\begin{table}%t1
\caption{List of X-ray bursts from \bron \label{tab1}. Bursts 2, 3
and 7\protect have been published before. Values between parentheses represent\protect
uncertainties in the last digit.}
%\centerline
{\begin{tabular}{llllll}
\hline\hline 
No. & Date & Instr.     & Peak         & Persistent & $\tau$ \\
   &  &                & flux         & flux       &        \\
   &  &                & \multicolumn{2}{c}{(Crab units$^\star$)}  &(s)   \\
\hline
1         & 1996 Oct. 1  & WFC  &  3.7(3) & 0.0048(5) & 117(2)     \\
2$^\dag$  & 1999 Jun. 10 & WFC  &  3.3(3) & 0.0037(5) & 29(4)      \\
3$^\ddag$ & 2000 May 12 & PCA  &  $>$$3.2$ & $<$$0.0146$ & 8.95(5) \\
4         & 2001 May 18 & WFC  &  2.5(3) & 0.0094(5) & 5.8(4)   \\
5         & 2001 Sep. 29 & ASM  &  2.9(1) & 0.0061(7)$^\P$ & 25(3)   \\
6         & 2003 Aug. 5  & ASM  &  2.1(1) & 0.0080(8)$^\P$ & 22(10)$^\times$   \\
7$^\ast$ & 2004 Jun. 18& PCA& 0.26(1)& 0.0126(3) & 12.5(5) \\
\hline 
\end{tabular}}
\par
\smallskip
 $^\star$ For a burst peak spectrum as
determined in this paper for the first burst, one Crab unit translates to a bolometric
flux of $2.7\times10^{-8}$~\ecs. For the persistent flux, one may adhere to a 2--10 keV
flux of $2.0\times10^{-8}$~\ecs\ (the bolometric correction is less certain in that case).\\
 $^\dag$ Cornelisse et~al. (\cite{Cornelisse02}). This burst was
erroneously dated four days earlier in that paper.\\
 $^\ddag$Jonker et~al. (\cite{Jonker01}). \\
 $^\ast$ Galloway et~al. (\cite{Galloway05}) this paper mentioned 2 more faint
bursts from \bron, but the data do not allow
confirmation as type-I X-ray bursts. \\
 $^\P$These are 14-d averages. \\
 $^\times$ This burst was only partly observed. The observation stopped 18 s after burst onset. \\
\end{table}