correlation functions. The only way to constrain the SHM relations then is to take the clustering data into account. By adopting different SHM relations for central and satellite populations it is even possible to produce a slightly better fit to the correlation functions [@wang06].

On the other hand, if one wants to [*predict*]{} clustering as a function of stellar mass (e.g. at higher redshift) then one has to make an assumption about how the SHM ratios of central and satellite galaxies are related. We made the very simple assumption, that the relation between the stellar mass of central galaxies and the virial mass of their host halo and the relation between the stellar mass of satellite galaxies and the mass of the subhalo at the time of accretion is the same, and have shown that this leads to very good predictions for the mass dependent clustering. We conclude that under this simple assumption we can use our model to predict clustering as a function of stellar mass.

The resulting stellar-to-halo mass relation {#masstomass}
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\[f:fig4\]

The upper panel of Figure \[f:fig4\] shows the derived stellar mass as a function of halo mass. The light shaded area gives the 68% confidence 