Venue: G. O. Jones 516
The distribution of primordial density perturbations is a key discriminant between different models for the origin of structure in the very early universe. Galaxies are biased tracers of this underlying matter distribution, and deviations from a simple Gaussian distribution can give rise to scale-dependent bias on the largest observable scales. Studying very large scales, close to the Hubble-horizon, requires a consistent relativistic interpretation, but standard treatments (and numerical simulations) are based on Newtonian gravity. I will show how Einstein's general relativity gives rise to a characteristic non-Gaussian signature in the primordial distribution of matter and hence galaxies on large scales.