Institute for Advanced Study Informal Astrophysics Seminar

I describe three methods to quantify dark matter clustering, making full use of precision measurements of galaxy clustering and weak lensing from recent galaxy redshift surveys. First, using galaxy clustering measurements on small scales, I infer the scale-dependent bias function, which makes it possible to extend the recovery of the primordial matter power spectrum over a large dynamic range, and thereby tighten constraints on cosmological parameters obtainable from the galaxy samples of the Sloan Digital Sky Survey. Second, I develop an analytic model for combining galaxy-galaxy lensing and galaxy clustering to constrain the matter density parameter (Omega_m) and the matter fluctuation amplitude (Sigma8). Finally, I present a novel method to constrain dark energy models using cluster-galaxy weak lensing and apply our method to the planned Dark Energy Survey (DES), forecasting our ability to measure cosmological parameters. Comprehensive analysis of galaxy clustering measurements with these complementary approaches will provide a unique opportunity for a complete description of dark matter clustering.