All Figures

Figure 1: XRT light curves, corrected for pile-up, PSF losses, and vignetting and background-subtracted. a) The 1-10 keV light curve for the whole campaign. Different colours denote different observations (Table 1), and points before Feb. 6 (MJD 54 137) and after Feb. 15 (MJD 54 146) are drawn from the sum of several observations. Filled circles are full detections (S/N>3), triangles marginal detections (2<S/N<3), while downward-pointing arrows are 3- upper limits. The vertical lines mark our time selections for spectroscopic analysis (observation 6, observations 7-8, observations 9-12, end of observation 18). The horizontal line marks the region shown enlarged in panel b). b) Detail of observation 6, with a binning that allowed us to achieve an S/N in excess of 6. The numbers mark the 5 flares on which we performed spectroscopic analysis. c) Detail of flare 1, showing the 1-4 keV, 4-10 keV count rates ( top and middle panel) and the hardness ratio 4-10/1-4 ( bottom). The data were rebinned in order to have at least 20 counts per bin in both the 1-4 keV and 4-10 keV bands. d) Same as c) for flare 2.

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In the text

	Figure 2: Folded 0.2-10 keV light curve of the combined observations 6 though 11, using a period of 186.78 s (Swank et al. 2007).
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In the text

	Figure 3: XRT time-selected spectroscopy. The contour levels for the column density in units of 1022 cm-2 vs. the photon index, with best-fit values indicated by crosses. Orange contours are from observation 6, while the blue ones are from the combined observations 7 though 18.
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In the text