A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), A. Cholden-Brown (PSU),
S. J. LaPorte (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), B. Mingo (U. Leicester), V. D'Elia (ASDC) and
report on behalf of the Swift-XRT team: report on behalf of the
We have analysed 8.0 ks of XRT data for GRB 170113A, from 50 s to 19.1
ks after the BAT trigger. The data comprise 243 s in Windowed Timing
(WT) mode (the first 7 s were taken while Swift was slewing) with the
remainder in Photon Counting (PC) mode.
The late-time light curve (from T0+5.2 ks) can be modelled with a
power-law decay with a decay index of alpha=1.14 (+/-0.10).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.88 (+/-0.07). The
best-fitting absorption column is 1.82 (+0.26, -0.24) x 10^21 cm^-2,
in excess of the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.77 (+/-0.08) and a
best-fitting absorption column of 1.43 (+0.26, -0.25) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.9 x 10^-11 (4.7 x 10^-11) erg cm^-2
A summary of the PC-mode spectrum is thus:
Total column: 1.43 (+0.26, -0.25) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 2.3 sigma
Photon index: 1.77 (+/-0.08)
If the light curve continues to decay with a power-law decay index of
1.14, the count rate at T+24 hours will be 0.030 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-12 (1.4 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
This circular is an official product of the Swift-XRT team.