{
  "bibcode": "2019GCN.24906....1D",
  "body": "P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi \n(INAF-IASFPA) , J.A. Kennea (PSU), B. Sbarufatti (PSU), D.N. Burrows\n(PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and E.\nSonbas (Adiyaman Univ.) report on behalf of the Swift-XRT team:\n\nWe have analysed 10 ks of XRT data for GRB 190627A (Sonbas et al. GCN\nCirc. 24888), from 121 s to 119.5 ks after the\tBAT trigger. The data\nare entirely in Photon Counting (PC) mode. The enhanced XRT position\nfor this burst was given by Evans et al. (GCN Circ. 24890).\n\nThe light curve can be modelled with an initial power-law decay with an\nindex of alpha=0.12 (+0.15, -0.19), followed by a break at T+22.1 ks to\nan alpha of 1.48 (+0.17, -0.16).\n\nA spectrum formed from the PC mode data can be fitted with an absorbed\npower-law with a photon spectral index of 1.96 (+0.16, -0.09). The\nbest-fitting absorption column is  consistent with the Galactic value\nof 1.8 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed\n(unabsorbed) 0.3-10 keV flux conversion factor deduced from this\nspectrum  is 3.6 x 10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. \n\nA summary of the PC-mode spectrum is thus:\nTotal column:\t     1.8 (+/-0.5) x 10^21 cm^-2\nGalactic foreground: 1.8 x 10^21 cm^-2\nExcess significance: <1.6 sigma\nPhoton index:\t     1.96 (+0.16, -0.09)\n\nThe results of the XRT-team automatic analysis are available at\nhttp://www.swift.ac.uk/xrt_products/00911609.\n\nThis circular is an official product of the Swift-XRT team.",
  "circularId": 24906,
  "createdOn": 1561816534000,
  "email": "pae9@leicester.ac.uk",
  "subject": "GRB 190627A: Swift-XRT refined Analysis",
  "submitter": "Phil Evans at U of Leicester  <pae9@leicester.ac.uk>",
  "eventId": "GRB 190627A"
}