GCN Circular 14716
A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), G. Stratta (ASDC) and V. D'Elia report on behalf of the Swift-XRT team: We have analysed 9.0 ks of XRT data for GRB 130528A (D'Elia et al. GCN Circ. 14711), from 68 s to 22.8 ks after the BAT trigger. The data comprise 842 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ 14714). The late-time light curve (from T0+4.9 ks) can be modelled with a power-law decay with a decay index of alpha=1.06 (+/-0.12). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.69 (+/-0.07). The best-fitting absorption column is 3.6 (+/-0.3) x 10^21 cm^-2, in excess of the Galactic value of 5.2 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 1.92 (+/-0.15) and a best-fitting absorption column of 3.6 (+/-0.6) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.4 x 10^-11 (6.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.6 (+/-0.6) x 10^21 cm^-2 Galactic foreground: 5.2 x 10^20 cm^-2 Excess significance: 8.5 sigma Photon index: 1.92 (+/-0.15) If the light curve continues to decay with a power-law decay index of 1.06, the count rate at T+24 hours will be 0.013 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.7 x 10^-13 (8.9 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00556870. This circular is an official product of the Swift-XRT team.