\begin{table}%T5
%\centering
\par
\caption{X-ray luminosities in the $0.4{-}2.5$~keV band for $d=160$~pc, X-ray to bolometric luminosity ratio,
and probability for variability of the source according to the KS-test. 
The flag in Col.~3 indicates the method used to derive $L_{\rm x}$: "S'' -- spectral fit with
2-T model and column density fixed to the value expected for the galactic 
$N_{\rm H}-A_{\rm V}$~relation; 
"L'' -- absorption from the literature and $\log{T}~[K] = 6.95$; "N'' -- absorption
newly derived in this paper from {\it JHK} colors and $\log{T}~[K] = 6.95$.}
\label{tab:lx}
\begin{tabular}{lrrrr} \hline\hline
Designation & $\log{L_{\rm x}}$ & Flag        & $\log{(L_{\rm x}/L_{\rm bol})}$ & KS prob. \\
            & [erg/s]          & $L_{\rm x}$ &  & \\
\hline
\multicolumn{5}{c}{Spectroscopically confirmed Cha~I~members} \\
\hline
KG~2001-19    &  $28.67$ & L     &  $-3.66$ & $-$     \\
CHXR-21        &  $30.83$ & S     &  $-2.40$ & 95\%  \\
HM~19         &  $29.44$ & L     &  $-3.52$ & $-$     \\
VW~Cha        &  $30.97$ & S     &  $-3.13$ & 100\% \\
CHXR-74        &  $30.30$ & S     &  $-2.57$ & $-$     \\
BYB~18        &  $29.36$ & S     &  $-3.25$ & 100\% \\
KG~2001-96    &  $28.90$ & L     &  $-3.45$ & $-$     \\
HD~97048      &  $29.58$ & S     &  $-5.72$ & $-$     \\
CCE~98-19     &  $30.92$ & S     &  $-2.41$ & $-$     \\
CHXR-73        &  $30.49$ & S     &  $-2.31$ & 100\% \\
CHXR-76        &  $29.92$ & S     &  $-2.62$ & $-$     \\
CHXR-26        &  $31.27$ & S     &  $-2.35$ & 100\% \\
CHXR-47        &  $30.77$ & S     &  $-3.75$ & $-$     \\
CHX-10a        &  $30.56$ & S     &  $-3.64$ & 99\%  \\
CHXR-15        &  $29.56$ & S     &  $-3.10$ & $-$ \\
BYB~43        &  $29.08$ & L     &  $-3.88$ & 100\% \\
Ced~110~IRS-2&  $31.16$ & S     &  $-3.69$ & 100\% \\
WX~Cha        &  $30.17$ & S     &  $-3.35$ & $-$ \\
CHXR-78~C     &  $28.96$ & L     &  $-3.44$ & $-$     \\
CCE~98-23     &  $30.33$ & L     &  $-3.32$ & $-$     \\
Sz~30         &  $30.62$ & S     &  $-2.86$ & 99\%  \\
CHXR-25        &  $29.82$ & S     &  $-2.63$ & 97\%  \\
CHXR-22~E     &  $30.94$ & S     &  $-2.87$ & $-$     \\
HM~15         &  $30.47$ & S     &  $-3.18$ & $-$     \\
CCE~98-32     &  $31.06$ & S     &  $-2.92$ & 100\% \\
HM~16         &  $31.00$ & S     &  $-3.31$ & $-$     \\
LH$\alpha$332-17& $31.09$ & S     &  $-3.70$ & 97\%  \\
Glass~I       &  $31.79$ & S     &  $-2.65$ & $-$     \\
CHXR-20        &  $30.03$ & S     &  $-3.49$ & $-$     \\
ChaH$\alpha$1  &  $28.25$ & L     &  $-3.39$ & $-$     \\
ChaH$\alpha$2  &  $28.49$ & L     &  $-3.52$ & $-$     \\
ChaH$\alpha$3  &  $29.11$ & S     &  $-3.03$ & $-$     \\
ChaH$\alpha$4  &  $28.41$ & L     &  $-3.85$ & $-$     \\
ChaH$\alpha$5  &  $29.21$ & L     &  $-2.98$ & $-$     \\
ChaH$\alpha$6  &  $28.91$ & L     &  $-3.12$ & $-$     \\
ChaH$\alpha$7  &  $28.27$ & L     &  $-3.14$ & $-$     \\
ChaH$\alpha$8  &  $28.44$ & L     &  $-3.39$ & 99\%  \\
ChaH$\alpha$9  & $<$27.92 & L     & ${<}{-}3.33$ & $-$ \\
ChaH$\alpha$10 & $<$27.78 & L     & ${<}{-}3.54$ & $-$ \\
ChaH$\alpha$11 & $<$27.67 & L     & ${<}{-}3.48$ & $-$ \\
ChaH$\alpha$12 & $<$28.19 & L     & ${<}{-}3.81$ & $-$ \\
ChaH$\alpha$13 &  $29.02$ & L     &  $-3.51$ & 97\%  \\
IR~Nebula     & $<$29.16 & L     & ${<}{-}4.77$ & $-$ \\
\hline
\multicolumn{5}{c}{Photometric candidates} \\
\hline
UX~Cha        &  $29.53$ & N     &  $-3.74$ & $-$      \\
KG~2001-78    &  $30.56$ & S     &  $-4.56$ & $-$      \\
KG~2001-5     &  $28.86$ & L     &  $-3.93$ & $-$      \\
2M~110506-773944&$29.51$ & N     &  $-3.34$ & $-$    \\
\hline
\end{tabular}
\end{table}