  In many observed galaxy clusters, jets launched by the accretion process on
to supermassive black holes, inflate large-scale cavities filled with
energetic, relativistic plasma. This process is thought to be responsible for
regulating cooling losses, thus moderating the inflow of gas on to the central
galaxy, quenching further star formation and maintaining the galaxy in a red
and dead state. In this paper, we implement a new jet feedback scheme into the
moving mesh-code arepo, contrast different jet injection techniques and
demonstrate the validity of our implementation by comparing against simple
analytical models. We find that jets can significantly affect the intracluster
medium (ICM), offset the overcooling through a number of heating mechanisms, as
well as drive turbulence, albeit within the jet lobes only. Jet-driven
turbulence is, however, a largely ineffective heating source and is unlikely to
dominate the ICM heating budget even if the jet lobes efficiently fill the
cooling region, as it contains at most only a few per cent of the total
injected energy. We instead show that the ICM gas motions, generated by
orbiting substructures, while inefficient at heating the ICM, drive large-scale
turbulence and when combined with jet feedback, result in line-of-sight
velocities and velocity dispersions consistent with the Hitomi observations of
the Perseus cluster.
