\begin{table}%t2
\caption{\label{t1}Best fit model parameters and inferred physical
system parameters. Here $C_{F}$ is the partial covering
coefficient, $F_{3-100}$ the observed X-ray flux in the 3--100~keV
band, $F_{0.1-100}$ the unabsorbed X-ray flux in the 0.1--100~keV
band, both in 10$^{-11}$~erg~cm$^{-2}$~s$^{-1}$ units. The
distances for V405 Aur, V709 Cas, PQ Gem and V2400 Oph are assumed.}
%\centerline
{\begin{tabular}{llllllllll}
\hline\hline
Name & $M_{\rm wd}$, & $C_{F}$ & $N_{\rm H}$, & $F_{3-100}$ & $F_{0.1-
100}$ & $\dot M$ & $L_{\rm x}$, 10$^{33}$ & $d$ & $\chi^2$ (d.o.f.)\\
    &  $M_\odot$  &       & $10^{22}$~cm$^{-2}$&& & 10$^{16}$ g
s$^{-1}$ & erg s$^{-1}$ & pc &\\
\hline
V1223 Sgr & $0.95\pm0.05$ & 1.0$^a$ & $3.7\pm1$ &  4.2 &7.3 & 12.6
& 24.3 &
527$^1$ & 105.4(63)\\
& & $0.57\pm0.05$ &  $28\pm3$&    & &\\
FO Aqr & $0.60\pm 0.05$&$0.9\pm0.1$&
$36\pm4$    & 1.5&4.9 & 10.2 &9.4 & 400$^2$ & 62.1(65)\\
EX Hya & $0.50 \pm 0.05$& 1.0
&  $0.6\pm1.0$  &1.5& 3.4 & 0.25 & 0.17 & 64.5$^3$ & 85.3(65) \\
AO Psc & $0.65\pm0.05$&$0.95\pm0.1$&  $10\pm5$      &  1.3 &2.5
&4.7 & 4.9 & 420$^4$ & 55.8(65)  \\
TVCol & $0.84\pm0.06$ & $0.81\pm0.3$ &  $21\pm5$ &  1.7  &3.5 &
3.4 & 5.7
&368$^5$ & 63.4(65) \\
GK Per & $0.59\pm0.05$& 1.0$^a$ & $20\pm2$& 12.5& 88.6 & 81.5
&156 & 340$^6$ & 110.5(63)\\
&               &$0.75\pm0.05$ & $125\pm10$&\\
V709 Cas &
$0.90\pm0.10$ &$0.5\pm 0.1$&$29\pm5$&2.3&3.7& 5.76 & 11.1 &
(500) & 56.3(65)\\
PQ Gem &
$0.65\pm 0.2$ & 1.0      &  $5\pm1$    &  0.80&1.3 & 3.7 &3.9 &
(500) & 38.7(65) \\
V2400 Oph& $0.59\pm0.05$ &$0.4\pm0.1$ &$29\pm10$&2.43&5.6 & 18.7
&16.75 &
(500) & 78.5(65)\\
BG CMi   & $0.85\pm0.12$ &$0.70\pm0.05$ &$25\pm6$&  0.77& 1.54
&5.3
& 9.0 & 700$^7$ & 57.4(65) \\
V405 Aur & $0.90\pm0.10$& $0.6\pm0.1$&$39\pm3$& 0.9 &1.7&
2.65 & 5.09 & (500) & 51.6(65)  \\
V1062 Tau & $1.00\pm0.20$& $0.6\pm0.1$ & $21\pm7$&
1.1&1.8 & 2.2 & 5.4& 500$^8$ & 45.6(65)  \\
DO Dra   & $0.75 \pm 0.05$ & $0.4\pm 0.1$
&  $20\pm5$ &  7.8 &14.4 &3.1 & 4.1 & 155$^9$ & 69.7(65)   \\
TX Col   & $0.70\pm0.30$ &
$<$0.4 &  $<$60   &  0.32& 0.58 & 1.8 & 2.1 & 550$^{10}$ & 52.6(65)   \\
\hline  
\end{tabular}}
\par
\smallskip
$^a$ -- For the systems V1223 Sgr and GK Per which have very
high mass accretion rates we used two absorbers.
\par
{\it References to distance estimates:} 1. Beuermann et~al. (\cite{Beu}); 2. 
McHardy et~al. (\cite{McH}); 3. Beuermann et~al.
(\cite{Beu2}); 4. Hellier et~al.  (\cite{HCM}); 5. McArthur
et~al. (\cite{McA}); 6. Warner (\cite{W87}); 7. Berriman (\cite{Be});
8. Szkody \& Silber (\cite{SS}); 9. Mateo et~al. 
(\cite{MSG}); 10.  Buckley \& Tuohy (\cite{BT}).
\end{table}