Non-kinematical anisotropies in galaxy clustering and cosmological tests of gravity

Our project aims to update the modelling of dust and molecular hydrogen within simulated galaxies. We will achieve this through the coupling of thermodynamic and chemical solvers in order to better model the rate at which dust populations grow and are destroyed. Furthermore, we add molecular hydrogen into the chemical network which allows us to explicitly calculate its abundance, rather than the approximate methods used before. This work will be done in collaboration with the SIMBA simulation project, and our new modelling procedures will be added to next-generation simulations within the group as standard. In doing this work we create a self-consistent and physically motivated model of dust and molecular hydrogen within the interstellar medium of simulated galaxies.