\begin{table}%t4
\caption{\label{ssnovae}Details on novae with detected supersoft X-ray emission (top 5~lines),
 N~LMC~2000, and recent recurrent novae (RN; last three lines). }
%\centerline
{
\begin{tabular}{lcccccccll}
  \hline\hline
  \noalign{\smallskip}
    Nova Name &   $t_2$ & $t_3$ & $M_{\rm WD}$ & log $\Delta M_{\rm ej}$ & 
       $V_{\rm expa}$$^{(c)}$ & $P_{\rm orb}$  &  log $\Delta M_{\rm ign}$
         &  Limits on supersoft  phase & Refs. \\
         & (days) & (days)& (\msun)$^{(a)}$ & $^{(b)}$  & (km~s$^{-1}$)& (days) && & $^{(d)}$ \\
 \noalign{\smallskip}
 \hline
 \noalign{\smallskip}
   GQ Mus      & 23.0  &  45  & 0.87 & --3.98 & 800 & 0.0593 & --3.4 & 10~yrs 
   & 1--3 \\
   N Cyg 1992  & 16.0  &  42  & 0.90 & --4.02  & 2000  & 0.0812 & --3.8 & turnoff at days 32--$38\times t_2$ & 4--6 \\
   N LMC 1995  &  12$^{(e)}$ & 16$^{(e)}$ & 1.23 & --4.22 & ~~900 & -- & & $>$6~yrs and continuing & 7--9 \\
   V382 Vel    &  4.5  &   9  & 1.17 & --4.18 & 2700 & 0.1461 & --4.8 &at $44\times t_2$; 
       none at $60\times t_2$ & 10 \\
   V1494 Aql   &  ~~~6.6$^{(f)}$ & ~~~16$^{(f)}$  & 1.09 &  --4.13 & 2800 &  0.1346 &
     --4.6 &  none \lax $28\times t_2$, but at 38--$45\times t_2$  & 11, 12 \\
 \noalign{\medskip}
   N LMC 2000  &  9.0  &  22  & 1.02 & --4.09  & 2200 & -- & & less than $5.5\times t_2$ & \\
 \noalign{\medskip}
   U Sco (RN)  & 5.0 & 7 & 1.20 &  ~~~--5.99$^{(g)}$ &4500 & 1.230 & --5.3 & at $4\times t_2$ & 13 \\
   IM Nor (RN) & ~~~20.5$^{(b)}$ &  ~~~47$^{(b)}$  & 0.85 & --3.99   & 1150 & -- & & 
      none at $1.1\times t_2$ & 12, 14 \\
   CI Aql (RN) & 30.0 &  36  & 0.94 & --3.95  &2400  & 0.6184 & --5.2 & less than $14\times t_2$ & 15, 16 \\
\hline
\end{tabular}}
\smallskip
$^{(a)}$ According to the $t_3-M_{\rm WD}$ relation (Livio \cite{Livio}). \\ 
          $^{(b)}$ 	According to  
              log $\Delta M_{\rm ej}  = 0.274\times  \log t_2 - 4.355$ 
              (Della Valle \etal\ \cite{Della2002}).\\
          $^{(c)}$ Usually derived for the H$\alpha$ line. For V382 Vel, lacking
               an estimate based on H$\alpha$, we used the number given for 
               UV lines and divide by a factor 2 (Shore \cite{Shore2002}). \\
          $^{(d)}$ References: 
             (1) \"Ogelman \etal\ (\cite{gelman}),
             (2) Pequignot \etal\ (\cite{Pequigno}),
             (3) Shanley \etal\ (\cite{Shanley}),
             (4) Krautter \etal\ (\cite{Krautter}),
             (5) Chochol \etal\ (\cite{hochol}),
             (6)~Balman \etal\ (\cite{alman}),
             (7) Della Valle \etal\ (\cite{Della1995e}),
             (8) Orio \& Greiner (\cite{Orio1999}), 
             (9) Orio \etal\ (1993),
            (10) Orio \etal\ (\cite{Orio2002}),
            (11) Venturini \etal\ (\cite{Venturini}),
            (12) Starrfield  \etal\ (\cite{Starrfield2002}),
            (13) Iijima (\cite{Iijima}),
            (14) Duerbeck \etal\ (\cite{Duerbeck2002}),
            (15) Greiner \& Di~Stefano (\cite{Greiner}),
            (16) Kiss \etal\ (\cite{Kiss}). \\
           $^{(d)}$ Determined here from the VSNET light curves. \\
           $^{(g)}$ Instead of the prediction we used the value as measured
               by Della Valle \etal\ (\cite{Della2002}).
                         \end{table}