The physical mechanism behind the acceleration of the universe remains one of the great mysteries of modern cosmology, with little progress to date in understanding dark energy. In the near future, we need new kinds of tests in addition to better data. One very effective way to test the consistency of the current LCDM paradigm is to isolate and separately constrain the growth of structure in cosmological measurements and compare to constraints from the purely geometrical measures. I will review such recent work applied to current data. I will also review efforts to use the galaxy maps in order to reconstruct the late-time Integrated Sachs-Wolfe contribution to the CMB anisotropy maps. Key to the success of these efforts and other tests with large-scale structure is exquisite control of the photometric calibration errors, and I will describe a general formalism to account for these pervasive systematics.
