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 0.260 sec. to 133.044 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.62525 ( -0.218807 0.216248 )
Norm@50keV : 1.64702E-03 ( -0.00020974 0.000209006 )
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#Fit statistic : Chi-Squared = 52.32 using 59 PHA bins.
# Reduced chi-squared = 0.9179 for 57 degrees of freedom
# Null hypothesis probability = 6.508868e-01
Photon flux (15-150 keV) in 132.8 sec: 0.213347 ( -0.028502 0.028673 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.03985e-06 ( -2.70888e-07 2.7226e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.260 sec. to 133.044 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.12341 ( -0.668672 1.03814 )
Epeak [keV] : 90.8202 ( -38.0095 -90.8203 )
Norm@50keV : 2.89880E-03 ( -0.000927615 0.00612164 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.36 using 59 PHA bins.
# Reduced chi-squared = 0.9171 for 56 degrees of freedom
# Null hypothesis probability = 6.509487e-01
Photon flux (15-150 keV) in 132.8 sec: 0.208131 ( -0.029936 0.030037 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.98503e-06 ( -2.90698e-07 2.89011e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 3.264 sec. to 4.264 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.74466 ( -0.853307 0.704125 )
Norm@50keV : 5.90895E-03 ( -0.00273216 0.00254552 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.32 using 59 PHA bins.
# Reduced chi-squared = 0.7424 for 57 degrees of freedom
# Null hypothesis probability = 9.265787e-01
Photon flux (15-150 keV) in 1 sec: 0.797461 ( -0.328344 0.331099 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.45494e-08 ( -2.42475e-08 2.51784e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 3.264 sec. to 4.264 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.808361 ( -1.42233 8.09071 )
Epeak [keV] : 69.6172 ( -69.7456 -69.7456 )
Norm@50keV : 1.62446E-02 ( -0.0162466 8.91626 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.98 using 59 PHA bins.
# Reduced chi-squared = 0.7497 for 56 degrees of freedom
# Null hypothesis probability = 9.177562e-01
Photon flux (15-150 keV) in 1 sec: 0.759325 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 5.31153e-08 ( -2.32078e-08 2.55005e-08 ) ergs/cm2
Time-resolved spectra
