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 -0.024 sec. to 6.936 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.65219 ( -0.186432 0.181809 )
Norm@50keV : 9.08508E-03 ( -0.00106275 0.00104959 )
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#Fit statistic : Chi-Squared = 70.19 using 59 PHA bins.
# Reduced chi-squared = 1.231 for 57 degrees of freedom
# Null hypothesis probability = 1.126069e-01
Photon flux (15-150 keV) in 6.96 sec: 1.18719 ( -0.12803 0.12811 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.88043e-07 ( -7.26137e-08 7.36229e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.024 sec. to 6.936 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.797536 ( -0.837134 1.11722 )
Epeak [keV] : 62.9985 ( -15.55 393.69 )
Norm@50keV : 2.68387E-02 ( -0.0268494 0.0850842 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.17 using 59 PHA bins.
# Reduced chi-squared = 1.199 for 56 degrees of freedom
# Null hypothesis probability = 1.457819e-01
Photon flux (15-150 keV) in 6.96 sec: 1.14958 ( -0.13469 0.13392 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.41451e-07 ( -8.51208e-08 8.69534e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.108 sec. to 1.108 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.38869 ( -0.215815 0.21602 )
Norm@50keV : 2.35565E-02 ( -0.00298107 0.00297546 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.13 using 59 PHA bins.
# Reduced chi-squared = 1.073 for 57 degrees of freedom
# Null hypothesis probability = 3.298810e-01
Photon flux (15-150 keV) in 1 sec: 2.86151 ( -0.37116 0.37202 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.28176e-07 ( -3.1564e-08 3.17621e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.108 sec. to 1.108 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.38549 ( -1.68663 0.77452 )
Epeak [keV] : 9997.29 ( -9997.38 -9997.38 )
Norm@50keV : 2.36444E-02 ( -0.0236444 0.0371112 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.13 using 59 PHA bins.
# Reduced chi-squared = 1.092 for 56 degrees of freedom
# Null hypothesis probability = 2.968244e-01
Photon flux (15-150 keV) in 1 sec: 2.86162 ( -0.37143 0.37066 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.28202e-07 ( -3.3249e-08 2.94183e-08 ) ergs/cm2
Time-resolved spectra
