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 -0.008 sec. to 0.312 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.25021 ( -0.212448 0.213026 )
Norm@50keV : 3.79243E-02 ( -0.00476747 0.00475549 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.66 using 59 PHA bins.
# Reduced chi-squared = 0.9764 for 57 degrees of freedom
# Null hypothesis probability = 5.255674e-01
Photon flux (15-150 keV) in 0.32 sec: 4.48561 ( -0.56266 0.56295 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.21462e-07 ( -1.73883e-08 1.75847e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.008 sec. to 0.312 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.04912 ( -0.393681 0.956696 )
Epeak [keV] : 240.147 ( -240.266 -240.266 )
Norm@50keV : 4.79588E-02 ( -0.0479518 0.0968152 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.48 using 59 PHA bins.
# Reduced chi-squared = 0.9907 for 56 degrees of freedom
# Null hypothesis probability = 4.944291e-01
Photon flux (15-150 keV) in 0.32 sec: 4.45732 ( -0.57601 0.57403 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.19627e-07 ( -1.95235e-08 1.82714e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.316 sec. to 0.684 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.29047 ( -0.292141 0.296961 )
Norm@50keV : 1.34318E-02 ( -0.00209979 0.00209324 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.85 using 59 PHA bins.
# Reduced chi-squared = 0.8570 for 57 degrees of freedom
# Null hypothesis probability = 7.703566e-01
Photon flux (15-150 keV) in 1 sec: 1.59969 ( -0.25302 0.25382 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.33058e-07 ( -2.3675e-08 2.40289e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.316 sec. to 0.684 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.2986 ( -0.283461 0.490238 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.34210E-02 ( -0.00210326 0.0140707 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.87 using 59 PHA bins.
# Reduced chi-squared = 0.8726 for 56 degrees of freedom
# Null hypothesis probability = 7.393461e-01
Photon flux (15-150 keV) in 1 sec: 1.59944 ( -0.25333 0.25366 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.34029e-07 ( -3.21276e-08 3.07569e-08 ) ergs/cm2
Time-resolved spectra
