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\end{figure}  We applied our pipeline to three of the image files available, High Noise File, High Noise PSF Applied File and Low Noise PSF Applied File. For the PSF Applied files, we checked that our Im2shape implementation can recover point-like objects by applying the PSF correction to each star. The images contain only the sheared galaxies, hence all the galaxies detected were considered as background galaxies at $z=0.8$, which is the average of the redshifts of the galaxies. We cut the catalogue discarding the galaxies with FWHM $<$ 5, with companions closer than 16 pixels and with $\sigma_{e} > 0.2$, where $\sigma_{e}$ is defined as the quadratic sum of the errors $\sigma_{e1}$ and $\sigma_{e2}$ given by IM2SHAPE. These cuts are made in order to consider, for the shear measurements, insulated galaxies with good shape measurements. Shear profiles are shown in Figure\,\ref{DES}. For the most complex image that we treated, we obtained a deviation parameter of 1.6, defined as the number of $\sigma$ that the result is away from the input value of $\sigma_{V} = 1250 km/sec$, i.e. $\sigma = \dfrac{result - input}{error}$ .  \begin{table*}  \centering  \caption{Summary of the weak lensing analysis}\label{tab:esp}  \label{table:2}  \begin{tabular}{@{}ccccccccc@{}}  \hline  \hline  \rule{0pt}{1.05em}%  [VMF\,98] & Density of background galaxies & $m_{L}$ & $m_{max}$ & $\langle\beta\rangle$ & $\sigma_{V}$ & M$^{(1)}$($r < 0.5 Mpc$) & $R_{200}$ & M$^{(2)}$($r < 0.5 Mpc$) \\  Id. & (galaxies/arcmin$^{2}$) & & & & (km/sec) & $10^{14} M_{\odot} h_{70}^{-1}$ & Mpc & $10^{14} M_{\odot} h_{70}^{-1}$ \\  \hline  \rule{0pt}{1.05em}%  001 & 33 & 23.0 & 27.0 & 0.42 & - & - & - & - \\   022 & 15 & 20.7 & 26.0 & 0.63 & 600 $\pm$ 30 & 1.3 & 1.7 $\pm$ 0.2 & 1.2 \\   093 & 9 & 22.3 & 25.0 & 0.50 & - & - & - & - \\  097 & 31 & 23.0 & 27.0 & 0.44 & 580 $\pm$ 40 & 1.2 & 1.2 $\pm$ 0.4 & 0.83 \\  102 & 26 & 22.7 & 26.9 & 0.50 & 450 $\pm$ 40 & 0.75 & 1.1 $\pm$ 0.1 & 0.62 \\  119 & 18 & 24.0 $^{(3)}$ & 26.4 & 0.30 & 860 $\pm$ 30 & 2.7 & 1.4 $\pm$ 0.1 & 1.4 \\  124 & 26 & 19.5 & 26.7 & 0.72 & - & - & - & - \\  148 & 19 & 24.0 $^{(3)}$ & 26.9 & 0.27 & 860 $\pm$ 140 & 2.7 & 1.4 $\pm$ 0.7 & 1.4 \\  \hline   \end{tabular}  \\  \begin{tablenotes}{\begin{footnotesize}  \end{footnotesize}  \begin{small}  \begin{flushleft}  \item [] (1) From the fit of the SIS profile  \item [] (2) From the fit of the NFW profile  \item [] (3) Here $m_{L}$ is defined as the lowest magnitude $r'$ such that the probability that the galaxy is behind the cluster is higher than 0.6}  \end{flushleft}  \end{small}  \end{tablenote}  \end{table*}