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 -0.212 sec. to 7.960 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.93172 ( -0.176372 0.169183 )
Norm@50keV : 4.47774E-03 ( -0.000497224 0.000486142 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.22 using 59 PHA bins.
# Reduced chi-squared = 0.9162 for 57 degrees of freedom
# Null hypothesis probability = 6.545041e-01
Photon flux (15-150 keV) in 8.172 sec: 0.651472 ( -0.057223 0.057247 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.36634e-07 ( -3.57506e-08 3.64772e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.212 sec. to 7.960 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.88966 ( -0.354955 0.697873 )
Epeak [keV] : 112.048 ( )
Norm@50keV : 4.73206E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.21 using 59 PHA bins.
# Reduced chi-squared = 0.9323 for 56 degrees of freedom
# Null hypothesis probability = 6.190456e-01
Photon flux (15-150 keV) in 8.172 sec: 0.650250 ( -0.060152 0.058299 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.35018e-07 ( -4.29744e-08 3.14937e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.120 sec. to 1.120 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.69298 ( -0.166368 0.161676 )
Norm@50keV : 1.43039E-02 ( -0.00151961 0.00149826 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.85 using 59 PHA bins.
# Reduced chi-squared = 1.103 for 57 degrees of freedom
# Null hypothesis probability = 2.767257e-01
Photon flux (15-150 keV) in 1 sec: 1.89516 ( -0.18078 0.18082 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.32532e-07 ( -1.47334e-08 1.49062e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.120 sec. to 1.120 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.17756 ( -0.584931 0.720243 )
Epeak [keV] : 73.4055 ( -20.9404 -73.4056 )
Norm@50keV : 2.73113E-02 ( -0.0137849 0.0389376 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.90 using 59 PHA bins.
# Reduced chi-squared = 1.087 for 56 degrees of freedom
# Null hypothesis probability = 3.042068e-01
Photon flux (15-150 keV) in 1 sec: 1.86533 ( -0.18453 0.18445 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.0665e-07 ( -1.85918e-08 1.60883e-08 ) ergs/cm2
Time-resolved spectra
