The kinetic channel is usually regarded as the dominant feedback process in radio-loud galaxies. However, its effect in radio-weak active galactic nuclei (AGN) is still uncertain and poorly assessed. In this seminar, we discuss recent results on this matter. In particular, we study the kinetic feedback in local radio-weak active galactic nuclei by means of the high-ionisation gas. We found that the [FeVII] and the [FeX] emission in the optical and [SiVI] in the near-infrared suitably traces that feedback mode. In all cases, the high-ionization gas is strongly aligned to the radio-jet, it is kinematically perturbed, and its morphology and extension also coincides with that of the extended X-ray emission, suggesting that it is shock-driven and strongly associated with the radio-jet. This strong relationship leads to the high-ionisation emission to extend to linear scales of up to a few kiloparsecs, allowing us to set a new limit to the size of the coronal line region in AGN. Models combining the effect of photoionization by central source and shocks nicely reproduced the observed emission line strengths of both low- and high-ionization gas. We show that the detection of extended coronal emission is a clear signature of the presence of the kinetic channel and that it plays a very important role even in radio-weak AGN.

For Zoom connection information, please contact Emanuele Paolo Farina (emanuele.farina_at_noirlab.edu).

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