All Tables

Table 1: XMM-Newton sources in the L1551 cloud region, as detected in the combined EPIC pn+MOS1+MOS2 image. If a counterpart is present in the SIMBAD catalog its name is listed in the "Id'' field. If only a magnitude is given, the counterpart is only present in the USNO A2 catalog. Counterparts have been searched within a radius of 15 arcsec from the X-ray source position. R magnitudes and B-R colors are from the USNO catalog. The X-ray count rate is expressed in "MOS equivalent'' units. r is the distance between the X-ray source and the candidate counterpart. The last column gives the number of the spectrum of the source as used in Table 2.
Table 1: continued. XMM-Newton sources in the L1551 cloud region.
Table 2: X-ray bright XMM-Newton sources in L1551 for which spectral and timing analysis has been performed from EPIC pn data. The ROSAT count rate is as given in Carkner et al. (1996). In the ROSAT PSPC observation HL Tau is unresolved from the nearby XZ Tau, as discussed in the text.
Table 3: Best fit spectral parameters for all the sources listed in Table 2 which are likely extra-galactic. The spectra were fit by an absorbed power-law model. P is the probability level for the fit.
Table 4: Best-fit spectral parameters for V1075 Tau during two consecutive time intervals of XMM-Newton observations.
Table 5: Best-fit spectral parameters for XZ Tau during three consecutive time intervals of XMM-Newton observation.
Table 6: Count rate (in counts per second) and flux level in the 0.5-2.0 keV band for all known X-ray observations of XZ Tau. Flux in units of 10^-13 erg cm^-2 s^-1.
Table 7: Best-fit spectral parameters for the X-ray-bright pre-main sequence stars detected in the XMM-Newton EPIC data. All spectra have been fit with an absorbed 2 temperature plasma model in the energy range 0.35-7.5 keV, apart from HL Tau whose spectrum has been fit with an absorbed 1 temperature plasma model over the energy range 1.0-7.5 keV (see text). In the column "type'', b indicates that the star is a known binary system, W stands for WTTS and C for CTTS.
Table 8: Best-fit spectral parameters for the X-ray sources for which variable abundance fits were performed.
Table 9: Intrinsic X-ray fluxes and luminosity in the 0.35-7.5 keV band ( $f_{\rm X}$ and $L_{\rm X}$ ) as derived from the EPIC pn spectral fits for the X-ray-bright PMS detected in L1551. Also given is the probability of constancy from the Kolmogorov-Smirnov (K-S) test for the XMM-Newton EPIC-pn light curves (shown in Fig. 3). The average flux level of the sources during the XMM-Newton, ROSAT and ASCA observations (when available) in the same bands as used by Carkner et al. (1996) is also reported. Carkner et al. provide ROSAT and ASCA fluxes over different energy ranges for each source; we report these energy ranges in the columns " $\Delta E_{\rm ROSAT}$ '' and " $\Delta E_{\rm ASCA}$ '' and provide the source flux over the same ranges derived from the fits to XMM-Newton spectral data. Energy ranges are in keV, flux units are 10^-13 erg cm^-2 s^-1 and X-ray luminosity is in units of 10²⁸ erg s^-1.