determined in Fu [et al. ]{}(2008) from the photometric redshift estimations of Ilbert [et al. ]{}(2006). We adopt the commonly used fitting function of $$n(z)=N(z/z_\mathrm{s})^\alpha\exp\left[-(z/z_\mathrm{s})^\beta\right]$$ with best-fit parameters $\alpha=1.47$, $\beta=2.15$, and $z_\mathrm{s}=0.90$, and a normalization constant $N$ that was determined by integrating up to $z_\mathrm{lim}\simeq 6$.

The shear power spectrum is integrated over the appropriate window function to obtain the mass variance in apertures $\theta$ [@map], $${\left<M^2_\mathrm{ap}( \theta )\right>}=\frac{288}{\pi\theta^4}\int\frac{{\mathrm{d}}\ell}{\ell^3}J^2_4(\ell\theta)P_\gamma(\ell),$$ where $J_4$ is the 4th-order Bessel function of the first kind.

All quantities relying on the background evolution depend on the equation-of-state of the various matter components. The neutrino equation-of-state is defined as $w_\nu(m_\nu,z)=
P(m_\nu,T(z))/\rho(m_\nu,T(z))$. We compute the pressure P and the energy density $\rho$ at points of a grid $(m_\nu,T(z))$, using the fact that the distribution of neutrinos in the phase space is a Fermi-Dirac distribution. The result is well approximated by the fitting function $$\label{eq:nz}
w_\nu(m_\nu,z)=\frac{1}{3}\left[1+\left(\frac{m_\nu}{(1+z)\,0.058\,\mathrm{eV} }\right)^{a}\right]^{-b},$$ where $a=1.652$ and $b=0.561$, and is shown in Fig. \[fig:wmz+deltaMap2\] (left panel). The transition to the non-relativistic regime occurs earlier for heavier particles, at the redshift given by Eq. (\[eq:ztrans\]) and indicated in the figure. The lensing efficiency window shows the redshift range probed by our data. At the upper end of 