Dr. Manami Roy

Contemporary galaxy formation models suffer from a critical bottleneck: vastly different sub-grid physics implementations in cosmological simulations can yield nearly identical statistical populations of galaxies at $z = 0$, yet they diverge dramatically in their predictions of these gas flow rates across the disk-halo interface. Because the CGM acts as the ultimate ledger for the mass, momentum, and energy transfer of this gaseous flow, it offers a uniquely powerful laboratory to break these simulation degeneracies and ground the next generation of galaxy evolution and feedback physics. In my talk, I will discuss macro-scale CGM phases and how the hot and cold phases in the CGM can be formed from different physical processes. On the other hand I will also talk about the poorly understood micro-physics--such as cosmic ray transport, magnetic fields, and plasma instabilities -- that regulate the thermodynamic state of this diffuse halo. I will show how CRs can significantly alter the evolution of ram-pressure stripped clouds from their satellite galaxy.