The study focuses on an adaptive mesh refinement simulation of galaxy cluster formation, emphasizing the passive evolution of magnetic fields. It reveals that structure formation significantly amplifies large-scale magnetic fields, with the resulting magnetic properties of the simulated cluster aligning well with recent observational data. This research contributes valuable insights into the interplay between cosmic structure and magnetism in the universe.
This investigation delves into the AGN-ICM interaction in cool core clusters, focusing on M87 in the Virgo cluster and Hydra A. The study identifies the first two classical AGN-driven shocks with spectroscopically confirmed temperature and pressure jumps, revealing consistent Mach numbers. 1D hydrodynamic simulations of the large-scale shock in Hydra A were conducted to estimate its Mach number, age, and energy. Additionally, 3D simulations indicate that a bulk flow of the ICM is essential to replicate the observed shock front shape. In M87, a “cold front” was discovered, suggesting bulk motions in the form of sloshing within the ICM. The presence of cool, metal-rich filaments, often resolved into multi-temperature components, highlights the AGN's role in uplifting chemical elements from the central galaxy into the ICM in both clusters. Detailed modeling in M87, supported by sufficient statistics, revealed a correlation between cooler gas and metal abundance, allowing for the estimation of metallicity in gas uplifted by the AGN. The study also estimates gas mass, Fe mass, and energy linked to the uplift in both clusters, comparing these energies to those required for the AGN-driven shocks. Furthermore, the mechanisms and timescales necessary to produce the observed metal quantities and abundance ratios are discussed.