\begin{table}%t2
\caption{\label{t2}Best-fit parameters for the X-ray spectra of 1ES 1210$-$646 
from the observations described in this paper.}
%\scriptsize
%%\centering

 \begin{tabular}{ccccc}
\hline\hline %\noalign{\smallskip}
Model & XRT \#1 & XRT \#2 & XRT \#3 & JEM-X+IBIS \\
parameter & (0.3--9~keV) & (0.3--9~keV) & (0.3--9~keV) & (3--100~keV) \\
%\noalign{\smallskip}
\hline
%\noalign{\smallskip}
\multicolumn{1}{l}{$powerlaw$ $(+Fe$ $line)$:} & & & & \\
${\chi^{2}}$/d.o.f. & 207.3/182 & 69.8/51 & 188.6/147 & --- \\
$N_{\rm H}$ ($\times$10$^{21}$ cm$^{-2}$) & 5.2~$\pm$~0.4 & 
$\rm 5.0^{+0.8}_{-0.7}$ & 5.1~$\pm$~0.5 & --- \\
$\Gamma$ & 1.80~$\pm$~0.07 & $\rm 1.63^{+0.15}_{-0.14}$ & 1.45~$\pm$~0.08 & --- \\
Normalisation\tablefootmark{*} & $\rm 11.5^{+0.9}_{-1.0}$ & $\rm 0.47^{+0.09}_{-0.07}$ & 33~$\pm$~3 & --- \\
$E$ (keV)       & $\rm 6.71^{+0.05}_{-0.03}$ & --- & --- & --- \\
$\sigma$ (keV)  & $\rm 0.16^{+0.05}_{-0.04}$ & --- & --- & --- \\
$I$ ($\times$10$^{-4}$ ph cm$^{-2}$ s$^{-1}$) & $\rm 5.8^{+1.3}_{-1.2}$ & --- & --- \\
\multicolumn{1}{l}{$bremsstrahlung$ $(+Fe$ $line)$:} & & & & \\
${\chi^{2}}$/d.o.f. & 221.7/182 & 72.3/51 & 186.3/147 & --- \\
$N_{\rm H}$ ($\times$10$^{21}$ cm$^{-2}$) & 4.3~$\pm$~0.3 & 
$\rm 4.3^{+0.7}_{-0.6}$ & 4.7~$\pm$~0.4 & --- \\
$kT_{\rm br}$ (keV) & $\rm 7.3^{+1.4}_{-1.1}$ & $\rm 12^{+9}_{-4}$ & 
$\rm 22^{+11}_{-6}$ & --- \\
Normalisation\tablefootmark{*} & $\rm 12.1^{+0.6}_{-0.5}$ & 0.56~$\pm$~0.04 & 48~$\pm$~2 & --- \\
$E$ (keV)       & 6.72~$\pm$~0.04 & --- & --- & --- \\
$\sigma$ (keV)  & $\rm 0.17^{+0.06}_{-0.04}$ & --- & --- & --- \\
$I$ ($\times$10$^{-4}$ ph cm$^{-2}$ s$^{-1}$) & $\rm 6.2^{+1.2}_{-1.3}$ & --- & --- \\
\multicolumn{1}{l}{$BB+powerlaw$:} & & & & \\
${\chi^{2}}$/d.o.f. & --- & --- & --- & 99.7/86 \\
$N_{\rm H}$ ($\times$10$^{21}$ cm$^{-2}$) & --- & --- & --- & [5.0] \\
$kT_{\rm BB}$ (keV) & --- & --- & --- & $\rm 1.54^{+0.06}_{-0.08}$ \\
$R_{\rm BB}$\tablefootmark{\dagger} (km) & --- & --- & --- & $\rm 5.9^{+1.5}_{-1.9}$ \\
$\Gamma$ & --- & --- & ---& 2.1~$\pm$~0.7 \\
$N$\tablefootmark{*}$_{\rm pow}$ & --- & --- & --- & $\rm 2.9^{+46.7}_{-2.8}$ \\
$C_{\rm calib}$ & --- & --- & --- & $\rm 2.0^{+3.5}_{-1.7}$ \\
\multicolumn{1}{l}{$bremsstrahlung+powerlaw$:} & & & & \\
${\chi^{2}}$/d.o.f. & --- & --- & --- & 120.4/86 \\
$N_{\rm H}$ ($\times$10$^{21}$ cm$^{-2}$) & --- & --- & --- & [5.0] \\
$kT_{\rm br}$ (keV) & --- & --- & --- & $\rm 8.7^{+2.7}_{-1.7}$ \\
$N$\tablefootmark{*}$_{\rm br}$ & --- & --- & --- & $\rm 72^{+10}_{-25}$ \\
$\Gamma$ & --- & --- & --- & $\rm 1.5^{+0.7}_{-4.3}$ \\
$N$\tablefootmark{*}$_{\rm pow}$ & --- & --- & --- & $\rm 1.7^{+32.1}_{-1.7}$ \\
$C_{\rm calib}$ & --- & --- & --- & $\rm 0.13^{+0.10}_{-0.06}$ \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\multicolumn{1}{l}{X-ray luminosity$\ddagger$:} & & & & \\
0.5--2   keV  & 0.2 & 0.1 & 0.7 & --- \\
  2--10  keV  & 0.4 & 0.2 & 1.9 & 2.0 \\
 20--100 keV  & --- & --- & --- & 0.1 \\
\hline
\end{tabular}
\tablefoot{The above luminosities, corrected for interstellar Galactic absorption, are computed
assuming a distance $d = 2.8$~kpc (Masetti et~al. \cite{Masetti2009}) and are expressed in units of
10$^{35}$~erg~s$^{-1}$. In the cases in which the  X-ray data could not completely cover
the X-ray interval of interest for the luminosity  
determination, an extrapolation of
the best-fit model is applied. 
\tablefoottext{*}{ In units of 10$^{-3}$.} 
\tablefoottext{\dagger}{ Computed assuming a distance $d = 2.8$~kpc 
to the source.} 
\tablefoottext{\ddagger}{ Computed using the powerlaw model for the XRT spectra and the BB+powerlaw model for the JEM-X+IBIS spectrum.}}
\end{table}