{"total":23,"items":[{"citing_arxiv_id":"2606.30594","ref_index":83,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Efficient Eccentric Effective-One-Body Dynamics via Near-Identity Averaging Transformations","primary_cat":"gr-qc","submitted_at":"2026-06-29T17:35:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Near-identity averaging transformations applied to osculating orbital elements reduce the computational cost of eccentric EOB inspirals by up to two orders of magnitude while maintaining accuracy for moderate to large eccentricities at NNLO.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28156","ref_index":98,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries","primary_cat":"gr-qc","submitted_at":"2026-06-26T14:52:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28716","ref_index":113,"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":"Additionally, theρ ℓm amplitude functions entering the QC part of the RR force include calibration parameters∆ρ (1) ℓm, which represent the linear-in-νcontributions at high PN or- ders, withν=m 1m2/(m1 +m 2)2 being the symmetric mass ratio. For all modes except (ℓ,|m|)=(2,2), these are fitted to numerical second-order gravitational self-force (2GSF) flux data as recalibrated in Ref. [113], following a correction to the original data [114] used in theSEOBNRv5models [115]. Since the leading-order Newtonian RR force inSEOBNRv6EHM differs from that ofSEOBNRv5, this constitutes an approxima- tion, as detailed in Ref. [103]. Instead,∆ρ (1) 22 is calibrated to an equal-mass, nonspinning QC NR waveform, as this yields a more regular calibration structure for spinning configurations."},{"citing_arxiv_id":"2605.28715","ref_index":216,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Accurate waveforms for generic planar-orbit binary black holes: The multipolar effective-one-body model SEOBNRv6EHM","primary_cat":"gr-qc","submitted_at":"2026-05-27T16:38:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SEOBNRv6EHM is a multipolar EOB model for eccentric planar-orbit BBHs calibrated to NR simulations, showing low waveform mismatches up to eccentricity 0.9.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"tion ofSEOBNRv6EHM(round markers), and the remaining 167 waveforms (star markers). We highlight in red the simulations SXS:BBH:4121andSXS:BBH:4123(top right corner). SEOBNRv6EHMbenefits from the merger-ringdown and input-value fits ofSEOBNRv5HM[220]. These were con- structed with additional 18 nonspinningSXSNR waveforms, oneEinstein Toolkitwaveform [216, 367], and 13 test- mass-limit waveforms computed using the Teukolsky equa- tion [368, 369]. These add up to the 442 NR+13 test-mass- limit waveforms quoted in Ref. [220]. The number 425 for SEOBNRv6EHMonly counts the simulations actually employed in the new calibration of the parameters{a 6, ˆdSO,∆t 22 ISCO}. C. RR force calibration The first part in our calibration procedure consists of de-"},{"citing_arxiv_id":"2605.27500","ref_index":82,"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":"2605.25623","ref_index":39,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A pre-merger-informed spectral-level ringdown inference framework for black-hole spectroscopy","primary_cat":"gr-qc","submitted_at":"2026-05-25T09:26:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SPRING framework propagates pre-merger information into spectral-level ringdown inference, improving Bayesian support for an agnostic two-damped-sinusoid model on GW250114 by ΔlnB ~5-10 while keeping remnant posteriors consistent with IMR estimates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16492","ref_index":24,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2605.11703","ref_index":229,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Yunes, Gravitational Wave Tests of Strong Field General Relativity with Binary Inspirals: Realistic Injections and Optimal Model Selection, Phys. Rev. D87, 102001 (2013), arXiv:1303.1185 [gr-qc]. [228] B. Edelmanet al., Constraining unmodeled physics with com- pact binary mergers from GWTC-1, Phys. Rev. D103, 042004 (2021), arXiv:2008.06436 [gr-qc]. [229] L. Pompiliet al., Laying the foundation of the effective- one-body waveform models SEOBNRv5: Improved accuracy 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"},{"citing_arxiv_id":"2604.17868","ref_index":96,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions","primary_cat":"gr-qc","submitted_at":"2026-04-20T06:28:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The gwNRHME framework constructs a multi-modal non-spinning eccentric gravitational waveform surrogate by modulating quasi-circular models with universal eccentric functions, achieving median mismatches of ~9e-5 against 156 NR waveforms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"circular multi-modal model in this construction leads to a slightly different multi-modal eccentric waveform model. In particular, NRHybSur3dq8 can be substituted with state-of- the-art quasi-circular models developed within other model- ing frameworks. Examples include perturbation-theory-based models such as BHPTNRSur1dq1e4 [95] and EOB models such as SEOBNRv5HM [96] and TEOBResumS-Dali [63, 97]. In the latter part of this paper (Section V), we perform this replace- ment explicitly for SEOBNRv5HM and TEOBResumS-Dali, and present the resulting waveform comparisons. We do not in- clude BHPTNRSur1dq1e4 at this stage, as it is trained for mass ratios q≥ 2.5, thereby covering only a limited portion of the NRSurE_q4NoSpin_22parameter space."},{"citing_arxiv_id":"2604.15431","ref_index":129,"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":"precessing systems and extreme mass ratios [ 30, 189-192]. We restrict our model to the dominant quadropolar mode and ignore higher modes for the current study. Their inclusion can be achieved with analogous methods and will be considered in future work. The model also neglects spherical-spheroidal mixing [119, 193-196] (although this is not a fundamental limitation [ 129]) and beyond-linear QNM couplings [166, 172, 175-183]. For each mode, the QNM rescaled complex amplitude ¯h(τ) is in turn factored in an amplitude and a phase ¯h(τ) = A¯h(τ)eiϕ¯h(τ). We use different ans¨ atze for the 4 quasi-circular and eccentric cases, introduced below. HypTan:TheHypTantemplate for the amplitude and phase is based on Ref. [113], and given by"},{"citing_arxiv_id":"2604.14112","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational Sommerfeld Effects: Formalism, Renormalization, and Perturbation to $O(G^{10})$","primary_cat":"hep-th","submitted_at":"2026-04-15T17:32:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Closed-form Sommerfeld factor via EFT connection matrix with analytic O(G^10) magnitude and phase for l=0,1,2 waves, plus a new RG equation for radiative multipole moments that improves waveform resummation beyond tail logarithms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"a long history in the EOB program. Damour and Na- gar [33, 34] pioneered a \"tail resummation factor\"Tℓm inspired by the Sommerfeld-Coulomb enhancement of quantum scattering, which captures the leading exponen- tiation ofπGMωand the Coulomb phase shift. This fac- tor has become a standard ingredient in the MPM wave- form factorization [35-37]. Recent progress was made by [38], who derived the universal anomalous dimension of generic multipole moments and proposed an improved resummation using the black hole perturbation theory (BHPT) renormalized angular momentumνin place of the integerℓ[38, 39], thereby capturing subleading uni- versal logarithms. Complementary to this, [40, 41] devel- oped a Born-series approach to solve the effective wave"},{"citing_arxiv_id":"2604.11903","ref_index":46,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"pyEFPEHM extends prior PN models to include higher-order quasi-circular phasing, generalized precession solutions, and eccentric corrections up to 1PN in selected multipoles for eccentric precessing binaries with matter effects.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"wavelength approximation [118] can be written as h=F +(α, δ, ψ)h+ +F ×(α, δ, ψ)h× ,(89) whereF + andF × are the detector antenna pattern func- tions, which depend on the sky location (α, δ) and polar- ization angleψ. For simplicity, during waveform compar- ison, we use that this detector strain can be expressed in terms of an effective polarization angleκ(α, δ, ψ) as [46] h=A(α, δ, ψ) \u0002 cos (2κ)h+ + sin (2κ)h× \u0003 ,(90) To quantify the difference between two strainsh 1 and h2, we compute their mismatchMM[115, 116] as MM(h1, h2) = 1− M(h 1, h2) = 1− ⟨h1|h2⟩p ⟨h1|h1⟩⟨h2|h2⟩ . (91) 10−5 10−4 10−3 10−2 10−1 100 ϵN 10−6 10−5 10−4 10−3 10−2 10−1 100 2∆ log L ρ2 opt = ⟨h0−hϵN |h0−hϵN ⟩ ⟨h0|h0⟩ Samples 90% C.L. Median ϵN FIG."},{"citing_arxiv_id":"2604.04957","ref_index":31,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"FluxMC: Rapid and High-Fidelity Inference for Space-Based Gravitational-Wave Observations","primary_cat":"astro-ph.IM","submitted_at":"2026-04-03T11:32:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FluxMC integrates flow matching with parallel tempering MCMC to converge in under five hours on high-fidelity IMRPhenomHM waveforms for massive black hole binaries, where standard methods fail after hundreds of hours and produce two to three orders of magnitude higher distributional error.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"103004 arXiv:1909.10010 [gr-qc] [30] London, L., Khan, S., Fauchon-Jones, E., Garc' ıa, C., Hannam, M., Husa, S., Jim' enez-Forteza, X., Kalaghatgi, C., Ohme, F., Pannarale, F.: First higher- multipole model of gravitational waves from spinning and coalescing black- hole binaries. Phys. Rev. Lett.120, 161102 (2018) https://doi.org/10.1103/ PhysRevLett.120.161102 [31] Pompili, L.,et al.: Laying the foundation of the effective-one-body waveform 22 models SEOBNRv5: Improved accuracy and efficiency for spinning nonprecessing binary black holes. Phys. Rev. D108(12), 124035 (2023) https://doi.org/10.1103/ PhysRevD.108.124035 arXiv:2303.18039 [gr-qc] [32] Ellis, J., Haasteren, R.: jellis18/PTMCMCSampler: Official Release (2017)."},{"citing_arxiv_id":"2601.23230","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Detectability of Gravitational-Wave Memory with LISA: A Bayesian Approach","primary_cat":"gr-qc","submitted_at":"2026-01-30T17:58:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian parameter estimation on simulated LISA data establishes conditions for detecting displacement memory in MBHB events and projects observation rates from population models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.23019","ref_index":169,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"direct access to the defining memory offset, and thereby to provide the necessary conceptual and mathematical tools to support a future claim of detection. Such an ob- servation would open a direct observational window onto the universal infrared structure of field theory, with di- rect links to questions in quantum gravity and physics beyond general relativity [18-30, 71, 108, 168, 169]. In the case of ordinary memory associated with un- bound matter, including linear memory from massive particles and null memory from electromagnetic radia- tion, a direct association between radiation and the re- sulting memory exists in principle. This isa priorinot the case for nonlinear memory sourced by gravitational waves themselves. Concretely, the issue can be illustrated"},{"citing_arxiv_id":"2601.13173","ref_index":45,"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":"2512.02274","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational radiation from hyperbolic orbits: comparison between self-force, post-Minkowskian, post-Newtonian, and numerical relativity results","primary_cat":"gr-qc","submitted_at":"2025-12-01T23:40:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Self-force calculations of radiated gravitational wave energy from hyperbolic orbits around Schwarzschild black holes agree with post-Minkowskian results for large impact parameters and velocities up to 0.7c, with further comparisons to post-Newtonian and numerical relativity.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"B. Wardell, and L. Barack, Gravitational self-torque and spin precession in compact binaries, Phys. Rev. D89, 064011 (2014), arXiv:1312.0775 [gr-qc]. [15] A. Le Tiec, The Overlap of Numerical Relativity, Per- turbation Theory and Post-Newtonian Theory in the Binary Black Hole Problem, Int. J. Mod. Phys. D23, 1430022 (2014), arXiv:1408.5505 [gr-qc]. [16] S. R. Dolan, P. Nolan, A. C. Ottewill, N. Warburton, and B. Wardell, Tidal invariants for compact binaries on quasicircular orbits, Phys. Rev. D91, 023009 (2015), arXiv:1406.4890 [gr-qc]. [17] S. Akcay, A. Le Tiec, L. Barack, N. Sago, and N. Warburton, Comparison Between Self-Force and Post-Newtonian Dynamics: Beyond Circular Orbits, Phys. Rev. D91, 124014 (2015), arXiv:1503."},{"citing_arxiv_id":"2510.16113","ref_index":161,"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":"2509.08099","ref_index":127,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"ference between the remnant massM f and spinχ f inferred from the low- (f<f IMR c ) and high-frequency (f>f IMR c ) portions of the GW signal [166-168]. The cutofff IMR c is taken to be the GW frequency of the (2,2)-mode at the in- nermost circular orbit of the remnant Kerr BH [169]. The remnant properties are calculated using NR-calibrated fits for the final-state [127, 170, 171] applied to the median val- ues of the redshifted component masses, spin magnitudes, and spin angles as inferred from the full IMR analysis [41- 43]. Inference is performed in each of the frequency regimes usingIMRPhenomXPHM SpinTaylor[160, 161], with priors that are uniform in component mass and spin magnitude, and isotropic in the spin orientation."},{"citing_arxiv_id":"2509.08054","ref_index":51,"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":"Sully, Black holes: Complementarity or firewalls?, JHEP2013(02), 062, arXiv:1207.3123 [hep-th]. [49] G. 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Cattaneoet al., The role of black holes in galaxy forma- tion and evolution, Nature460, 213 (2009), arXiv:0907."},{"citing_arxiv_id":"2504.07862","ref_index":99,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Resummation of Universal Tails in Gravitational Waveforms","primary_cat":"hep-th","submitted_at":"2025-04-10T15:39:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A universal anomalous dimension for multipole moments in GR is derived via two EFT methods and applied to resum short-distance logarithmic tails in binary gravitational waveforms.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2407.18319","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2404.14286","ref_index":181,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Newtonian e ffective-one-body scheme for spin-precessing compact-binary waveforms up to merger, Phys. 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