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 -1.140 sec. to 5.352 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.5787 ( -0.0454658 0.0453813 )
Norm@50keV : 7.39963E-02 ( -0.00197593 0.00197582 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 76.37 using 59 PHA bins.
# Reduced chi-squared = 1.340 for 57 degrees of freedom
# Null hypothesis probability = 4.432090e-02
Photon flux (15-150 keV) in 6.492 sec: 9.44752 ( -0.27869 0.27931 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.50535e-06 ( -1.24197e-07 1.24197e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.140 sec. to 5.352 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.902599 ( -0.200912 0.210102 )
Epeak [keV] : 89.1621 ( -9.35093 15.3628 )
Norm@50keV : 0.152299 ( -0.0287345 0.0372382 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 40.05 using 59 PHA bins.
# Reduced chi-squared = 0.7152 for 56 degrees of freedom
# Null hypothesis probability = 9.468694e-01
Photon flux (15-150 keV) in 6.492 sec: 9.09207 ( -0.29291 0.29402 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.37621e-06 ( -1.31595e-07 1.31213e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.060 sec. to 1.060 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26808 ( -0.0671409 0.0672229 )
Norm@50keV : 0.144177 ( -0.0059853 0.00598526 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.19 using 59 PHA bins.
# Reduced chi-squared = 1.267 for 57 degrees of freedom
# Null hypothesis probability = 8.465227e-02
Photon flux (15-150 keV) in 1 sec: 17.1038 ( -0.7386 0.7393 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.43632e-06 ( -6.4175e-08 6.42975e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.060 sec. to 1.060 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.655967 ( -0.281713 0.300529 )
Epeak [keV] : 122.632 ( -23.3173 55.8743 )
Norm@50keV : 0.277369 ( -0.0704392 0.101206 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.45 using 59 PHA bins.
# Reduced chi-squared = 1.026 for 56 degrees of freedom
# Null hypothesis probability = 4.213166e-01
Photon flux (15-150 keV) in 1 sec: 6.05113 ( -1.28509 1.28412 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.40984e-06 ( -6.68586e-08 6.66823e-08 ) ergs/cm2
Time-resolved spectra
