to calculate the model projected correlation functions. Note that for now, we do not take into account any possible scatter in the $m(M)$ relation. We will consider scatter in §\[s:scattersec\].

We see in Figure \[f:fig1\] that our fit produces excellent agreement with the observed SMF. Using the approach described above we also compute the errors on the parameters. The results are summarized in Table \[t:mfresults\].

Having derived the best-fit parameters, we can predict the projected CFs. We present the results both including and not including orphan galaxies, where we have fitted to the SMF for each case.

Figure \[f:fig2\] shows a comparison between our model and the SDSS projected correlation functions in five stellar mass bins ranging from $\log m/{\!\,{\rm M}_\odot}=9.0$ to $\log m/{\!\,{\rm M}_\odot}=11.5$ with a binsize of $0.5 {\rm~dex}$. The correlation function that has been derived without orphans is too low at small scales and can be regarded as a lower limit. Neglecting these galaxies results in an underprediction of satellite galaxy clustering. As on small scales the projected CF depends mainly on the one-halo term this results in the underprediction of $w_p(r_p)$. This effect weakens for the clustering of more massive galaxies as they are more likely 