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 -1.200 sec. to 13.548 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.8137 ( -0.18285 0.176925 )
Norm@50keV : 3.42799E-03 ( -0.000388214 0.000380674 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.15 using 59 PHA bins.
# Reduced chi-squared = 0.7220 for 57 degrees of freedom
# Null hypothesis probability = 9.435459e-01
Photon flux (15-150 keV) in 14.75 sec: 0.474927 ( -0.045967 0.04599 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.65352e-07 ( -5.29774e-08 5.38446e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.200 sec. to 13.548 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.73731 ( -0.63565 0.778326 )
Epeak [keV] : 148.485 ( -153.305 -153.317 )
Norm@50keV : 3.78739E-03 ( -0.00200988 0.0066049 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.12 using 59 PHA bins.
# Reduced chi-squared = 0.7343 for 56 degrees of freedom
# Null hypothesis probability = 9.318330e-01
Photon flux (15-150 keV) in 14.75 sec: 0.473461 ( -0.047963 0.047057 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.61405e-07 ( -6.48696e-08 5.69794e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.184 sec. to 1.184 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.57664 ( -0.357902 0.344453 )
Norm@50keV : 6.75070E-03 ( -0.00147938 0.00144931 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.24 using 59 PHA bins.
# Reduced chi-squared = 0.7761 for 57 degrees of freedom
# Null hypothesis probability = 8.915194e-01
Photon flux (15-150 keV) in 1 sec: 0.861364 ( -0.17563 0.175826 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.33286e-08 ( -1.47327e-08 1.51082e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.184 sec. to 1.184 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.978177 ( -0.907957 1.02667 )
Epeak [keV] : 79.3276 ( )
Norm@50keV : 1.41796E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.62 using 59 PHA bins.
# Reduced chi-squared = 0.7790 for 56 degrees of freedom
# Null hypothesis probability = 8.857956e-01
Photon flux (15-150 keV) in 1 sec: 0.843040 ( -0.180359 0.18023 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.00095e-08 ( -1.63388e-08 1.66931e-08 ) ergs/cm2
Time-resolved spectra
