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 -0.020 sec. to 2.956 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.788878 ( -0.304357 0.333927 )
Norm@50keV : 3.10088E-03 ( -0.000555197 0.000537287 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.50 using 59 PHA bins.
# Reduced chi-squared = 0.7808 for 57 degrees of freedom
# Null hypothesis probability = 8.858992e-01
Photon flux (15-150 keV) in 2.976 sec: 0.356536 ( -0.060619 0.061008 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.08359e-07 ( -1.85324e-08 1.86354e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.020 sec. to 2.956 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.781617 ( -0.382729 1.07028 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 3.12305E-03 ( -0.000556881 -0.0031232 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.51 using 59 PHA bins.
# Reduced chi-squared = 0.7949 for 56 degrees of freedom
# Null hypothesis probability = 8.655589e-01
Photon flux (15-150 keV) in 2.976 sec: 0.358239 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.0918e-07 ( -1.94612e-08 1.77059e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.504 sec. to 1.504 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.52736 ( -0.379199 0.434258 )
Norm@50keV : 4.52933E-03 ( -0.00108671 0.00100731 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.94 using 59 PHA bins.
# Reduced chi-squared = 0.7357 for 57 degrees of freedom
# Null hypothesis probability = 9.325174e-01
Photon flux (15-150 keV) in 1 sec: 0.534104 ( -0.105094 0.106327 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.00247e-08 ( -1.13907e-08 1.14184e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.504 sec. to 1.504 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.516865 ( -0.489563 1.32312 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 4.56582E-03 ( -0.00109102 -0.00456661 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.95 using 59 PHA bins.
# Reduced chi-squared = 0.7491 for 56 degrees of freedom
# Null hypothesis probability = 9.182996e-01
Photon flux (15-150 keV) in 1 sec: 0.541876 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 6.00772e-08 ( -1.47854e-08 1.47036e-08 ) ergs/cm2
Time-resolved spectra
