{"total":15,"items":[{"citing_arxiv_id":"2606.31350","ref_index":27,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Compactness Inference in Gravitational-Wave Mergers with PhenomDECO: Catalog Benchmarks and Robustness Diagnostics","primary_cat":"gr-qc","submitted_at":"2026-06-30T08:47:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Compactness inference on GWTC-3 events confirms consistency with binary black hole sources after frequency-cut diagnostics show low-compactness modes are noise artifacts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28716","ref_index":163,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Eccentric and unbound compact binaries in the LIGO-Virgo-KAGRA catalog: parameter estimation and waveform systematics with SEOBNRv6EHM","primary_cat":"gr-qc","submitted_at":"2026-05-27T16:38:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SEOBNRv6EHM reduces parameter biases for eccentric binaries versus prior models and shows mild support for eccentricity in five catalog events plus comparable unbound fits for three high-mass events.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"black hole simulations with unequal masses,Phys. Rev. Research.1(2019) 033015 [1905.09300]. [162] J. E. Thompson, E. Hamilton, L. London, S. Ghosh, P. Kolitsidou, C. Hoy et al.,PhenomXO4a: a phenomenological gravitational-wave model for precessing black-hole binaries with higher multipoles and asymmetries, Phys. Rev. D109(2024) 063012 [2312.10025]. [163] S. Bini, K. Kr 'ol, K. Chatziioannou and M. Isi,Impact of waveform systematics and Gaussian noise on the interpretation of GW231123,Phys. Rev. D113(2026) 083036 [2601.09678]. [164] H. Baumgardt and M. Hilker,A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters,Mon. Not. Roy. Astron. Soc."},{"citing_arxiv_id":"2605.27500","ref_index":85,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraining Gravitational Wave Memory with Hierarchical Inference","primary_cat":"gr-qc","submitted_at":"2026-05-26T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hierarchical Bayesian inference on GWTC-5.0 constrains the memory enhancement factor to 0.26 with large uncertainties consistent with the GR value of 1 and forecasts that 2000 detections are needed for a 1σ constraint away from zero.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16425","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Polarization Birefringence and Waveform Systematics in GW231123","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T15:23:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Analysis of GW231123 with IMRPhenomXPHM, IMRPhenomXO4a and NRSur7dq4 yields no waveform-independent evidence for polarization birefringence, with 90% upper limits on the derived coefficient of 0.378, 0.097 and 0.273 respectively.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.14270","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Fast neural network surrogate for multimodal effective-one-body gravitational waveforms from generically precessing compact binaries","primary_cat":"gr-qc","submitted_at":"2026-04-15T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Neural network surrogate approximates precessing compact binary gravitational waveforms up to 1000x faster than the base EOB model with validated accuracy.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"state-of-the-art effective-one-body model describing the inspiral, merger and ringdown of quasicircular, precess- ing, black hole binaries, including higher-order multipole modes. Surrogate models are fast, data-driven models designed to accurately predict the output of a slower base model across a fixed region of intrinsic parameter space. Reduced-order modelling techniques [17, 18, 39, 40] are used to reduce the complexity of this task, efficiently representing long time-series data in terms of the min- imal number of parameters that must be interpolated across parameter space. Neural network surrogates are a subclass of reduced order surrogate models that make use of artificial neural networks to perform this interpo- lation [32, 41-43]."},{"citing_arxiv_id":"2604.13182","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Bilinear products and the orthogonality of quasinormal modes on hyperboloidal foliations","primary_cat":"gr-qc","submitted_at":"2026-04-14T18:05:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bilinear products for black hole quasinormal modes on hyperboloidal foliations are divergent due to CPT transformations but can be regularized to define orthogonal modes and excitation coefficients.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In this context, the calculation of QNM excitation coefficients is obtained via finite computations carried out directly across the entire black hole exterior region [38-40]. In a broader perspective, the hyperboloidal framework arises within the context of conformal methods in general relativity, which are particularly suited for the rigorous treatment of spacetime infinities [41]. Conformal methods have become central to general relativity, providing funda- mental insights into the geometry of black hole horizons, the nature of singularities, and the global causal structure of spacetime [42]. Beyond their mathematical elegance, they also provide powerful geometrical tools for formu- lating black hole perturbation theory in a fully regular"},{"citing_arxiv_id":"2604.08179","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GW231123: False Massive Graviton Signatures from Unmodeled Point-Mass Lensing","primary_cat":"gr-qc","submitted_at":"2026-04-09T12:35:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Unmodeled point-mass lensing produces a spurious nonzero graviton mass posterior in GW231123 that vanishes when lensing is included in the analysis.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"controlled injection-recovery studies. Using an unlensed IMRPhenomXPHM template augmented by a massive- graviton propagation term, we find an apparent nonzero graviton-mass posterior. Once point-mass lensing is in- cluded, however, this preference disappears. Moreover, with lensing included, the inferences obtained with IMR- PhenomXPHM, IMRPhenomXO4a [20], and NRSur7dq4 become mutually consistent and show no evidence for nonzero graviton mass. This indicates that the appar- ent graviton-mass signal is more naturally explained by unmodeled lensing than by modified propagation. We then turn this interpretation into a controlled test. We construct a GW231123-like injection using the maximum-posterior parameters from a lensed NR-"},{"citing_arxiv_id":"2604.07388","ref_index":36,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GW190711_030756 and GW200114_020818: astrophysical interpretation of two asymmetric binary black hole mergers in the IAS catalog","primary_cat":"astro-ph.HE","submitted_at":"2026-04-08T05:45:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Two asymmetric BBH mergers are characterized with mass ratios 0.35 and ≤0.20; one shows high spins, negative χ_eff, and strong precession, suggesting an emerging population of massive rapidly spinning systems.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"the dominant and subdominant harmonic modes of precess- ing binary black holes,\" Phys. Rev. D103, 104056 (2021), arXiv:2004.06503 [gr-qc]. [35] Hang Yu, Javier Roulet, Tejaswi Venumadhav, Barak Zackay, and Matias Zaldarriaga, \"Accurate and efficient waveform model for precessing binary black holes,\" Phys. Rev. D108, 064059 (2023), arXiv:2306.08774 [gr-qc]. [36] Jonathan E. Thompson, Eleanor Hamilton, Lionel London, Shrobana Ghosh, Panagiota Kolitsidou, Charlie Hoy, and Mark Hannam, \"PhenomXO4a: a phenomenological gravitational- wave model for precessing black-hole binaries with higher multipoles and asymmetries,\" Phys. Rev. D109, 063012 (2024), arXiv:2312.10025 [gr-qc]. [37] Eleanor Hamiltonet al., \"PhenomXPNR: An improved grav-"},{"citing_arxiv_id":"2601.23019","ref_index":179,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Toward claiming a detection of gravitational memory","primary_cat":"gr-qc","submitted_at":"2026-01-30T14:27:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A framework using scale separation in the Isaacson description defines observable gravitational memory rise for compact binary coalescences, providing a basis for hypothesis testing in LISA data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.13173","ref_index":72,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2601.09678","ref_index":33,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The impact of waveform systematics and Gaussian noise on the interpretation of GW231123","primary_cat":"gr-qc","submitted_at":"2026-01-14T18:22:32+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The high mass and high spin magnitudes inferred for GW231123 using NRSur7dq4 are robust to waveform systematics and Gaussian noise.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.17550","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GW231123: Overlapping Gravitational Wave Signals?","primary_cat":"gr-qc","submitted_at":"2025-12-19T13:13:49+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GW231123 data favors an overlapping two-signal model over a single merger with Bayes factors of 100-10000, mitigating waveform-dependent discrepancies and suggesting possible gravitational lensing.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.16113","ref_index":168,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary","primary_cat":"gr-qc","submitted_at":"2025-10-17T18:00:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.08054","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GW250114: testing Hawking's area law and the Kerr nature of black holes","primary_cat":"gr-qc","submitted_at":"2025-09-09T18:00:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GW250114 data confirm the remnant black hole ringdown frequencies lie within 30% of Kerr predictions and that the final horizon area is larger than the sum of the progenitors' areas to high credibility.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The Shadow of the Su- permassive Black Hole, Astrophys. J. Lett.875, L1 (2019), arXiv:1906.11238 [astro-ph.GA]. [55] K. Akiyamaet al.(Event Horizon Telescope), First Sagittar- ius A* Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way, Astrophys. J. Lett.930, L12 (2022), arXiv:2311.08680 [astro- ph.HE]. [56] A. M. Ghezet al., Measuring Distance and Properties of the Milky Way's Central Supermassive Black Hole with Stel- lar Orbits, Astrophys. J.689, 1044 (2008), arXiv:0808.2870 [astro-ph]. [57] S. Gillessen, F. Eisenhauer, S. Trippe, T. Alexander, R. Gen- zel, F. Martins, and T. Ott, Monitoring stellar orbits around the Massive Black Hole in the Galactic Center, Astrophys."},{"citing_arxiv_id":"2505.23895","ref_index":280,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Black hole spectroscopy: from theory to experiment","primary_cat":"gr-qc","submitted_at":"2025-05-29T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review summarizing the state of the art in black hole quasinormal modes, ringdown waveform modeling, current LIGO-Virgo-KAGRA observations, and prospects for LISA and next-generation detectors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"approach was later extended to Kerr, and applied to compute perturbative corrections to the Kerr frequencies [71, 94, 200, 201]. Later, motivated by the practicalities of GW signal modeling, situations in which the Kerr QNM spheroidal harmonics are complete have been pointed out [35], and this motivates special functions which enable QNM orthogonality over the solid angle [280-283]. More recently, a product under which the Kerr QNMs display full spatial orthogonality was presented [284]. A notable technical complication in the definition of Kerr QNM products arises from 2. The quasinormal mode spectrum in general relativity 44 r r+r− 𝒞 Figure 2.11. Integration contour for QNM products (C, solid black line) in the Boyer-Lindquist coordinate r."}],"limit":50,"offset":0}