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    0.000 sec. to    0.068 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -3.79848     ( -0.853731   0.439971 )
Norm@50keV  : 2.44386E-03    ( -0.00159132   0.00157306 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          97.49 using 59 PHA bins.
# Reduced chi-squared =          1.710 for     57 degrees of freedom 
# Null hypothesis probability =   6.744175e-04
 
Photon flux (15-150 keV)    in 0.068 sec: 1.26843 ( -0.541475  0.54015 ) ph/cm2/s
Energy fluence (15-150 keV)             : 3.18397e-09 ( -1.40155e-09  1.38627e-09 ) ergs/cm2
 

Cutoff power-law model

Time interval is from    0.000 sec. to    0.068 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -1     (       )
Epeak [keV] : 80.0000      (   )
Norm@50keV  : 0.0    (     )
------------------------------------------------------------
#Fit statistic : Chi-Squared =         112.41 using 59 PHA bins.
# Reduced chi-squared =         2.0074 for     56 degrees of freedom 
# Null hypothesis probability =   1.173343e-05
 
Photon flux (15-150 keV)    in 0.068 sec:  (    ) ph/cm2/s
Energy fluence (15-150 keV)             : 1.51241e-08 ( -3.40702e-09  3.40436e-09 ) ergs/cm2
 

1-s peak spectrum fit

Power-law model

Time interval is from   -0.464 sec. to    0.536 sec.
 
Spectral model in power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: -0.84917     ( -0.71902   0.916926 )
Norm@50keV  : 2.65570E-03    ( -0.00135904   0.00131039 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          53.24 using 59 PHA bins.
# Reduced chi-squared =         0.9341 for     57 degrees of freedom 
# Null hypothesis probability =   6.168036e-01
 
Photon flux (15-150 keV)    in 1 sec: 0.304420 ( -0.145885  0.152104 ) ph/cm2/s
Energy fluence (15-150 keV)             : 3.04502e-08 ( -1.4735e-08  1.5057e-08 ) ergs/cm2
 

Cutoff power-law model

Time interval is from   -0.464 sec. to    0.536 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters  : value       lower 90%   higher 90%
Photon index: 9.57437     ( -10.0973   -9.5419 )
Epeak [keV] : 52.1721      ( -10.1821 184.148 )
Norm@50keV  : 393.047    ( -362.379   6319.03 )
------------------------------------------------------------
#Fit statistic : Chi-Squared =          50.04 using 59 PHA bins.
# Reduced chi-squared =         0.8936 for     56 degrees of freedom 
# Null hypothesis probability =   6.987688e-01
 
Photon flux (15-150 keV)    in 1 sec: 0.236238 ( -0.099803  0.160789 ) ph/cm2/s
Energy fluence (15-150 keV)             : 1.80443e-08 ( -7.77502e-09  1.85135e-08 ) ergs/cm2
 

Time-resolved spectra