{"total":11,"items":[{"citing_arxiv_id":"2605.11703","ref_index":231,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GW240925 and GW250207: Astrophysical Calibration of Gravitational-wave Detectors","primary_cat":"gr-qc","submitted_at":"2026-05-12T07:58:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"The first informative astrophysical calibration of gravitational-wave detectors is reported using GW240925 and GW250207.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"and efficiency for spinning nonprecessing binary black holes, Phys. Rev. D108, 124035 (2023), arXiv:2303.18039 [gr-qc]. [230] R. Abbottet al.(LIGO Scientific Collaboration, Virgo Col- laboration), Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational-wave transient cat- alog, Phys. Rev. D103, 122002 (2021), arXiv:2010.14529 [gr- qc]. [231] E. M. S ¨angeret al., Tests of General Relativity with GW230529: a neutron star merging with a lower mass-gap compact object, arXiv e-prints (2024), arXiv:2406.03568 [gr- qc]. [232] A. Pai and K. G. Arun, Singular value decomposition in parametrised tests of post-Newtonian theory, Classical Quan- tum Gravity30, 025011 (2013), arXiv:1207.1943 [gr-qc]."},{"citing_arxiv_id":"2605.04224","ref_index":53,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Black-Hole Scattering in Einstein-scalar-Gauss-Bonnet: Numerical Relativity Meets Analytics","primary_cat":"gr-qc","submitted_at":"2026-05-05T19:08:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Numerical relativity simulations of black hole scattering in Einstein-scalar-Gauss-Bonnet gravity agree closely with effective-one-body analytic predictions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"i up to 3PM order are given by [51, 52] αi =− λ µ2 i , βi = dαi dφ φ0 =− 2λ2 µ4 i , β′ i = dβi dφ φ0 =− 8λ3 µ6 i ,(2) with{µ i}i=1,2 being the irreducible BH masses. The most stringent observational bound on EsGB the- ory comes from comparing the black hole-neutron star GW signal GW230529 to PN results and give a con- straint of √ λ≲0.75 km [53]. For comparison, assuming an equal-mass system with the component BH masses being 3.6M ⊙ (the smallest BH observed so far [54]), the highest coupling value considered here is √ λ∼1.9 km, which is above the observational constraints but remains within the same order of magnitude (see [33] for further details). 2 We setφ 0 = 0, appropriate for asymptotically flat spacetimes as"},{"citing_arxiv_id":"2604.24526","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Tests of scalar polarizations with multi-messenger events","primary_cat":"gr-qc","submitted_at":"2026-04-27T14:27:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of GW170817 with PPE framework and EM polarization constraints shows mild preference for scalar mode in quadrupole harmonics and improves bounds on non-GR parameters by up to 60%.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"inspiral and taper toward merger-ringdown; the leading −1PN parameterδϕ −2 captures possible indirect dipole ra- diation. Other parameterized tests, such as [60, 61], do arXiv:2604.24526v1 [gr-qc] 27 Apr 2026 2 include extra polarizations with waveforms motivated by specific gravity theories. This is the approach that will be used in this paper. Alternatively, in [26, 54, 56], the null-stream method forms linear combinations of detector outputs that can- cel the GR tensor modes, so any residual indicates non- tensor polarizations. This approach is model-independent and does not assume a specific waveform, but it does not use full alternative-polarization waveforms; residuals are treated phenomenologically, so constraints depend on de-"},{"citing_arxiv_id":"2604.09350","ref_index":136,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Gravitational Memory from Hairy Binary Black Hole Mergers","primary_cat":"gr-qc","submitted_at":"2026-04-10T14:22:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Gravitational memory from hairy binary black hole mergers in scalar-Gauss-Bonnet gravity differs from GR by a few percent due to altered nonlinear dynamics, with direct scalar contributions suppressed, and including memory increases GR-sGB mismatch by more than an order of magnitude.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"happens when the two black holes are close to but be- low the point of spontaneous scalarization when isolated. However, if put in a binary, a scalar field can develop when the distance between the two black holes decreases below a certain threshold (the effect resembles well the dynamical scalarization of neutron stars in pure scalar- tensor theories [136, 137]). It is clear then that the GR initial data are the true quasi-stationary solution when the two black holes are far away from each other. The most stringent observational bound on shift- symmetric sGB gravity comes from comparing the black hole-neutron star GW signal GW230529 to Post- Newtonian results for EsGB and give a constraint of√ λ≲0.75 km [138]."},{"citing_arxiv_id":"2604.08668","ref_index":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Minimum mass, maximum charge and hyperbolicity in scalar Gauss-Bonnet gravity","primary_cat":"gr-qc","submitted_at":"2026-04-09T18:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In scalar Gauss-Bonnet gravity, black hole solutions below a tunable minimum mass lose hyperbolicity in perturbations, corresponding to EFT breakdown, but scalar charge stays bounded above.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Sotiriou, L. Gualtieri, J. Sakstein, and E. Berti, Stability of scalarized black hole solutions in scalar-Gauss-Bonnet gravity, Phys. Rev. D 99, 064011 (2019), arXiv:1812.05590 [gr-qc]. [51] S¨ anger, Elise M. and others, Tests of General Relativity with GW230529: a neutron star merging with a lower mass-gap compact object, (2024), arXiv:2406.03568 [gr- qc]. [52] P. Kanti, N. E. Mavromatos, J. Rizos, K. Tamvakis, and E. Winstanley, Dilatonic black holes in higher curvature string gravity. 2: Linear stability, Phys. Rev. D57, 6255 (1998), arXiv:hep-th/9703192."},{"citing_arxiv_id":"2604.02214","ref_index":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quadratic gravity corrections to scalar QNMs of rapidly rotating black holes","primary_cat":"gr-qc","submitted_at":"2026-04-02T16:06:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Leading-order deviations from general relativity in scalar quasinormal modes of rotating black holes are computed numerically up to dimensionless spins of 0.99 in quadratic-curvature scalar-tensor theories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.18615","ref_index":107,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Two Parameter Deformation of Embedding Class-I Compact Stars in Linear $f(Q)$ Gravity","primary_cat":"gr-qc","submitted_at":"2026-02-20T21:09:23+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A controlled two-parameter deformation in linear f(Q) gravity with gravitational decoupling enlarges the stellar mass window for compact objects while satisfying causality and regularity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.13173","ref_index":95,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Plunge-Merger-Ringdown Tests of General Relativity with GW250114","primary_cat":"gr-qc","submitted_at":"2026-01-19T15:57:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GW250114 data constrains GR deviations in merger amplitude to 10% and frequency to 4% at 90% CL, with first bounds on the (4,4) mode frequency at 6%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.16879","ref_index":72,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Accelerating parameter estimation for parameterized tests of general relativity with gravitational-wave observations","primary_cat":"gr-qc","submitted_at":"2025-11-21T01:08:52+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Relative binning accelerates TIGER parameterized GR tests by factors of 10-100 while recovering unbiased posteriors on simulated signals and real events like GW150914.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.11793","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black hole mergers beyond general relativity: a self-force approach","primary_cat":"gr-qc","submitted_at":"2025-10-13T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Self-force theory is extended to compute merger and ringdown waveforms in beyond-GR black hole binaries under the extreme mass-ratio approximation, with first calculations of self-force corrections to the merger waveform.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"GW230529: a neutron star merging with a lower mass- gap compact object, (2024), arXiv:2406.03568 [gr-qc]. [10] E. Bertiet al., Testing General Relativity with Present and Future Astrophysical Observations, Class. Quant. Grav.32, 243001 (2015), arXiv:1501.07274 [gr-qc]. [11] E. Barausseet al., Prospects for Fundamental Physics with LISA, Gen. Rel. Grav.52, 81 (2020), arXiv:2001.09793 [gr-qc]. [12] S. E. Perkins, N. Yunes, and E. Berti, Probing Fundamen- tal Physics with Gravitational Waves: The Next Genera- tion, Phys. Rev. D103, 044024 (2021), arXiv:2010.09010 [gr-qc]. [13] K. G. Arunet al.(LISA), New horizons for fundamen- tal physics with LISA, Living Rev. Rel.25, 4 (2022), arXiv:2205.01597 [gr-qc]. [14] S. Vagnozziet al., Horizon-scale tests of gravity theories"},{"citing_arxiv_id":"2509.08099","ref_index":144,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black Hole Spectroscopy and Tests of General Relativity with GW250114","primary_cat":"gr-qc","submitted_at":"2025-09-09T19:17:32+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GW250114 data confirm the remnant is consistent with a Kerr black hole and bound the dominant quadrupolar mode frequency to within a few percent of the GR prediction, with constraints tighter than prior multi-event catalogs.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"22 andδˆτ220 =−0.14 +0.25 −0.23, while the 440 mode remains unconstrained. While less stringent thanpSEOBNR, this analysis quantifies the constraints achievable when isolat- ing the remnant's relaxation. The stringentpSEOBNRresults can improve current con- straints on gravity theories beyond GR [139-143], and constrain properties of exotic compact objects [144, 145]. As a concrete example, we consider dynamical Chern- Simons (dCS) gravity [146], a parity-violating extension of GR in which the QNM spectrum receives corrections controlled by a coupling length √αdCS [147]. Mapping the bound on the 220 QNM frequency to the predicted dCS correction yields an approximate constraint on the dCS coupling length of √αdCS <32."}],"limit":50,"offset":0}