JWST Maps the Missing Link: Kiloparsec Filaments to Black-Hole Disks in Centaurus Cluster Core

The arXiv preprint (v1, June 2026) from Hlavacek-Larrondo et al. uses JWST NIRSpec integral-field spectroscopy to resolve the inner 618 pc of NGC 4696 at ~10 pc scales, revealing an S-shaped, rotating multiphase circumnuclear disk directly connected to the larger filament network. This is a single-object study relying on tailored magnetohydrodynamic simulations for kinematic interpretation, not a statistical sample. While the work correctly identifies the disk as the intermediary that allows kiloparsec-scale cooling flows to lose angular momentum and reach the black hole, it underplays how the observed inflow rates align with—or challenge—prior X-ray cavity power measurements in the same system. Comparable structures in NGC 1275 (Perseus) suggest a common channel, yet the Centaurus data add the first spatially resolved velocity field tying hot, warm, and cold phases on sub-100 pc scales. Mainstream coverage has focused on the visual 'swirl' while missing the quantitative implication: these disks may stabilize accretion against rapid variability, helping explain why radio-mode feedback remains steady over Gyr timescales. Limitations include the absence of direct molecular-gas kinematics at matching resolution and the risk that the tailored simulations overfit the observed morphology. Broader synthesis with earlier work on multiphase condensation (e.g., Voit et al. 2015 on precipitation thresholds and Li et al. 2015 on filament formation) indicates that the observed CND represents the final stage of a cascade previously mapped only statistically across clusters.