2004A&A...426..415A

We report on the X-ray observations of the X-ray flash (XRF) which occurred on 2002 April 27, three days before BeppoSAX was switched off. The event was detected with the BeppoSAX Wide Field Cameras but not with the Gamma ray Burst Monitor. A follow-up observation with the BeppoSAX Narrow Field Instruments was soon performed and a candidate afterglow source was discovered. We present the results obtained. We also include the results obtained from the observations of the XRF field with the Chandra X-ray satellite. The spectral analysis of the prompt emission shows that the peak energy of the EF(E) spectrum is lower than 5.5keV, with negligible spectral evolution. The X-ray afterglow spectrum is consistent with a power law model with photon index of ∼2, while the 2-10keV flux fades as a power law with a decay index -1.33. Both these indices are typical of GRBs. A very marginal excess at ∼4.5-5keV is found in the afterglow spectrum measured by BeppoSAX. As for many GRBs, the extrapolation of the 2-10keV fading law back to the time of the prompt emission is consistent with the X-ray flux measured during the second part of the event. We estimate a possible range of values of the redshift and discuss our results in the light of current models of XRFs.