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 -7.216 sec. to 40.084 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.63682 ( -0.29381 0.261606 )
Norm@50keV : 7.06398E-04 ( -0.000156998 0.000159246 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.07 using 59 PHA bins.
# Reduced chi-squared = 0.8434 for 57 degrees of freedom
# Null hypothesis probability = 7.941485e-01
Photon flux (15-150 keV) in 47.3 sec: 0.151290 ( -0.018349 0.018357 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.48049e-07 ( -5.3308e-08 5.5876e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -7.216 sec. to 40.084 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.48808 ( -1.36551 2.06835 )
Epeak [keV] : 23.3179 ( -21.3976 6.02428 )
Norm@50keV : 1.81330E-02 ( -0.0183863 0.440327 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.35 using 59 PHA bins.
# Reduced chi-squared = 0.7384 for 56 degrees of freedom
# Null hypothesis probability = 9.282342e-01
Photon flux (15-150 keV) in 47.3 sec: 0.151276 ( -0.018271 0.018377 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.0519e-07 ( -4.54312e-08 5.23961e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 9.504 sec. to 10.504 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.81651 ( -0.717126 0.609304 )
Norm@50keV : 2.84842E-03 ( -0.00115969 0.00101735 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.56 using 59 PHA bins.
# Reduced chi-squared = 0.9922 for 57 degrees of freedom
# Null hypothesis probability = 4.916281e-01
Photon flux (15-150 keV) in 1 sec: 0.395070 ( -0.116898 0.116889 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.62114e-08 ( -9.80286e-09 1.02741e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 9.504 sec. to 10.504 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.35308 ( -1.03144 1.36008 )
Epeak [keV] : 127.822 ( )
Norm@50keV : 1.46525E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.57 using 59 PHA bins.
# Reduced chi-squared = 0.9923 for 56 degrees of freedom
# Null hypothesis probability = 4.912038e-01
Photon flux (15-150 keV) in 1 sec: 0.398249 ( -0.120245 0.114004 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.18328e-08 ( -1.24037e-08 1.00723e-08 ) ergs/cm2
Time-resolved spectra
