{"total":10,"items":[{"citing_arxiv_id":"2605.18742","ref_index":77,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A universal framework to identify eccentric binary mergers: GW200105 case study","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T17:58:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A reference-frequency-independent detection statistic for eccentric binary mergers is introduced and applied to GW200105, yielding ln B ≤ 0.9 in favor of the eccentric aligned-spin model over the quasi-circular precessing model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.11903","ref_index":142,"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":", BILBY: A user-friendly Bayesian in- ference library for gravitational-wave astronomy, Astro- phys. J. Suppl.241, 27 (2019), arXiv:1811.02042 [astro- ph.IM]. [141] R. J. E. Smith, G. Ashton, A. Vajpeyi, and C. Tal- bot, Massively parallel Bayesian inference for transient gravitational-wave astronomy, Mon. Not. Roy. Astron. Soc.498, 4492 (2020), arXiv:1909.11873 [gr-qc]. [142] I. M. Romero-Shawet al., Bayesian inference for com- pact binary coalescences with bilby: validation and ap- plication to the first LIGO-Virgo gravitational-wave transient catalogue, Mon. Not. Roy. Astron. Soc.499, 3295 (2020), arXiv:2006.00714 [astro-ph.IM]. [143] J. S. Speagle, DYNESTY: a dynamic nested sampling package for estimating Bayesian posteriors and evi-"},{"citing_arxiv_id":"2512.09978","ref_index":82,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational-wave parameter estimation to the Moon and back: massive binaries and the case of GW231123","primary_cat":"gr-qc","submitted_at":"2025-12-10T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LGWA could observe more than one third of known binary black hole events, detect ~90 mergers per year, and measure chirp mass better than third-generation detectors for massive systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2406.03568","ref_index":103,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":134,"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":"models used in this paper, and review the method introduced in Refs. [132, 133] to measure eccentricity directly from the waveform. Furthermore, in Sec. IV A we discuss the settings of the trained networks and priors employed in the DINGO analysis, while in Sec. IV B we validate the neural-networks 3 with zero-noise synthetic signals and comparisons to paral- lel Bilby (pBilby) [134]. From Secs. IV C through IV F, we present the analysis of 57 GWs and discuss in depth the events that support eccentricity. In Secs. V A and V B, we investigate the impact on parameter estimation of neglect- ing eccentricity and higher modes in waveform models, re- spectively. In Sec. VI A, we incorporate astrophysical BBH merger-rate estimates of eccentric and quasi-circular events"},{"citing_arxiv_id":"2010.14529","ref_index":125,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Rev. D99, 123029 (2019), [Erratum: Phys. Rev. D100, 089903(E) (2019)], arXiv:1902.07527 [gr-qc]. [123] M. Isi, M. Giesler, W. M. Farr, M. A. Scheel, and S. A. Teukol- sky, Phys. Rev. Lett.123, 111102 (2019), arXiv:1905.00869 [gr-qc]. [124] P. A. R. Adeet al.(Planck Collaboration), Astron. Astrophys. 594, A13 (2016), arXiv:1502.01589 [astro-ph.CO]. [125] J. Bovy, D. W. Hogg, and S. T. Roweis, Astrophys. J.700, 1794 (2009), arXiv:0905.2980 [astro-ph.GA]. [126] B. P. Abbottet al.(LIGO Scientific and Virgo Collaboration), Astrophys. J. Lett.882, L24 (2019), arXiv:1811.12940 [astro- ph.HE]. [127] C. E. Shannon, Bell Syst. Tech. J.27, 379 (1948), [Bell Syst. Tech. J.27, 623 (1948)]. [128] B. Carpenter, A."},{"citing_arxiv_id":"2010.14527","ref_index":230,"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":"with some of the more computationally costly waveform models, such as waveforms with HMs and precession ef- fects, especially for long-duration signals. For these, we also use RIFT, which performs a hybrid exploration of the parameter space split into intrinsic and extrinsic pa- rameters [227-229], and Parallel Bilby, based on a dis- tributed implementation of nested sampling [230-233], which was also used in previously published analyses of GW190412 [234], GW190425 [32], and GW190814 [33]. The raw posterior samples from the analyses described above are then collated to a common format using the PESummary package [235]. C. Priors Each event is analysed independently using a prior dis- tribution on the source parameters that is chosen to en-"},{"citing_arxiv_id":"2006.12611","ref_index":247,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GW190814: Gravitational Waves from the Coalescence of a 23 M$_\\odot$ Black Hole with a 2.6 M$_\\odot$ Compact Object","primary_cat":"astro-ph.HE","submitted_at":"2020-06-22T20:56:34+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.00714","ref_index":153,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Bayesian inference for compact binary coalescences with BILBY: Validation and application to the first LIGO--Virgo gravitational-wave transient catalogue","primary_cat":"astro-ph.IM","submitted_at":"2020-06-01T04:46:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"BILBY is validated on simulated compact binary signals and reproduces the eleven GWTC-1 results with configuration and output files provided for reproduction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2004.06503","ref_index":100,"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":"dataset","top_context_polarity":"use_dataset","context_text":"Parallel Bilby code [88] with the Dynesty [87] nested sampler. We perform these runs using2048live points and 5 ACTs without any kind of marginalization and 4 independent seeds which are then merged together. The noise spectral den- sity used for evaluating the likelihood function is the projected sensitivity for Advanced LIGO obtained from simulations of O4 data [100]. The orientation of the detector at the time of in- jectionisspecifiedthroughtheinjectiontime(within3minutes of the event GW150914) and at right ascension and declina- tion angles α=1.375 rad andδ=-1.2108 rad (consistent with GW150914 [26]). We specify the line of sight relative to the binary at the reference frequency of 20 Hz through the angles ι=1."}],"limit":50,"offset":0}