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

Time interval is from -135.196 sec. to   21.728 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -2.62427     ( -0.424854   0.359798 )
Norm@50keV  : 5.46619E-04    ( -0.0001682   0.000169508 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          54.70 using 59 PHA bins.
# Reduced chi-squared =         0.9596 for     57 degrees of freedom 
# Null hypothesis probability =   5.619548e-01
 
Photon flux (15-150 keV)    in 156.9 sec: 0.116124 ( -0.0183443  0.018364 ) ph/cm2/s
Energy fluence (15-150 keV)             : 8.8978e-07 ( -1.83881e-07  1.96302e-07 ) ergs/cm2
 

Cutoff power-law model

Time interval is from -135.196 sec. to   21.728 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.93445     (       )
Epeak [keV] : 3.40084      (   )
Norm@50keV  : 1.49599E-03    (     )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          54.96 using 59 PHA bins.
# Reduced chi-squared =         0.9814 for     56 degrees of freedom 
# Null hypothesis probability =   5.143180e-01
 
Photon flux (15-150 keV)    in 156.9 sec: 0.114238 ( -0.0180655  0.018173 ) ph/cm2/s
Energy fluence (15-150 keV)             : 8.78017e-07 ( -1.1111e-07  2.25255e-07 ) ergs/cm2
 

1-s peak spectrum fit

Power-law model

Time interval is from   19.056 sec. to   20.056 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -2.319     ( -1.10838   0.794689 )
Norm@50keV  : 3.39942E-03    ( -0.00221256   0.00217299 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          69.76 using 59 PHA bins.
# Reduced chi-squared =          1.224 for     57 degrees of freedom 
# Null hypothesis probability =   1.194955e-01
 
Photon flux (15-150 keV)    in 1 sec: 0.600491 ( -0.255364  0.255531 ) ph/cm2/s
Energy fluence (15-150 keV)             : 3.26084e-08 ( -1.65216e-08  1.86447e-08 ) ergs/cm2
 

Cutoff power-law model

Time interval is from   19.056 sec. to   20.056 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.92829     (       )
Epeak [keV] : 6.74952      (   )
Norm@50keV  : 6.00403E-03    (     )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          69.70 using 59 PHA bins.
# Reduced chi-squared =          1.245 for     56 degrees of freedom 
# Null hypothesis probability =   1.032194e-01
 
Photon flux (15-150 keV)    in 1 sec: 0.596047 ( -0.252655  0.254355 ) ph/cm2/s
Energy fluence (15-150 keV)             : 0 ( 0  0 ) ergs/cm2
 

Time-resolved spectra