\begin{table}%t4
\caption{\label{tab4}Birth rates of hot subdwarfs from the stable RLOF channel
of intermediate-mass binaries (our model) and other channels (Han et~al. \cite{Han03}) (in 10$^{-3}$~yr$^{-1}$).}
 %%\centerline

{\small
\begin{tabular}{lccccccc}
 \hline
 \hline
 $Z$  &  $q_{\rm crit}$  &  $\nu_{\rm IMR}$  & $\nu_{\rm FR}$
 & $\nu_{\rm FCE}$ & $\nu_{\rm SR}$ & $\nu_{\rm SCE}$ & $\nu_{\rm M}$\\
\hline
0.02   &  1.5  &  4.18  &   29.89& 8.41 &0.00&8.38&17.22\\
0.02  &  1.2  &  4.14  &   22.25 &10.71 &0.00&5.43&7.99\\
\hline
\end{tabular}}
\par
\medskip
$Z$ = metallicity; $q_{\rm crit}$ = the critical mass ratio for
the first stable RLOF on the FGB; $\nu_{\rm IMR}$ = Galactic birth rates
of hot subdwarfs from the stable RLOF channel of intermediate-mass
binaries; $\nu_{\rm FR}$ = the first stable RLOF channel; $\nu_{\rm FCE}$ = the
first CE ejection channel; $\nu_{\rm SR}$ = the second RLOF channel;
$\nu_{\rm SCE}$ = the second CE ejection channel; $\nu_{\rm M}$ = the helium WD
merger channel.
\end{table}