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 -15.232 sec. to 64.768 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.45827 ( -0.0575513 0.0575992 )
Norm@50keV : 8.27748E-03 ( -0.000264413 0.00026441 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.36 using 59 PHA bins.
# Reduced chi-squared = 1.147 for 57 degrees of freedom
# Null hypothesis probability = 2.091905e-01
Photon flux (15-150 keV) in 80 sec: 1.02222 ( -0.036004 0.03611 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.32805e-06 ( -2.1145e-07 2.11685e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -15.232 sec. to 64.768 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.03482 ( -0.234054 0.246729 )
Epeak [keV] : 127.708 ( -27.4131 84.3873 )
Norm@50keV : 1.28618E-02 ( -0.002713 0.00364041 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.44 using 59 PHA bins.
# Reduced chi-squared = 0.9899 for 56 degrees of freedom
# Null hypothesis probability = 4.961602e-01
Photon flux (15-150 keV) in 80 sec: 0.994243 ( -0.03874 0.038947 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.18842e-06 ( -2.26589e-07 2.26034e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 8.268 sec. to 9.268 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.21583 ( -0.183058 0.185889 )
Norm@50keV : 2.87879E-02 ( -0.00300973 0.00299931 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.23 using 59 PHA bins.
# Reduced chi-squared = 0.8987 for 57 degrees of freedom
# Null hypothesis probability = 6.904280e-01
Photon flux (15-150 keV) in 1 sec: 3.38686 ( -0.37412 0.37529 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.9081e-07 ( -3.21257e-08 3.21956e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 8.268 sec. to 9.268 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.21137 ( -0.22433 0.496946 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 2.89240E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.24 using 59 PHA bins.
# Reduced chi-squared = 0.9150 for 56 degrees of freedom
# Null hypothesis probability = 6.553400e-01
Photon flux (15-150 keV) in 1 sec: 3.39810 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 2.90743e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
