MIRACLE. III. JWST/MIRI expose the hidden role of the AGN outflow in NGC 1068

We present new JWST/MIRI integral field spectroscopy (IFS) observations of the prototypical Seyfert 2 galaxy NGC 1068. These observations, combined with archival VLT/MUSE data, allow us to investigate the outflow from the active galactic nucleus (AGN) and radio jet and its interaction with the circumnuclear multiphase gas. MIRI data trace the ionized and warm molecular gas emission up to ∼ 400 pc from the nucleus at 20--60 pc spatial resolution, unveiling a clumpy ionized structure surrounding the radio hot-spots and a rotating warm molecular disk. Mid-infrared (mid-IR) and optical diagnostic diagrams show that AGN photoionization dominates across the entire MIRI field of view, with no evidence of star formation excitation, supporting the scenario of an AGN-driven wind. Density sensitive mid-IR transitions reveal compact high-density clumps (n_̊m e ge 10 4 cm^-3) along the outflow edges, consistent with gas compression by the expanding wind. Combining multi-cloud kinematic (and photo-ionization (HOMERUN) modeling, we identify two distinct ionized outflow components: a dust-poor component dominating the optical line emission and a dust-rich component responsible for the mid-IR high-ionization emission. The latter traces gas that is ∼300 ̨ms faster than the optical component and carries most of the ionized mass, demonstrating that a large fraction of the outflow is hidden from classical optical diagnostics. Kinematic and photoionization models consistently point to a two-stage acceleration scenario, with velocities reaching ∼2000 ̨ms, consistent with an energy-driven wind. Our multi-cloud modeling indicates that the outflow entrains up to a few 10^ 6 of ionized gas and couples efficiently with the surrounding interstellar medium, injecting substantial turbulence and strongly impacting the host-galaxy environment.