\begin{table}%t2
\caption{\label{table:progs}List of progenitors used in the simulations. $M_{{\rm Fe-Si}}$
  and $M_{{\rm Si-O}}$ are the enclosed masses at composition
  interfaces defined by entropy jumps. With (e) we denote that a shell
  interface is connected with a gradual enrichment of the lighter nucleus,
  i.e.~these cases are Fe--FeSi and Si--SiO interfaces where the mass
  fractions of Si or O grows gradually outwards. The underlined numbers
  indicate an entropy increase of more than $1\kb$ per nucleon
  in case of an Fe--Si interface and an entropy increase of more than
  $2\kb$/by in case of a Si--O interface.}
\small%\centering
\par
\begin{tabular}{llllll}
\hline\hline
Model~& $M_{\rm ZAMS}$ [$\msol$] & Reference   &
        $M_{{\rm Fe-Si}}$ [$\msol$] & $M_{{\rm Si-O}}$ [$\msol$] &
        Notes
      \\
\hline
s1b       & $>$2.26 & Woosley, personal comm.
                                      & 1.34 & 1.38 & model for Type Ib supernova\\
s11.2     & 11.2    & \cite{wooheg02} & 1.24 & \underline{1.30}(e) & from {\tt www.stellarevolution.org} \\
n13       & 13      & \cite{nomhas88} & \underline{1.18} & 1.50 & \\
s15s7b2   & 15      & \cite{woowea95} & 1.28(e) & \underline{1.43}(e) & \\
l15       & 15      & \cite{limstr00} & 1.16(e) & 1.60 & \\
s15a28    & 15      & \cite{heglan01} & 1.42(e) & 1.81 & \\
s20.0     & 20.0    & \cite{wooheg02} & \underline{1.46} & 1.82 & from {\tt www.stellarevolution.org} \\
l25       & 25      & \cite{limstr00} & 1.58 & 1.84(e) & \\
s25a28    & 25      & \cite{heglan01} & 1.62 & \underline{1.98}(e) & \\
\hline 
\end{tabular}
\end{table}