\begin{table}%t1
\caption{Parallaxes and proper motions for the CNS candidates in the Torino
Program. Columns are: target name, positions at J2000, number of reference stars,
number of frames, proper motions, absolute parallax, correction applied to the
relative parallax to obtain an absolute parallax, the interval of time for
which we have observations, apparent magnitude {in the $I$~band from
in-house data unless discussed in Sect.~2,} the CNS parallax
along with the source. \label{results}}
%\centerline
 {\begin{tabular}{lrrrrrrrrrrr}%lllllllll}
\hline \hline   
 Name    & RA ~~~ & Dec ~~~     &$N_*, N_{\rm f}$& $\mu_{\alpha}$  & $\mu_{\delta}$  &  $\pi$       & COR    &$\Delta T$&  $I$~~   & $\pi_{\rm CNS}^{\rm source}$   \\
         & h:m:s ~~ & d:\arcmin:\arcsec\  &          &   mas/yr        &     mas/yr      & mas             & mas    &years   &       &  mas                    \\
\hline  \\	  
\object{LHS~1050} & 0:15:47&+13:33:08 & 8, 81& 606.3 $\pm$ 1.5 & 336.9 $\pm$ 1.5 &  89.0 $\pm$ 3.5 & 1.84 & 5.07 & 10.04 & 86.6 $\pm$ 13.4$^Y$ \\% lhs1050 
\object{GD 806   } & 1:12:28&--01:51:19  & 11, 64&  14.9 $\pm$ 1.4 & --73.7 $\pm$ 1.4 &  8.4 $\pm$ 3.3 & 2.04 & 5.41 & 13.55 & 99.0 $\pm$ 11.0$^w$ \\% n1119  
\object{GJ 3140  } & 2:10:14&+11:32:11  & 8, 170& --20.0 $\pm$ 0.6 &  3.6 $\pm$ 0.8 &  5.3 $\pm$ 1.8 & 2.56 & 5.41 & 9.85 & 90.0 $\pm$ 30.0$^p$ \\% n1211  
\object{LP 475-70} & 4:25:53&+12:11:47  & 20, 67& --102.1 $\pm$ 1.1 & --232.8 $\pm$ 1.1 &  59.4 $\pm$ 2.8 & 1.35 & 5.31 & 14.77 & 81.0 $\pm$ 11.0$^w$ \\% n1411  
\object{LHS~1675} & 4:31:07&--05:20:26 &11, 39& --175.0$\pm$ 2.1 & --507.8 $\pm$ 2.7 &  28.5 $\pm$ 3.6 & 1.83 & 5.32 & 11.00 & 87.0 $\pm$ 10.2$^H$ \\% lhs1675 
Cl* Mel.$^a$ & 4:35:00&+17:33:40&17, 31& 3.4 $\pm$ 1.8 & --18.0 $\pm$ 1.5 & 2.7 $\pm$ 3.8 & 1.62 & 5.24 & 12.55 & 94.0 $\pm$ 17.0$^p$ \\% n1440  
\object{LP 60-179} & 9:02:51&+68: 3:18  &13, 48& 182.9 $\pm$ 1.4 & 345.3 $\pm$ 2.0 &  85.3 $\pm$ 3.8 & 2.47 & 5.25 & 9.75 & 98.0 $\pm$ 10.6$^Y$ \\% n1754  
\object{LHS~295 } &10:52:04&+13:59:51 &11, 71&--1119.0 $\pm$ 1.1 & 206.8 $\pm$ 1.6 &  80.2 $\pm$ 2.7 & 1.90 & 5.37 & 9.95 & 83.9 $\pm$ 25.7$^Y$ \\% lhs295 
\object{GJ 3667  } &11:29:19&+18:16:35  &10, 55&  6.2 $\pm$ 1.2 &  6.5 $\pm$ 1.1 &  1.3 $\pm$ 2.9 & 2.21 & 6.09 & 13.23 & 114.0 $\pm$ 13.0$^w$ \\% n1965  
\object{LHS~2472} &11:54:08&+09:48:56 & 5, 38&  89.6 $\pm$ 2.0 & --796.7 $\pm$ 1.9 &  82.7 $\pm$ 4.4 & 2.06 & 5.13 & 9.92 & 96.1 $\pm$ 19.7$^Y$ \\% lhs2472 
\object{GJ 1167a } &13:09:36&+28:59:10  & 5, 15& --337.5 $\pm$ 2.4 & --203.1 $\pm$ 2.3 &  83.1 $\pm$ 6.3 & 2.04 & 4.22 & 11.14 & 86.0 $\pm$ 12.5$^H$ \\% GJ 1167a 
\object{LHS~369 } &14:20:09&--09:36:35 & 8, 32& --607.0 $\pm$ 1.2 & --826.8 $\pm$ 1.9 &  68.1 $\pm$ 3.8 & 1.85 & 6.15 & 10.25 & 91.1 $\pm$ 15.0$^Y$ \\% lhs369 
\object{LHS~3872} &22:54:45&--05:28:37 & 6, 32& 610.1 $\pm$ 1.6 & 354.4 $\pm$ 2.1 &  40.4 $\pm$ 4.9 & 2.18 & 5.09 & 11.21 & 94.0 $\pm$ 23.0$^H$ \\% lhs3872 
\hline 
\end{tabular}}
\par
\smallskip
Source: $Y=\rm Yale$ Parallax catalog, $w$~=~photometric parallax assuming white
dwarf {with the \citet{mcc99} calibration,} $p$~=~photometric parallax
assuming main sequence star, $H$~=~Parallax from Heintz (1994),  $a$~=~Cl* Mel.
is \object{Cl* Melotte 25 LH 27}.
\end{table}