the probability distribution has been normalized to have unit area we seek $A_1$ and $A_2$ such that

$$\int_{0}^{A_1} {\rm prob(}A\vert I) {\rm d}A = \int_{A_2}^{\infty}
{\rm prob(}A\vert I) {\rm d}A = \frac{1-X}{2} .$$

Finally the parameter $A$ is given as $A = A_{\rm best}\text{
}_{-\sigma_{-}}^{+\sigma_{+}}$ with $\sigma_{+} = A_2 - A_{\rm best} $ and $\sigma_{-} = A_{\rm best} - A_1$. The errors derived in this way only include sources that have been considered when computing $\chi^2$. The calculation of the errors applies for uncorrelated data points. Since in our case the data points are correlated the values of the errors are slightly modified. Also errors caused by cosmic variance are not included.

Fitting results {#s:results}
===============

Here we present the results we obtain by fitting to the stellar mass function only, and for the combined fit to the SMF and the projected CF.

The stellar mass function fit
-----------------------------

[lllllll]{}\[hb!\] best fit & 11.884 & 0.02820 & 1.057 & 0.556 & 1.56 & 3.83\
$\sigma^+$ &   0.030 & 0.00061 & 0.054 & 0.010 & &\
$\sigma^-$ &   0.023 & 0.00053 & 0.046 & 0.004 & &\
\[t:mfresults\]

First we fit to the SDSS SMF and use the derived best-fit parameters 