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Fig. 2


Light curve of the 2013 outburst recorded from IGR J18245–2452 and observed by Swift/XRT (black circles, bin time of 500 s), XMM-Newton/Epic-pn (red circles, with a time bin of 200 s as reported in Ferrigno et al. 2014) and INTEGRAL/ISGRI (green circles, the integration time is one science window of ~ 2–3 ks). The arrows indicate the onset of the three type-I X-ray bursts detected from the source (see Sect. 6). IGR J18245–2452 shows a rapid flux variability.

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