\begin{table}%t3
%\centering
\par
\caption{\label{tab:fitparam}Spectral fit parameters for the CXB, the GRXE and the Earth emission.}
\begin{tabular}{@{}lcccccc@{}}
\hline \hline \noalign{\smallskip}
Spectra (model\tablefootmark{a}) & $\Gamma_1$\tablefootmark{b} & $N_1$\tablefootmark{c} & $E\dmrm{0}$\tablefootmark{d} & $\Gamma_2$\tablefootmark{b} & $N_2$\tablefootmark{c} & $\chi\dmrm{red}^2$ \\
\noalign{\smallskip}\hline
CXB (bknpow) & 1.68 & 15.2 & 28.7 & 2.42	& --   & 0.51 \\
CXB (cutoff)\tablefootmark{e} 	& 1.95\tablefootmark{f}& 44.1	& 127	& --	& --   & 0.85 \\
GRXE (cutoff)		& 0.0\tablefootmark{f} 	& 0.43	& 8.83	& 1.55\tablefootmark{f}  & 0.82 & 0.25 \\
GRXE (bremss)\tablefootmark{e} & --  & 13.9	& 14.7	& 1.55\tablefootmark{f} & 0.79 & 0.34 \\
Earth (bknpow) & 0.37 & 0.050	& 49.4	& 1.78	& --   & 0.05 \\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{Model is either a broken powerlaw (bknpow), a cutoff powerlaw (cutoff) or bremsstrahlung (bremss), with or without an extra powerlaw.}
\tablefoottext{b}{Photon index of low-- (1)~or high-energy (2)~powerlaw.}
\tablefoottext{c}{Normalization at 1~keV in \phcmskeVsr.}
\tablefoottext{d}{Characteristic energy in keV. Either the break energy (bknpow), the cut-off energy (cutoff) or the $kT$ energy (bremss).}
\tablefoottext{e}{The more physical model.}  
\tablefoottext{f}{Fixed parameter value.}}
\end{table}