{"total":15,"items":[{"citing_arxiv_id":"2606.30594","ref_index":147,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"method for sampling the waveform described in Sec.V B. Their mismatches ofM 22 ∼10 −8 indicate that the NIT mismatches are dominated by the order at which we trun- cate the NIT expansion. One could push to higher PA or- ders to achieve further accuracy. A conservative estimate for the SNR at which the EOB and 2PA NIT waveforms would be distinguishable is given by∼1/ √ 2M[147]. ForM 22 ∼10 −6, this would be an SNR of∼700. Thus going beyond 2PA order would be unnecessary for most comparable mass binaries, bar exceptionally loud MBHB signals that one might observe with LISA [10, 11, 148]. In the following sections, we will see that these results broadly hold across the eccentric BHB parameter space for current ground-based detectors."},{"citing_arxiv_id":"2606.28161","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Finite Coherence in Gravitational Waves from Tidally Excited Axion Clouds","primary_cat":"gr-qc","submitted_at":"2026-06-26T14:57:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Finite coherence during tidal Bohr crossings in axion clouds produces distinct, localized gravitational-wave waveforms and orbital responses in black-hole binaries.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27429","ref_index":98,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Massive scalar fields in eccentric regime: Detectability and constraints from LISA observations of extreme mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-06-25T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Computes scalar and tensor fluxes for eccentric EMRIs with massive scalars, quantifies dephasing, and shows via Fisher matrix that LISA can constrain scalar charge and mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11705","ref_index":127,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Horizon absorption in eccentric precessing binary black hole inspirals and its importance for gravitational wave data analysis","primary_cat":"gr-qc","submitted_at":"2026-06-10T06:29:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First leading-PN derivation of horizon absorption in eccentric precessing BBH inspirals, incorporated into pyEFPEHM, with estimates showing parameter biases in eccentric systems at moderate SNR.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10104","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Fifth RIT Catalog of Binary Black Hole Simulations: Multiple-Resolution Studies of Eccentric Orbits","primary_cat":"gr-qc","submitted_at":"2026-06-08T19:31:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Fifth RIT catalog adds 248 new binary black hole waveforms emphasizing eccentric orbits with convergence studies on 10 simulations, reaching 2129 total cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02690","ref_index":127,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Speed and accuracy for long signals: Frequency-domain effective-one-body waveforms for compact binary coalescences","primary_cat":"gr-qc","submitted_at":"2026-06-01T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hybrid SPA-plus-FFT frequency-domain version of SEOBNRv5THM for quasi-circular spin-aligned BNS systems matches time-domain baseline accuracy while cutting computational cost for long signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28716","ref_index":134,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"Network matched-filter SNRρ N mf and log-likelihood logL(median and 90% credible interval) for the high-eccentricity NR configurations recovered with three waveform models. The in- jected SNR values are given in parentheses in the first column. (ℓ,|m|)=(3,2) mode. Biases from neglecting higher-order modes in eccentric inference grow with mass ratio and incli- nation [134] (see also Fig. 14 of Ref. [103]); the systematic differences reported below therefore mostly reflect the differ- 9 5 (20) 10 (40) 15 (60) 20 (80) 25 (100) 30 (120) ⟨ fref ⟩ [Hz] for M = 80M ⊙ (for M = 20M ⊙ ) 0.0 0.2 0.4 0.6 egw SXS:BBH:1355 (M =80 M⊙) SXS:BBH:1359 (M =80 M⊙) SXS:BBH:1362 (M =80 M⊙) SXS:BBH:2525 (M =80 M⊙) SXS:BBH:2527 (M =80 M⊙)"},{"citing_arxiv_id":"2605.15265","ref_index":105,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eccentric Stellar-mass Binary Black Holes: Population, Detectability, and Waveform Analysis in the LISA and LIGO Era","primary_cat":"astro-ph.HE","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations of dynamical channels predict ~36 eccentric stellar-mass BBHs detectable by LISA in the Milky Way at SNR>1 over 10 years, a local merger rate of ~9 Gpc^{-3} yr^{-1}, and hundreds of faint extragalactic mHz sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03756","ref_index":47,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resonances as signatures of scalar clouds in eccentric extreme-mass-ratio inspirals","primary_cat":"gr-qc","submitted_at":"2026-05-05T13:41:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Eccentric EMRIs exhibit relativistic resonances in scalar fluxes that enhance interactions with scalar clouds and amplify waveform dephasing relative to circular orbits.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"resonance band in∼1month. The orbital evolution starts at pi = 8.2and we take a dipolar cloud with the same parameters as in Fig. 1. The solid lines show the cases withei = 0.2and ei = 0.02, whereas the dashed line shows the dephasing of an analogous system withe= 0. the phase shift accumulated throughout the full inspiral remains well above the threshold for detection [47], in agreement with previous work which focused on circular orbits [14]. To quantify the detectability of the resonant transitions, we compute the phase shift∆Ψ φaccumulated during the n = 2resonance ( p≈8.2→7.9) for two different 5 cases, still keeping the cloud mass fixed atMb/M = 0.05. We consider a case where the eccentricity atp = 8.2is e = 0."},{"citing_arxiv_id":"2604.21859","ref_index":58,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mitigating Systematic Errors in Parameter Estimation of Binary Black Hole Mergers in O1-O3 LIGO-Virgo Data","primary_cat":"astro-ph.HE","submitted_at":"2026-04-23T16:52:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reanalysis of flagged LVK events with waveform uncertainty models produces consistent spin and precession inferences across raw/deglitched data and multiple waveform approximants.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the state-of-the-art waveform models, which use higher- order multiple modes and spin-induced quadruple mo- ments [79]. Apart from waveform modelling uncertainties, data analysis artifacts, such as the presence of glitches near the signal, can also affect the PE results. Typically, the LIGO-Virgo interferometers encounter glitches at the rate ofO(1) per minute [58]. Some of them tend to oc- cur in the vicinity of a gravitational wave signal. Such glitches need to be carefully reconstructed and subtracted from the data before the signal can be analysed; other- wise, their presence may introduce biases in the measure- ment of the source properties of the signals and in sub- sequent science cases. For the gravitational wave tran-"},{"citing_arxiv_id":"2604.14270","ref_index":75,"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":"background","top_context_polarity":"background","context_text":"02444 [gr-qc]. [73] L. Lindblom, B. J. Owen, and D. A. Brown, Model Waveform Accuracy Standards for Gravitational Wave Data Analysis, Phys. Rev. D78, 124020 (2008), arXiv:0809.3844 [gr-qc]. [74] S. T. McWilliams, B. J. Kelly, and J. G. Baker, Observ- ing mergers of non-spinning black-hole binaries, Phys. Rev. D82, 024014 (2010), arXiv:1004.0961 [gr-qc]. [75] M. Hannam, S. Husa, F. Ohme, and P. Ajith, Length requirements for numerical-relativity waveforms, Phys. Rev. D82, 124052 (2010), arXiv:1008.2961 [gr-qc]. [76] E. Baird, S. Fairhurst, M. Hannam, and P. Mur- phy, Degeneracy between mass and spin in black-hole- binary waveforms, Phys. Rev. D87, 024035 (2013), arXiv:1211.0546 [gr-qc]. [77] K. Chatziioannou, A."},{"citing_arxiv_id":"2604.11903","ref_index":139,"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":"background","top_context_polarity":"background","context_text":"ThepyEFPEHMwaveforms shown are generated using the time-domain implementation up to the ISCO. A 2 Hz high-pass filter is applied to both waveforms to reduce the visual impact of GW memory. coalescence phase and time, the luminosity distance, the sky location (right ascension and declination), and the polarization angle. Nonetheless, the accuracy of pa- rameter recovery cannot be inferred from mismatches alone [139]. While mismatches quantify overall wave- form agreement, parameter biases depend on the detailed structure of waveform errors and on whether these errors can be absorbed by shifts in the inferred parameters. Fur- thermore, for such a high-dimensional parameter space, a typical PE analysis requiresO 108\u0001 likelihood evalu- ations, making PE a demanding test of the numerical"},{"citing_arxiv_id":"2604.11895","ref_index":93,"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":"method","top_context_polarity":"use_method","context_text":"Barausse, Phys. Rev. D112, 104031 (2025), arXiv:2506.21181 [gr-qc]. [90] S. H. Völkel and A. Dhani, Phys. Rev. D112, 084076 (2025), arXiv:2507.22122 [gr-qc]. [91] N.Afshordiet al.(LISAConsortiumWaveformWorking Group), Living Rev. Rel.28, 9 (2025), arXiv:2311.01300 [gr-qc]. [92] E. E. Flanagan and S. A. Hughes, Phys. Rev. D57, 4566 (1998), arXiv:gr-qc/9710129. [93] L. Lindblom, B. J. Owen, and D. A. Brown, Phys. Rev. D78, 124020 (2008), arXiv:0809.3844 [gr-qc]. [94] S. Bhagwat, C. Pacilio, P. Pani, and M. Mapelli, Phys. Rev. D108, 043019 (2023), arXiv:2304.02283 [gr-qc]. [95] E. Berti, A. Sesana, E. Barausse, V. Cardoso, and K. Belczynski, Phys. Rev. Lett.117, 101102 (2016), arXiv:1605.09286 [gr-qc]. [96] S."},{"citing_arxiv_id":"2601.09678","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"1906.11055","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Retrieving the True Masses of Gravitational-wave Sources","primary_cat":"astro-ph.HE","submitted_at":"2019-06-26T12:52:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hydrodynamic drag makes BBH waveforms resemble higher-mass vacuum sources, biasing matched-filter chirp-mass estimates upward for LISA sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}