Astronomy & Astrophysics

All Tables

Table 2: Parameters of X-ray flares detected on TMC members during the XEST: amplitude $A_{\rm F}$ and derivative $[MAX(\Delta )]_{\rm F}$ are used to identify flares; the duration $\tau _{\rm F}$ , characteristic luminosity $L_{\rm ch}$ and flare luminosity $L_{\rm F}$ , and the flare energy $E_{\rm F}$ are derived as described in Sect. 3.1; the last column provides a flag that classifies the shape of the lightcurve (see Franciosini et al. 2007).
Table 3: XEST X-ray variability statistics for different types of young stars in the broad, soft, and hard bands derived with the MLB technique. For each energy band the number of detected sources, the number of variable sources, and the number fraction of variables are given; see text for details.
Table 4: XEST X-ray flare statistics for different types of young stars in the 0.3-7.8 keV broad band derived with the MLB technique. For each YSO class, the number of detected sources and the number of flares are given, as is the fraction of flares with respect to the total sample.
Table 5: XEST X-ray variability statistics for different spectral types in the 0.3-7.8 keV broad band; see Tables 3 and 4, and the text in Sect. 4 for details.
Table 1: X-ray variability of TMC members during the XEST. Columns 1-4 give the XEST number, stellar identification, young star class, and spectral type (see Güdel et al. 2007, for details on these classifications). The summed broad band GTI after removal of time intervals with high background is given in Col. 5. The analysis is based on EPIC/pn data; exceptions are marked with labels M1 for MOS 1 and M2 for MOS 2. The remaining columns represent the number of source photons ("Cts''), the number of segments (" $N_{\rm b}$ ''), the confidence level of the MLB test (" $CL_{\rm corr}$ ''), and the probability for variable source according to the KS-test (" $P_{\rm KS,eff}$ ''). Results are given for the broad (0.3-7.8 keV), soft (0.3-1.0 keV) and hard (1.0-7.8 keV) band.