3:30–4:30 pm
Transitioning from a "Static" View of Galaxy Clusters into a Full Dynamic Picture
Clusters of galaxies continuously grow through matter accretion along cosmic filaments and occasional violent mergers with other clusters and groups, releasing a vast amount of energy that eventually dissipates and heats the intracluster medium (ICM) through shocks and gas motions. At the same time, the feedback processes from central supermassive black holes regulate star formation by stirring the gas and mixing different gas phases. Despite being such dynamic environments, current X-ray observations largely yield only a static picture of the ICM, and a plethora of motions-related multi-scale physics remains unexplored both numerically and observationally. In this talk, I will present some of our recent efforts toward understanding a full dynamic picture of the ICM, from core regions to outskirts and from micro to macro scales. I will discuss observational constraints on transport properties of the ICM that are important for sustaining and dissipating motions, recent updates on feedback-driven gas dynamics, and numerical studies of mergers-driven physics in cluster outskirts. I will briefly review the status of the next X-ray satellite, XRISM, and related science we will be working on immediately after its launch next year.
