Identifying heating processes from jets in a galaxy cluster

We investigate how jets heat the intracluster medium (ICM) by disentangling the contributions from different heating channels. To this end, we implement a heating estimation method based on passive entropy tracers and validate it using controlled tests and in-situ shock detection. Using these diagnostics, we simulate single high-power jet outbursts with varying jet densities in a cluster environment. Light jets inflate wider bubbles and displace more gas from the cluster core, while denser jets propagate more efficiently to larger distances with minimal core disturbance. At early times, shock heating dominates for all jets. At later stages, light jets heat the ICM mainly through turbulent dissipation, whereas denser jets continue to deposit energy primarily via shocks. Turbulent and mixing-driven heating dominates inside the cocoon, while shocks and acoustic compressions prevail outside. Light-jet shocks weaken rapidly, whereas dense jets sustain strong shocks to large radii.