Most of the baryonic mass in a galaxy cluster is in the form of hot, diffuse plasma that fills the space between the member galaxies. This hot diffuse plasma, also known as the intra-cluster medium (ICM), undergoes radiative cooling that leads to the precipitation of cold gas from the ICM into the cluster core. The precipitating cold gas in-falls and accretes onto the supermassive black hole that is located in the cluster's central galaxy, fueling outbursts of powerful jets that are known as active galactic nuclei (AGN). The AGN outbursts compensates for the radiative cooling losses of the ICM by transferring the energy back into the ICM through shocks, turbulence, and cavities. In my project work, I will analyze the data of 3D hydrodynamic AGN feedback simulations with the intent of understanding how AGN outburst energy is partitioned between shocks, turbulence, and cavities. Specifically, I'll be using a software called yt in order to analyze simulation data in hopes of better understanding AGN feedback.