TITLE:   GCN CIRCULAR
NUMBER:  15777
SUBJECT: GRB 140129B: Swift-XRT refined Analysis
DATE:    14/01/30 10:57:45 GMT
FROM:    Maria Grazia Bernardini at INAF/Brera  <grazia.bernardini@brera.inaf.it>

M. G. Bernardini (INAF-OAB) reports on behalf of the Swift-XRT team:

We have analysed 1.8 ks of XRT data for GRB 140129B (Bernardini  et al.
GCN Circ. 15765),  from 322 s to 6.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN. Circ 15770).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.24 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.12 (+0.21, -0.20). The
best-fitting absorption column is  1.1 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 5.6 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     1.1 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 5.6 x 10^20 cm^-2
Excess significance: 1.9 sigma
Photon index:	     2.12 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
1.24, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x
10^-14 (8.3 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/00585149.

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