This is a theoretical and observational program to identify and understand competing dynamical signatures imprinted on the gaseous media inside and around galaxy clusters. The intra-cluster medium (ICM) is the principal baryonic component of clusters and carries unique indicators of the history and state of clusters. A proper interpretation of the structures seen in X-ray and radio studies of clusters, and of cluster physical properties and inflows, depends on an improved understanding of external influences (notably gravitational infall) and internal disturbances (especially from active galaxies).
The research will include a systematic study of shocks in and around clusters, using very high-resolution cosmological simulations, a careful investigation of ICM interactions with high-energy plasma ejected by active galaxies, using magneto-hydrodynamic simulations of realistic media and relativistic particles, and radio surveys intended to identify extragalactic structures on scales of a few mega-parsecs. The use of 'synthetic observations' bridges the critical gap between the data and the theories.
This work contributes to the broader understanding of cosmic magnetic fields, the energetics of active galaxies, and the development of structure in the Universe. It will train students in cutting-edge science, data analysis, and simulation techniques, and it will contribute to the PIs' major public education efforts, involving K-12 schools, the local planetarium, and national public television
