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 -169.224 sec. to   15.192 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.97743     ( -0.368532   0.334637 )
Norm@50keV  : 1.38686E-03    ( -0.000334658   0.000321157 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          65.96 using 59 PHA bins.
# Reduced chi-squared =          1.157 for     57 degrees of freedom 
# Null hypothesis probability =   1.946693e-01
 
Photon flux (15-150 keV)    in 184.4 sec: 0.205914 ( -0.038595  0.038603 ) ph/cm2/s
Energy fluence (15-150 keV)             : 2.35624e-06 ( -5.25361e-07  5.42573e-07 ) ergs/cm2
 

Cutoff power-law model

Time interval is from -169.224 sec. to   15.192 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1.5767     ( -0.577837   1.51886 )
Epeak [keV] : 44.6046      (   )
Norm@50keV  : 2.36455E-03    (     )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          65.64 using 59 PHA bins.
# Reduced chi-squared =          1.172 for     56 degrees of freedom 
# Null hypothesis probability =   1.774432e-01
 
Photon flux (15-150 keV)    in 184.4 sec: 0.203449 ( -0.039207  0.039243 ) ph/cm2/s
Energy fluence (15-150 keV)             : 2.26877e-06 ( -5.668e-07  5.78389e-07 ) ergs/cm2
 

1-s peak spectrum fit

Power-law model

Time interval is from    3.580 sec. to    4.580 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -2.15755     ( -0.597257   0.477675 )
Norm@50keV  : 1.32371E-02    ( -0.00482045   0.00434636 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          57.32 using 59 PHA bins.
# Reduced chi-squared =          1.006 for     57 degrees of freedom 
# Null hypothesis probability =   4.631886e-01
 
Photon flux (15-150 keV)    in 1 sec: 2.14390 ( -0.62392  0.62529 ) ph/cm2/s
Energy fluence (15-150 keV)             : 1.23788e-07 ( -3.82695e-08  3.82997e-08 ) ergs/cm2
 

Cutoff power-law model

Time interval is from    3.580 sec. to    4.580 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -2.22477     ( -0.419484   1.8628 )
Epeak [keV] : 168.643      (   )
Norm@50keV  : 1.22107E-02    (     )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          57.32 using 59 PHA bins.
# Reduced chi-squared =          1.023 for     56 degrees of freedom 
# Null hypothesis probability =   4.261260e-01
 
Photon flux (15-150 keV)    in 1 sec:  (    ) ph/cm2/s
Energy fluence (15-150 keV)             : 0 ( 0  0 ) ergs/cm2
 

Time-resolved spectra