{"total":12,"items":[{"citing_arxiv_id":"2606.31304","ref_index":54,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A parametric signal plus noise inference framework for short duration non-Gaussian noise transients","primary_cat":"gr-qc","submitted_at":"2026-06-30T08:17:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bilby-antiglitch jointly models astrophysical signals and quasi-physical glitches to recover true source properties from simulated gravitational wave data contaminated by loud non-Gaussian transients.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21691","ref_index":49,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Getting Tilted: Random Walk of Binary Black Hole Spin-Orbit Alignment in Dense Star Clusters","primary_cat":"astro-ph.HE","submitted_at":"2026-06-19T19:00:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Models BBH spin-orbit alignment as random walk on sphere, deriving exact distribution after n encounters and showing alignment survives several strong encounters before isotropy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.08961","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Rapid intermediate-mass black hole formation via runaway mergers of black holes","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T03:00:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"According to the expression of J. Binney & S. Tremaine (1987, Eq. 7.194), the formula abouttc is 1 tc = 4√πnσ \u0012 r2 coll + Gm σ2 rcoll \u0013 ,(10) wherer coll denotes the pericenter distance of the BBH. And the GW merger timescaletGW. The formula fortGW is taken from P. C. Peters (1964): c0 = a(1−e 2) e12/19 1 (1 + 121 304 e2)870/2299 (11) β= 64 5 G3m1m2(m1 +m 2) c5 (12) tGW = 12 19 c4 0 β × Z e 0 dee29/19[1 + (121/304)e2]1181/2299 (1−e 2)3/2 (13) The two timescales intersect ata∼102-103 R⊙, consistent with the location of the second peak in Figure 2. Below this threshold,tGW < tc, implying that binaries merge via GW emission before subsequent close encounters can disrupt them. 3.4.BBH Merger Property and Gravitational Wave Events"},{"citing_arxiv_id":"2606.07505","ref_index":239,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Primordial Black Hole Triggered Type Ia Supernovae II: Comparison with Supernova Remnants and Galactic Chemical Evolution","primary_cat":"astro-ph.HE","submitted_at":"2026-06-05T17:56:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"PBH-triggered SN Ia models across metallicities match some observed light curves and remnants, constrain the explosion channel fraction via chemical evolution modeling, and indicate PBHs as a potentially major early-universe SN Ia source.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06209","ref_index":137,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The first decade of gravitational-wave measurements of black hole spins","primary_cat":"gr-qc","submitted_at":"2026-06-04T14:14:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"A review summarizing formation-channel predictions, waveform effects, and population-level constraints on stellar-mass black hole spins from the first decade of gravitational-wave observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"a tilt angle with respect to the orbital angular momentum, θ, and two azimuthal angles, ϕ12 andϕ JL . Spins have two primary effects on the evolution of a compact-object binary and its emitted gravitational radiation. If the spins are misaligned to the orbital angular momen- tum, ⃗L, for most parameter configurations, the binary will undergo simple precession [137]. In this case, the spin and orbital angular momentum vectors precess about the total angular momentum, ⃗J, at a frequency that is small compared to the frequency of the GW radiation. A binary that sweeps through the band of ground-based GW detectors from ∼ 10 − 500 Hz will undergo O(10) precession cycles, with most of these precession cycles occurring at low"},{"citing_arxiv_id":"2606.04082","ref_index":130,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamics and detectability of long-lived non-accretion phases for massive black hole binaries in cold, thermally regulating disks","primary_cat":"astro-ph.HE","submitted_at":"2026-06-02T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Self-consistent thermal regulation in circumbinary disks permits long-lived non-accretion phases that suppress binary feeding rates toward the Eddington limit while leaving optical/near-IR detectability intact.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29759","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Gyroscopic Precession in Axisymmetric Kerr Spacetime: Horizon Regularity and Coordinate Effects","primary_cat":"gr-qc","submitted_at":"2026-05-28T11:08:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In Kerr spacetime, the Frenet-Serret precession frequency for timelike trajectories remains finite near the horizon in horizon-penetrating coordinates, demonstrating that Boyer-Lindquist divergences are coordinate effects dependent on the trajectory being timelike.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27225","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2026-05-26T16:09:49+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":8.0,"formal_verification":"none","one_line_summary":"GWTC-5.0 adds 161 new compact binary coalescence candidates from O4b with p_astro >= 0.5, detailed properties for 104, all binary black holes, for a cumulative total of 390.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"List of O4b candidates with FAR <1 yr −1, for which glitch mitigation was performed. Candidate GPS time [s] Detector Time window [s] Frequency range [Hz]f low [Hz] GW240413_022019 - L - - 30 GW240514_121713 1399724251.72 L [0.70,2.00] [20, 35] - GW240515_005301 1399769599.11 L[−4.01,−3.01][10, 50] - GW240520_213616 1400276194.97 L [−0.28,−0.04] [60, 90] - GW240525_031210 1400641948.64 L[−4.64,−4.24][10, 30] - GW240531_075248 1401177186.46 V [−0.30,−0.20] [120, 200] - GW240601_061200 1401257538.36 L[0.52,0.73][200, 300] - GW240601_231004 1401318622.03 L [−5.30,−4.55] [20, 30] - GW240612_081540 - L - - 30 GW240615_160735 1402502873.33 L [−0.05,−0.01] [100, 300] - GW240621_200935 1403035793.53 L[0.30,0.40][200, 300] - GW240621_200935 1403035793."},{"citing_arxiv_id":"2605.27223","ref_index":38,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2026-05-26T16:09:47+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"GWTC-5.0 is a data release documenting over 300 gravitational-wave events from compact binary mergers observed through early 2025.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.18082","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-4.0: Updating the Gravitational-Wave Transient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run","primary_cat":"gr-qc","submitted_at":"2025-08-25T14:46:09+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.08219","ref_index":139,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2006.12611","ref_index":41,"ref_count":1,"confidence":0.88,"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}],"limit":50,"offset":0}