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We explore three different methods based on weak lensing to extractcosmological constraints from the large-scale structure. In the first approach(method I), small-scale galaxy lensing measurements of their halo mass providea constraint on the halo bias, which can be combined with the large-scalegalaxy clustering to measure the dark matter clustering. In the second approach(method II), large-scale galaxy clustering and large-scale galaxy-galaxylensing can be combined into a direct measurement of the dark matterclustering. These two methods can be combined into one method I+II to make useof lensing measurements on all scales. In the third approach (method III), weadd abundance information to the method I. We explore the statistical power ofthese three approaches as a function of galaxy luminosity to investigate theoptimal mass range for each method and their cosmological constraining power.In the case of the SDSS, we find that the three methods give comparableconstraints, but not in the same mass range: the method II works best for halosof M~10^13 Msun, and the methods I and III work best for halos of M~10^14 Msun.We discuss the robustness of each method against various systematics.Furthermore, we extend the analysis to the future large-scale galaxy surveysand find that the cluster abundance method is not superior to the combinedmethod I+II, both in terms of statistical power and robustness againstsystematic errors. The cosmic shear-shear correlation analysis in the futuresurveys yields constraints as strong as the combined method, but suffer fromadditional systematic effects. We thus advocate the combined analysis ofclustering and lensing (method I+II) as a powerful alternative to otherlarge-scale probes. Our analysis provides a guidance to observers planninglarge-scale galaxy surveys such as the DES, Euclid, and the LSST.

Joint Analysis of Gravitational Lensing, Clustering and Abundance: Toward the Unification of Large-Scale Structure Analysis