Table 5: 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 JHK colors and $\log{T}~[K] = 6.95$.
Designation $\log{L_{\rm x}}$ Flag $\log{(L_{\rm x}/L_{\rm bol})}$ KS prob.
  [erg/s] $L_{\rm x}$    
Spectroscopically confirmed Cha I members
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 -
Photometric candidates
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 -


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