GCN Circular 27863

A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), J. D. Gropp (PSU), J.A.
Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), A. Melandri (INAF-OAB) and V. D'Elia report
on behalf of the Swift-XRT team:

We have analysed 3.7 ks of XRT data for GRB 200529A (D'Elia et al. GCN
Circ. 27845
Not found
 
 
), from 197 s to 44.3 ks after the  BAT trigger. The data
comprise 51 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 27848
Not found
 
 
).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.0 (+/-0.6), followed by a break at T+580 s to an alpha
of 0.44 (+0.19, -0.17).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 2.29 (+0.29, -0.20). The
best-fitting absorption column is  consistent with the Galactic value
of 2.4 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 2.8 x 10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:	     2.4 (+/-0.8) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:	     2.29 (+0.29, -0.20)

If the light curve continues to decay with a power-law decay index of
0.44, 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 3.7 x
10^-13 (5.9 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/00974942.

This circular is an official product of the Swift-XRT team.