{"total":15,"items":[{"citing_arxiv_id":"2605.21640","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Wave Hyperbolic Catalog: Reanalyzing High-Mass Gravitational Wave Signals Using Hyperbolic Waveforms","primary_cat":"gr-qc","submitted_at":"2026-05-20T18:51:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reanalysis finds GW190521 prefers hyperbolic waveforms over quasi-circular precessing ones with ln Bayes factor 3.71, while other high-mass events and GW231123 favor the latter; mock signals indicate distinguishability challenges for high-mass precessing cases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04579","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Impact of Spin Priors on Parameterized Tests of General Relativity","primary_cat":"gr-qc","submitted_at":"2026-05-06T07:30:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Spin prior choices propagate into tests of GR via the 1.5PN deviation parameter δφ̂3 in a non-trivial, event-dependent way, with stronger effects for short-inspiral events and partial degeneracy with χ_eff when the deviation is included.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Spin effects enter the gravitational-wave waveform through spin-orbit and spin-spin couplings, contributing to higher-order corrections in the phase at post-Newtonian (PN) orders beyond the leading point-mass terms[11, 19]. In gravitational-wave analyses, the spin effects of binary black holes are commonly characterized by the effective inspiral spin parameterχ effand the effective precession spin parameterχ p. They are defined as[20, 21]: χeff= m1⃗ χ1 · ˆL+m 2⃗ χ2 · ˆL m1 +m 2 ,(2) χp = max \u0012 χ1⊥, 4q+ 3 4 + 3q q χ2⊥ \u0013 .(3) The effective inspiral spin parameterχ effis defined as the mass-weighted projection of the compo- nent spins along the orbital angular momentum ˆL. It is the dominant spin parameter entering the waveform phase evolution at leading post-Newtonian order and remains approximately conserved"},{"citing_arxiv_id":"2604.15885","ref_index":37,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational-wave astronomy requires population-informed parameter estimation","primary_cat":"gr-qc","submitted_at":"2026-04-17T09:31:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Population-informed hierarchical parameter estimation is required for unbiased astrophysical interpretation of gravitational-wave events rather than using standard individual posteriors with reference priors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Katz, Mon. Not. R. Astron. Soc.508, 69 (2021), arXiv:2106.05212 [astro-ph.HE]. [34] A. G. Abacet al., Astrophys. J. Lett.993, L21 (2025), arXiv:2510.26931 [astro-ph.HE]. [35] R. Abbottet al., Astrophys. J. Lett.900, L13 (2020), arXiv:2009.01190 [astro-ph.HE]. [36] A. G. Abacet al., Astrophys. J. Lett.970, L34 (2024), arXiv:2404.04248 [astro-ph.HE]. [37] E. Racine, Phys. Rev. D78, 044021 (2008), arXiv:0803.1820 [gr-qc]. [38] W. M. Farr, Res. Notes Am. Astron. Soc.3, 66 (2019), arXiv:1904.10879 [astro-ph.IM]. [39] R. Essick and W. Farr, arXiv:2204.00461 [astro-ph.IM] (2022). [40] C. Talbot and J. Golomb, Mon. Not. R. Astron. Soc.526, 3495 (2023), arXiv:2304.06138 [astro-ph.IM]. [41] J. Heinzel and S."},{"citing_arxiv_id":"2604.14270","ref_index":112,"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":"the difference between the two may be greater than for χeff). Regardless of the waveform model used, and in line with the standard LVK analyses [98], our reported results are marginalized over the uncertainty in detector calibra- tion. This is achieved by allowing frequency-dependent phase and amplitude shifts to the strain in each inter- ferometer, described by spline models [112], with the values at the spline nodes treated as sampling parame- ters. Using 10 spline nodes, this gives 20 extra sampling parameters per interferometer. For GW150914 we de- termine the priors for each calibration parameter from the in-situ calibration envelopes [113] provided by the LVK collaboration, and use Gaussian priors for each node for GW200129 and GW250114 (see Table X for"},{"citing_arxiv_id":"2604.11903","ref_index":106,"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":"D107, 084006 (2023), arXiv:2212.13095 [gr-qc]. [104] B. M. Barker and R. F. O'Connell, Gravitational Two-Body Problem with Arbitrary Masses, Spins, and Quadrupole Moments, Phys. Rev. D12, 329 (1975). [105] E. Racine, Analysis of spin precession in binary black hole systems including quadrupole-monopole interac- tion, Phys. Rev. D78, 044021 (2008), arXiv:0803.1820 [gr-qc]. [106] T. Colin, S. Tanay, and L. Bernard, Analytical So- lution of Spinning, Eccentric Binary Black Hole Dy- namics at the Second Post-Newtonian Order, (2026), arXiv:2603.20031 [gr-qc]. [107] A. Bohe, S. Marsat, G. Faye, and L. Blanchet, Next-to- next-to-leading order spin-orbit effects in the near-zone metric and precession equations of compact binaries,"},{"citing_arxiv_id":"2604.06090","ref_index":103,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Posterior Predictive Checks for Gravitational-wave Populations: Limitations and Improvements","primary_cat":"gr-qc","submitted_at":"2026-04-07T17:03:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Maximum-likelihood-based posterior predictive checks detect model misspecification better than event-level versions for uncertain spin tilts, but current detector sensitivity limits their power; the Gaussian Component Spins model underpredicts high spin magnitudes and overpredicts anti-aligned tilts","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"06503 [gr-qc]. [100] S. Sinharay and H. S. Stern, Journal of Statistical Plan- ning and Inference111, 209 (2003). [101] T. Callister, Reweighting single event posteriors with hyperparameter marginalization (2021). [102] M. Vallisneri, P. M. Meyers, K. Chatziioannou, and A. J. K. Chua, Phys. Rev. D108, 123007 (2023), arXiv:2306.05558 [astro-ph.HE]. [103] P. M. Meyers, K. Chatziioannou, M. Vallisneri, and A. J. K. Chua, Phys. Rev. D108, 123008 (2023), arXiv:2306.05559 [astro-ph.HE]. [104] G. Agazieet al.(NANOGrav), Phys. Rev. D111, 042011 (2025), arXiv:2407.20510 [astro-ph.HE]. [105] R. van Haasteren, Phys. Rev. D112, 103009 (2025), arXiv:2506.10811 [astro-ph.IM]. [106] M. J. Bayarri and J. O. Berger, Journal of the American"},{"citing_arxiv_id":"2603.20031","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Analytical Solution of Spinning, Eccentric Binary Black Hole Dynamics at the Second Post-Newtonian Order","primary_cat":"gr-qc","submitted_at":"2026-03-20T15:17:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An analytical 2PN solution is constructed for the orbital and spin dynamics of eccentric, arbitrarily spinning binary black holes, with spin oscillations retained only at 1.5PN accuracy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.07908","ref_index":61,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Signatures of a subpopulation of hierarchical mergers in the GWTC-4 gravitational-wave dataset","primary_cat":"gr-qc","submitted_at":"2026-01-12T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"GWTC-4 data show a transition to nearly all hierarchical mergers above 46 solar masses, with the hierarchical rate peaking at 15.7 solar masses, indicating mass-dependent substructure in black hole spins.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"troduce systematic biases in measurements of individual systems, including their spins [14, 54-57]. When per- arXiv:2601.07908v1 [gr-qc] 12 Jan 2026 2 forming and interpreting population analyses, we there- fore turn to effective parameters, whose measurements may be more trustworthy than those of component spins and tilts [58-60]. Effective inspiral spin [61, 62] is typ- ically the best-measured combination of spin parame- ters [63], defined as the mass-weighted projection of the spin vectors onto the orbital angular momentum: χeff = (a1 cosτ 1 +qa 2 cosτ 2)/(1+q); whereqdenotes the mass ratio (defined on the range 0< q≤1),a 1 anda 2 are the respective spin magnitudes of the primary (heav- ier) and secondary (lighter) black holes, andτ 1,2 are the"},{"citing_arxiv_id":"2508.21125","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"PRECESSION 2.1: black-hole binary spin precession on eccentric orbits","primary_cat":"gr-qc","submitted_at":"2025-08-28T18:00:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Version 2.1 of the precession code extends post-Newtonian modeling of spinning black-hole binaries to eccentric orbits via a decorator-based adaptation and new evolutionary equations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.23663","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Disentangling spinning and nonspinning binary black hole populations with spin sorting","primary_cat":"gr-qc","submitted_at":"2025-07-31T15:40:32+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Spin sorting with the default spin model distinguishes spinning and nonspinning binary black hole populations in simulations and shows real data rule out a fully nonspinning population but allow mixed ones with up to 80% nonspinning sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.08219","ref_index":148,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GW231123: a Binary Black Hole Merger with Total Mass 190-265 $M_{\\odot}$","primary_cat":"astro-ph.HE","submitted_at":"2025-07-10T23:52:46+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":9.0,"formal_verification":"none","one_line_summary":"A new gravitational wave event reveals a binary black hole merger with total mass 190-265 solar masses, indicating black holes can form via gravitational-wave driven mergers beyond standard stellar channels.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.14286","ref_index":136,"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":"E. Smith, G. Ashton, A. Vajpeyi, and C. Talbot, Mas- sively parallel Bayesian inference for transient gravitational- wave astronomy, Mon. Not. Roy. Astron. Soc. 498, 4492 (2020), arXiv:1909.11873 [gr-qc]. [135] T. Damour, Coalescence of two spinning black holes: an ef- fective one-body approach, Phys. Rev. D 64, 124013 (2001), arXiv:gr-qc/0103018. [136] E. Racine, Analysis of spin precession in binary black hole systems including quadrupole-monopole interaction, Phys. Rev. D 78, 044021 (2008), arXiv:0803.1820 [gr-qc]. [137] L. Santamaria et al. , Matching post-Newtonian and numeri- cal relativity waveforms: systematic errors and a new phe- nomenological model for non-precessing black hole binaries,"},{"citing_arxiv_id":"2111.03606","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run","primary_cat":"gr-qc","submitted_at":"2021-11-05T16:43:17+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GWTC-3 catalogs 90 compact binary coalescence events with p_astro > 0.5 from LIGO and Virgo's first three observing runs, including the first confident neutron star-black hole binaries.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2108.01045","ref_index":186,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2004.06503","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"30, 075017 (2013), arXiv:1212.5520 [gr-qc]. [55] T. Damour, P. Jaranowski, and G. Schäfer, Phys. Rev.D89, 064058 (2014), arXiv:1401.4548 [gr-qc]. [56] L. Bernard, L. Blanchet, G. Faye, and T. Marchand, Phys. Rev. D97, 044037 (2018), arXiv:1711.00283 [gr-qc]. [57] L. Blanchet and A. Le Tiec, Class. Quant. Grav.34, 164001 (2017), arXiv:1702.06839 [gr-qc]. [58] S. Marsat, Class. Quant. Grav. 32, 085008 (2015), arXiv:1411.4118 [gr-qc]. [59] J. Vines and J. Steinhoff, Phys. Rev.D97, 064010 (2018), arXiv:1606.08832 [gr-qc]. [60] N. Siemonsen, J. Steinhoff, and J. Vines, Phys. Rev.D97, 124046 (2018), arXiv:1712.08603 [gr-qc]. [61] N.K.Johnson-McDaniel,A.Gupta,P.Ajith,D.Keitel,O.Birn- holtz, F. Ohme, and S. Husa,Determining the final spin of a"}],"limit":50,"offset":0}