{"total":13,"items":[{"citing_arxiv_id":"2605.24704","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Shaping black hole resonances I. Black hole ringdown as a spectral filtering process","primary_cat":"gr-qc","submitted_at":"2026-05-23T19:05:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Quasinormal mode excitation in black hole ringdown equals the Fourier transform of the perturbation evaluated at the mode frequency, so black holes act as resonant spectral filters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15271","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Polarization Analysis of Ringdown Signals","primary_cat":"gr-qc","submitted_at":"2026-05-14T18:00:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Constrained polarization model for Kerr ringdown modes enables inclination inference from two-detector data for non-precessing mergers but introduces biases when applied to precessing systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.15431","ref_index":193,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms","primary_cat":"gr-qc","submitted_at":"2026-04-16T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Polynomial models for the (2,2) post-merger waveform amplitudes of eccentric non-spinning binary black holes are constructed from numerical-relativity data as functions of symmetric mass ratio and two merger-time dynamical parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"D100, 084031 (2019), arXiv:1901.05901 [gr-qc]. [190] H. Lim, G. Khanna, A. Apte, and S. A. Hughes, Phys. Rev. D100, 084032 (2019), arXiv:1901.05902 [gr-qc]. [191] X. Li, L. Sun, R. K. L. Lo, E. Payne, and Y. Chen, Phys. Rev. D105, 024016 (2022), arXiv:2110.03116 [gr-qc]. [192] H. Zhuet al., Phys. Rev. D111, 064052 (2025), arXiv:2312.08588 [gr-qc]. [193] E. Berti, V. Cardoso, and M. Casals, Phys. Rev. D73, 024013 (2006), [Erratum: Phys.Rev.D 73, 109902 (2006)], arXiv:gr-qc/0511111. [194] B. J. Kelly and J. G. Baker, Phys. Rev. D87, 084004 (2013), arXiv:1212.5553 [gr-qc]. [195] E. Berti and A. Klein, Phys. Rev. D90, 064012 (2014), arXiv:1408.1860 [gr-qc]. [196] L. London and E. Fauchon-Jones, Class."},{"citing_arxiv_id":"2604.14638","ref_index":116,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing bulk geometry via pole skipping: from static to rotating spacetimes","primary_cat":"gr-qc","submitted_at":"2026-04-16T05:28:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Pole-skipping data encodes enough information to reconstruct the full metric of 3D rotating black holes and the radial functions of 4D separable rotating black holes, with Einstein equations becoming algebraic constraints on that data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Separation constantλBefore proceeding to the explicit computation of the metric derivatives, some remarks on the separation constantλare in order. Conventionally, in physical analysis on a rotating background (e.g., Kerr-AdS black hole), the requirement of regularity at the poles (y1(x0) = 0) in (4.6) discretizes the sep- aration constantλ, and the corresponding regular eigenfunctions are known as spheroidal harmonics [116]. For a givenωand integerk, the separation constantλat which regular - 16 - solutions exist can be indexed by an integerl, where regularity constrains−l≤k≤land l≥0. In general,λ(ω, k, l)must be computed numerically [117]. In the present work, however, we relax the regular boundary conditions and treatλas a generic complex vari- able. As pointed out in [14], this treatment is necessary because the pole-skipping points"},{"citing_arxiv_id":"2604.11895","ref_index":117,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Novel ringdown tests of general relativity with black hole greybody factors","primary_cat":"gr-qc","submitted_at":"2026-04-13T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GreyRing model based on greybody factors reproduces numerical relativity ringdown signals with mismatches of order 10^{-6} and enables a new post-merger consistency test of general relativity applied to GW250114.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[114] R. Brito, V. Cardoso, and P. Pani, Lect. Notes Phys. 906, pp.1 (2015), arXiv:1501.06570 [gr-qc]. [115] A. Buonanno, G. B. Cook, and F. Pretorius, Phys. Rev. D75, 124018 (2007), arXiv:gr-qc/0610122. [116] E. Berti, V. Cardoso, J. A. Gonzalez, U. Sperhake, M. Hannam, S. Husa, and B. Bruegmann, Phys. Rev. D76, 064034 (2007), arXiv:gr-qc/0703053. [117] E. Berti, V. Cardoso, and M. Casals, Phys. Rev. D 73, 024013 (2006), [Erratum: Phys.Rev.D 73, 109902 (2006)], arXiv:gr-qc/0511111. [118] C. García-Quirós, M. Colleoni, S. Husa, H. Estel- lés, G. Pratten, A. Ramos-Buades, M. Mateu-Lucena, and R. Jaume, Phys. Rev. D102, 064002 (2020), arXiv:2001.10914 [gr-qc]. [119] LIGO Scientific Collaboration, \"LIGO Algorithm Li-"},{"citing_arxiv_id":"2604.02164","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Echoes of a hairy black hole from gravitational decoupling","primary_cat":"gr-qc","submitted_at":"2026-04-02T15:30:54+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"21, 787 (2004), arXiv:gr-qc/0309007. [13] M. Giesler, M. Isi, M. A. Scheel, and S. Teukolsky, Phys. Rev. X9, 041060 (2019), arXiv:1903.08284 [gr-qc]. [14] S. Bhagwat, X. J. Forteza, P. Pani, and V. Ferrari, Phys. Rev. D101, 044033 (2020), arXiv:1910.08708 [gr-qc]. [15] P. K. Kovtun and A. O. Starinets, Phys. Rev. D72, 086009 (2005), arXiv:hep-th/0506184. [16] E. Berti, V. Cardoso, and M. Casals, Phys. Rev. D73, 024013 (2006), [Erratum: Phys.Rev.D 73, 109902 (2006)], arXiv:gr-qc/0511111. [17] H. Yang, D. A. Nichols, F. Zhang, A. Zimmerman, Z. Zhang, and Y. Chen, Phys. Rev. D86, 104006 (2012), arXiv:1207.4253 [gr-qc]. [18] S. R. Dolan, Phys. Rev. D82, 104003 (2010), arXiv:1007.5097 [gr-qc]. [19] R. A. Konoplya and Z."},{"citing_arxiv_id":"2512.15877","ref_index":52,"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":"2510.05354","ref_index":46,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Quasinormal modes of Kerr-Newman black holes: revisiting the Dudley-Finley approximation","primary_cat":"gr-qc","submitted_at":"2025-10-06T20:27:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reassessment of the Dudley-Finley decoupling approximation for Kerr-Newman quasinormal modes with direct comparisons to the coupled system and new analysis of near-extremal zero-damped modes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.23895","ref_index":34,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Black hole spectroscopy: from theory to experiment","primary_cat":"gr-qc","submitted_at":"2025-05-29T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review summarizing the state of the art in black hole quasinormal modes, ringdown waveform modeling, current LIGO-Virgo-KAGRA observations, and prospects for LISA and next-generation detectors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The spin-weighted spheroidal harmonics are generalizations of the spin-weighted spherical harmonics sYℓm(θ, ϕ) = sSℓm(θ, ϕ; 0), and the factor of1/ √ 2π in Eq.(2.10) guarantees that the functions and harmonics can be individually normalized: Z 1 −1 |sSℓm(x; c)|2dx = I |sSℓm(θ, ϕ; c)|2dΩ = 1. (2.11) For fixed values ofc, s, and m, the spin-weighted spherical functions, while they can be normalized, are not orthogonal in general [34, 35]. That is, Z 1 −1 sS∗ 'ℓm(x; c)sSℓm(x; c)dx = sαm'ℓℓ(c) ̸∝ δ'ℓℓ, (2.12) and when m is allowed to vary, I sS∗ 'ℓ 'm(θ, ϕ; c)sSℓm(θ, ϕ; c)dΩ = sαm'ℓℓ(c)δ 'mm. (2.13) For the special cases ofc = 0, or s = 0 with c2 real, the functions and harmonics are orthogonal. However, for fixed values ofc, s, and m, the spin-weighted spheroidal functions are biorthogonal [35-38], which means that"},{"citing_arxiv_id":"2505.08877","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the universality of late-time ringdown tail","primary_cat":"gr-qc","submitted_at":"2025-05-13T18:05:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Analytical proof establishes universality of late-time ringdown tails for any effective potential decaying as 1/r², with different power-law behavior for 1/r^α (1<α<2), covering charged black holes, Kerr, exotic objects, modified gravity, and environmental matter distributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2501.12213","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black holes surrounded by dark matter spike: Spacetime metrics and gravitational wave ringdown waveforms","primary_cat":"gr-qc","submitted_at":"2025-01-21T15:30:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Black hole spacetimes in dark matter spikes are solved analytically from TOV equations; ringdown quasinormal frequencies differ from Schwarzschild by up to order 10^{-4}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1501.06570","ref_index":244,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Superradiance -- the 2020 Edition","primary_cat":"gr-qc","submitted_at":"2015-01-26T21:00:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Black-hole superradiance extracts energy via the ergoregion and can trigger instabilities with applications to dark matter, beyond-Standard-Model physics, and laboratory analogs.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"where K≡ (r2 + a2)ω− am and λ≡ Aslm + a2ω2−2amω. Together with the orthonormality condition ∫ 2π 0 ∫ π 0 |S|2 sin ϑdϑdϕ = 1 , (4.76) the solutions to the angular equation (4.75) are known as spin-weighted spheroidal harmonics eimϕS≡ Sslm(aω, ϑ, ϕ). When aω = 0 they reduce to the spin-weighted spherical harmonics Yslm(ϑ, ϕ) [243]. For small aω the angular eigenvalues are (cf. Ref. [244] for higher-order terms) Aslm = l(l + 1)− s(s + 1) +O(a2ω2) . (4.77) The computation of the eigenvalues for generic spin can only be done numerically [244]. Besides these equations, to have complete information about the gravitational and EM fluctuations, we need to find the relative normalization between φ0 and φ2 for EM fields and between Ψ 0 and Ψ 4 for gravitational perturbations."},{"citing_arxiv_id":"0905.2975","ref_index":154,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Quasinormal modes of black holes and black branes","primary_cat":"gr-qc","submitted_at":"2009-05-19T05:15:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Quasinormal modes are eigenmodes of dissipative gravitational systems whose spectra encode near-equilibrium transport coefficients in dual quantum field theories and enable tests of general relativity through gravitational wave observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"variableψ is related to the perturbation fields by the relations listed in Table 1 (see also Appendix B of Ref. [149]). Relations between the Regge- Wheeler-Zerilli and the Teukolsky variables are explored in Ref. [22]. Reconstr ucting the metric from the Teukolsky functions is a highly non-trivial problem which i s still not completely solved (see e.g. [154, 155, 156, 157, 158, 159]). Quasinormal modes of black holes and black branes 17 3. Defining quasinormal modes 3.1. Quasinormal modes as an eigenvalue problem In a spherically symmetric background, the study of BH pertu rbations due to linearized fields of spin s can be reduced to the study of the differential equation (10). Henceforth, to simplify the notation, we will usually drop the s-subscript in"}],"limit":50,"offset":0}