\begin{table}%t2
\caption{\label{table:fitnight_summary}Average number of images and nights per band for 
each SNLS light-curve. Note that there is less data in~$\gme$ and~$\zme$.
The~$\chi^2_n$~column refers to the last fit that imposes equal
fluxes on a given night. The expected value is~1.25 (due to pixel correlations),
so we face a moderate scatter excess of about~12\% over photon statistics. 
The larger values in~$\ime$ and~$\zme$ indicate that fringes play a role in this excess. The last column displays the average wavelength of the effective
filters in~\AA.}
%\centering
\par
\begin{tabular}{c|cccc}
\hline\hline
Band   & Average nb. & Average nb. &~$\chi^2_n$ & Central\\
       & of images      &  of epochs          &  per d.o.f. & wavelength \\
\hline
$\gme$ & 40 & 9.8 & 1.50    & 4860\\
$\rme$ & 75 & 14.4 &  1.40  & 6227\\
$\ime$ & 100 & 14.8 &  1.63 & 7618\\
$\zme$ & 60 & 7.9 &  1.70   & 8823\\ 
\hline
\end{tabular}
\end{table}