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 0.000 sec. to 0.704 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.871042 ( -0.432356 0.484856 )
Norm@50keV : 5.55413E-03 ( -0.00151806 0.00147005 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.90 using 59 PHA bins.
# Reduced chi-squared = 0.9982 for 57 degrees of freedom
# Null hypothesis probability = 4.789418e-01
Photon flux (15-150 keV) in 0.704 sec: 0.637445 ( -0.168771 0.170742 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.43887e-08 ( -1.1668e-08 1.17629e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 0.704 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.102342 ( -1.34968 3.55555 )
Epeak [keV] : 131.178 ( -131.171 -131.171 )
Norm@50keV : 1.40483E-02 ( -0.0140496 0.241909 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.29 using 59 PHA bins.
# Reduced chi-squared = 1.005 for 56 degrees of freedom
# Null hypothesis probability = 4.639199e-01
Photon flux (15-150 keV) in 0.704 sec: 0.611278 ( -0.181219 0.18052 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.27379e-08 ( -1.26776e-08 1.24371e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.148 sec. to 0.852 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.751514 ( -0.489665 0.572986 )
Norm@50keV : 3.96075E-03 ( -0.00128996 0.00121924 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.44 using 59 PHA bins.
# Reduced chi-squared = 0.9025 for 57 degrees of freedom
# Null hypothesis probability = 6.827511e-01
Photon flux (15-150 keV) in 1 sec: 0.456228 ( -0.135662 0.138454 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.72596e-08 ( -1.34648e-08 1.35427e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.148 sec. to 0.852 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.535785 ( -1.71288 3.85862 )
Epeak [keV] : 126.719 ( -126.683 -126.683 )
Norm@50keV : 1.23244E-02 ( -0.0123328 0.842291 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.81 using 59 PHA bins.
# Reduced chi-squared = 0.9074 for 56 degrees of freedom
# Null hypothesis probability = 6.709195e-01
Photon flux (15-150 keV) in 1 sec: 0.429913 ( -0.148389 0.149521 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.53618e-08 ( -1.4873e-08 1.4361e-08 ) ergs/cm2
Time-resolved spectra
