\begin{table}%t5
  \caption{\label{deabs}Best power-law fits to the HESS spectra corrected for 
 EBL absorption following \citet{franceschini}.}  
 \small     %\centering
\par
      \begin{tabular}{l c c c}
	 \hline\hline
	 \noalign{\smallskip}
	  Epoch  & $\Gamma_{\rm int}$\tablefootmark{a} & $\nu F_{\nu} ({\rm 1 TeV})$\tablefootmark{b} & $\chi^2$~(NDF)  \\
     		 &	    & [$10^{-12}$ erg cm$^{-2}$~s$^{-1}$] &   \\
	  \hline
	 2004 &  $3.1\pm0.4$ & $1.8\pm0.4$ & 6.4~(7)  \\
     	 2005 &  $2.6\pm0.2$ & $2.7\pm0.4$ & 13.2~(6)  \\
     	 2006 &  $2.4\pm0.2$ & $2.9\pm0.4$ & 4.3~(7)  \\
     	 2007 &  $3.1\pm0.7$ & $1.2\pm0.9$  & 0.5~(2)  \\
	 \noalign{\smallskip}
	  2005 7$-$8\tablefootmark{c} & $3.2\pm0.4$ & $2.4\pm0.6$ & 9.2~(4) \\
     	 2005 ~~9\tablefootmark{c}    & $2.5\pm0.3$ & $2.9\pm0.5$ & 4.7~(6) \\
	 \noalign{\smallskip}
	  Total &  $2.69\pm0.16$ & $2.34\pm0.20$ & 8.9~(8) \\ 
	 \hline 
    \end{tabular}
    \tablefoot{\tablefoottext{a}{Only the statistical errors are shown.}
  \tablefoottext{b}{The normalization at 1 TeV, in $\nu F_{\nu}$ units.}
  \tablefoottext{c}{The HESS spectrum in 2005, extracted in two different epochs 
  (see Fig.~\ref{nightly_plots}):  before the XMM pointings (observing periods 
  2005, 7$-$8) 
  and during the XMM epoch (period 2005, 9).} }  
\end{table}