interval while the dark and light shaded areas together give the 95% confidence interval. These have been derived using a set of different models computed on a mesh, as described in §\[s:probdis\].

For the SHM ratio we apply the same procedure. The result is shown in the lower panel of Figure \[f:fig4\]. We see that the SHM ratio has the form we expected: it increases with increasing halo mass, reaches its maximum value around $M_1$ and then decreases again.

Meaning of parameters and correlations {#s:parameters}
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\[f:fig5\]

We now explore the effects of changing each parameter in order to understand how they affect the SMF. \[ratio\] If we keep $M_1$, $\beta$ and $\gamma$ fixed and only vary $(m/M)_0$, this corresponds to changing the stellar mass of the galaxy that lives inside each halo by a constant factor. This has no impact on the form of the SMF. Its shape stays the same, while only the position on the stellar mass axis changes. Due to the monotonic form of the SMF this directly determines the value of the normalization $\phi^*$. For a larger value of $(m/M)_0$ we get a larger value of $\phi^*$.

\[m1\] Varying only $M_1$ we find that the 