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 -1.632 sec. to 8.512 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.79814 ( -0.0593986 0.0589687 )
Norm@50keV : 6.72284E-02 ( -0.00216022 0.0021545 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.62 using 59 PHA bins.
# Reduced chi-squared = 0.9232 for 57 degrees of freedom
# Null hypothesis probability = 6.399405e-01
Photon flux (15-150 keV) in 10.14 sec: 9.25775 ( -0.32305 0.32423 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.27709e-06 ( -2.0458e-07 2.04898e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.632 sec. to 8.512 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.69018 ( -0.183057 0.225878 )
Epeak [keV] : 150.793 ( )
Norm@50keV : 7.57532E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.90 using 59 PHA bins.
# Reduced chi-squared = 0.9268 for 56 degrees of freedom
# Null hypothesis probability = 6.307199e-01
Photon flux (15-150 keV) in 10.14 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 6.23316e-06 ( -2.23111e-07 2.22014e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.220 sec. to 0.780 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.51895 ( -0.0588431 0.0586277 )
Norm@50keV : 0.432918 ( -0.0145364 0.0145295 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.27 using 59 PHA bins.
# Reduced chi-squared = 0.9346 for 57 degrees of freedom
# Null hypothesis probability = 6.156731e-01
Photon flux (15-150 keV) in 1 sec: 54.3267 ( -1.95 1.9535 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.09496e-06 ( -1.4557e-07 1.45862e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.220 sec. to 0.780 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.33136 ( -0.206989 0.231958 )
Epeak [keV] : 195.029 ( -78.5271 -195.031 )
Norm@50keV : 0.530316 ( -0.102683 0.146671 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.19 using 59 PHA bins.
# Reduced chi-squared = 0.9141 for 56 degrees of freedom
# Null hypothesis probability = 6.572656e-01
Photon flux (15-150 keV) in 1 sec: 53.8004 ( -2.0369 2.042 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.37219e-06 ( -1.87046e-07 1.83217e-07 ) ergs/cm2
Time-resolved spectra
