\begin{table}%t2
%\centering
\par
\caption{\label{table:pahs}The 4 S-type stars with significant emission features at~6.2, 7.9, and 11.2~\um.}
\par
\tiny\begin{tabular}{ccccccccccccc}
\hline\hline\noalign{\smallskip}
\multicolumn{3}{c}{Stellar parameters} & 6.2~\um & \multicolumn{4}{c}{7.9~\um} & 11.2~\um \\
\hline\noalign{\smallskip}
Name & $T_{{\rm eff}}$\tablefootmark{a} & C/O\tablefootmark{a} & Flux\tablefootmark{b} & Class\tablefootmark{c} & $\lambda_{\rm peak}$ & $\lambda_{\rm cen}$ & Flux\tablefootmark{b} & Flux\tablefootmark{b} \\
& K & & erg~cm$^{-2}$~s$^{-1}$ & & \um & \um & erg~cm$^{-2}$~s$^{-1}$ & erg~cm$^{-2}$~s$^{-1}$ \\
\hline\noalign{\smallskip}
CSS 173      & $3600 \pm 150$  & $0.97 \pm 0.01$ & $3.0 \pm 0.7 \times 10^{-13}$  & C & $8.25 \pm 0.05$ & $8.38 \pm 0.10$ & $1.6 \pm 0.2 \times 10^{-12}$ & $1.1 \pm 0.2 \times 10^{-13}$ \\
KR Cam       & $3400 \pm 150$  & $0.97 \pm 0.01$ & $6.2 \pm 0.6 \times 10^{-13}$  & C & $8.16 \pm 0.05$ & $8.31 \pm 0.06$ & $1.5 \pm 0.1 \times 10^{-12}$ & $1.3 \pm 0.2 \times 10^{-13}$ \\
BZ CMa       & $3400 \pm 150$   & $0.98 \pm 0.01$ & $20  \pm 2   \times 10^{-13}$  & B & $7.97 \pm 0.04$ & $8.02 \pm 0.04$ & $3.4 \pm 0.2 \times 10^{-12}$ & $9.8 \pm 0.5 \times 10^{-13}$ \\
CSS 757      & $3400 \pm 150$  & $0.97 \pm 0.01$ & $5.6 \pm 0.7 \times 10^{-13}$  & C & $8.27 \pm 0.05$ & $8.47 \pm 0.06$ & $2.2 \pm 0.2 \times 10^{-12}$ & $1.1 \pm 0.3 \times 10^{-13}$ \\
\hline  
\end{tabular}
\tablefoot{\tablefoottext{a}{Derived from the comparison of low-resolution spectroscopy with a dedicated grid of {\sc marcs} model atmospheres for S-type stars \citep[Plez et~al. in preparation,][]{Gustafsson2008}. The low-resolution spectroscopy was obtained for the complete sample of S-type stars, with the William Hershel Telescope on La~Palma for the sources in the northern sky (range: 4100~\AA--8300~\AA; resolution: 2~\AA) and with the 1.9~m telescope at the South African Astronomical Observatory for the southern targets (range: 4900~\AA--7800~\AA; resolution: 4~\AA). The entire dataset will be presented in a forthcoming paper.}
\tablefoottext{b}{Integrated line flux of the residual flux in the interval [6.12,6.5]~\um, [7.4,9.0] \um, or [10.9,11.8]~\um.}
\tablefoottext{c}{According to \citet{Peeters2002}.}}
 \end{table}