\begin{table}%t5
\caption{Results of the analysis when using different limits for the scale radius $r_{\rm s}$.}\label{tab5}
%\centerline
 {\small \begin{tabular}{cccccc}
\hline\hline
Limits (kpc) & $r_{\rm s}$ (\footnotesize{kpc}) & $c_{200}$ & $\alpha$ & $\Delta$($\log(E_{\rm v}$)) & $\Delta(\chi^2)$\\
\hline
\noalign{\smallskip}
(0) 150--750 & $\rm 727.0^{+13.84}_{-76.77}$ & $\rm 3.1^{+0.34}_{-0.07}$ & $\rm 1.09^{+0.015}_{-0.036}$ & --  & -- \\
(1) 200--300 & $\rm 299.5^{+0.09}_{-3.28}$   & $\rm 6.9^{+0.16}_{-0.12}$ & $\rm 0.77^{+0.032}_{-0.021}$ & 19.6 & --41 \\ 
(2) 300--400 & $\rm 398.8^{+0.09}_{-3.28}$   & $\rm 5.4^{+0.20}_{-0.12}$ & $\rm 0.91^{+0.020}_{-0.032}$ & 8.9 & --19 \\
(3) 400--600 & $\rm 598.8^{+1.27}_{-41.18}$  & $\rm 3.7^{+0.24}_{-0.08}$ & $\rm 1.03^{+0.024}_{-0.021}$ & 1.9 &  --4\\
(4) 600--800 & $\rm 719.3^{+22.94}_{-61.96}$ & $\rm 3.0^{+0.32}_{-0.01}$ & $\rm 1.09^{+0.019}_{-0.026}$ & --3.9 & --1 \\
\hline
\end{tabular}}
\smallskip
Error bars correspond to 1$\sigma$ confidence level as inferred from the \textsc{mcmc} optimization.
When the posterior probability distribution is not Gaussian, we report the mode and asymmetric error bars. (0) corresponds to the results of the mass model presented in Table~\ref{tab4}. The following lines corresponds to models obtained when assuming a different prior for the scale radius.
For each model ($i$), we report the results on the parameters of the dark matter clump.
To compare the different lines, we report $\Delta$($\log(E_{\rm v}$)) and $\Delta(\chi^2)$.
\end{table}