Surface-brightness maps (left) and velocity maps (right) of the H₂ lines 0–0 S(1) at 17 μm, and S(5) at 6.9 μm, with central spaxels masked due to spectral fringing (see Sect. 2.2). The FWHM of the MRS PSF of the respective channel is shown in the lower right corner. The black contours on the top left map are 8.5 GHz radio VLA contours (0.22, 3.3, and 16 mJy beam⁻¹) from Hardcastle et al. (2003), tracing the jet that aligns with a central cavity seen on the S(1) (note that the VLA beam has a strong north-south elongation). The orange contours on the top left map are 434 μm ALMA CO(6–5) contours (0.01, 0.07, 0.12, 0.18, 0.24, and 0.30 Jy km s⁻¹ beam⁻¹), while those in the bottom left panel are 870 μm ALMA CO(3–2) contours (−0.10, 1.17, 2.45, 3.72, 5.00, and 6.28 Jy km s⁻¹ beam⁻¹) from Espada et al. (2017). CO(6-5) is scarce, and most of CO(3–2) shows large cavities filled by warm H₂ emission. The black contours on the bottom left map are JWST IR contours tracing [Ne VI] at 10.51 μm, which features an alignment with the H₂ 0–0 S(5) hot patches and with the jet. The dashed gray contours on the left maps highlight the two bright hotspots (a) and (b) visible on the S(1) map. The hotspots align with the filaments on the S(5) map and the northern filament visible in CO(3–2) and CO(6–5). The same contours are superimposed in green on the right-hand maps, along with the gray contours tracing the relative surface-brightness maps, and the dashed black line tracing the line of the nodes of the warped-disk model from Neumayer et al. (2007). The contours of the hot S(5) patches aligned with the jet < 20 pc from the AGN are labeled (c) and (d) in the bottom right panel.