\begin{table}%t1
\caption{\label{tab1}Comparison of white dwarf mass determinations from
different methods.} 
\small%\centerline
{
\begin{tabular}{lcccccc}
\hline\hline
Name& $T_{\rm eff }$ &     $\log\ g$ &  $M_{\rm spec}$&      $M_{\rm other}$&    Notes   & Ref.\\
&(K)&&($M_{\odot}$)&($M_{\odot}$)&&\\
 \hline
Sirius B    &   24~700  $\pm$  300 &   8.61   $\pm$  0.04    &   0.998  $\pm$ 0.024   &   1.003  $\pm$  0.016   &   1   &   1,3 \\
40 Eri B    &   16~700   $\pm$ 300 &   7.77    $\pm$ 0.01    &   0.493   $\pm$ 0.006   &   0.501   $\pm$ 0.011   &   1   &   1,4 \\
Sirius B    &   25~193  $\pm$  37 &   8.566   $\pm$  0.01    &   0.978  $\pm$ 0.005   & 1.02  $\pm$  0.02   &   2   &   14 \\
GD279   &   13~500   $\pm$ 200 &   7.83    $\pm$ 0.03    &   0.514   $\pm$ 0.016   &   0.44    $\pm$ 0.02    &   2   &   1,12    \\
Feige 22    &   19~100   $\pm$ 400 &   7.78    $\pm$ 0.04    &   0.505   $\pm$ 0.020   &   0.41    $\pm$ 0.03    &   2   &   1,12    \\
EG21    &   16~200   $\pm$ 300 &   8.06    $\pm$ 0.05    &   0.649   $\pm$ 0.030   &   0.5 $\pm$ 0.02    &   2   &   1,12    \\
EG50    &   21~000   $\pm$ 300 &   8.10    $\pm$ 0.05    &   0.682   $\pm$ 0.030   &   0.58    $\pm$ 0.05    &   2   &   1,12    \\
GD140   &   21~700   $\pm$ 300 &   8.48   $\pm$  0.05    &   0.917  $\pm$  0.031   &   0.79  $\pm$   0.02    &   2   &   1,12    \\
G226-29 &   12~000   $\pm$ 200 &   8.29   $\pm$  0.03    &   0.784   $\pm$ 0.019   &   0.75   $\pm$  0.03    &   2   &   1,12    \\
WD2007-303  &   15~200   $\pm$ 700 &   7.86    $\pm$ 0.05    &   0.534 $\pm$   0.028   &   0.44   $\pm$  0.05    &   2   &   1,12    \\
Wolf1346    &   20~000   $\pm$ 300 &   7.83    $\pm$ 0.05    &   0.532   $\pm$ 0.026   &   0.44    $\pm$ 0.01    &   2   &   1,12    \\
G93-48  &   18~300   $\pm$ 300 &   8.02  $\pm$   0.05    &   0.630  $\pm$  0.029   &   0.75   $\pm$  0.06    &   2   &   1,12    \\
L711-10 &   19~900  $\pm$  400 &   7.93   $\pm$  0.05     &  0.584  $\pm$  0.028   &   0.54   $\pm$  0.04    &   2   &   1,12    \\
CD-38 10~980 &   24~000  $\pm$  200 &   7.92  $\pm$   0.04    &   0.588 $\pm$   0.021   &   0.74   $\pm$  0.04    &   2   &   1,12    \\
Wolf 485A   &   14~100  $\pm$  400 &   7.93  $\pm$   0.05    &   0.570  $\pm$  0.018   &   0.59   $\pm$  0.04    &   2   &   1,12    \\
G154-B5B    &   14~000  $\pm$  400 &   7.71   $\pm$  0.05    &   0.457  $\pm$  0.015   &   0.53    $\pm$ 0.05    &   2   &   1,12    \\
G181-B5B    &   13~600  $\pm$  500 &   7.79  $\pm$  0.05    &   0.495  $\pm$  0.016   &   0.46    $\pm$ 0.08    &   2   &   1,12    \\
G238-44 &   20~200  $\pm$  400 &   7.90   $\pm$  0.05    &   0.568  $\pm$  0.028   &   0.42   $\pm$  0.01    &   2   &   1,12    \\
LB 1497 &   31~660   $\pm$ 350 &   8.78    $\pm$ 0.049   &   1.097   $\pm$ 0.025   &   1.025  $\pm$  0.043   &   3,5 &   2,6,12  \\
HZ 4    &   14~770  $\pm$  350 &   8.16    $\pm$ 0.049   &   0.707   $\pm$ 0.032   &   0.632   $\pm$ 0.042   &   3,5 &   2,7,12  \\
GH 7-112    &   15~190  $\pm$  350 &   8.3 $\pm$ 0.049   &   0.795   $\pm$ 0.031   &   0.783   $\pm$ 0.039   &   3,5 &   2,7,12  \\
40 Eri B    &   16~570  $\pm$  350 &   7.86   $\pm$  0.049   &   0.538   $\pm$ 0.026   &   0.52   $\pm$  0.4 &   3,5 &   2,8,12  \\
%40 Eri B    &   16~570   $\pm$ 350 &   7.86   $\pm$  0.049   &  0.538 $\pm$   0.026   &   0.554  $\pm$  0.019   &   3,5 &   2,9,12  \\
GH 7-191    &   19~570   $\pm$ 350 &   8.09   $\pm$  0.049   &   0.674 $\pm$   0.030   &   0.669  $\pm$  0.036   &   3,5 &   2,7,12  \\
GH 7-233    &   24~420  $\pm$  350 &   8.11   $\pm$  0.049   &   0.695  $\pm$  0.029   &   0.617  $\pm$  0.028   &   3,5 &   2,7,12  \\
HZ 7    &   21~340  $\pm$  350 &   8.04   $\pm$  0.049   &   0.648  $\pm$ 0.029   &   0.665  $\pm$  0.077   &   3,5 &   2,7,12  \\
HZ 14   &   27~390  $\pm$  350 &   8.07   $\pm$  0.049   &   0.678  $\pm$  0.028   &   0.51   $\pm$  0.086   &   3,5 &   2,7,12  \\
G191-B2B    &   64~100  $\pm$  350 &   7.69  $\pm$  0.049   &   0.580  $\pm$  0.010   &   0.538  $\pm$  0.043   &   3,5 &   2,10,12 \\
G163-50 &   15~070   $\pm$ 350 &   7.83   $\pm$  0.049   &   0.519   $\pm$ 0.026   &   0.465  $\pm$  0.046   &   3,5 &   2,5,12  \\
%G163-50 &   15~070  $\pm$  350 &   7.83   $\pm$  0.049   &   0.519  $\pm$  0.026   &   0.459   $\pm$ 0.043   &   3,5 &   2,8,12  \\
G148-7  &   15~480  $\pm$  350 &   7.97   $\pm$  0.049   &   0.595  $\pm$  0.028   &   0.558  $\pm$  0.038   &   3,5 &   2,8,12  \\
Wolf 485A   &   14~100  $\pm$  350 &   7.93   $\pm$  0.049   &   0.570   $\pm$ 0.028   &   0.529  $\pm$ 0.042   &   3,5 &   2,5,12  \\
%Wolf 485A   &   14~100   $\pm$ 350 &   7.93   $\pm$  0.049   &   0.570  $\pm$  0.028   &   0.529  $\pm$  0.039   &   3,5 &   2,8,12  \\
L762-21 &   18~580  $\pm$  350 &   8.32   $\pm$  0.049   &   0.813  $\pm$  0.032   &   0.808  $\pm$  0.099   &   3,5 &   2,5,12  \\
%G19-20  &   13~620   $\pm$ 350 &   7.79  $\pm$   0.049   &   0.495  $\pm$  0.025   &   0.466  $\pm$  0.043   &   3,5 &   2,8,12  \\
G154-B5B    &   13~950   $\pm$    350 &   7.71     $\pm$   0.049   &   0.457    $\pm$   0.024   &   0.524     $\pm$  0.04    &   3,5 &   2,8,12  \\
G142-B2A    &   14~040     $\pm$  350 &   7.84     $\pm$   0.049   &   0.521     $\pm$  0.026   &   0.561     $\pm$  0.037   &   3,5 &   2,8,12  \\
L587-77A    &   9330     $\pm$   350 &   7.87     $\pm$   0.049   &   0.524     $\pm$  0.028   &   0.657     $\pm$  0.035   &   3,4,5   &   2,5,12  \\
G86-B1B &   9140     $\pm$   350 &   8.3   $\pm$  0.049   &   0.785    $\pm$  0.032   &   0.454     $\pm$  0.118   &   3,4,5   &   2,11,12 \\
G111-71 &   7710      $\pm$  350 &   8.15     $\pm$   0.049   &   0.685    $\pm$   0.032   &   0.632     $\pm$  0.125   &   3,4,5   &   2,11,12 \\
G116-16 &   8750     $\pm$   350 &   8.29     $\pm$   0.049   &   0.778    $\pm$   0.032   &   1.009     $\pm$  0.06    &   3,4,5   &   2,11,12 \\
G121-22 &   10~260     $\pm$  350 &   6.12      $\pm$  0.049   &   0.651    $\pm$   0.035   &   1.084     $\pm$  0.023   &   3,4,5   &   2,11,12 \\
G61-17  &   11~000   $\pm$    350 &   8.04    $\pm$   0.049   &   0.626   $\pm$   0.030   &   0.552   $\pm$  0.038   &   3,4,5   &   2,11,12 \\
L619-50 &   10~080  $\pm$   350 &   8.17   $\pm$  0.049   &   0.703 $\pm$   0.032   &   0.502  $\pm$   0.069   &   3,4,5   &   2,5,12  \\
LP696-4 &   10~470   $\pm$  350 &   8.11   $\pm$  0.049   &   0.667  $\pm$  0.031   &   0.44   $\pm$   0.12    &   3,4,5   &   2,11,12 \\
LP25-436    &   8440    $\pm$   350 &   8.52   $\pm$   0.049   &   0.926  $\pm$   0.032   &   0.644   $\pm$   0.056   &   3,4,5   &   2,11,12 \\
G156-64 &   7160    $\pm$   350 &   8.43    $\pm$   0.049   &   0.866   $\pm$   0.032   &   0.548   $\pm$   0.052   &   3,4,5   &   2,11,12 \\
G216-B24B   &   9860    $\pm$    350 &   8.2   $\pm$  0.049   &   0.722    $\pm$   0.032   &   0.832     $\pm$  0.047   &   3,4,5   &   2,11,12 \\
L557-71 &   8780     $\pm$   350 &   8.29     $\pm$   0.049   &
0.778    $\pm$ 0.032   &   0.549    $\pm$   0.038   &   3,4,5   &
2,11,12\\
G19-20  &   13~620  $\pm$  350 &   7.79   $\pm$  0.049   &   0.495   $\pm$ 0.025   &   0.489   $\pm$ 0.084   &   3,5 &   2,5,12\\
\hline
\smallskip
\end{tabular}}
\smallskip
\emph{Note}: $M_{\rm spec}$ refers to spectroscopic mass derived with the
evolutionary model of Panei (\cite{Panei2000}) from the spectral
parameters($T_{\rm eff}$ and $\log g$) and~$M_{\rm other}$~refers to the
mass derived from 1: orbital parameters, 2:
parallaxes and $\log\ g$, and 3: gravitational redshift. Note~4 denotes low temperature
WDs ($T_{\rm eff} <12~000$~K) and~5~denotes that the individual errors of $T_{\rm eff}$
and $\log\ g$ of each WD~is not available, so we assumed the errors of
$T_{\rm eff}$ and $\log\ g$ being the mean errors of the sample the WD
belongs to.\\
\emph{References}: (1) Provencal et~al. (\cite{Provencal1998}); (2) Bergeron et~al. (\cite{Bergeron1995a}); 
(3) Gatewood \& Gatewood (\cite{Gatewood1978}); (4) Shipman et~al. (\cite{Shipman1997}); (5) Koester 
(\cite{Koester1987}) (6) Wegner et~al. (\cite{Wegner1991e}) (7) Wegner et~al.
(\cite{Wegner1989e}); (8) Wegner \& Reid (\cite{Wegner1987}); (9) Koester \& Weidemann (\cite{Koester1991}); (10)
Reid \& Wegner (1988); (11) Wegner \& Reid (\cite{Wegner1991}); (12) BSL and
Bragaglia et~al. (\cite{Bragaglia1995}); (13) McCook \& Sion (\cite{McCook1999}); (14) Barstow et~al. (\cite{Barstow2005}).
\end{table}