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GCN Circular 22486

GRB 180314A: Swift-XRT refined Analysis
2018-03-14T14:45:07Z (6 years ago)
Phil Evans at U of Leicester <>
S. J. LaPorte (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU) and
P. D'Avanzo report on behalf of the Swift-XRT team:

We have analysed 8.7 ks of XRT data for GRB 180314A (D'Avanzo et al.
GCN Circ. 22478), from 165 s to 37.0 ks after the  BAT trigger. The
data comprise 181 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN Circ. 22480).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.60 (+0.04, -0.17). At T+328 s  the decay
steepens to an alpha of 5.8 (+2.2, -1.0) before breaking again at T+401
s to a final decay with index alpha=0.94 (+/-0.03).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 2.34 (+0.08, -0.04). The
best-fitting absorption column is  consistent with the Galactic value
of 1.5 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.77 (+/-0.07) and a best-fitting absorption column
consistent with the Galactic value. 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 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.5 x 10^21 cm^-2
Intrinsic column:    1.5 (+0.8, -0.0) x 10^21 cm^-2 at z=1.445
Photon index:	     1.77 (+/-0.07)

If the light curve continues to decay with a power-law decay index of
0.94, the count rate at T+24 hours will be 0.014 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.7 x
10^-13 (6.9 x 10^-13) 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.
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