\begin{table}%t4
%\centering
\par
\caption{\label{tab:results}Best-fit parameters for spectra of the \amin[3] around the centre of the galaxy clusters. } 
\begin{tabular}{lllll}
\hline \hline \noalign{\smallskip}
Parameter  &  \src{\codee}{\codeeexp} (\XMM)\tablefootmark{a,}\tablefootmark{b}  & \src{\codee}{\codeeexp} (\Chandra)\tablefootmark{a} &  \src{\codef}{\codefexp}\tablefootmark{a}  &  \src{\codet}{\codetexp} \\
 \hline 
Background scaling factor  &  0.99 $\pm$ 0.02  &   0.976 $\pm$ 0.013   &  -- \\
%\hline
Hydrogen column density (\unit[${\rm 10^{24}}$]{m^{-2}})  &  20.0 $\pm$ 0.4 ($\pm$ 0.2)  & 17.2 $\pm$ 1.3 &   6.6 $\pm$  0.4 ($\pm$ 0.3)  &  29 $\pm$ 2  \\
Hydrogen \unit[21]{cm} column density\tablefootmark{d} (\unit[${\rm 10^{24}}$]{m^{-2}}) & 8.38 & 8.38 & 6.25 & 22.1 \\
Emission measure\tablefootmark{c} (\unit[$10^{73}$]{m^{-3}}) & 2.57  $\pm$  0.04 ($\pm$ 0.01) & 2.44 $\pm$ 0.07 & 9.2  $\pm$  0.2 ($\pm$ 0.2) & 2.80 $\pm$ 0.16\\
Temperature (keV)\tablefootmark{e}  &  3.03  $\pm$  0.15 ($\pm$ 0.08)  & 3.50 $\pm$ 0.11 &  8.24 $\pm$ 0.58  ($\pm$ 0.97) &   3.2 $\pm$ 0.2  \\
$1/\alpha$\tablefootmark{f}  &  0.48 $\pm$ 0.09 ($\pm$ 0.03) & 0.48 (fixed) & --   &  --  \\
Fe abundance  &  0.61  $\pm$ 0.03  ($\pm$ 0.02) & 0.57 $\pm$ 0.07 &   0.58 $\pm$  0.10   ($\pm$ 0.06)  &    0.37 $\pm$ 0.10  \\
  Si/Fe abundance   &  0.65  $\pm$  0.12 ($\pm$ 0.01)  & -- &   --   &   --  \\
  Ni/Fe abundance  &  2.81   $\pm$  0.56 ($\pm$ 0.02)  & -- &   --  &    --  \\
Flux (\unit[0.1--2.4]{keV}) [\unit[${\rm 10^{-14}}$]{W~m^{-2}}]  &  1.03 $\pm$ 0.02  ($\pm$ 0.01)  & 1.03 $\pm$ 0.03 &  0.99   $\pm$  0.02 ($\pm$ 0.02)  &  0.66  $\pm$ 0.04  \\
Flux (\unit[2--10]{keV}) [\unit[${\rm 10^{-14}}$]{W~m^{-2}}]  & 1.11  $\pm$  0.02 ($\pm$ 0.04)  & 1.23 $\pm$ 0.03 & 1.70 $\pm$  0.04 ($\pm$ 0.13)  &   0.88 $\pm$ 0.05 \\
 C-stat / d.o.f.   &   270/229   & 389/295 &  252/224   & --\\
$\chi^{2}$ / d.o.f.    & -- & -- & -- &  189/134  \\
\hline 
\end{tabular}
\tablefoot{\tablefoottext{a}{The first quoted uncertainty is the statistical uncertainty on the value. The uncertainty between parentheses is due to the uncertainty in background estimation (Sect.~\ref{subsec:flares}).} 
\tablefoottext{b}{For this source, we fitted a ``\textit{wdem}'' model.}
\tablefoottext{c}{The emission measure is defined as $Y=\int n_{{\rm e}} n_{{\rm H}} {\rm d}V$, see also Sect.~\ref{sec:models}.}
\tablefoottext{d}{Deduced from the \unit[21]{cm} map by \citet{DIC90}.}
\tablefoottext{e}{For \textit{wdem}: ``mean temperature'', see Eq.~(\ref{eq:wdem_mean}).}  \tablefoottext{f}{As defined in Eq.~(\ref{eq:wdem_dydt}).}}
\end{table}