\begin{table}%[!ht]%T14
%\centering
\par
\caption{Application of the coronal loop models of Aschwanden \& Schrijver
(\cite{aschwanden02}) to the innermost three shells of 2A~0335+096. 
$M_{13}$ is the total cluster mass in $10^{13}~M_{\sun}$ within the radius
$R$ (kpc), for which we take the average radius of the shell.
$\overline{\rho_l}/\rho_{{\rm tot}}$ is the average mass density of the loops
divided by the total mass density of the cluster (including dark matter etc.).
The total mass density profile was taken from Ettori et~al. (\cite{ettori02}).
In this table, $f$ is the volume filling factor of the loops.
}
\label{tab:2a0335loop}
\begin{tabular}{lrrr}
\hline\hline
 shell    & 1 & 2 & 3 \\
$M_{13}$  & 0.0025 & 0.07 & 0.5 \\
$R$ (kpc) & 14 & 43 & 86 \\
$\Gamma$  & 4--6 & 7--40 & 1--100 \\
$L$ (kpc) & 3.6$f^{0.5}$ & 11$f^{0.5}$ & 44$f^{0.5}$ \\
$\overline{\rho_l}/\rho_{{\rm tot}}$ & 0.64$f^{0.5}$ & 0.33$f^{0.5}$ & 0.15$f^{0.5}$\\
$N$ & 7--11~$f^{0.5}$ & 14--70~$f^{0.5}$ & 12--500~$f^{0.5}$ \\
\hline
\end{tabular}
\end{table}