\begin{table}%T2
   \caption{Observations of four epochs.}
     \label{obstab}
 %\centerline
{
  \begin{tabular}{ccccccccc}
    \hline\hline
     \noalign{\smallskip}
       \rm{Epoch} & \hskip.6cm  & \rm{Date} & \hskip.6cm &
       \rm{Duration~(UT)} & \hskip.6cm &
       \rm{Stellar~phase$^{{a}}$} & \hskip.6cm &
       \rm{Restoring~beam~(mas)$^{{b}}$} \\
     \noalign{\smallskip}
     \hline
      \rm{I}   & & 1998/09/04 & & 08:33 $\sim$ 12:30 & & $\phi$ = 0.52 & &
       $\sim$0.6 $\times$ 0.4\\
      \rm{II}  & & 2000/05/12,13$^{{c}}$ & & 19:09 $\sim$ 01:00 & &
       $\phi$ = 0.60 & & ${\sim}$1.05 $\times$ 0.6 \\
      \rm{III} & & 2000/09/05  & & 10:01 $\sim$ 15:00  & &$\phi$ = 0.83  & &
       ${\sim}$0.4 $\times$ 0.2 \\
      \rm{IV}  & & 2001/01/06 & & 02:31 $\sim$ 07:30 & &$\phi$ = 0.05  & &
        $\sim$0.5 $\times$ 0.2 \\
     \hline
  \end{tabular}}
\par
 \medskip
 $^{{a}}$ Stellar phase, $\phi$ varies from 0 to 1
          during one cycle. $\phi=0$ for visual maximum. The stellar
          phases given here are determined using the same method as
          that of Diamond \& Kemball (\cite{diamond03}) with the
          optical maximum at JD = 2~450~773.0 and a mean period of
          557.4 days.\\
$^{{b}}$ 1~mas corresponds to $0.5685\times10^{11}$m
          at the assumed distance to TX~Cam.\\
$^{{c}}$ The Los Alamos antenna was not used.
\end{table}