While my astronomical interests are broad, my own work mostly revolves around the formation of galaxies, their evolution, and their connection to large-scale structure. I approach these topics from the theoretical side and use numerical simulations (both collisionless and hydrodynamical) to explore, for example, the effects that galaxy formation can have on the distribution of matter, and conversely what measurements of the distribution of galaxies can tell us about the physical processes that play a role in their formation.

The parameters that describe our Universe, including the abundances of dark matter and dark energy, determine the statistical distribution of the galaxies that inhabit it. By measuring this distribution — that is, the clustering of galaxies — we can therefore learn a lot about our Universe as a whole. However, as the precision of our measurements increases, so too must the precision of the theoretical models we use to interpret these. Consequently, understanding the complex details of how processes involved in the formation of galaxies (such as supernova and AGN feedback) affect the clustering of matter is of growing importance. A large part of my research is focused on this interplay between galaxy evolution and the large-scale properties of the Universe.