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We use an empirical approach to model the stellar mass of galaxies accordingto their host dark-matter haloes and subhaloes ('HASH'), where each galaxyresides in a subhalo taken from a large N-body cosmological simulation. Thisapproach allows us to study the mass relation between subhaloes and galaxies(MR) using: the weak lensing signal (WL), the two point auto-correlationfunction (CF), and the stellar mass function of galaxies (SMF). Our method isbased on modeling the lensing signal directly from the cosmological simulation,and should thus be more accurate than other methods based on analytic halomodels. We find that the WL does not provide a strong constraint on the MR,allowing for more than a factor of 10 freedom in the subhalo mass of centralgalaxies, for a given stellar mass. The freedom for satellite galaxies is muchlarger, providing a very poor constraint on the fraction of satellite galaxies(0.05-0.8). These results are not significantly modified when using both theSMF and WL as constraints. We show that for the most massive galaxies,observational constraints based on the CF with 0.1 dex errors, are equivalentto 0.05 dex error in the WL. For intermediate and low mass galaxies the WL andCF constrain the MR in a different way. Although the WL is currently not addingmuch information at these masses, it has the potential of being important usingfuture, more accurate measurements. The models found here do not matchsimultaneously the observed CF and WL signals, and show a limited ability tomatch the WL & SMF. We suspect that this is partially due to the cosmologicalmodel assumed here and we therefore adopt a mock WL signal through most of thiswork. In comparison to previous models in the literature, the method presentedhere is probably more general, as it reveals a larger range of solutions for agiven set of observational constraints [abridged].

Looking at the relation between haloes and galaxies under the lens