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 -2.504 sec. to 3.896 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.40285 ( -0.364618 0.316967 )
Norm@50keV : 1.24363E-03 ( -0.000345836 0.0003488 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.60 using 59 PHA bins.
# Reduced chi-squared = 1.291 for 57 degrees of freedom
# Null hypothesis probability = 6.864064e-02
Photon flux (15-150 keV) in 6.4 sec: 0.230504 ( -0.039349 0.039424 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.76858e-08 ( -1.68513e-08 1.79235e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -2.504 sec. to 3.896 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.424057 ( -1.79331 2.97302 )
Epeak [keV] : 29.3726 ( -6.112 6.09983 )
Norm@50keV : 8.48896E-02 ( -0.105401 7.77763 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.64 using 59 PHA bins.
# Reduced chi-squared = 1.172 for 56 degrees of freedom
# Null hypothesis probability = 1.772524e-01
Photon flux (15-150 keV) in 6.4 sec: 0.224847 ( -0.037723 0.037979 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.70304e-08 ( -1.2864e-08 1.46372e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.196 sec. to 2.196 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.45752 ( -0.649458 0.52224 )
Norm@50keV : 1.78545E-03 ( -0.000833327 0.000873598 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.01 using 59 PHA bins.
# Reduced chi-squared = 0.9301 for 57 degrees of freedom
# Null hypothesis probability = 6.253061e-01
Photon flux (15-150 keV) in 1 sec: 0.341837 ( -0.098294 0.098801 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.76555e-08 ( -6.29624e-09 7.06857e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.196 sec. to 2.196 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 2.08521 ( -2.92824 -0.872542 )
Epeak [keV] : 25.7262 ( -25.4187 9.00788 )
Norm@50keV : 3.09049 ( -3.02745 3.37487e+06 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.79 using 59 PHA bins.
# Reduced chi-squared = 0.8890 for 56 degrees of freedom
# Null hypothesis probability = 7.077506e-01
Photon flux (15-150 keV) in 1 sec: 0.334891 ( -0.092244 0.09326 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
