GCN Circular 9237
R. Margutti (Univ. Bicocca & INAF-OAB), C. Guidorzi (Univ. Ferrara), J. Mao (INAF-OAB) and J. K. Cannizzo (NASA/UMBC) report on behalf of the Swift-XRT team: We have analysed the first 2 orbits of Swift-XRT data obtained for GRB 090424 (Cannizzo et al. GCN Circ. 9223), covering 1732 s of Windowed Timing (WT) and 1329 s of Photon Counting (PC) mode data, respectively, between 88 s and 8 ks after the trigger. The UVOT-enhanced XRT position was given by Goad et al. in GCN Circ. 9232. The light-curve can be modelled by a double broken power-law, with a first decaying index alpha_1= 1.29 +/- 0.05 and a first break time of about 260 s. The decay then flattens to alpha_2= 0.74 +/- 0.02. After 1450 s the decay is best modelled by a power-law index alpha_3= 1.15 +/- 0.05. The very good statistics allows us to observe spectral evolution in WT data before the first break, with the simple power law photon index evolving from 2.6 to 2.1 . A spectrum extracted from WT mode data in the time interval 0.4-1.4 ks can be modelled with an absorbed power-law with a photon index Gamma= 2.13 +/- 0.05 and best-fitting absorption column NH = (0.20 +/- 0.01) x10^22 cm^-2, in excess of the Galactic value of 1.9 x 10^20 cm^-2 (Kalberla et al. 2005). The spectrum extracted from PC data in the time interval 6.1-8 ks can be modelled with an absorbed power-law, with Gamma = 2.06 +/- 0.09 and a column density of NH = (0.27 +/- 0.03)x10^22 cm^-2. The observed (unabsorbed) 0.3 -10 keV flux over this time interval is 4.2x10^-11 (6.7x10^-11) erg cm^-2 count^-1. Uncertainties are given at 90% confidence. If the light-curve continues to decay with alpha ~1.15, the count rate 24 hours after the burst is estimated to be 0.10 count s^-1, which corresponds to an observed (unabsorbed) flux of 4.2x10^-12 (6.7x10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00350311. This circular is an official product of the Swift-XRT team.