Active galactic nuclei
Active supermassive black holes show a variety of different signatures, from electromagnetic radiation with extremely high luminosity to powerful, collimated outflows that extend out to galactic scales. My main interests lie in the interaction of these energetic phenomena with the surrounding gas in the host galaxy or galaxy cluster and the growth history of the supermassive black holes over cosmic time.
Galaxies, like our own Milky Way, are the result of the complex interplay of a variety of different physical processes. Identifying and disentangling the different mechanisms at work to explain why the galaxies in the Universe look like they do today is one of the main motivations for my research. In this context, I am particularly interested in understanding the formation and evolution of massive galaxies.
Clusters of galaxies are the largest collapsed objects in the Universe. They can not only be used to test cosmological models but also give important insights in how interactions affect galaxies or serve as a laboratory for plasma physics. Currently, my research focuses on the hot intra-cluster gas, its dynamics and how it is affected by energetic, collimated outflows powered by supermassive black holes.
For my reserach, I use computer simulations of both, idealized (magneto-) hydrodynamical problems and cosmological simulations of structure formation. I am interested in modeling astrophysical phenomena in these kind of simulations and in improving existing numerical techniques. For most of my research, I use the finite-volume moving-mesh magnetohydrodynamics code Arepo. In the past, I have also used the tree N-body code PKDGRAV and the TreePM/SPH code Gadget.