data probes thus both the scale-independent and the scale-dependent suppression effects of the sub-free-streaming regime.

![image](11077fg1a.ps){width="7cm"} ![image](11077fg1b.ps){width="7cm"}

We proceed by presenting in Sect. 2 the methodology followed to compute the spectra. In the same section we introduce the statistical analysis performed and the datasets used. Cosmological constraints are obtained and discussed in Sect. 3 and our conclusions are presented in Sect. 4.

Methodology {#sec2}
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Implementing massive neutrinos in cosmic-shear 2-point correlation functions {#sec2a}
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We perform a statistical analysis of a mixed dark-matter scenario by considering a 8+1 dimensional parameter space (see Sect. \[sec2b\]). For each sampled model of this parameter space the cosmic-shear power spectrum $P_\gamma(\ell)$ is computed by integrating the non-linear *total* matter power spectrum $P_{\mathrm{m}}^{\mathrm nl}$ along the line-of-sight, up to the limiting redshift of the survey $z_\mathrm{lim}$, to account for the distribution of source galaxies $n(z)$. It is given by $$\label{eq:pgamma}
P_\gamma(\ell)=\frac{9{\Omega_{\mathrm{m}}}^2 H_0^4}{4c^4}
\int_0^{z_\mathrm{lim}} \frac{{\mathrm{d}}z}{H(z)} \, (1+z)^2 W^2(z) P_{\mathrm{m}}^{\mathrm {nl}} (k,z),$$ where $k=\ell/S_K(\chi(z))$ and $$W(z)= \int_z^{z_\mathrm{lim}}{\mathrm{d}}z' n(z')
\frac{S_K[\chi(z')-\chi(z)]}{S_K[ \chi(z')]}$$ defines the lensing efficiency window function, and $S_K[\chi(z)]$ denotes the comoving angular diameter distance as function of redshift, which reduces to the comoving radial distance $\chi(z)$ for spatial flatness $K=0$. The redshift distribution of sources was 