All Tables

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.
Table 1: List of all candidate members. "XEST id'' refers to the name of the X-ray source in the XEST catalogue (Güdel et al. 2007a, the first 2 digits mark the field of the survey). RA X and Dec X are the coordinates of the X-ray source (corrected for boresight shift). CR is the equivalent on-axis count-rate for the PN in the 0.5-7.3 keV band, averaged over the entire observation (see notes for the quiescent level of the sources with strong flares). $L_{\rm X}$ is estimated in the 0.3-10 keV band from CR (see text), except where noted. A "y'' in the column "var'' means that the X-ray source was found to be variable according to the maximum likelihood algorithm described in Sect. 5. The 7 ${\rm th}$ column is the designation of the infrared counterpart in the 2MASS catalogue; "offset'' is the distance between the positions of the X-ray source and its IR counterpart; J, H and $K_{\rm s}$ are the infrared magnitudes reported in the 2MASS catalogue. Sources in bold face are the most probable candidates on the basis of light curve and/or spectral analysis (Sect. 5).