subsample. We follow the procedure used in several previous works (cf. Croft et al. 1999, Padilla et al., 2001) consisting on calculating the auto-correlation function of galaxies in two coordinates, one parallel ($\sigma$) and one perpendicular ($\pi$) to the line of sight, $\xi(\sigma,\pi)$, and integrating over the $\pi$ direction to avoid the effect of redshift space distortions. The result from this integration is the projected correlation function (see for instance, Croft et al., 2001), $\Xi(\sigma)$, $$\Xi(\sigma)=2\int_{\pi_{min}}^{\pi_{max}}\xi(\sigma,\pi) d\pi,
\label{eq:Xi}$$ which in turn can be inverted to obtain the real-space correlation function via $$\begin{aligned}
&\xi(r)=\frac{-1}{\pi}\sum_{j\geq i}\frac{\Xi(\sigma_{j+1})-\Xi(\sigma_{j})}
{\sigma_{j+1}-\sigma_{j}}
 \ln{\left(\frac{\sigma_{j+1}+\sqrt{\sigma_{j+1}^{2}-
\sigma_{i}^{2}}}{\sigma_{j}+
\sqrt{\sigma_{j}^{2}-\sigma_{i}^{2}}}\right)},&\end{aligned}$$ where the sum is performed over the bins in $\sigma$ where the projected correlation function has been calculated. The masses of host haloes can then be obtained by finding the bias between the resulting real-space correlation functions and the matter correlation functions in a $\Lambda$CDM cosmology (both in the 2-halo regime), which we obtain by Fourier transforming the non-linear matter power spectrum (from Peacock & Smith, 2000) for the same cosmological parameters used in the numerical simulations. With an estimate of the bias, the mass of the host haloes can be found by using the Sheth, Mo & Tormen (2001) formalism. Note 