\begin{table}%t2
\caption{\label{tbl:werte}Detected IPs with masses from XSPEC fit with the model from \cite{suleimanov05}. The temperature is from a bremsstrahlung fit, and is provided for comparison.}
\par
\small%\centerline
 {
\begin{tabular}{lrlrclcr}
 \hline 
 \hline
%&&&&&&& \\[-8pt]
   Name & $kT$~~~~ & ~~~Mass &  $F_{14-195}$~~~ &  Distance$^A$  & $L_{14-195}$  & \mdot & $\chi^2_{\rm red}$ \\
        & (keV)~~ & ~~~(\msun)  & (10$^{-11}$ erg/cm$^2$/s) & ~~(pc) & (10$^{32}$ erg/s) & (10$^{16}$ g/s) & \\
   \hline 
%&&&&&&& \\[-8pt]
 FO Aqr  & 15.2 $\pm$ 1.6  & 0.61  $\pm$  0.05 & 4.7 $\pm$ 0.5 & 400$^1$ & 9.00 &29.0 &1.4  \\
 XY Ari  & 29.1 $\pm$ 6.2  & 0.96  $\pm$  0.12 & 2.3  $\pm$  0.4 & 270$^2$    &  2.01 &2.8 &1.3  \\
 V405 Aur& 22.1 $\pm$ 4.2  & 0.89  $\pm$  0.13$^C$ & 2.2  $\pm$  0.5 &  -- & -- & &0.5  \\
 MU Cam  & 19.6 $\pm$ 4.7  & 0.74  $\pm$  0.13 & 1.3  $\pm$  0.3 &  -- & -- & &1.7  \\
 V709 Cas& 30.0 $\pm$ 2.5  & 0.96  $\pm$  0.05$^C$ & 7.2  $\pm$  0.6 &  -- & -- & &1.0  \\
 V1025 Cen&10.8 $\pm$ 7.7  & 0.46  $\pm$  0.31 & 0.4  $\pm$  0.3 &  -- & -- & &0.6  \\
 BG CMi   &18.9 $\pm$ 5.5  & 0.67  $\pm$  0.19 & 2.0  $\pm$  0.4 &  700$^3$    & 11.73 &32.3 &0.7  \\
 TV Col   &21.6 $\pm$ 2.4  & 0.78  $\pm$  0.06 & 5.0  $\pm$  0.5 &  386$^4$    &  8.92 & 18.8&0.9  \\
 TX Col   &17.0 $\pm$ 3.2  & 0.67  $\pm$  0.10 & 1.7  $\pm$  0.3 &  550$^5$    &  6.15 & 16.9&0.7  \\
 V2306 Cyg&20.5 $\pm$ 5.7  & 0.77  $\pm$  0.16 & 1.2  $\pm$  0.3 &  -- & -- & &1.0  \\
 DO Dra   &12.0 $\pm$ 2.6  & 0.50  $\pm$  0.11$^C$ & 1.0  $\pm$  0.3 &  155$^6$    &  0.29 &1.3 &0.7  \\
 PQ Gem   &16.8 $\pm$ 2.8  & 0.65  $\pm$  0.09 & 2.5  $\pm$  0.4 &  -- & -- & &1.0  \\
 EX Hya   &19.4 $\pm$ 4.4  & 0.66  $\pm$  0.17 & 2.1  $\pm$  0.5 &  64.5$^7$   &  0.10 & 0.28 & 0.4  \\
 NY Lup   &39.1 $\pm$ 4.3  & 1.09  $\pm$  0.07 & 7.1  $\pm$  0.6 & 690$^8$    & 40.45 & 25.3 &1.1  \\
 V2400 Oph&21.1 $\pm$ 2.8  & 0.81  $\pm$  0.10 & 4.3  $\pm$  0.6 &  -- & -- & &1.0  \\
 GK Per   &26.2 $\pm$ 5.4  & 0.90  $\pm$  0.12$^{B,C}$$\!\!$& 2.8  $\pm$  0.5 &  340$^9$    & 10.24 & 16.2 &0.8  \\
 AO Psc   &13.1 $\pm$ 1.9  & 0.55  $\pm$  0.06 & 2.8  $\pm$  0.4 & 420$^{10}$   & 10.13 &38.6 & 0.7  \\
 V1223 Sgr&17.0 $\pm$ 1.3  & 0.65  $\pm$  0.04 & 8.5  $\pm$  0.8 & 527$^{11}$ & 28.25 & 82.0 &1.0  \\
 V1062 Tau&18.3 $\pm$ 5.8  & 0.72  $\pm$  0.17 & 1.6  $\pm$  0.4 &  500$^{12}$ &  4.79 & 11.6 & 0.4 \\
 RX J2133 &27.1 $\pm$ 2.9  & 0.91  $\pm$  0.06 & 4.6  $\pm$  0.4 &  $>$600$^{13}$   & -- & &0.6  \\
 Swift J0713&21.7 $\pm$ 4.1 & 0.79  $\pm$  0.11 & 2.5  $\pm$  0.4 &  -- & -- & &0.9  \\
 IGR J00234&$\rm 22.8^{+30.0}_{-11.5}$ & 0.85  $\pm$  0.39 & 0.7  $\pm$  0.3 &  -- & -- & &0.8  \\
 IGR J17303&37.1 $\pm$ 4.4 & 1.08 $\pm$ 0.07 & 6.6 $\pm$ 0.6 & -- & -- & &1.1  \\
 \hline 
 \end{tabular}}
\medskip
$^A$ References to the distances: 1. \cite{mchardy87}; 2. \cite{littlefair01};
   3. \cite{berriman87}; 4. \cite{mcarthur01}; 5. \cite{buckley89}; 
   6. \cite{mateo91}; 7. \cite{beuermann03}; 8. \cite{demartino06}; 
   9. \cite{warner87}; 10. \cite{hellier91}; 11.~\cite{beuermann04}; 
  12. \cite{szkody96}; 13 \cite{Bonnet-Bidaud06}. \\
$^B$ All numbers correspond to the measured spectrum during the low-flux period; but see Sect.~3.2. \\
$^C$ The derived mass is likely a lower limit due to the fast rotation of the WD; see Sect.~3.1.
\end{table}