\begin{table}%t1
\caption{\label{tab:sample}Sample of BD companions to MS stars observed with {\em Chandra} ACIS-S. 
The left hand side of the table represents a summary of stellar parameters. The distances
are from {\em Hipparcos}, references for the other parameters are given in brackets. 
On the right hand side we list X-ray properties derived from the {\em Chandra} data: 
X-ray luminosity, ratio of X-ray to bolometric luminosity attributing all X-ray emission
to either of the components for unresolved binaries, and median photon energy. The labels~"A'', "Q'', and~"F''~denote average, quiescent, and flare luminosities.} 
%\centerline
{
\begin{tabular}{llrrrrrrrl|crrr}
 \hline\hline
\multicolumn{10}{c}{} & \multicolumn{2}{|c}{[0.5$-$8~keV]} \\
Name            & \multicolumn{1}{c}{Sep}              & \multicolumn{1}{c}{PA}      & Dist                     &  SpT  & \multicolumn{1}{c}{$M$}               & \multicolumn{1}{c}{$T_{\rm eff}$} & \multicolumn{1}{c}{Age} & \multicolumn{1}{c}{$\log{\frac{L_{\rm bol}}{L_\odot}}$} & Ref. & & $\log{L_{\rm x}}$ & $\log{\frac{L_{\rm x}}{L_{\rm bol}}}$ & $\langle E_{\rm ph} \rangle$ \\
                & \multicolumn{1}{c}{[$^{\prime\prime}$]} & \multicolumn{1}{c}{[$^\circ$]} & \multicolumn{1}{c}{[pc]} &       & \multicolumn{1}{c}{[${M_\odot}$]} & [K]                               & [Gyr]                  &                                                         &      & & [erg/s]           &                                       &                              \\
                 \hline
HR~7329~B         &  $4.097$ & $166.9$ & $47.7$  & M~7.5  & $0.020{-}0.045$ & $2600$ & $0.012$     & $-2.59$ & (1,2)  & A & $27.2$   & $-3.8$   & $0.87$ \\
Gl~569~Bab        &  $4.89$  &  $30.0$ &  $9.8$  &       &               &        & $0.2{-}0.4$   &         & (3)    & A & $26.8$   &          & $0.85$ \\
                    &          &         &         &       &               &        &             &         &        & Q & $25.8$   &          & $0.67$ \\
                    &          &         &         &       &               &        &             &         &        & F & $27.5$   &          & $0.87$ \\
\hspace*{1cm} Ba    &          &         &         & M~8.5  & $0.055{-}0.087$ & $2450$ &             & $-3.35$ & (4)    & A &          & $-3.2$   &        \\
\hspace*{1cm} Bb    &          &         &         & M~9    & $0.034{-}0.070$ & $2450$ &             & $-3.58$ & (4)    & A &          & $-3.4$   &        \\
HD~130948~BC       &  $2.64$  & $104.5$ & $17.9$  &       &               &        & $0.3{-}0.8$  &         & (5)    & A & $<$$25.6$  &          & $-$    \\
\hspace*{1cm} B$^*$  &          &         &         & L4    & $0.040{-}0.065$ & $1900$ &            & $-3.81$ & (5,6)  & A &          & $<$$-4.2$  &        \\
\hspace*{1cm} C$^*$  &          &         &         & L4    & $0.040{-}0.065$ & $1900$ &            & $-3.93$ & (5,6)  & A &         & $<$$-4.1$  &        \\
\hline
\end{tabular}}
\smallskip
 References: (1)   \citet{Guenther01.1}, (2)   \citet{Lowrance00.1}, (3)   \citet{Lane01.1}, (4)   \citet{Zapatero04.1}.  \\
 (5)   \citet{Potter02.1}, (6)   \citet{Goto02.1};  \\
 $^*$ Bolometric luminosity estimated from the $K$ band magnitude and the bolometric correction for the $K$ band given by \cite{Leggett01.1}.  \\
\end{table}