Notes:

• 1) The fitting includes the systematic errors.
• 2) When the burst includes telescope slew time periods, the fitting uses an average response file made from multiple 5-s response files through out the slew time plus single time preiod for the non-slew times, and weighted by the total counts in the corresponding time period using addrmf. An average response file is needed becuase a spectral fit using the pre-slew DRM will introduce some errors in both a spectral shape and a normalization if the PHA file contains a lot of the slew/post-slew time interval.
• 3) For fits to more complicated models (e.g. a power-law over a cutoff power-law), the BAT team has decided to require a chi-square improvement of more than 6 for each extra dof.

Time averaged spectrum fit using the average DRM

Power-law model

Multiple GTIs in the spectrum
tstart tstop
XSPEC12>exit
 XSPEC: quit
 
 
Photon index:       (       )
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index:      (     )
Norm@50keV  :     (     )
------------------------------------------------------------
 
Photon flux (15-150 keV)    in  sec:  (    ) ph/cm2/s
Energy fluence (15-150 keV)             : 0 ( 0  0 ) ergs/cm2
 

Cutoff power-law model

Multiple GTIs in the spectrum
tstart tstop
 XSPEC: quit
 
 
Photon index:       (       )
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index:      (     )
Epeak [keV] :       (   )
Norm@50keV  :     (     )
------------------------------------------------------------
 
Photon flux (15-150 keV)    in  sec:  (    ) ph/cm2/s
Energy fluence (15-150 keV)             : 0 ( 0  0 ) ergs/cm2
 

1-s peak spectrum fit

1-s peak spectrum unavailable, likely because there are no event data in the 1-s peak range.

Time-resolved spectra