\begin{table}%t3
\caption{\label{fitresults1}Listed are the best fit parameters deduced from our full spectral fitting.}
\par
%\centerline
{\small
\begin{tabular}{lrllllll}
\hline \hline
Name & $\chi^2$ &  $T_{\rm dust1}$ & $T_{\rm dust2}$ & Fraction & $T_{\rm cont1}$ & $T_{\rm cont2}$ & Fraction \\
    &          &     (K)     & (K)         & $T_{\rm dust1}$--$T_{\rm dust2}$    & (K)         & (K)         & $T_{\rm cont1}$--$T_{\rm cont2}$   \\
\hline
EP~Lyr & 5.4 &$ 114_{\rm  14}^{  122}$ &$ 228_{\rm  89}^{ 488}$ &$ 0.9_{\rm 0.6}^{ 0.1}- 0.1_{\rm 0.1}^{ 0.6}$ &$ 205_{\rm 103}^{  702}$ &$ 641_{\rm 301}^{  331}$ &$ 0.96_{\rm 0.06}^{ 0.02}- 0.04_{\rm 0.02}^{ 0.06}$\\
HD~52961  & 50.0 &$ 200_{\rm  0}^{  10}$ &$ 724_{\rm  96}^{ 186}$ &$ 0.9_{\rm 0.1}^{ 0.0}- 0.1_{\rm 0.0}^{ 0.1}$ &$ 111_{\rm 11}^{  356}$ &$ 996_{\rm 111}^{  4}$ &$ 0.99_{\rm 0.03}^{ 0.00}- 0.01_{\rm 0.00}^{ 0.03}$\\
\end{tabular}} 
\par
%\centerline
{\small
\begin{tabular}{lccccc}
\hline    
Name & Olivine & Pyroxene & Forsterite & Enstatite & Continuum\\
      & Small  -  Large & Small  -  Large &  Small  -   Large & Small  -   Large &\\
\hline
EP~Lyr    &$ 6_{\rm 6}^{ 41}$--$5_{\rm 5}^{25}$    &$8_{\rm7}^{34}$--$6_{\rm6}^{23}$    &$\rm 34_{15}^{19}$--$\rm 9_{ 8}^{33}$    &$ 5_{\rm 5}^{20}$--$\rm 28_{21}^{17}$    &$\rm 53_{ 20}^{11}$\\
HD~52961    &$ 0_{\rm 0}^{ 13}$--$1_{\rm  1}^{41}$    &$\rm 55_{18}^{12}$--$\rm 2_{2}^{43}$    &$\rm 6_{5}^{18}$--$33_{\rm 18}^{13}$    &$\rm  1_{ 1}^{8}$--$\rm 3_{3}^{26}$    &$\rm 69_{4}^{4}$\\
\hline
\end{tabular}}
\par
\medskip
Note: Top part: The $\chi^2$, dust and continuum temperatures and their
relative fractions. Bottom part: The abundances of small (0.1~$\mu$m) and large (2.0~$\mu$m) 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. The errors were obtained using a Monte-Carlo simulation based on 100 equivalent spectra. Details of the modelling
method are explained in \citet{gielen08}. 
\end{table}