All Tables

Table 1: Observing log for the XMM-Newton observation of Cha I on April 9, 2002 (Obs-ID 0002740501; Revolution number 427). "Start'' and "Stop'' refer to start and end of exposures.
Table 6: Best fit parameters of an absorbed power-law model for X-ray bright unidentified X-ray sources in the Cha I XMM-Newton field.
Table 2: X-ray sources detected in the EPIC observation of Cha I at ${\it ML} > 20$ . The columns denote X-ray source number, instrument by which the source was detected, X-ray position, maximum likelihood of source existence, number of broad band source counts, exposure time, hardness ratios, optical/IR counterpart, and distance between the X-ray source and the counterpart. For sources detected in the merged image we list the hardness ratios computed from the corresponding source found in pn, and no hardness ratio is computed if the source is detected only in the merged image.
Table 3: Optical and IR properties for all Cha I members and candidate members in the XMM-Newton FOV. The H ${\alpha }$ equivalent width ( $W_{\rm H\alpha }$ ) is negative for emission. If more than one H ${\alpha }$ measurement is available for a given star we list the maximum and the minimum value observed. The T Tauri type given in Col. 6 of the same table is assigned on the basis of $W_{\rm H\alpha }$ using the criteria put forth by Martin98.1. Columns 7 and 8 represent the extinction and magnitude used to derive $L_{\rm bol}$ ; referring to the band given in Col. 9. The bolometric luminosity, effective temperature, age and mass have been computed as described in Sect. 3.3. $L_{\rm bol}$ has been calculated for d=160 pc. We assign an age of $5 \times 10^5$ yr to objects on the birthline.
Table 4: Spectral parameters of bright X-ray sources in the Cha I XMM-Newton field. The columns represent: source number, identification, number of counts in the background-subtracted spectrum, reduced $\chi ^2$ of best fit, absorbing hydrogen column density derived from A_J using the relation by Paresce84.1 and held fixed during the fitting process, X-ray temperature(s) of 2-component thermal MEKAL model, and emission measures of each temperature component assuming a distance of 160 pc.
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 $\log{T}~[K] = 6.95$ .