\begin{table}%[!]%T3
\caption{\textit{Erratum for Table~3 in \citet{gielen09}}: best-fit parameters deduced from our full spectral fitting.}
\begin{tabular}{lrllllll}
\hline \hline\noalign{\smallskip}
Name & $\chi^2$ &  $T_{\rm \rm dust1}$ & $T_{\rm \rm dust2}$ & Fraction & $T_{\rm \rm cont1}$ & $T_{\rm \rm cont2}$ & Fraction \\
    &          &     (K)     & (K)         & $T_{\rm \rm dust1}{-}T_{\rm \rm dust2}$    & (K)         & (K)         & $T_{\rm \rm cont1}-T_{\rm \rm cont2}$   \\
\hline\noalign{\smallskip}
EP~Lyr & 5.4 &$ 100_{\rm 50}^{50}$ &$ 200_{\rm 50}^{50}$ &$ 0.90_{\rm 0.05}^{0.10}{-}0.10_{\rm 0.10}^{0.05}$ &$ 100_{\rm 50}^{50}$ &$ 643_{\rm 50}^{302}$ &$ 0.98_{\rm 0.04}^{0.01}{-}0.02_{\rm 0.01}^{0.04}$\\
HD~52961  & 50.0 &$ 200_{\rm 50}^{50}$ &$ 700_{\rm 50}^{50}$ &$ 0.90_{\rm 0.05}^{0.05}{-}0.10_{\rm 0.05}^{0.05}$ &$ 100_{\rm 50}^{50}$ &$ 1000_{\rm 50}^{50}$ &$ 0.99_{\rm 0.01}^{0.01}{-}0.01_{\rm 0.01}^{0.01}$\\
\end{tabular}
\begin{tabular}{lccccc}
\hline \hline\noalign{\smallskip}   
Name & Olivine & Pyroxene & Forsterite & Enstatite & Continuum\\
      & small--large & small--large &  small--large &small--large &\\
\hline\noalign{\smallskip}   
EP~Lyr    &$ 0.24_{\rm 0.24}^{16.83}{-}8.74_{\rm 7.64}^{7.92}$    &$7.17_{\rm 4.79}^{13.69}{-}8.09_{\rm 7.24}^{12.67}$    &$35.18_{\rm 2.78}^{3.04}{-}2.08_{\rm 1.89}^{2.61}$    &$ 0.00_{\rm 0.00}^{0.00}{-}38.50_{\rm 3.46}^{4.30}$    &$57.99_{\rm 3.60}^{2.53}$\\
\par
HD~52961    &$ 0.00_{\rm 0.00}^{0.00}   {-}  0.00_{\rm 0.00}^{0.00}$    &$59.17_{\rm 0.69}^{0.72}{-}0.00_{\rm 0.00}^{0.00}$    &$0.77_{\rm 0.69}^{1.46}  {-}  40.06_{\rm 1.62}^{1.02}$    &$ 0.00_{\rm 0.00}^{0.00}{-}0.00_{\rm 0.00}^{0.00}$    &$68.88_{\rm 0.46}^{0.42}$\\
\noalign{\smallskip}   \hline
\end{tabular}
\tablefoot{Listed are the $\chi^2$, dust, and continuum temperatures and their relative fractions. Best-fit parameters deduced from our full spectral fitting. 
The abundances of small and large grains of the various
dust species are given as fractions of the total mass, excluding the dust responsible for the continuum emission.
The last column gives the continuum flux contribution, listed as a percentage of the total integrated flux over the 
full wavelength range.}
%\vspace*{2mm}
\end{table}