Furthermore, the derived constraint does not take account of degeneracies with dark energy. In more general scenarios with non-vanishing curvature or with non-cosmological-constant dark energy, both growth of structure and distances, as functions of redshift, depend on both the dark-energy density parameter $\Omega_{\mathrm{de}}$ and the equation-of-state $w_{\mathrm{de}}$. To effectively break the ${\Omega_\nu}-{\Omega_{\mathrm{m}}}$ degeneracy, it will thus be necessary to use a measure that is not degenerate in $\Omega_{\mathrm{de}}$ and $w_{\mathrm{de}}$. One possibility is to exploit the lens efficiency at different redshift bins with tomography [e.g., @denutom]. However, even with tomography, some direct neutrino-dark energy degeneracy will remain due to the transition epoch from matter to dark-energy domination [@denu].

Regarding the effective number of relativistic species, cosmic shear is sensitive to it via the change in the matter-radiation equality. A higher ${N_\mathrm{eff}}$ implies a longer radiation-dominated era, and thus a more efficient suppression of growth. Hence, the relative amplitude of small and large scales changes and the shear power spectrum tilts. The effect is however weak and we find an essentially flat likelihood in the probed range of ${N_\mathrm{eff}}\in
[2,4]$, meaning that the data do not constrain this parameter.

![image](11077fg4a.ps){width="6cm"} ![image](11077fg4b.ps){width="6cm"} ![image](11077fg4c.ps){width="6cm"}

Joint analysis {#sec3b}
--------------

We now explore the parameter 