GCN Circular 28660

A. D'Ai (INAF-IASFPA), J. D. Gropp (PSU), J.A. Kennea (PSU), A.
Tohuvavohu (U. Toronto), 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 7.2 ks of XRT data for GRB 201015A (D'Elia et al. GCN
Circ. 28632
Not found
 
 
), from 3.2 ks to 57.3 ks after the	BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN Circ. 28647
Not found
 
 
).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.49 (+0.24, -0.21).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+/-0.4). The
best-fitting absorption column is  2.3 (+4.6, -2.3) x 10^21 cm^-2, at a
redshift of 0.426, in addition to the Galactic value of 3.6 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 4.0 x
10^-11 (7.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 3.6 x 10^21 cm^-2
Intrinsic column:    2.3 (+4.6, -2.3) x 10^21 cm^-2 at z=0.426
Photon index:	     2.2 (+/-0.4)

If the light curve continues to decay with a power-law decay index of
1.49, the count rate at T+24 hours will be 10.0 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.0 x
10^-14 (7.7 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01000452.

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