{"total":40,"items":[{"citing_arxiv_id":"2606.31350","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Compactness Inference in Gravitational-Wave Mergers with PhenomDECO: Catalog Benchmarks and Robustness Diagnostics","primary_cat":"gr-qc","submitted_at":"2026-06-30T08:47:30+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":"2606.29576","ref_index":105,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quark and hybrid stars with renormalization group improvement of NNLO perturbative QCD","primary_cat":"nucl-th","submitted_at":"2026-06-28T19:42:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"RGOPT-resummed NNLO pQCD EoS for massive quarks in beta equilibrium is fitted and applied to construct pure quark stars (X=3.08-3.58) and hybrid stars (X~2-2.98) compatible with PSR J0740+6620 and GW190814.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28156","ref_index":90,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Joint inference of line-of-sight acceleration and orbital eccentricity in neutron-star--black-hole binaries","primary_cat":"gr-qc","submitted_at":"2026-06-26T14:52:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"All five NSBH events are consistent with zero line-of-sight acceleration; the joint posterior for GW200105_162426 disfavors both zero LOSA and zero eccentricity at 90% credibility.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18081","ref_index":59,"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":"2606.10011","ref_index":248,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Multi-Wavelength View of the First Type Ic-BL Supernova with an Einstein Probe X-ray Shock Breakout","primary_cat":"astro-ph.HE","submitted_at":"2026-06-08T18:01:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First definitive X-ray shock breakout from a Type Ic-BL supernova, with radio constraints and a rate calculation implying most such supernovae produce fainter signals than observed here.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.08838","ref_index":71,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Line-of-sight acceleration in compact binaries with higher harmonics and eccentricity","primary_cat":"gr-qc","submitted_at":"2026-06-07T21:06:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Implements consistent line-of-sight acceleration corrections in quasi-circular and eccentric GW waveform models, applies them to GWTC-3 events, and reports no substantial evidence for acceleration while warning of bias from inconsistent harmonic treatment.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04810","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Fast gravitational waveform models for quasi-circular coalescences of neutron star--black hole binaries","primary_cat":"gr-qc","submitted_at":"2026-06-03T12:35:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Presents new NSBH waveform models IMRPhenomXHM_NSBH, SEOBNRv5HM_ROM_NRTidalv3_NSBH, and IMRPhenomXPHM_NSBH incorporating higher modes and tidal effects via NRTidalv3 extensions, validated against NR simulations and applied to GWTC events.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02966","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Sensitivity of the Neutron Star Equation of State Inferences to Mass and Radius Measurements","primary_cat":"astro-ph.HE","submitted_at":"2026-06-02T00:08:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Theoretical inputs and the 2 solar mass lower limit dominate neutron star equation of state constraints across most densities, while radius data refines low densities and higher masses affect wider ranges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28716","ref_index":148,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Eccentric and unbound compact binaries in the LIGO-Virgo-KAGRA catalog: parameter estimation and waveform systematics with SEOBNRv6EHM","primary_cat":"gr-qc","submitted_at":"2026-05-27T16:38:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SEOBNRv6EHM reduces parameter biases for eccentric binaries versus prior models and shows mild support for eccentricity in five catalog events plus comparable unbound fits for three high-mass events.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"tected to date, to test the robustness ofSEOBNRv6EHM for highly asymmetric binaries. GW241011 233834 and GW241110 124123 [86] are asymmetric, high- spin BBH events from O4b, identified as potential products of hierarchical mergers and found consistent with QC orbits withSEOBNRv5EHMandTEOBResumS- Dal' ı[86]. GW231123135430, the most massive BBH event observed to date, is also included [148]; evi- dence for the EAS hypothesis over QCAS has been re- ported withTEOBResumS-Dal' ı[93, 101] andIMRPhe- nomTEHM[100], although in both cases the QCP hypoth- esis is preferred; withSEOBNRv5EHMthe EAS hypothe- sis is disfavored even relative to QCAS [87]. The sam- ple is completed by the benchmark events GW150914 and GW170817 discussed in Sec. IV A."},{"citing_arxiv_id":"2605.26308","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nuclear Physics of Binary Neutron Star Mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-05-25T19:59:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"densities not too far from saturation, typically up to a few timesn 0, with the precise range determined by the convergence properties of the series. Within this domain, however, the expansion provides a transparent way to identify how individual nuclear matter properties influence the EoS and how their uncertainties propagate to neutron star observables. The stiffness of the EoS is conveniently characterized by the speed of sound, c2 s = dP dϵ ,(5) which measures how efficiently pressure responds to changes in energy density. A stiffer EoS, corresponding to a larger c2 s, supports more massive and generally larger neutron stars. Causality requiresc s ≤c, while a non-interacting gas of massless particles - relevant to the asymptotically free quarks at very high (energy) densities - givesc 2 s = 1/3, known"},{"citing_arxiv_id":"2605.25705","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Ces\\`aro convergence of the high-order WKB method and its applications to black-hole overtones and long-lived modes","primary_cat":"gr-qc","submitted_at":"2026-05-25T11:03:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"High-order WKB with Padé approximants and Cesàro means enables computation of black-hole overtones and long-lived quasinormal modes, with a noted limitation that apparent convergence can be incorrect for some metrics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02593","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hybrid stars among mass gap objects are excluded by twin stars at $1.4\\,M_\\odot$","primary_cat":"astro-ph.HE","submitted_at":"2026-05-21T17:57:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of generic hybrid EOS with first-order deconfinement shows mass-gap hybrids require early transition and stiff quark matter, but data favor twins at 1.4 M_sun that exclude them.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21580","ref_index":50,"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":"2605.17647","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Scattering, absorption and greybody factor of scalar particles by Lorentz-violating charged black holes","primary_cat":"gr-qc","submitted_at":"2026-05-17T20:52:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Partial-wave calculations of scattering cross sections, absorption, and greybody factors for spin-0 particles on charged black holes in bumblebee and Kalb-Ramond Lorentz-violating models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13036","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Inspiral gravitational waveforms from charged compact binaries with scalar hair","primary_cat":"gr-qc","submitted_at":"2026-05-13T05:44:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In Einstein-scalar-Maxwell theories, charged compact binaries produce gravitational waveforms containing a leading -1 post-Newtonian dipole correction controlled by one deviation parameter b.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"125, 101102 (2020), arXiv:2009.01075 [gr-qc]. [14] R. Abbottet al.(LIGO Scientific and Virgo),Astrophys. J. Lett.896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]. [15] R. Abbottet al.(LIGO Scientific, Virgo and KAGRA),Astrophys. J. Lett.969, L34 (2024), arXiv:2404.04248 [astro-ph.HE]. [16] L. Hui and A. Nicolis,Phys. Rev. Lett.110, 241104 (2013), arXiv:1202.1296 [hep-th]. [17] M. Minamitsuji, K. Takahashi, and S. Tsujikawa,Phys. Rev. D105, 104001 (2022), arXiv:2201.09687 [gr-qc]. [18] M. Minamitsuji, K. Takahashi, and S. Tsujikawa,Phys. Rev. D106, 044003 (2022), arXiv:2204.13837 [gr-qc]. [19] G. W. Horndeski,Int. J. Theor. Phys.10, 363 (1974). [20] S. W. Hawking,Commun. Math. Phys.25, 152 (1972). [21] J. D. Bekenstein,Phys."},{"citing_arxiv_id":"2605.11703","ref_index":110,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"unclear","context_text":"Localization of Compact Binary Sources with Second Genera- tion Gravitational-wave Interferometer Networks, Astrophys. J.902, 71 (2020), arXiv:1909.12961 [astro-ph.HE]. [109] M. Emma, T. F. de Nobrega, and G. Ashton, Comparing advanced-era interferometric gravitational-wave detector net- work configurations: Sky localization and source properties, Phys. Rev. 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Messenger, P."},{"citing_arxiv_id":"2605.05005","ref_index":53,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Characterizing the quark-hadron mixed phase in compact star cores : sensitivity to nuclear saturation and quark-model parameters at finite-temperature","primary_cat":"nucl-th","submitted_at":"2026-05-06T15:06:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The quark-hadron mixed phase width in hybrid stars is mainly controlled by effective nucleon mass and symmetry energy, with temperature reducing the width and softening the EOS while strong vector repulsion is needed to match massive pulsar and NICER data.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"values of the compressibility(K sat), symmetry energy(J) and its slope (L). contribution of the speed of sound (Fig. 3(c)), quanti- fied by ∆ ′. The quantity ∆ ′ can assume both positive and negative values, depending on the thermodynamic regime. For the hadronic phase, ∆′ is always negative (for the details of the thermodynamic decomposition refer to [53].) In the pure hadronic phase, lower temperatures are associated with smaller values of ∆ ′. In contrast, within the mixed phase, ∆ ′ exhibits a sign change; increasing temperature leads to an enhancement of ∆ ′. We have systematically studied the behavior of the speed of sound for different nuclear and quark matter parameters, as shown in Figs. 3 and 4."},{"citing_arxiv_id":"2605.01737","ref_index":64,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Axial $w$-modes of anisotropic neutron stars","primary_cat":"gr-qc","submitted_at":"2026-05-03T06:25:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Axial w-mode frequencies of anisotropic neutron stars decrease monotonically with mass, depend approximately linearly on compactness with anisotropy modifying slope and intercept, damping times increase with mass, and empirical expressions are given for both as functions of compactness and anisotrop","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Zheng, PSR J0952−0607: The Fastest and Heav- iest Known Galactic Neutron Star, Astrophys. J. Lett. 934, L17 (2022), arXiv:2207.05124 [astro-ph.HE]. [63] R. Abbottet al.(LIGO Scientific, Virgo), GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object, Astrophys. J. Lett.896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]. [64] N. Andersson and G. L. Comer, Relativistic fluid dynam- ics: Physics for many different scales, Living Rev. Rel. 10, 1 (2007), arXiv:gr-qc/0605010. [65] Y. Kojima, Equations governing the nonradial oscilla- tions of a slowly rotating relativistic star, Phys. Rev. D 46, 4289 (1992). [66] E. W. Leaver, An Analytic Representation for the Quasi- Normal Modes of Kerr Black Holes, Proc."},{"citing_arxiv_id":"2604.12020","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Beyond the Standard Model of Cosmology: Testing new paradigms with a Multiprobe Exploration of the Dark Universe","primary_cat":"astro-ph.CO","submitted_at":"2026-04-13T20:05:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Proposes primordial black holes from modified small-scale fluctuations and entropic acceleration in expanding spacetime as explanations for dark matter and dark energy.","context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"long-duration events with small chirp masses and mass ratios. We are actively contributing to the O4 SSM analysis, and I also plan to study correlations between pipelines and signal coherent tests among the three LVK detectors on simulated SSM signals and background triggers, in order to properly assess the significance of the SSM candidates. In the lower mass gap, there are two confirmed compact objects [55], both most likely black holes, due to their mass and lack of tidal deformation. No known supernova core-collapse models can generate these types of objects. In particular, GW190814 [56], with its secondary BH in the LMG, highly asymmetric masses and zero spin, challenges all existing astrophysical models [56], while events like this one are expected in the THM [18]."},{"citing_arxiv_id":"2604.11845","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Quasi-resonances in the vicinity of Einstein-Maxwell-dilaton black hole","primary_cat":"gr-qc","submitted_at":"2026-04-12T21:06:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Increasing the mass of a perturbing scalar field around Einstein-Maxwell-dilaton black holes strongly suppresses damping in several quasinormal branches, producing quasi-resonant long-lived oscillations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cosmol.31, 423 (2025). [4] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [5] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [6] R. Abbottet al.(LIGO Scientific, Virgo), Astrophys. J. Lett.896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]. [7] R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr- qc]. [8] B. P. Abbottet al.(KAGRA, LIGO Scientific, Virgo), Living Rev. Rel.19, 1 (2016), arXiv:1304.0670 [gr-qc]. [9] R. A. Konoplya, Gen. Rel. Grav.34, 329 (2002), arXiv:gr-qc/0109096. [10] R. A. Konoplya, Phys. Rev. D66, 084007 (2002), arXiv:gr-qc/0207028."},{"citing_arxiv_id":"2604.07388","ref_index":51,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GW190711_030756 and GW200114_020818: astrophysical interpretation of two asymmetric binary black hole mergers in the IAS catalog","primary_cat":"astro-ph.HE","submitted_at":"2026-04-08T05:45:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Two asymmetric BBH mergers are characterized with mass ratios 0.35 and ≤0.20; one shows high spins, negative χ_eff, and strong precession, suggesting an emerging population of massive rapidly spinning systems.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"vation of a Binary-Black-Hole Coalescence with Asymmetric Masses,\" Phys. Rev. D102, 043015 (2020), arXiv:2004.08342 [astro-ph.HE]. [50] Tousif Islam, Scott E. Field, Carl-Johan Haster, and Rory Smith, \"Improved analysis of GW190412 with a precessing numerical relativity surrogate waveform model,\" Phys. Rev. D 103, 104027 (2021), arXiv:2010.04848 [gr-qc]. [51] R. Abbottet al.(LIGO Scientific, Virgo), \"GW190814: Gravi- tational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object,\" Astrophys. J. Lett.896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]. [52] Tousif Islam, Avi Vajpeyi, Feroz H. Shaik, Carl-Johan Haster, Vijay Varma, Scott E. Field, Jacob Lange, Richard"},{"citing_arxiv_id":"2603.10844","ref_index":104,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Long-lived quasinormal modes, shadows and particle motion in four-dimensional quasi-topological gravity","primary_cat":"gr-qc","submitted_at":"2026-03-11T14:52:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Massive scalar quasinormal modes in quasi-topological black holes become long-lived as scalar mass grows, while photon-sphere radius, shadow size, and ISCO exhibit moderate deviations from Schwarzschild.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D 94, 069902 (2016)], arXiv:1404.3197 [gr-qc]. [101] B. C. Lütfüoğlu, A. Shermatov, J. Ray- imbaev, M. Matyoqubov, and O. Sir- ajiddin, Eur. Phys. J. C 85, 1484 (2025), arXiv:2511.22366 [gr-qc]. [102] R. A. Konoplya and A. Zhi- denko, Phys. Rev. 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D 77, 084019 (2008),"},{"citing_arxiv_id":"2602.11001","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Two types of quasinormal modes of Casadio-Fabbri-Mazzacurati brane-world black holes","primary_cat":"gr-qc","submitted_at":"2026-02-11T16:23:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Quasinormal modes of massive scalars in CFM brane-world black holes split into two types, with modes disappearing at critical masses where real or imaginary frequency parts reach zero.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"26, 163001 (2009), arXiv:0905.2975 [gr-qc]. [4] S. V. Bolokhov and M. Skvortsova, Grav. Cosmol. 31, 423 (2025), arXiv:2504.05014 [gr-qc]. [5] B. P. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. Lett. 116, 061102 (2016), arXiv:1602.03837 [gr-qc]. [6] B. P. Abbott et al. (LIGO Scientific, Virgo), Phys. Rev. Lett. 119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [7] R. Abbott et al. (LIGO Scientific, Virgo), Astrophys. J. Lett. 896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]. [8] S. Babak, J. Gair, A. Sesana, E. Barausse, C. F. Sop- uerta, C. P. L. Berry, E. Berti, P. Amaro-Seoane, A. Pe- titeau, and A. Klein, Phys. Rev. D 95, 103012 (2017), arXiv:1703.09722 [gr-qc]. [9] L. Randall and R. Sundrum, Phys. Rev. Lett."},{"citing_arxiv_id":"2601.17906","ref_index":69,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Telling tails and quasi-resonances in the vicinity of Dymnikova regular black hole","primary_cat":"gr-qc","submitted_at":"2026-01-25T16:54:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Massive scalar perturbations on the Dymnikova regular black hole exhibit growing oscillation frequencies, reduced damping rates leading to quasi-resonances, power-law oscillatory tails, and mass-dependent suppression of grey-body factors.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Time-Domain Integration A powerful method for determining quasinormal fre- quencies is to solve the perturbation equation directly in the time domain. Rewriting the master equation in terms of the null coordinates u = t − r∗ and v = t + r∗ , one discretizes the resulting wave equation on a characteris- tic grid following the well-known algorithm of [69]. An initial Gaussian pulse is propagated through the effective potential, producing the full time evolution of the field 4 /Minus20 /Minus10 10 20 30 40 r/Star 0.05 0.10 0.15 0.20 0.25 0.30 0.35 V /LParen1r/Star/RParen1 /Minus20 /Minus10 10 20 30 40 r/Star 0.05 0.10 0.15 0.20 0.25 0.30 0.35 V /LParen1r/Star/RParen1 FIG. 1. Effective potential as a function of the tortoise coor dinate r∗ for ℓ = 0 (left) and ℓ = 1 (right), µ = 0."},{"citing_arxiv_id":"2512.24194","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Impact of Anisotropy on Neutron Star Structure and Curvature","primary_cat":"gr-qc","submitted_at":"2025-12-30T12:53:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Moderate positive pressure anisotropy raises neutron star maximum mass to about 2.4 solar masses and compactness by up to 20 percent, with curvature scalars tied to matter showing strong sensitivity while the Weyl scalar stays largely insensitive.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.22698","ref_index":42,"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":"2509.14924","ref_index":64,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Residual Test for the Third Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2025-09-18T13:00:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Residuals after subtracting best-fit waveforms from GWTC-3 events show no significant deviation from noise according to three standard goodness-of-fit tests.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.14849","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Robust and Efficient F-statistic-based Framework for Consistent Bayesian Inference of Compact Binary Coalescences","primary_cat":"gr-qc","submitted_at":"2025-09-18T11:14:14+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"F-statistic framework analytically maximizes over distance and polarization to enable faster Bayesian inference of compact binary coalescences with a new evidence formulation that matches full frequency-domain results at lower cost.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.13638","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"An Implementation to Identify the Properties of Multiple Population of Gravitational Wave Sources","primary_cat":"gr-qc","submitted_at":"2025-09-17T02:25:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GWKokab is a new modular JAX framework that uses normalizing flow samplers for efficient inference on subpopulations of compact binary mergers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.15951","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter","primary_cat":"hep-ph","submitted_at":"2025-07-21T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Future high-frequency-sensitive GW detectors can distinguish binary neutron star from low-mass black hole mergers in late phases, enabling separation of merger rates and constraints on heavy non-annihilating dark matter via transmuted black holes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"hole (BH) binaries and provided a new way to study general relativity. During the O3a+b observing runs, the LIGO-Virgo-KAGRA (LVK) Collabora- tion [4] has reported a number of compact binary coalescence (CBC) events with com- ponent masses that resist clear classification as either neutron stars (NSs) or low-mass black holes (LMBHs). Examples include GW190425 [5], GW190814 [6], GW230529 [7], - 1 - and SSM200308 [8], where at least one of the components is either in the lower mass- gap region, viz. 2 .5 − 5 M⊙, or even lighter [9-11]. Such LMBHs are not expected as a product of standard stellar evolution, and thus the current practice is to provisionally classify CBCs as NSs or BHs using the inferred mass. Nevertheless, such a classification"},{"citing_arxiv_id":"2506.22363","ref_index":24,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Binary black holes in the heat of merger","primary_cat":"gr-qc","submitted_at":"2025-06-27T16:25:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Develops a frequency-domain approximant for tidal heating in nonspinning black hole binaries that extends to merger and includes horizon parameters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2406.03568","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2311.01300","ref_index":210,"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":"vironments fill the mass gap from pair-instability supernovae [123, 208, 209]. LISA will be particularly sensitive to more massive BBHs. Most observed BBHs have mass ratiosq ≲ 3.3, which is consistent with the bulk of model predictions, but systems with more extreme mass ratios are possible, such as GW190814, which involved a 23 M⊙ BH and a ∼ 2.6M⊙ companion [210]. As mentioned above, most observed BBHs have low to moderate companion spins, though it remains unclear whether this is a generic feature of stellar-mass BHs [211, 212]. Lastly, high eccentricities and generic spin-orbit misalignments could be a telltale sign of dynamical formation in dense stellar environments or in hierarchical triples (see Refs."},{"citing_arxiv_id":"2204.05305","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Galaxy and halo angular clustering in LCDM and Modified Gravity cosmologies","primary_cat":"astro-ph.CO","submitted_at":"2022-04-11T17:58:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"N-body light-cone mocks show 2-4 sigma deviations in third-order angular clustering between LCDM and f(R)/nDGP models at z=0.15-0.3 for halos and galaxies, with stronger signals in the dark-matter field.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2112.06861","ref_index":139,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Tests of General Relativity with GWTC-3","primary_cat":"gr-qc","submitted_at":"2021-12-13T18:19:04+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"No evidence for physics beyond general relativity is found in the analysis of 15 GW events from GWTC-3, with consistency in residuals, PN parameters, and remnant properties.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"system and a higher SNR would be needed for them to be confidently detected [5, 136, 137]. We perform Bayesian parameter estimation using either the Python-based package bilby [138, 139] or the soft- ware library LALInference [140], which belongs to the LIGO Scientific Collaboration Algorithm Library Suite [141]. Runs performed with bilby are automated through the pack- age bilby pipe [139] and rely on static nested sampling [142] as available through the package dynesty [143], while LALInference runs use either nested or Markov-chain Monte Carlo sampling [ 144]. One of the ringdown tests presented here makes use of pyRing [145], which relies on cpnest 14 TABLE II. List of O3b events considered in this paper. The first block of columns gives the names of the events and lists the instruments (LIGO"},{"citing_arxiv_id":"2108.01045","ref_index":41,"ref_count":1,"confidence":0.9,"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":"these have astrophysically interesting source properties under the default prior. Two of the new candidates pre- sented here have a primary component mass in the pair instability gap [32-40], and one of those shows support for high spin and unequal masses. We also find a new candidate whose masses are consistent with a neutron star-black hole binary (NSBH), although as in the case of GW190814 [41], we cannot rule out the possibility that the secondary component of the candidate could be a low-mass black hole. In this work, all the analyses make use of the final version of the strain data with improved calibration and noise subtraction, which includes non-linear subtraction around the 60 Hz frequency of the US power grid [42, 43]. The data used in this work have been released to the"},{"citing_arxiv_id":"2010.14529","ref_index":70,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"method","top_context_polarity":"use_method","context_text":"Lett. 896, L44 (2020), arXiv:2006.12611 [astro-ph.HE]. [67] B. P. Abbottet al.(LIGO Scientific and Virgo Collaboration), Astrophys. J. Lett.892, L3 (2020), arXiv:2001.01761 [astro- ph.HE]. [68] A. H. Nitzet al., PyCBC software, https://github.com/ ligo-cbc/pycbc(2018). [69] T. Dal Cantonet al., Phys. Rev. D90, 082004 (2014), arXiv:1405.6731 [gr-qc]. [70] S. A. Usmanet al., Classical Quantum Gravity33, 215004 (2016), arXiv:1508.02357 [gr-qc]. [71] S. Sachdevet al., arXiv:1901.08580 [gr-qc] (2019). [72] C. Messicket al., Phys. Rev. D95, 042001 (2017), arXiv:1604.04324 [astro-ph.IM]. [73] B. S. Sathyaprakash and S. V . Dhurandhar, Phys. Rev. D44, 3819 (1991). [74] L. Blanchet, T. Damour, B. R. Iyer, C."},{"citing_arxiv_id":"2010.14527","ref_index":33,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"background","top_context_polarity":"unclear","context_text":"itational wave candidate events from O3a have already been published separately due to their interesting prop- erties: GW190425 [32] is the second gravitational wave event consistent with a BNS coalescence; GW190412 [32] is the first BBH observation with definitively asymmet- ric component masses, which also produced detectable gravitational radiation beyond the leading quadrupolar order; GW190814 [33] is an even more asymmetric sys- tem having a ∼23 M⊙ object merging with a ∼2.6 M⊙ object, making the latter either the lightest black hole or heaviest neutron star known to be in a double compact object system; GW190521 [34, 35] is a BBH with total mass∼ 150 M⊙ having a primary mass above 65 M⊙ at 99% credibility. Here we present 13 candidate events for the first time"},{"citing_arxiv_id":"2006.02838","ref_index":293,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Primordial Black Holes as Dark Matter: Recent Developments","primary_cat":"astro-ph.CO","submitted_at":"2020-06-03T17:57:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Primordial black holes in specific mass ranges could account for some or all dark matter while resolving structure-formation and seed problems in standard cosmology.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"LIGO/Virgo collaboration has reported the detection of three events, all of which (remarkably) fall within the predicted regions. Two of the them (GW190425 and GW190814) involve mergers with one component in the 2 − 5 M⊙ mass gap [291, 292] and populate regions 4 or 5 of Fig. 5. The first could be a merger of PBHs at the \"proton\" peak , while the second corresponds to the \"pion\" plateau, as also argued in Reference [293]. The third event (GW190521) involves a merger with at least one component in the pair-instability mass gap [294, 295] and populates region 2 of Fig. 5. Second, for a given PBH mass distribution, one can calculate the number of supermassive PBHs for each halo. It is found that there is one 10 8 M⊙ PBH per 10 12 M⊙ halo, with 10 times as many smaller ones for ns≈ 0."},{"citing_arxiv_id":"2006.00714","ref_index":215,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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}],"limit":50,"offset":0}