The Kinematics of the Hot and X-ray Emitting Circumgalactic Medium: Predictions from Simulations

          @misc{ scivideos_PIRSA:25070032,
            doi = {10.48660/25070032},
            url = {https://pirsa.org/25070032},
            author = {ZuHone, John},
            keywords = {Cosmology},
            language = {en},
            title = {The Kinematics of the Hot and X-ray Emitting Circumgalactic Medium: Predictions from Simulations},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2025},
            month = {jul},
            note = {PIRSA:25070032 see, \url{https://scivideos.org/index.php/pirsa/25070032}}
          }
          

Abstract

In massive galaxies a significant fraction by mass of the circumgalactic medium is expected to be in the hot, X-ray emitting phase. Little is known about this gas since it is faint and is outshone by the Milky Way's own hot circumgalactic medium, and X-ray observatories with CCDs are unable to distinguish the emission lines of the former from the latter. Future observatories with X-ray IFUs would be able to measure key emission lines of the hot CGM, and use them to map the velocity structure of this phase. In this talk, I will show predictions from galaxies from a range of cosmological simulations for the velocity field of the hot CGM, showing signatures of rotation, inflows, and outflows from AGN and SNe feedback. Crucially, the velocity structure depends on the feedback model used, so that future observations may be used to constrain models used in cosmological simulations.