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 -0.416 sec. to 12.140 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.29207 ( -0.101387 0.102096 )
Norm@50keV : 1.12661E-02 ( -0.000658653 0.000658625 )
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#Fit statistic : Chi-Squared = 65.16 using 59 PHA bins.
# Reduced chi-squared = 1.143 for 57 degrees of freedom
# Null hypothesis probability = 2.141087e-01
Photon flux (15-150 keV) in 12.56 sec: 1.34214 ( -0.08158 0.08171 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.40117e-06 ( -8.96946e-08 9.01131e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.416 sec. to 12.140 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.927809 ( -0.347129 0.435702 )
Epeak [keV] : 155.913 ( -57.7794 -155.913 )
Norm@50keV : 1.68791E-02 ( -0.00577492 0.0100619 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.68 using 59 PHA bins.
# Reduced chi-squared = 1.119 for 56 degrees of freedom
# Null hypothesis probability = 2.512991e-01
Photon flux (15-150 keV) in 12.56 sec: 1.32082 ( -0.08491 0.08487 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.36811e-06 ( -9.78885e-08 9.73686e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 6.040 sec. to 7.040 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.18388 ( -0.159007 0.161979 )
Norm@50keV : 2.70122E-02 ( -0.00265387 0.00265341 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.80 using 59 PHA bins.
# Reduced chi-squared = 0.9087 for 57 degrees of freedom
# Null hypothesis probability = 6.700499e-01
Photon flux (15-150 keV) in 1 sec: 3.16369 ( -0.3203 0.32088 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.7534e-07 ( -2.93372e-08 2.94846e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 6.040 sec. to 7.040 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.363833 ( -0.689633 0.825911 )
Epeak [keV] : 106.161 ( -29.7707 240.873 )
Norm@50keV : 6.70443E-02 ( -0.0352791 0.0949648 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.58 using 59 PHA bins.
# Reduced chi-squared = 0.8496 for 56 degrees of freedom
# Null hypothesis probability = 7.809998e-01
Photon flux (15-150 keV) in 1 sec: 3.08297 ( -0.32966 0.3292 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.62997e-07 ( -3.20087e-08 3.17979e-08 ) ergs/cm2
Time-resolved spectra
