Table 2: Parameters of the best-fit coronal models (with 1$\sigma $ errors) for the brightest candidate members. $T_{\rm av}$ is the EM-weighted logarithmic average temperature, defined as $\log T_{\rm av} = (EM_1~\log T_1+EM_2~\log T_2)/(EM_1+EM_2)$ (see also Güdel et al. 2007a). The model flux (in the 0.3-10 keV band ) is unabsorbed and the luminosity is calculated from it assuming d=140 pc.
Source $N_{\rm H}$ T1 T2 EM2/EM1 $T_{\rm av}$ $F_{\rm X}$ $L_{\rm X}$ $\chi^2_{\nu}\ ({\rm d.o.f.})$ Flare
  (1022 cm-2) (MK) (MK)   (MK) (10-13 cgs) (1028 cgs)    
XEST-09-042 0.12 $\pm$ 0.01 7.9 $\pm$ 0.3 20 $\pm$ 2 0.71 $\pm$ 0.07 11 7.3 172 0.95 (147)  
XEST-08-049 a 0.30 $\pm$ 0.02 9.2 $\pm$ 0.6 23 $\pm$ 2 1.4 $\pm$ 0.3 16 4.9 115 1.29 (86)  
XEST-08-003 0.24 $\pm$ 0.02 8.9 $\pm$ 0.7 50 $\pm$ 6 2.8 $\pm$ 0.6 31 13 290 0.81 (79) yes
XEST-20-071 0.41 $\pm$ 0.04 7.8 $\pm$ 0.6 18 -2+3 0.50 $\pm$ 0.15 10 7.3 171 0.74 (49)  
XEST-08-014 <0.02 4.7 $\pm$ 0.4 17 -2+3 0.88 $\pm$ 0.16 8.6 1.3 30 1.50 (30) yes
XEST-09-033 a 0.25 $\pm$ 0.05 14.5 $\pm$ 0.8 - - 14.5 2.9 68 1.38 (26)  
XEST-08-033 0.40 $\pm$ 0.10 4.8 -0.7+1.8 16.1 -1.7+1.3 0.8 $\pm$ 0.4 8.3 1.6 38 1.47 (22)  
XEST-17-059 0.18 $\pm$ 0.03 13.0 $\pm$ 0.6 - - 13 1.7 40 1.09 (27)  
XEST-05-027 1.10 $\pm$ 0.15 48 -11+20 - - 48 8.6 202 0.89 (17)  
XEST-15-034 <0.02 6.0 $\pm$ 0.7 - - 6.0 0.42 10 0.78 (19)  
XEST-27-084 0.07 $\pm$ 0.04 9.1 $\pm$ 0.8 33 -9+17 0.8 $\pm$ 0.3 17 0.57 13 0.67 (21) yes

a These two sources have the same 2MASS counterpart.


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