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 0.004 sec. to 0.320 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.20452 ( -0.195473 0.19507 )
Norm@50keV : 5.45680E-02 ( -0.00597822 0.00597635 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.51 using 59 PHA bins.
# Reduced chi-squared = 0.8160 for 57 degrees of freedom
# Null hypothesis probability = 8.380601e-01
Photon flux (15-150 keV) in 0.316 sec: 6.40929 ( -0.71795 0.71915 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.74738e-07 ( -2.15773e-08 2.17008e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.004 sec. to 0.320 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.20007 ( -0.243279 0.564312 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 5.48305E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.52 using 59 PHA bins.
# Reduced chi-squared = 0.8307 for 56 degrees of freedom
# Null hypothesis probability = 8.127764e-01
Photon flux (15-150 keV) in 0.316 sec: 6.43685 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.74992e-07 ( -2.28538e-08 2.23901e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.336 sec. to 0.664 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26773 ( -0.256151 0.258017 )
Norm@50keV : 1.81503E-02 ( -0.00264424 0.00264421 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 68.04 using 59 PHA bins.
# Reduced chi-squared = 1.194 for 57 degrees of freedom
# Null hypothesis probability = 1.503185e-01
Photon flux (15-150 keV) in 1 sec: 2.15305 ( -0.32715 0.32892 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.80834e-07 ( -2.86742e-08 2.88668e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.336 sec. to 0.664 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.07477 ( -0.00834442 0.10594 )
Epeak [keV] : 27.8869 ( )
Norm@50keV : 4.21643E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.88 using 59 PHA bins.
# Reduced chi-squared = 1.194 for 56 degrees of freedom
# Null hypothesis probability = 1.514097e-01
Photon flux (15-150 keV) in 1 sec: 2.13552 ( -0.33622 0.33701 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.79382e-07 ( -2.98135e-08 2.95572e-08 ) ergs/cm2
Time-resolved spectra
