\begin{table}%t1
%\centering
\par
\caption{\label{overview_uncertainties_cohen}
 Summary of uncertainties attributed to the standard star spectra in
the CWW network in the 2--200~\mic\ range.}
\begin{tabular}{llll}\hline \hline
  \rule[-3mm]{0mm}{8mm}Description & Uncertainty & Spectral type
  & Wavelength region \\ 
\par
\hline \rule[-0mm]{0mm}{5mm}$\bullet$ propagation of systematic
  errors & & & \\
\par
\phantom{$\bullet$ } e.g.\ due to use of Vega as prime calibrator & &
  & \\
\par
\phantom{$\bullet$ } $\rightarrow$ absolute flux calibration of Sirius
   w.r.t.\ Vega & 1--3\% & A--M & 2--200~\mic \\
\par
$\bullet$ use of Engelke function \citep{Engelke1992AJ....104.1248E} &
3\% & A-dwarfs & 22--35~\mic \\
\par
 & 8\% & K-giants & 22--35~\mic \\
\par
$\bullet$ creation of "template'' spectrum & & & \\
\par
\phantom{$\bullet$ }$\rightarrow$ molecular features & up to 8\% &
  G--K & around 2.3, 4.0, 4.2, 8~\mic \\
\par
\phantom{$\bullet$ }$\rightarrow$ continuum & up to 4\% & A--M &
  2--200~\mic \\
\par
$\bullet$ presence of chromosphere/ionised wind & $\ga$10\% & G--M &
$\lambda > 100$~\mic \\
\par
\phantom{$\bullet$ }presence of circumstellar dust & $\ga$10\% &
A--M & $\lambda > 2$~\mic \\
\par
$\bullet$ systematic difference with new Engelke & & & \\
\par
\rule[-3mm]{0mm}{3mm}\phantom{$\bullet$ } standards \citep{Engelke2006AJ....132.1445E} &
  \raisebox{1.5ex}[0pt]{4--7\% } & \raisebox{1.5ex}[0pt]{G2--M5 } &
  \raisebox{1.5ex}[0pt]{1--4~\mic}\\
\par
\hline
  \end{tabular}
\end{table}