Speaker
Description
The large-scale distribution of galaxies encodes cosmological information on the history and matter content of the Universe. The full, non-Gaussian galaxy distribution can be analysed on large scales using a perturbative formulation of galaxy bias, which is the effective field theory of large-scale structure. State-of-the art full-shape analyses of past surveys such as BOSS and currently operational Stage IV campaigns such as DESI and Euclid typically employ at most third-order perturbation theory. Going beyond this order has the potential of enhancing the information extraction from the galaxy distribution, but poses several challenges, both theoretically and numerically. In this talk, I will discuss recent (and ongoing) progress on fourth- and fifth-order perturbation theory for galaxies and the remaining steps to be taken towards application to current and future survey data.