{"total":16,"items":[{"citing_arxiv_id":"2606.18081","ref_index":120,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Chirp-Mass Ladder: A New Rung Emerges","primary_cat":"astro-ph.HE","submitted_at":"2026-06-16T15:45:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The chirp-mass distribution of GW-detected binary black holes shows a ladder of peaks doubling in mass, with a new intermediate peak at 19 solar masses confirming a prior prediction from the hierarchical merger model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12792","ref_index":76,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Identification of Lensed Gravitational-Wave Beat Patterns by LISA","primary_cat":"astro-ph.CO","submitted_at":"2026-06-11T01:23:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Strong lensing of MBHBs produces identifiable beat patterns in about 7% of detectable two-image LISA events, with Bayesian inference recovering time delay and magnification parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11705","ref_index":126,"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":"2606.03346","ref_index":88,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Model-Independent Search Discards Faint Lensed-Pairs of Gravitational Wave Events in the Sub-Threshold Candidates of GWTC-4","primary_cat":"gr-qc","submitted_at":"2026-06-02T08:57:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A cross-correlation search of ~11,000 event pairs in GWTC-4 including sub-threshold candidates finds no lensed GW pairs above 3σ, setting an upper bound of ≤1.5/yr on the lensing rate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02690","ref_index":124,"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":"2605.21640","ref_index":10,"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":"2605.15749","ref_index":40,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on primordial black holes from the first part of LIGO-Virgo-KAGRA fourth observing run","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T09:07:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LIGO-Virgo-KAGRA O4a data yields the strongest constraints on primordial black hole abundance for 0.6-100 solar masses, with resolvable mergers dominating the limits and no compelling evidence for a PBH contribution in joint fits with astrophysical black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11703","ref_index":221,"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":"background","top_context_polarity":"background","context_text":"(LIGO Scientific Collaboration, Virgo Col- laboration), Effects of waveform model systematics on the interpretation of GW150914, Classical Quantum Gravity34, 104002 (2017), arXiv:1611.07531 [gr-qc]. [220] K. S. Thorne, Gravitational radiation, inThree hundred years of gravitation, edited by S. W. Hawking and W. Israel (Cam- bridge University Press, Cambridge, 1987) Chap. 9, pp. 330- 458. [221] L. S. Finn and D. F. Chernoff, Observing binary inspiral in gravitational radiation: One interferometer, Phys. Rev. D47, 2198 (1993), arXiv:gr-qc/9301003. [222] B. F. Schutz, Networks of gravitational wave detectors and three figures of merit, Classical Quantum Gravity28, 125023 (2011), arXiv:1102.5421 [astro-ph.IM]. [223] B. P. Abbottet al.(LIGO Scientific Collaboration, Virgo Col-"},{"citing_arxiv_id":"2605.09660","ref_index":10,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Testing the consistency of cosmological models with multimessenger astronomy","primary_cat":"gr-qc","submitted_at":"2026-05-10T17:16:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Derives multimessenger consistency relations for luminosity distances in the Friedmann model, including a curvature parameter expressed solely in terms of flatness-biased distances and a cosmological-constant relation independent of flatness assumptions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.22441","ref_index":96,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"How lonely are the Binary Compact Objects Detected by the LIGO-Virgo-KAGRA Collaboration?","primary_cat":"astro-ph.HE","submitted_at":"2026-04-24T10:59:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"No three-body encounter signatures detected in GW170817, GW190814, and GW230627_015337, constraining intermediate-mass black holes above 100 solar masses within roughly 0.1 AU of these binaries.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"S. Finn and D. F. Chernoff, Observing binary inspi- ral in gravitational radiation: One interferometer, Phys. Rev. D47, 2198 (1993), arXiv:gr-qc/9301003. [95] B. Allen and J. D. Romano, Detecting a stochastic background of gravitational radiation: Signal process- ing strategies and sensitivities, Phys. Rev. D59, 102001 (1999), arXiv:gr-qc/9710117. [96] B. Abbottet al.(LIGO Scientific), Upper limit map of a background of gravitational waves, Phys. Rev. D76, 082003 (2007), arXiv:astro-ph/0703234. [97] B. P. Abbottet al.(LIGO Scientific, Virgo), Up- per Limits on the Stochastic Gravitational-Wave Back- ground from Advanced LIGO's First Observing Run, Phys. Rev. Lett.118, 121101 (2017), [Erratum: Phys."},{"citing_arxiv_id":"2604.11903","ref_index":117,"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":"024007 (2017), arXiv:1705.02369 [gr-qc]. [115] B. S. Sathyaprakash and S. V. Dhurandhar, Choice of filters for the detection of gravitational waves from co- alescing binaries, Phys. Rev. D44, 3819 (1991). [116] L. S. Finn and D. F. Chernoff, Observing binary inspi- ral in gravitational radiation: One interferometer, Phys. Rev. D47, 2198 (1993), arXiv:gr-qc/9301003. [117] B. P. Abbottet al.,Noise curves used for Simulations in the update of the Observing Scenarios Paper, Tech. Rep. LIGO-T2000012 (LIGO Virgo KAGRA Collaboration, 2020). [118] B. F. Schutz and M. Tinto, Antenna patterns of inter- ferometric detectors of gravitational waves - I. Linearly polarized waves, Mon. Not. Roy. Astron. Soc.224, 131 (1987). [119] I."},{"citing_arxiv_id":"2603.06010","ref_index":53,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Accelerated Time-domain Analysis for Gravitational Wave Astronomy","primary_cat":"gr-qc","submitted_at":"2026-03-06T08:07:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Presents a practical fully time-domain end-to-end likelihood for gravitational-wave inference with structured linear algebra and GPU acceleration.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Divakarla, P. J. Easter, B. Goncharov,et al., Astrophys. J. Suppl. Ser.241, 27 (2019). 20 [51] P. D. Welch, IEEE Transactions on Audio and Electroa- coustics15, 70 (1967). [52] N. J. Cornish, T. B. Littenberg, B. B' ecsy, K. Chatzi- ioannou, J. A. Clark, S. Ghonge, and M. Mill- house, Physical Review D103, 044006 (2021), arXiv:2011.09494 [gr-qc]. [53] G. L. Turin, IRE Transactions on Information Theory 6, 311 (1960). [54] C. W. Helstrom,Statistical Theory of Signal Detection, 2nd ed. (Pergamon Press, 1968). [55] L. A. Wainstein and V. D. Zubakov,Extraction of Sig- nals from Noise(Dover Publications, 1970). [56] B. Owen and B. Sathyaprakash, Phys. Rev. D60, 022002 (1999), arXiv:gr-qc/9808076 . [57] N."},{"citing_arxiv_id":"2512.15877","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling the frequency-domain ringdown amplitude of comparable-mass mergers with greybody factors","primary_cat":"gr-qc","submitted_at":"2025-12-17T19:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A four-parameter greybody factor model reproduces the frequency-domain ringdown amplitude of comparable-mass aligned-spin mergers with mismatches of order 10^{-5}, improving existing models by two orders of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2004.06503","ref_index":49,"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":"of Scientists and Engineers I, Asymptotic Methods and Pertur- bation Theory(Springer, New York, 1999). 33 [46] E. Racine, Phys. Rev.D78, 044021 (2008), arXiv:0803.1820 [gr-qc]. [47] A. Klein, N. Cornish, and N. Yunes, Phys. Rev.D88, 124015 (2013), arXiv:1305.1932 [gr-qc]. [48] M.Kesden,D.Gerosa,R.O'Shaughnessy,E.Berti, andU.Sper- hake, Phys. Rev. Lett.114, 081103 (2015), arXiv:1411.0674 [gr-qc]. [49] K. Chatziioannou, A. Klein, N. Yunes, and N. Cornish, Phys. Rev.D88, 063011 (2013), arXiv:1307.4418 [gr-qc]. [50] A. Klein, N. Cornish, and N. Yunes, Phys. Rev.D90, 124029 (2014), arXiv:1408.5158 [gr-qc]. [51] M. Cabero, A. B. Nielsen, A. P. Lundgren, and C. D. Capano, Phys. Rev.D95, 064016 (2017), arXiv:1602.03134 [gr-qc]. [52] L. Blanchet, Living Rev."},{"citing_arxiv_id":"1912.11716","ref_index":107,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo","primary_cat":"gr-qc","submitted_at":"2019-12-25T21:15:52+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The LIGO and Virgo collaborations have released the gravitational-wave strain time series data from O1 and O2 observing runs, sampled at 16384 Hz, together with data-quality information through the Gravitational Wave Open Science Center.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Virgo operated with a duty factor of 85.1% during O2 (see table 1 of [7]). If we define thenetwork duty factor by the time percentage during which all the detectors in the network are in science mode simultaneously, we find 42.8% for the LIGO network during O1 and 46.1% during O2 [14]. For the LIGO-Virgo network it was 35%. It is customary to quantify the detector sensitivity by therange [107, 108], i.e., the distance to which sources can be observed. In Figs. 1 and 2, theBNS range iscalculatedassumingthattheobservedsourceisacoalescenceofcompact objects of masses of 1.4 M⊙ each, the observation has a minimum threshold in signal-to-noise ratio (SNR) of 8, and the range is averaged over all possible sky locations and orientations of the source, following [107]."},{"citing_arxiv_id":"1403.7377","ref_index":138,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Confrontation between General Relativity and Experiment","primary_cat":"gr-qc","submitted_at":"2014-03-28T14:04:31+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Experiments confirm general relativity to high precision in weak-field and strong-field regimes, with gravitational wave damping matching predictions to better than 0.5 percent.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}