The imprint of cluster physics on the Sunyaev-Zel’dovich effect -from bubbles to cosmological parameters

          @misc{ pirsa_PIRSA:09040038,
            doi = {10.48660/09040038},
            url = {https://pirsa.org/09040038},
            author = {},
            keywords = {Cosmology},
            language = {en},
            title = {The imprint of cluster physics on the Sunyaev-Zel{\textquoteright}dovich effect -from bubbles to cosmological parameters},
            publisher = {Perimeter Institute},
            year = {2009},
            month = {apr},
            note = {PIRSA:09040038 see, \url{https://pirsa.org}}
          }
          

Abstract

Clusters of galaxies provide us the opportunity to study an "ecosystem" - a volume that is a high-density microcosm of the rest of the Universe. At the same time clusters are excellent laboratories for studying plasma physical processes as well as for studying how super-massive black holes interact with the ambient cluster plasma. Guided by high-resolution simulations of galaxy clusters that self-consistently follow dissipative gas and cosmic ray physics, I will show how non-thermal processes in clusters build up over cosmic time. This enables us to understand how the Sunyaev-Zel'dovich effect and hydrostatic masses of galaxy clusters are expected to change - a finding which is critical in calibrating clusters as high-precision cosmological probes. On small scales, the Chandra X-ray Observatory is finding a large number of cavities in the X-ray emitting intra-cluster medium which often coincide with the lobes of the central radio galaxy. These are thought to provide the key for understanding the thermal evolution of galaxy clusters. I will argue that high-resolution observations of the Sunyaev-Zel'dovich effect are uniquely suited to unveil the composition of radio plasma bubbles. Solving this enigma would yield further insight into the complex physical processes within the cooling cores of clusters as well as provide hints about the composition of relativistic outflows of radio galaxies.