\begin{table}%T3
\caption{Characteristics of our program stars and their nebulae. The last column
gives the references for stellar parameters and PN shape. The main-sequence
(MS) mass is inferred from Weidemann's (2000)  initial-final mass relation. The MS
radius is estimated using \cite{Allen:76}. The future white dwarf (WD) radius is
estimated from the mass-radius relation of \cite{Wood:94}. EGB~5 is not on a post-AGB
evolutionary track as a result of close-binary evolution \citep{Karl-etal:03}.
\label{tab_targets}}
%\begin{center}
{
\begin{tabular}{l r r r r r r r r r}
\hline
\hline
%\noalign{\smallskip}
Object  & \Teff & \logg & mass      & MS mass   & radius    & MS radius & WD radius &PN shape& Ref.\\
&  [K]  & (cgs) &[$M_\odot$]&[$M_\odot$]&[$R_\odot$]&[$R_\odot$]&[$R_\odot$]& &        \\
%\noalign{\smallskip}
\hline
%\noalign{\smallskip}
 NGC~1360 &  97~000 & 5.3   & 0.65      & 2.7       & 0.30      & 2.3  &  0.011    & elliptical & A, B\\
 Abell 36  & 113~000 & 5.6   & 0.60      & 2.7       & 0.21      & 2.3  &  0.012    & irregular & A, B\\
 LSS~1362 & 114~000 & 5.7   & 0.60      & 2.0       & 0.18      & 1.6  &  0.012    & ellip.ring & A, C\\
 EGB 5     &  34~000 & 5.8\rlap{5}   &   0.48\rlap{$^*$}    &        &   0.14   &         &       & elliptical & D\\
% \noalign{\smallskip}
 \hline
 \end{tabular}}
   References:
A: \cite{Traulsen-etal:05},
B: \cite{Phillips:03},
C: \cite{Heber-etal:88},
D: \cite{Lisker-etal:04}.\\
$^*$ Canonical mass of a hot subdwarf is assumed.
\end{table}