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 -0.436 sec. to 52.232 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.81609 ( -0.149863 0.145432 )
Norm@50keV : 1.73976E-03 ( -0.000166159 0.000163875 )
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#Fit statistic : Chi-Squared = 65.68 using 59 PHA bins.
# Reduced chi-squared = 1.152 for 57 degrees of freedom
# Null hypothesis probability = 2.014012e-01
Photon flux (15-150 keV) in 52.67 sec: 0.241260 ( -0.019775 0.019782 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.43284e-07 ( -8.10407e-08 8.2359e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.436 sec. to 52.232 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.983158 ( -0.631421 0.7553 )
Epeak [keV] : 52.6785 ( -9.96112 33.9666 )
Norm@50keV : 5.11702E-03 ( -0.00281918 0.0085548 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.35 using 59 PHA bins.
# Reduced chi-squared = 1.078 for 56 degrees of freedom
# Null hypothesis probability = 3.213758e-01
Photon flux (15-150 keV) in 52.67 sec: 0.233034 ( -0.020654 0.020669 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.74665e-07 ( -9.14093e-08 9.53032e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.700 sec. to 1.700 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.49564 ( -0.189272 0.186697 )
Norm@50keV : 1.16832E-02 ( -0.00133545 0.00132233 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.02 using 59 PHA bins.
# Reduced chi-squared = 1.070 for 57 degrees of freedom
# Null hypothesis probability = 3.336298e-01
Photon flux (15-150 keV) in 1 sec: 1.45686 ( -0.15888 0.15895 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.10928e-07 ( -1.39574e-08 1.41238e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.700 sec. to 1.700 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.37992 ( -0.72615 0.68182 )
Epeak [keV] : 246.342 ( -255.185 -255.185 )
Norm@50keV : 1.34492E-02 ( -0.00563135 0.0167295 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.92 using 59 PHA bins.
# Reduced chi-squared = 1.088 for 56 degrees of freedom
# Null hypothesis probability = 3.034442e-01
Photon flux (15-150 keV) in 1 sec: 1.45125 ( -0.16148 0.16129 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.09845e-07 ( -1.51995e-08 1.48819e-08 ) ergs/cm2
Time-resolved spectra
