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% Table 6, Post-flare optical
\begin{deluxetable}{lllll}
\tablenum{6}
\tablecaption{Post-flare optical observations}
\footnotesize
\tablehead{
\colhead{Date} & \colhead{Wavelength} & \colhead{Magnitude} & 
  \colhead{Flux density} & \colhead{Source of data} \\ 
\colhead{}     & \colhead{(A)}        & \colhead{}          & 
  \colhead{(mJy)}       & \colhead{}
}
\startdata
1998 Jul 22 & 7000 (R-band)  & $16.11\pm0.10$  & $1.022\pm0.094$ & Woomera\\
1998 Aug 09 & 5480 (V-band)  & $16.36\pm0.03$  & $1.049\pm0.029$ & CTIO\\
1998 Aug 09 & 7000 (R-band)  & $16.03\pm0.03$  & $1.022\pm0.028$ & CTIO\\
1998 Aug 09 & 9000 (I-band)  & $15.66\pm0.03$  & $1.225\pm0.034$ & CTIO\\ 
1998 Sep 16 & 5480 (V-band)  & $16.44\pm0.10$  & $0.974\pm0.090$ & Woomera\\
1998 Sep 16 & 7000 (R-band)  & $15.96\pm0.10$  & $1.173\pm0.108$ & Woomera\\
\enddata
\tablecomments{The observations were made at Woomera and CTIO (this paper).
The magnitudes and energy flux are corrected for interstellar extinction 
using $E_{B-V}=0.035$,
which was derived using the relation $E_{B-V}=1.3\times 10^{-22}
N_{\rm{H}} (cm^{-2})$ of Bohlin et al. (1978) and the HI column 
density $N_{\rm{H}}=2.35 \times 10^{20}\rm{cm}^{-2}$ published in Brinkmann 
et al. (1994). The magnitude corrections vary 
from $\sim0.01$mag to $\sim 0.14$mag.
The transformations given in Zombeck (1982) are used to convert 
magnitudes into energy flux. The uncertainty is calculated using standard 
error propagation.
}

\end{deluxetable}

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