Table 5: Results of the analysis when using different limits for the scale radius $r_{\rm s}$.
Limits (kpc) $r_{\rm s}$ (kpc) c200 $\alpha $ $\Delta$( $\log(E_{\rm v}$)) $\Delta(\chi^2)$

(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 $\rm 299.5^{+0.09}_{-3.28}$ $\rm 6.9^{+0.16}_{-0.12}$ $\rm0.77^{+0.032}_{-0.021}$ 19.6 -41
(2) 300-400 $\rm 398.8^{+0.09}_{-3.28}$ $\rm 5.4^{+0.20}_{-0.12}$ $\rm0.91^{+0.020}_{-0.032}$ 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
Error bars correspond to 1$\sigma$ confidence level as inferred from the 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 4. 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 $\Delta(\chi^2)$.

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