{"total":10,"items":[{"citing_arxiv_id":"2605.18742","ref_index":58,"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":"2605.12818","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Assessing the imprint of eccentricity in GW signatures using two independent waveform models","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T23:23:08+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dual-model analysis of 162 GW sources disfavors eccentricity for most events but finds potential evidence in GW200129, GW231001, and GW231123.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"reflects astrophysical context. In the data release accom- panying our publication, we provide these likelihoods to facilitate this and other downstream reanalyses. A recent reanalysis of GW200105 162426 has already performed a systematic investigation of that source with multiple waveforms using RIFT, while adopting superior settings to the default choices adopted here [28], includ- ing higher sampling rates and more conservative internal analysis settings (e.g. grid sizes). In this work, we there- fore do not provide an equally comprehensive analysis of this candidate, focusing instead on the remainder of the population. TABLE I: A table showing the total events analyzed. The columns con- tain the minimum FAR [6, 7, 59], key source parameters, starting fre-"},{"citing_arxiv_id":"2605.11947","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Inferring host environment properties and gravitational-wave decay time from the eccentricity measurement of dynamically captured binaries","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T10:56:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Eccentricity posteriors of dynamically captured binaries can be mapped to capture parameters and compared against environment velocity distributions to constrain host and infer decay time.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"units whereG=c=1.) Neglecting any perturbations out- side the binary, the GW energy loss transitions the unbound binary to a bound one withe≲1. For a given (b, v ∞), we can express the periapsis dis- tance and initial semi-major axis of the newly formed binary as (R. M. O'Leary et al. 2009) rp =  s 1 b2 + M2 b4v4∞ + M b2 v2∞  −1 ,(3) ai = M2η 2 1 2 µv2∞ −∆E GW .(4) The corresponding eccentricity immediately after capture is ei =1−r p/ai. For a fixed value ofv ∞, the maximum impact parameter for which a GW capture occurs can be obtained from the above (R. M. O'Leary et al. 2009): bmax = 340π 3 !1/7 η1/7M v9/7 ∞ .(5) Expressing the semi-latus rectump=a(1−e 2) in a di- mensionless form asx≡p/M, the PN orbital evolution due"},{"citing_arxiv_id":"2605.00124","ref_index":20,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Merger remnant and eccentricity dynamics surrogates for eccentric nonspinning black hole binaries","primary_cat":"gr-qc","submitted_at":"2026-04-30T18:25:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Two new surrogate models, trained on NR simulations, predict remnant properties and eccentricity dynamics for nonspinning eccentric black hole binaries with q ≤ 4 and e < 0.23.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Haney, \"Reanalysis of binary black hole gravitational wave events for orbital eccentricity signatures,\" Phys. Rev. D 112, 123004 (2025), arXiv:2504.15833 [gr-qc]. [19] Keisi Kacanja, Kanchan Soni, and Alexander Harvey Nitz, \"Eccentricity signatures in LIGO-Virgo-KAGRA's binary neutron star and neutron-star black holes,\" Phys. Rev. D112, 122007 (2025), arXiv:2508.00179 [gr-qc]. [20] Aasim Jan, Bing-Jyun Tsao, Richard O'Shaughnessy, Deirdre Shoemaker, and Pablo Laguna, \"GW200105: A detailed study of eccentricity in the neutron star- black hole binary,\" Phys. Rev. D113, 024018 (2026), arXiv:2508.12460 [gr-qc]. [21] Antoni Ramos-Buades, Sascha Husa, Geraint Pratten, Héctor Estellés, Cecilio García-Quirós, Maite Mateu- Lucena, Marta Colleoni, and Rafel Jaume, \"First sur-"},{"citing_arxiv_id":"2604.17868","ref_index":21,"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":"[19] Avinash Tiwari, Sajad A. Bhat, MD Arif Shaikh, and Shashvath J. Kapaida, \"Testing the nature of GW200105 by probing the frequency evolution of eccentricity,\" (2025), 17 arXiv:2509.26152 [astro-ph.HE]. [20] Keisi Kacanja, Kanchan Soni, and Alexander Harvey Nitz, \"Eccentricity signatures in LIGO-Virgo-KAGRA's BNS and NSBH binaries,\" (2025), arXiv:2508.00179 [gr-qc]. [21] Aasim Jan, Bing-Jyun Tsao, Richard O'Shaughnessy, Deirdre Shoemaker, and Pablo Laguna, \"GW200105: A detailed study of eccentricity in the neutron star-black hole binary,\" (2025), arXiv:2508.12460 [gr-qc]. [22] Khun Sang Phukon, Patricia Schmidt, Gonzalo Morras, and Geraint Pratten, \"Detection of GW200105 with a targeted ec- centric search,\" (2025), arXiv:2512."},{"citing_arxiv_id":"2604.11903","ref_index":30,"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":"lencia, First Eccentric Inspiral-Merger-Ringdown Anal- ysis of Neutron Star-Black Hole Mergers, Astrophys. J. 995, 47 (2025), arXiv:2506.01760 [astro-ph.HE]. [29] A. Jan, B.-J. Tsao, R. O'Shaughnessy, D. Shoemaker, and P. Laguna, GW200105: A detailed study of eccen- tricity in the neutron star-black hole binary, Phys. Rev. D113, 024018 (2026), arXiv:2508.12460 [gr-qc]. [30] K. Kacanja, K. Soni, and A. H. Nitz, Eccentricity sig- 35 natures in LIGO-Virgo-KAGRA's binary neutron star and neutron-star black holes, Phys. Rev. D112, 122007 (2025), arXiv:2508.00179 [gr-qc]. [31] A. Tiwari, S. A. Bhat, M. A. Shaikh, and S. J. Kapa- dia, Testing the Nature of GW200105 by Probing the Frequency Evolution of Eccentricity, Astrophys."},{"citing_arxiv_id":"2602.11030","ref_index":43,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Population Properties of Binary Black Holes with Eccentricity","primary_cat":"astro-ph.HE","submitted_at":"2026-02-11T16:55:29+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"First joint population inference on binary black hole eccentricity from GWTC-4 bounds the eccentric branching ratio below 5% at 90% confidence, with results consistent with quasi-circular models but highly model-dependent.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.20060","ref_index":47,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measuring Eccentricity and Addressing Waveform Systematics in GW231123","primary_cat":"gr-qc","submitted_at":"2025-12-23T05:24:54+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reanalysis of GW231123 shows no significant eccentricity, with parameter estimate differences explained by waveform model disagreements at strong spin precession.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.10803","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Detection of GW200105 with a targeted eccentric search","primary_cat":"gr-qc","submitted_at":"2025-12-11T16:46:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Targeted eccentric search detects GW200105 with SNR 13.4 and FAR <1/1000 yr, consistent with dynamical formation of the NSBH binary.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.10735","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constants of motion and fundamental frequencies for elliptic orbits at fourth post-Newtonian order","primary_cat":"gr-qc","submitted_at":"2025-11-13T19:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Derives the 4PN conservative map between constants of motion and fundamental frequencies for eccentric orbits, resummed over eccentricity and validated against circular-orbit and self-force results.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}