Evidence for the existence of some form of dark energy -- a smooth component that causes the accelerated expansion of the universe and contributes about 70 percent of the total energy density -- is by now very solid. However, very little progress has been made in understanding its nature and the underlying physical mechanism. In this talk I describe the prospects of several promising methods to improve the measurements of dark energy properties within the next decade. In addition to type Ia supernovae, these include weak gravitational lensing, counts of clusters of galaxies, and cosmic microwave background anisotropies. I comment on specific upcoming surveys, and challenges in controlling the systematic errors so that these probes can achieve their full potential and help us understand the nature of dark energy.