\begin{table}%T5
\par
\caption{\label{uncertainties}{Estimated uncertainties of the
    different instrumental artifacts present in band~3 for the~10
    AOT~01 speed 4 spectra of our sample of standard stars.}}
%\centerline
{\begin{tabular}{lccc}  \hline\hline
\rule[-3mm]{0mm}{8mm} {\bf{Uncertainty source}} & {\bf{3A}} &
{\bf{3C}} & {\bf{3D}}\\
\hline \hline
bad detector data points, scan jumps \& glitches & $\sim$2\% &
 $\sim $2.5\% & $\sim$4\% \\
\hline
fringe residuals &  &  &  \\
 $\ \ \ \ $before correction with {\texttt{resp\_inter}} \&
 {\texttt{fringes}} & $\sim$8\% & $\sim$4\% & $\sim $3\% \\
 $\ \ \ \ $after correction with {\texttt{resp\_inter}} \&
 {\texttt{fringes}} & $\sim $2\% & $\sim$2\% & $\sim $2\% \\
\hline
baseline ripples & $\sim $2\% & $\sim$2\% & $\sim$1\% \\
\hline
leakage at 27.5~$\mu$m $^a$ &  &  & $\sim$30\% \\
\hline
RSRF artifact at 12.3~$\mu$m & $\sim$4\% &  &  \\
\hline
Photometric calibration (scaling factors) $^b$ & $\sim$6.5\% ($\sim$9.5\%)  & $\sim$5.5\%
($\sim$9.5\%) & $\sim$9\% ($\sim$12\%) \\
\hline
\end{tabular}}
\smallskip
Notes:\\
 $^a$ Calculated as $F_{27.5~\mu\mbox{\scriptsize
     m}}/$$G_{27.5~\mu\mbox{\scriptsize m}}$ with~$F$ the flux of the
 SWS spectrum, $G$ the flux of the synthetic spectrum.\\
 $^b$ The estimated errors originate from our scaling factors. Between
brackets: the mean of the scaling factors,\\
 with inclusion of higher scanner speed observations of the sample of
standard stars.
\end{table}