\begin{table}%T3
\caption{Characteristic parameters of the 1D~models for the phases of
  collapse, prompt shock propagation, and neutrino burst. $t_{\rm coll}$
  is the time between the moment when the collapsing core reaches a
  central density of~$10^{11}\gcm$ and the moment of shock creation
  (which is nearly identical with the time of core bounce),
  i.e.~the time when the entropy behind the shock first
  reaches a value of~$3\kb$/by. The shock creation radius~$r_{\rm sc}$ and enclosed mass~$M_{\rm sc}$ are defined by the
  radial position where this happens.
  The energy loss $E_{\rm coll}^{\nu,{\rm loss}}$
  via neutrinos during the collapse phase is evaluated by integrating
  the total neutrino luminosity (for an observer at rest at
  $r=400$~km) over time from the moment when the core reaches
  $\rho_{\rm c} = 10^{11}\gcm$ until the moment when the dip in the
  $\nue$ luminosity is produced around 2.5~ms after shock
  formation. We call the time when the velocities behind the shock
  drop below $10^7~\cms$ the end of the prompt shock propagation
  phase. This time, $t_{\rm pse}$, is measured relative to the moment
  of shock creation. At the end of the prompt shock propagation phase,
  the shock is at radius $r_{\rm pse}$ and its enclosed mass is
  $M_{\rm pse}$. The time of the $\nue$ burst,
  $t_{\nue-{\rm burst}}$, is defined as the post-bounce time when
  the $\nue$ luminosity maximum is produced at the shock, which then
  is located at the radius $r_{\nue-{\rm burst}}$ and mass
  $M_{\nue-{\rm burst}}$. Finally, the energy emitted during the
  prompt $\nue$ burst is defined as the time-integrated $\nue$
  luminosity for the FWHM of the burst, $E_{\rm burst}^\nu$,
  evaluated at 400~km for an observer at rest.
%
}
\small%\centerline
{
\begin{tabular}{llllllllllll}
\hline\hline\noalign{\smallskip}
Model~&
    $t_{\rm coll}$ & $r_{\rm sc }$ & $M_{\rm sc }$ &
    $E_{\rm coll}^{\nu, {\rm loss}}$ &
    $t_{\rm pse }$ & $r_{\rm pse}$ & $M_{\rm pse}$ &
    $t_{\nue-{\rm burst}}$ & $r_{\nue-{\rm burst}}$ &
    $M_{\nue-{\rm burst}}$ & $E_{\rm burst}^\nu$ \\
 & [ms] & [km] & [$\msol$] & [$10^{51}~{\rm erg}$]
 & [ms] & [km] & [$\msol$]
 & [ms] & [km] & [$\msol$] & [$10^{51}~{\rm erg}$] \\
\hline
s1b      & 23.9 & 10.7 &0.49 &1.00 &0.87 &32 &0.78 &3.8 &64 &1.00 &1.48 \\
s11.2    & 25.2 & 10.7 &0.50 &1.00 &0.87 &32 &0.78 &3.7 &63 &1.00 &1.38 \\
n13      & 28.9 & 10.7 &0.50 &0.96 &0.88 &32 &0.78 &3.7 &61 &0.98 &1.29 \\
s15s7b2~$^\dagger$
         & 23.9 & 10.7 &0.49 &1.01 &0.91 &32 &0.78 &3.8 &64 &1.00 &1.47 \\
l15      & 20.9 & 10.6 &0.50 &1.04 &1.03 &35 &0.82 &4.1 &68 &1.04 &1.74 \\
s15a28   & 21.6 & 10.7 &0.49 &1.03 &0.95 &33 &0.79 &4.0 &66 &1.02 &1.60 \\
s20.0    & 22.7 & 10.6 &0.49 &1.03 &0.91 &32 &0.79 &3.8 &64 &1.01 &1.50 \\
l25      & 20.0 & 10.7 &0.49 &1.06 &1.15 &37 &0.83 &4.1 &68 &1.03 &1.82 \\
s25a28   & 19.8 & 10.6 &0.48 &1.06 &1.00 &34 &0.79 &4.1 &68 &1.03 &1.93 \\
\hline 
\end{tabular}}
\smallskip
 $^\dagger$ This model is identical with Model~s15Gio\_1d.b in
\cite{burram06:I} except for a slightly different, improved implementation of
the relativistic corrections to the gravitational potential. This difference
causes only small changes in
the neutrino luminosities of a few percent, but otherwise has no
visible consequences.
\label{table:evol}
\end{table}