{"total":14,"items":[{"citing_arxiv_id":"2606.31757","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The location of the upper edge of the pair-instability supernovae black hole mass gap","primary_cat":"astro-ph.HE","submitted_at":"2026-06-30T14:45:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The upper edge of the PISN black hole mass gap shifts by up to 30 solar masses due to nuclear reaction rate uncertainties, primarily the 12C(α,γ)16O rate, while remaining robust to resolution variations unlike the lower edge.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21824","ref_index":117,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A grid of fast-rotating, chemically-homogeneous, supernova and/or long-GRB progenitors","primary_cat":"astro-ph.HE","submitted_at":"2026-06-20T01:25:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Presents a grid of 113 fast-rotating, chemically-homogeneous massive star models at Z=0.001 reaching core collapse with high angular momentum for use as supernova and GRB progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21691","ref_index":83,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.18081","ref_index":254,"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":"2606.02725","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Can current models predict the local black hole merger rate?","primary_cat":"astro-ph.HE","submitted_at":"2026-06-01T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Theoretical predictions for local BBH merger rates exceed observations by a factor >10 under conservative SFRD and metallicity assumptions, indicating need for revisions in stellar evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21640","ref_index":38,"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":"2605.21580","ref_index":232,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15310","ref_index":81,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T18:23:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Lumina runs a 500 cMpc radiation-hydrodynamic simulation combining IllustrisTNG galaxy formation with six-bin M1 radiation transport to predict late stellar-driven HI reionization ending around z=4.75 and AGN-driven HeII reionization nearly complete by z=3.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.02413","ref_index":92,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Black Hole Mass Gap as a New Probe of Millicharged Particles","primary_cat":"hep-ph","submitted_at":"2026-04-02T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Millicharged particles weaken pulsational pair-instability in massive stars, shifting the lower edge of the black hole mass gap upward and turning gravitational wave observations into a probe for particles with masses 35-200 keV and charges 10^{-10} to 10^{-9}.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"To estimate if the BHMG probe is competitive with existing constraints, we compare with analogous condi- tions in other stellar environments. For the TRGB con- straint, one requiresε χ < ε RG ν ≃10 erg g −1 s−1, eval- uated atT RG = 8.6 keVandρ RG ≃10 6 g/cm3, while for SN 1987A one findsεχ < ε SN ≃10 19 erg g−1 s−1 at TSN = 30 MeVandρ SN ≃3×10 14 g/cm3 [92]. In the low- mass limit, MCP production is dominated by plasmon decay,Q Dec ∼q 2α2T 3ω2 pl, so TRGB constraints domi- nate over the BHMG sensitivity in this regime. In con- trast, matching the relative importance of MCP and neu- trino cooling in the two environments-Compton emis- sion at HD and plasmon decay in supernovae-suggests the BHMG can surpass SN bounds for MCP masses"},{"citing_arxiv_id":"2602.11282","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Measurement prospects for the pair-instability mass cutoff with gravitational waves","primary_cat":"astro-ph.HE","submitted_at":"2026-02-11T19:00:22+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations show a 40-50 solar-mass black-hole cutoff is not guaranteed to be confidently recovered from GWTC-4-like catalogs, spurious detections are unlikely, and O4 data would reduce cutoff-mass uncertainty by at least 20 percent while yielding only a lower bound on the carbon-alpha reaction rate","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"form directly via stellar collapse [23-27]. Though there are candidate PISN observations, these are not confirmed (see, e.g., Refs. [28, 29] and references therein). There are also significant theoretical uncertainties that impact the location of the purported mass gap [27, 30-34]-most notably, nuclear reaction rates for 12C(α, γ)16O carbon- oxygen burning [25, 26, 35-37]. As GW observations constrain the source BH proper- ∗ matthew.mould@nottingham.ac.uk ties such as mass, they can be used to search for the im- prints of (pulsational) PISNe. Following the first GW transient catalog (GWTC-1) [6], Ref. [14] found that <1% of sources in the underlying population have masses >45M ⊙, potentially consistent with a PISN gap."},{"citing_arxiv_id":"2510.22698","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A new group of low-spin $50-70M_\\odot$ Black Holes and the high pair-instability mass cutoff","primary_cat":"astro-ph.HE","submitted_at":"2025-10-26T14:48:06+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":238,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"masses, the spins of GW231123's source are more con- sistent with the known population as it does not rule out large values. 6.3.Possible formation channels From theoretical predictions for the late-stage evolu- tion of massive stars (Fowler & Hoyle 1964; Barkat et al. 1967; Rakavy & Shaviv 1967; Fraley 1968; Bond et al. 1984; Woosley et al. 2002; Woosley 2017), contraction of the core leads to electron-positron pair production that reduces internal pressure support, causing further contraction that powers explosive nuclear burning and a rebounding shock. For helium-core masses≈32-64M ⊙, multiple pulsational episodes can eject sufficient mate- rial to reduce the mass below the pair-instability regime, ending with a BH remnant."},{"citing_arxiv_id":"2311.01300","ref_index":188,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Waveform Modelling for the Laser Interferometer Space Antenna","primary_cat":"gr-qc","submitted_at":"2023-11-02T15:15:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of existing waveform models for LISA sources and the challenges that must still be overcome.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"evolve only a negligable amount inband. 26 2.5. Stellar origin black hole binaries (SOBHBs) Coordinators: Antoine Klein and Ilya Mandel Contributor: D. Gerosa 2.5.1. Description Stellar origin BH binaries are BBHs with component masses ranging from a few solar masses up to about ∼ 50-100M⊙, where models of pair- instability supernovae predict a mass gap to appear [188-190]. Those systems are in a mass range such that they can be observed by both LISA and by ground-based detectors, as they sweep through a few decades in frequency during the last stage of their inspiral. This broad coverage of the GW frequency spectrum makes it possible to probe the evolutionary history of such binaries [141, 191]. A circular BBH with two 45 M ⊙ components will merge in about 10 years from a GW"},{"citing_arxiv_id":"2108.01045","ref_index":32,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"threshold Search for Strongly-lensed Gravitational-wave Events,\" arXiv e-prints (2019), arXiv:1904.06020 [gr- qc]. [31] Connor McIsaac, David Keitel, Thomas Collett, Ian Harry, Simone Mozzon, Oliver Edy, and David Ba- con, \"Search for strongly lensed counterpart images of binary black hole mergers in the first two LIGO observing runs,\" Phys. Rev. D 102, 084031 (2020), arXiv:1912.05389 [gr-qc]. [32] S. E. Woosley, \"Pulsational Pair-instability Supernovae,\" Astrophys. J. 836, 244 (2017), arXiv:1608.08939 [astro-ph.HE]. [33] S. E. Woosley, \"The Evolution of Massive Helium Stars, Including Mass Loss,\" Astrophys. J. 878, 49 (2019), arXiv:1901.00215 [astro-ph.SR]. [34] Simon Stevenson, Matthew Sampson, Jade Powell, Ale- jandro Vigna-G' omez, Coenraad J."}],"limit":50,"offset":0}