joint bounds combining the events that occurred during the first three ob-"},{"citing_arxiv_id":"2010.14529","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2020-10-27T18:01:34+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No evidence for deviations from general relativity is found in LIGO-Virgo binary black hole events, with improved constraints on waveform parameters, graviton mass, and ringdown properties.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"ments of strong gravitational fields, large spacetime curvature, and velocities comparable to the speed of light; high post- Newtonian (PN) order calculations and numerical relativity (NR) simulations are required to accurately model the emitted GW signal [5, 6, 14, 15]. We report results from tests of GR on binary black hole (BBH) signals using the second Gravitational-wave Transient catalog (GWTC-2) [16]. The GWTC-2 catalog includes all observations reported in the first catalog (GWTC-1) [17], cov- ering the first (O1) and second (O2) observing runs, as well as new events identified in the first half of the third observ- ing run (O3a) of the Advanced LIGO and Advanced Virgo detectors [16]. We focus on the most significant signals, requir- ing them to have been detected with a false-alarm rate (FAR)"},{"citing_arxiv_id":"1907.08010","ref_index":120,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological searches for the neutrino mass scale and mass ordering","primary_cat":"astro-ph.CO","submitted_at":"2019-07-18T12:03:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Thesis summarizing an upper limit of 0.12 eV on the neutrino mass sum, bias calibration via CMB lensing cross-correlations, and tighter limits plus stronger normal-ordering preference in non-phantom dynamical dark energy models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1807.06209","ref_index":33,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The Planck result is therefore sensitive to the details of the polarization modelling at the 0 .5 σ level, and the tension cannot be quantified robustly beyond this level. Combining DES with the baseline Planck likelihood pulls the Planck result to lower Ωm and slightly lower σ8, giving S 8 = 0.811± 0.011, Ωm = 0.3040± 0.0060, σ8 = 0.8062± 0.0057,  68 %, Planck TT,TE,EE +lowE+lensing+DES. (33) A similar shift is seen without including Planck lensing, and is disfavoured by Planck CMB with a total∆χ2 eff≈ 13 for the CMB 30 Planck Collaboration: Cosmological parameters likelihoods (comparing the Planck-only best fit to the fit when combined with DES). The shift in parameters is also larger than would be expected for Gaussian distributions, given the small"}],"limit":50,"offset":0}