the effect of the neutrinos opposes that of the cold dark matter. The contours also broaden, since many more preferred models exist now. For example, on angular scales of between 10and 100, ${\left<M^2_\mathrm{ap}( \theta )\right>}$ of the best-fit models of the full grid and the massless neutrino sub-grid, differ by less than 5%. As the contours broaden, their shape remains unchanged, implying that the CDM effect on the cosmic shear signal is more significant than that of the neutrinos. The degeneracy direction in the case of massive neutrinos is now fitted by $$\sigma_8\,({\Omega_{\mathrm{m}}}/0.35)^{0.64}=0.711 \pm 0.076 \,,$$ where we chose a higher pivot ${\Omega_{\mathrm{m}}}$.

![Confidence contours (68% and 95%) from the aperture-mass dispersion between 1and 230, for ${\Omega_\nu}=0$ (red, smaller) and marginalized over $\omega_\nu$ (blue, larger). Both cases are marginalized over the source redshift distribution and the remaining cosmological parameters.[]{data-label="fig:nufu"}](11077fg2.ps){width="7cm"}

![image](11077fg3a.ps){width="6cm"} ![image](11077fg3b.ps){width="6cm"} ![image](11077fg3c.ps){width="6cm"}

Figure \[fig:wlcont\] (left panel) shows the massless and massive neutrino best-fit models, ($m_\nu=0$ eV, ${\Omega_{\mathrm{m}}}=0.30$) and ($m_\nu=0.53$ eV, ${\Omega_{\mathrm{m}}}=0.44$), respectively. They have the same values of $\sigma_8$ and $h$ and differ in ${n_\mathrm{s}}$. The difference between the two models, shown in the inset normalized by the massless neutrino model, increases on larger scales with the approach to the 