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 -33.440 sec. to 26.568 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.69478 ( -0.0709923 0.069818 )
Norm@50keV : 5.09150E-03 ( -0.000217147 0.000216117 )
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#Fit statistic : Chi-Squared = 101.88 using 59 PHA bins.
# Reduced chi-squared = 1.7874 for 57 degrees of freedom
# Null hypothesis probability = 2.403709e-04
Photon flux (15-150 keV) in 60.01 sec: 1.13262 ( -0.04079 0.04105 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.24536e-06 ( -1.02804e-07 1.0293e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -33.440 sec. to 26.568 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.31013 ( -0.392354 0.430507 )
Epeak [keV] : 19.4000 ( -7.81523 4.78919 )
Norm@50keV : 3.26550E-02 ( -0.0133526 0.0258606 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.08 using 59 PHA bins.
# Reduced chi-squared = 1.001 for 56 degrees of freedom
# Null hypothesis probability = 4.720185e-01
Photon flux (15-150 keV) in 60.01 sec: 1.02936 ( -0.047413 0.04783 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.88339e-06 ( -1.25903e-07 1.28877e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.35426 ( -0.118344 0.113651 )
Norm@50keV : 2.26582E-02 ( -0.0018425 0.00182101 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.05 using 59 PHA bins.
# Reduced chi-squared = 0.8956 for 57 degrees of freedom
# Null hypothesis probability = 6.966815e-01
Photon flux (15-150 keV) in 1 sec: 4.08330 ( -0.25306 0.25333 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.18887e-07 ( -1.46897e-08 1.48029e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.04341 ( -0.589639 0.677103 )
Epeak [keV] : 28.9783 ( -9.46651 5.10873 )
Norm@50keV : 0.134901 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 34.35 using 59 PHA bins.
# Reduced chi-squared = 0.6134 for 56 degrees of freedom
# Null hypothesis probability = 9.900016e-01
Photon flux (15-150 keV) in 1 sec: 3.90261 ( -0.26261 0.26355 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
