to be evaluated properly [see e.g., @quintlens for a weak-lensing analysis of quintessence].

The log-likelihood is defined as usual to be $$\label{eq:logL}
\log\mathcal{L}=-\frac{1}{2}\sum_{ij}\Delta{\left<M^2_\mathrm{ap}( \theta_i )\right>}(\mathsf{Cov}^{-1})_{ij}\Delta{\left<M^2_\mathrm{ap}( \theta_j )\right>},$$ where $\Delta{\left<M^2_\mathrm{ap}( \theta_i )\right>}$ is the difference between the observed and the theoretical values of the aperture mass variance computed at angles $1 \arcmin \leq \theta_i \leq
230\arcmin$ and $\mathsf{Cov}$ is the corresponding covariance matrix.

We sample the likelihood over a regular grid of the parameter space, for a total of $\sim 10^7$ models. The domain of the grid is : $\omega_{\mathrm{b}}\in[0.0186,0.0249]$, $\omega_{\mathrm{cdm}}\in[0.110,0.152]$, $\omega_\nu \in[0,0.042]$, $h \in[0.62,0.80]$, ${N_\mathrm{eff}}\in[2,4]$, $\tau \in[0,0.225]$, ${n_\mathrm{s}}\in[0.87,1.02]$, $\sigma_8 \in[0.65,0.92]$.

In this work we use the aperture mass vector and covariance matrix obtained in Fu [et al. ]{}(2008), which was measured over 57 square degrees (35 square degrees of effective area) in three connected patches of the sky, using $2.5 \times 10^6$ galaxies with magnitudes $21.5 < i_\mathrm{AB} < 24.5$. The covariance matrix includes shape noise in the shear estimator, non-Gaussian cosmic variance, and the residual B-mode. The shear-measurement pipeline was tested on STEP2 simulations [@step2] and shown to be slightly biased, underestimating the shear on average by 2% [@Fu]. Moreover, this analysis showed that highly anisotropic point-spread-functions (PSF) may 