\begin{table}%t1
\par
\caption{\label{tab:instrum}Instruments used for \corot\ photometric follow-up.}
%\centerline
 { { 
\begin{tabular}{l l}
\noalign{\smallskip}
\hline\hline
Instrument&Observatory\\
\hline
BEST 0.2-m$^a$&  Observatoire de Haute Provence, France\\
BESTII 0.25-m$^a$&  Cerro Armazones, Chile\\
TEST 0.3-m&Th\"uringer Landessternwarte, Germany\\
Vienna 0.8-m& Vienna Observatory, Austria\\
IAC 80-cm& Observatorio del Teide, Canary Islands, Spain\\
WISE 0.46-m, 1-m& WISE Observatory, Israel\\
OHP 1.2-m& Observatoire de Haute Provence, France\\
Euler 1.2-m telescope&La Silla, Chile\\
Tautenburg  2-m &Th\"uringer Landessternwarte, Germany\\
CFHT/Megacam 3.6-m &Mauna Kea, Hawaii\\
%VLT/FORS 8m&Paranal, Chile\\
\hline
\end{tabular}
}}
\par
\smallskip
 {$^a$ The small BEST and BEST II telescopes are not used in the follow-up as decribed here. They obtained previous timeseries of \corot's sample fields \citep{kabath+07, karoff+07, kabath+08, kabath+lrc2, kabath+lra2, rauer+09} which are routinely checked against the detections from \corot. They will also be used for future surveying of \corot-short run fields.} 
\par
\normalsize
\rm
\end{table}