of neutrinos.

The right panel of Fig. \[fig:wmz+deltaMap2\] shows the aperture mass dispersion in the presence of massive and massless neutrinos, computed from the total matter power spectrum, for the same ${\Omega_{\mathrm{m}}}$. The models are similar on large scales where the neutrinos behave like cold dark matter and show a scale-dependent deviation on intermediate scales. On small scales, which stay always inside the free-streaming length, the suppression is constant. Linear perturbation theory predicts the small-scale suppression to be, $[P^{{\small\mathrm{lin}}}_{\mathrm{m}}(f_\nu,z=0) -
  P^{{\small\mathrm{lin}}}_{\mathrm{m}}(f_\nu=0,z=0)] /P^{{\small\mathrm{lin}}}_{\mathrm{m}}(f_\nu,z=0) \sim -8f_\nu$ [@hudeltap]. For the non-linear power spectrum, the suppression is higher, around $-10f_\nu$, as predicted by both numerical simulations [@nunbody] and one-loop corrections [@Wong08]. For the aperture mass dispersion, the models shown in Fig. \[fig:wmz+deltaMap2\] have a small-scale suppression of $\sim
-5f_\nu$.

Likelihood analysis {#sec2b}
-------------------

### Cosmic shear alone

The statistical analysis evaluates a mixed dark matter scenario with nine parameters, including the reduced Hubble parameter $h$, the density of baryons $\omega_{\mathrm{b}}\equiv{\Omega_\mathrm{b}}{h^2}$, cold dark matter, $\omega_{\mathrm{cdm}}\equiv{\Omega_\mathrm{cdm}}{h^2}$, and massive neutrinos, $\omega_\nu\equiv{\Omega_\nu}{h^2}$, the effective number of relativistic degrees of freedom ${N_\mathrm{eff}}$, the optical depth to reionization $\tau$, the primordial spectral index ${n_\mathrm{s}}$, the rms of the matter perturbations extrapolated to redshift $z=0$ and filtered over the $8h^{-1}$ Mpc 