Kerr-Newman Quasinormal modes

Quasinormal-mode frequencies of Kerr–Newman black holes, computed from thecoupled gravito-electromagnetic perturbation equations with SpectralPINN — ahybrid pseudospectral physics-informed solver (Chebyshev collocation, float64,HAdamD warm-up + Newton–Raphson refinement, numerical continuation towardextremality). Companion data release for: A. M. Pombo, "Coupled by Design:Computing Kerr–Newman Quasinormal Modes with a Hybrid SpectralPINN Solver",submitted to JCAP (2026), [arXiv:2607.14216]. Contents — 312 plain-text tables, 94,337 frequencies: - Photon-sphere (PS) modes for (n,l,m) = (0,2,0), (0,2,2), (0,3,3), (0,4,4) and (1,2,2), in both the gravitationally-led and electromagnetically-led sector: fixed-spin sweeps in charge (a = 0 to 0.999, step 0.05 with near-extremal refinement), sweeps along the diagonal a = Q, and Reissner–Nordström (a = 0) reference curves.- Near-horizon (NH) modes for the gravitationally-led (0,2,0) and (0,2,2) families at fixed charge Q/M = 0.95 – 0.9995, swept in spin toward extremality.- Equations/: Mathematica notebooks with the factorized coupled perturbation equations (s = -2 and s = -1 sectors) and a PyTorch implementation of the coefficient functions. Units G = c = M = 1; tabulated values are the dimensionless Re(ωM), Im(ωM)with time convention e^{-iωt} (all modes damped). File formats, grids andconventions are documented in the included Readme.txt. Note: data withQ/Q_ext ≳ 0.97 approach the conditioning limit of double precision; see theReadme for guidance. If you use this dataset, please cite the companion paper and this record.