\begin{table}%t8
\caption{\label{lensmodel_results}Most likely mass model parameters.} 
\small%\centerline
{
\begin{tabular}{cccccccc}
\hline
\hline
\noalign{\smallskip}
Clump & X            & Y           & $\epsilon$ & $\theta$ & $\sigma_0$ & $r_{\rm core}$ & $r_{\rm cut}$  \\
      & ($\arcsec$)  & ($\arcsec$) &            & (deg)    &            & (kpc)          & (kpc)          \\
\hline
\noalign{\smallskip}
Cluster & $\rm -0.5^{+4.1}_{-1.2}$  & 2.7~$\pm$~1.5 & $\rm 0.69^{+0.0}_{-0.1}$ & 31.3~$\pm$~1.1 & 1144.8~$\pm$~36 & 60.8~$\pm$~24 & [1500] \\
\noalign{\smallskip}
L$^*$ elliptical galaxy & -- & -- &-- & -- & 135.1~$\pm$~43.9 & [0] & $\rm 30.1^{+43.6}_{-4.9}$ \\
\noalign{\smallskip}
\hline
\end{tabular}}
\smallskip
The columns show:
position respect to the brightest cluster galaxy (X,Y), ellipticity of
the mass distribution ($\epsilon$, expressed as $a^2-b^2/a^2+b^2$,
were $a$ and $b$ are the semi-major and semi minor axes of the ellipse
that describes the light distribution of the clump), position angle
($\theta$), velocity dispersion~($\sigma_0$), core radius ($r_{\rm
core}$) and scale radius ($r_{\rm cut}$). Error bars correspond to
$1\sigma$ confidence level as inferred from the \textsc{mcmc}
optimization.  Values into brackets are not optimized.  When the
posterior distribution is not Gaussian, we report the mode and
asymmetric error bars. The coordinates of the brightest cluster galaxy
are $\rm RA=4^{h} 54^{m} 10.87^{s}$, $\rm Dec=-3^{\circ} 0\arcmin
54.00\arcsec$.
\end{table}