GCN Circular 22602

A. Tohuvavohu (PSU), S. J. LaPorte (PSU), K.L. Page (U. Leicester),
A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), J.A. Kennea (PSU)
and J.D. Gropp report on behalf of the Swift-XRT team:

We have analysed 3.9 ks of XRT data for GRB 180404A (Gropp et al. GCN
Circ. 22589
Not found
 
 
), from 90 s to 52.0 ks after the  BAT trigger. The data
comprise 26 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. 22592
Not found
 
 
).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.5 (+nan, -nan).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.62 (+0.27, -0.22). The
best-fitting absorption column is  consistent with the Galactic value
of 3.1 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.1 x 10^-11 (4.2 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     3.1 (+/-5.1) x 10^20 cm^-2
Galactic foreground: 3.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:	     1.62 (+0.27, -0.22)

If the light curve continues to decay with a power-law decay index of
0.5, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-13 (4.5 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/00821881.

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