{"total":16,"items":[{"citing_arxiv_id":"2605.16492","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dynamical quasinormal mode excitation II: propagation and convergence in Schwarzschild","primary_cat":"gr-qc","submitted_at":"2026-05-15T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Refined propagation prescription for quasinormal modes excited by plunging particles confirms a bounce radius at r_*=0 and yields accurate reproduction of the post-bounce oscillatory waveform component from first principles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.15431","ref_index":124,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms","primary_cat":"gr-qc","submitted_at":"2026-04-16T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dynamical parameters.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"(2007), arXiv:0705.2519 [gr-qc]. [121] W. Del Pozzo and A. Nagar, Phys. Rev. D95, 124034 (2017), arXiv:1606.03952 [gr-qc]. [122] R. Cotesta, A. Buonanno, A. Boh' e, A. Taracchini, I. Hin- der, and S. Ossokine, Phys. Rev. D98, 084028 (2018), arXiv:1803.10701 [gr-qc]. [123] T. Damour and A. Nagar, Phys. Rev. D90, 044018 (2014), arXiv:1406.6913 [gr-qc]. [124] A. Boh' eet al., Phys. Rev. D95, 044028 (2017), arXiv:1611.03703 [gr-qc]. [125] A. Nagaret al., Phys. Rev. D98, 104052 (2018), arXiv:1806.01772 [gr-qc]. [126] H. Estell' es, A. Ramos-Buades, S. Husa, C. Garc'ia- Quir' os, M. Colleoni, L. Haegel, and R. Jaume, Phys. Rev. D103, 124060 (2021), arXiv:2004.08302 [gr-qc]. [127] H. Estell' es, S. Husa, M."},{"citing_arxiv_id":"2604.11895","ref_index":100,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Novel ringdown tests of general relativity with black hole greybody factors","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GreyRing model based on greybody factors reproduces numerical relativity ringdown signals with mismatches of order 10^{-6} and enables a new post-merger consistency test of general relativity applied to GW250114.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"GreyRingto the Fourier transform of the GW250114 4 56 64 72 80 (1 + z) M [M⊙] 0.2 0.4 0.6 0.8 χ 0.2 0.4 0.6 0.8 χ GreyRing L VK 220tstart = 13M L VK 220+221tstart = 8M FIG. 3.90%credible region of the joint posterior distribu- tion for the redshifted remnant mass and spin of GW250114. The blue contour corresponds to our greybody-factor model applied in the frequency rangef∈[100,512] Hz. The red and green contours show the results of a standard QNM anal- ysis performed withpyRing[75] using the220mode and the220 + 221modes, respectively [23, 71, 74]. Black dashed lines mark the maximum-likelihood estimate from the LIGO- Virgo-KAGRAanalysiswiththeNRSur7dq4inspiral-merger- ringdown waveform model [76]. time series. The resulting posteriors (blue contours) are"},{"citing_arxiv_id":"2604.07388","ref_index":40,"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":"and Mark Hannam, \"Including higher order multipoles in gravitational-wave models for precessing binary black holes,\" Phys. Rev. D101, 024056 (2020), arXiv:1911.06050 [gr-qc]. [39] Andrea Taracchiniet al., \"Effective-one-body model for black- hole binaries with generic mass ratios and spins,\" Phys. Rev. D 89, 061502 (2014), arXiv:1311.2544 [gr-qc]. [40] Alejandro Bohéet al., \"Improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors,\" Phys. Rev. D95, 044028 (2017), arXiv:1611.03703 [gr-qc]. [41] Roberto Cotesta, Alessandra Buonanno, Alejandro Bohé, An- drea Taracchini, Ian Hinder, and Serguei Ossokine, \"Enriching"},{"citing_arxiv_id":"2507.22862","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Parameter Estimation with Targeted Eccentric Numerical-Relativity Simulations for GW200208_22 and GW190620","primary_cat":"gr-qc","submitted_at":"2025-07-30T17:38:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian parameter estimation with targeted eccentric numerical-relativity waveforms yields eccentricity estimates of e20 ≈ 0.2 for GW200208_22 and e10 ≈ 0.19 for GW190620, reinforcing the eccentric hypothesis.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2407.18319","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational wave surrogate model for spinning, intermediate mass ratio binaries based on perturbation theory and numerical relativity","primary_cat":"gr-qc","submitted_at":"2024-07-25T18:19:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"BHPTNRSur2dq1e3 is a new surrogate model for spinning intermediate-mass-ratio black hole binary gravitational waves, constructed from ppBHPT training data with domain decomposition for retrograde modes and calibrated to NR simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2406.03568","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with GW230529: a neutron star merging with a lower mass-gap compact object","primary_cat":"gr-qc","submitted_at":"2024-06-05T18:30:33+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Parameterized inspiral tests on GW230529 find consistency with GR, with |δφ̂_{-2}| ≲ 8×10^{-5} and ℓ_GB ≲ 0.51 M_⊙ in ESGB theories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.14286","ref_index":117,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA","primary_cat":"gr-qc","submitted_at":"2024-04-22T15:37:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Bayesian inference on LVK O1-O3 events with eccentric aligned-spin waveforms yields log10 Bayes factors of 1.77-4.75 favoring eccentricity for GW200129, GW190701 and GW200208_22, and >99.5% probability that at least one of 57 events is eccentric under an astrophysically motivated rate prior.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Remarkably, DINGO yields posterior dis- tributions within O(min - hours) without sacrificing accuracy [115, 116]. However, it is currently limited to GW signals shorter than 16sec. In this study, we employ a set of waveform mod- els from the e ffective-one-body (EOB) family SEOBNR. We use the multipolar aligned-spin quasi-circular model SEOBNRv4HM [117, 118] and the multipolar aligned-spin ec- centric model SEOBNRv4EHM [119, 120] to analyze 57 GW events from the first (O1), second (O2) and third (O3) ob- serving runs of the LVK Collaboration [4, 121, 122]. We find log10 Bayes factors, between the eccentric against quasi- circular hypothesis, greater than 1 for three events. We also do a comprehensive study to understand the impact of glitch sub-"},{"citing_arxiv_id":"2112.06861","ref_index":122,"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":"method","top_context_polarity":"use_method","context_text":"same m index but different ℓ indices. Mode mixing, especially of ℓ = |m| = 2 mode, is expected to be negligible for the modes that we consider here [120]. We present two analyses of ringdown: the time-domain ring- down analysis pyRing [258, 259], based on damped sinusoids, and the parametrized ringdown analysis pSEOB, based on the SEOBNRv4HM waveform model [122]. 1. The pyRing analysis pyRing employs a time-domain approach. The three types of templates used in the analysis areKerr220, Kerr221, and KerrHM. Kerr220 has only the fundamental modes, i.e., ( ℓ, |m|, n) = (2, 2, 0), Kerr221 has the fundamental modes and its first over- tones (both ±m, with the same damping time and frequencies of opposite sign)."},{"citing_arxiv_id":"2108.01045","ref_index":120,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GWTC-2.1: Deep Extended Catalog of Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2021-08-02T17:09:29+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GWTC-2.1 adds eight new high-significance compact binary coalescence events to the prior catalog, extending the observed black hole mass range and including candidates inside the pair-instability mass gap.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"These three regions are allowed to contribute equally to the background, while within each of them we sum the background contributions from all the templates. The pBNS, pNSBH, pBBH, and derived pastro quanti- ties are computed as the fraction of recovered simulated events, representative of an astrophysical population, to this foreground plus background estimate provided by the pipeline [120]. The parameterizations of the popula- tions are described in Sec. IV D, with thePower Law + Peak model used for BBH [121]. The rate of each type of source is adjusted using a multicomponent population analysis [26]. To follow the population and background evolution across the parameter space, 165 subregions are used. This finer resolution has the benefit of revealing"},{"citing_arxiv_id":"2010.14529","ref_index":81,"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":"background","top_context_polarity":"background","context_text":"relying on the waveform models described in [ 73-76] and [77]), and by one pipeline that does not (coherentWa veBurst, henceforthcWB [ 78-80]). Making use of a measure of sig- nificance that assumes the validity of GR could potentially lead to biases in the selection of events to be tested, system- atically disfavoring signals in which a GR violation would be most evident (e.g., [81]).cWB would detect at least some of the conceivable chirp-like signals with sufficient departures from GR that they would be missed by the templated searches. Nonetheless, we cannot fully discard the existence of a hid- den population of signals exhibiting large deviations from GR, which could escape both modeled and unmodeled searches. Out of all the events reported in [16], only the massive event"},{"citing_arxiv_id":"2010.14527","ref_index":156,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2020-10-27T18:01:31+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"LIGO and Virgo detected 39 compact binary coalescence events in O3a, including 13 new ones, with black hole binaries up to 150 solar masses and the first significantly asymmetric mass ratios.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"to improve the collection of background statistics in the last region shown in Table II by a grid of templates dis- tributed uniformly in the logarithm of component mass to improve detection efficiency for systems with primary mass mdet 1 above 50 M⊙ [8, 145]. The TaylorF2 waveform approximant [138, 146-155]. was used for templates with Mdet < 1.73 M⊙ and the SEOBNRv4 ROM waveform approximant [156] for templates with M≥ 1.73 M⊙. The PyCBC analysis used a template bank covering the same parameter space as for GWTC-1 [8] shown in Figs. 3 and 7 of [157]. Unlike the previous work, the template bank here was created using a hybrid geometric-random method described in [158, 159]. This new method provides a more efficient template bank- in terms of covering the full parameter space with fewer"},{"citing_arxiv_id":"2004.06503","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Computationally efficient models for the dominant and sub-dominant harmonic modes of precessing binary black holes","primary_cat":"gr-qc","submitted_at":"2020-04-14T13:46:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"IMRPhenomXPHM is a new computationally efficient phenomenological model for precessing binary black hole gravitational-wave signals that incorporates higher-order modes via twisting-up maps from non-precessing waveforms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"of the remnant is much less affected by precession, since the scalar quantity of radiated energy is not significantly affected bytheprecessingmotionduetoitsslowertimescalecompared to the orbital motion. An important shortcoming of this construction as presented here is that it does not include the asymmetries in the(ℓ,|m|) = (2, 2)modes that are responsible for large recoils, see e.g. [21]. For brevity we will refer to the approximations that are used in the \"twisting up\" procedure as the \"twisting approximation\". Forarecentdetaileddiscussionoftheeffectoftheseapproxima- tions, with special consideration of the effect on sub-dominant harmonics, see [22, 23]. Our model currently uses two alternative descriptions for the Euler angles that characterize the approximate map: the"},{"citing_arxiv_id":"1905.09300","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Surrogate models for precessing binary black hole simulations with unequal masses","primary_cat":"gr-qc","submitted_at":"2019-05-22T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"New surrogate models NRSur7dq4 and RemnantModel accurately predict waveforms and remnant properties for precessing unequal-mass binary black holes up to q=4, outperforming existing models by an order of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1905.00869","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Testing the no-hair theorem with GW150914","primary_cat":"gr-qc","submitted_at":"2019-05-02T17:35:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Ringdown analysis of GW150914 with overtones measures remnant mass and spin consistent with a Kerr black hole, supporting the no-hair theorem at the 10% level.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1903.04467","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with the Binary Black Hole Signals from the LIGO-Virgo Catalog GWTC-1","primary_cat":"gr-qc","submitted_at":"2019-03-11T17:43:43+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Binary black hole signals in GWTC-1 are consistent with general relativity predictions, with an improved graviton mass bound of mg ≤ 4.7 × 10^{-23} eV/c² at 90% credible level.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Gravitational Waveforms from Numerical Relativity Simula- tions of Precessing Binary Black Hole Mergers,\" Phys. Rev. D, 95, 104023 (2017), arXiv:1701.00550 [gr-qc]. [24] S. Khan, K. Chatziioannou, M. Hannam, and F. Ohme, \"Phe- nomenological model for the gravitational-wave signal from precessing binary black holes with two-spin effects,\" Phys. Rev. D, 100, 024059 (2019), arXiv:1809.10113 [gr-qc]. [25] B. P. Abbott et al. (LIGO Scientific Collaboration and Virgo Collaboration), \"E ffects of waveform model systematics on the interpretation of GW150914,\" Classical Quantum Gravity, 34, 104002 (2017), arXiv:1611.07531 [gr-qc]. [26] LIGO Scientific Collaboration and Virgo Collabora- tion, \"Data release for testing GR with GWTC-1,\" https://dcc.ligo.org/LIGO-P1900087/public (2019)."}],"limit":50,"offset":0}