we can evaluate the benefit of using large scales independent of a gain due to better statistics. We obtain constraints similar to the ones obtained for the data up to 230, the extension to $\theta=20\degr$ only adding a small number of independent points. Since the cosmic shear signal on large scales becomes very small, better statistics are needed in attempting to break the ${\Omega_\mathrm{cdm}}-{\Omega_\nu}$ degeneracy with cosmic shear data alone.

Using either CFHTLS-T0003 data or its extension to $\theta=20\degr$, the marginalized upper bound on the neutrino mass is, $$\sum m_\nu < 3.3\,\mbox{eV (95\% C.L.)}.
\label{res33}$$ This constraint, while very loose when compared with the combined constraints mentioned in Sect. 2, is comparable to the ones obtained from SDSS or 2dF galaxy redshift surveys alone (see e.g., Kristiansen [et al. ]{}2007, who find ${\sum m_\nu}\lesssim 5.2 $ eV).

We note that the 95% C.L. contours in Fig. \[fig:nufu\] do not close inside the range of the parameters probed. This implies that our grid limits are an effectively strong prior, in particular implying ${\Omega_{\mathrm{m}}}\in[0.2,0.6]$ and $\sigma_8 \in[0.65,0.92]$. In other words, the constraint in Eq. (\[res33\]) includes a marginalisation over an arbitrary and relatively narrow range of parameters values, and is thus optimistic. 