\begin{table}%t1
\caption{Summary of the initial scientific requirements and top level specifications for AMBER.}\label{tab:specs}
%\centerline
{\begin{tabular}{lccccc}
\hline\hline
Scientific topic  &Spectral &Spectral &Minimum~$K$ &Maximum&Imaging\\
&coverage &resolution$^a$ &band magnitude &visibility error$^b$ &(closure phase)\\
\hline
Key programs&&&&&\\
Young stellar objects &$J$, $H$, $K$, lines &medium &9 &$10^{-2}$ &\fbox{yes} \\
AGN dust tori &$K$  &low &\fbox{11} &$10^{-2}$ &yes \\
Extrasolar planets&\fbox{$J+H+K$}&low &5 &\fbox{$10^{-4}$} &no$^c$\\
\noalign{\smallskip}\hline
General programs&&&&&\\
Stellar structure  &lines  &\fbox{high} &2         &$10^{-4}$        &yes \\
 Circumstellar envelopes &$J$, $H$, $K$ &medium      &4         &$10^{-2}$        &yes \\
 Binary &$K$ &low         &9         &$10^{-3}$        &yes \\
QSO and AGN BLR  &$J$, $H$, $K$, lines &medium &11        &$10^{-2}$ &no \\ 
    \hline
  \end{tabular}}
  \smallskip
 $^a$~At the time when it was specified, low spectral resolution meant about 35, medium  resolution about 1000 and high resolution at least 10000. $^b$~Error on either  visibility amplitude (in normalized visibility units) or differential phase (in radians). $^c$~As phase is likely to be more critical for ESP than simultaneous  $J+H+K$ observations.
\end{table}