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 0.000 sec. to 7.824 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.05874 ( -0.364644 0.390199 )
Norm@50keV : 9.84124E-03 ( -0.00230339 0.00226739 )
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#Fit statistic : Chi-Squared = 54.85 using 59 PHA bins.
# Reduced chi-squared = 0.9624 for 57 degrees of freedom
# Null hypothesis probability = 5.559899e-01
Photon flux (15-150 keV) in 7.824 sec: 1.13732 ( -0.272072 0.2789 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.16051e-07 ( -1.82999e-07 1.83647e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 7.824 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: 1.6965 ( -2.36687 5.62386 )
Epeak [keV] : 80.7036 ( -17.0895 113.44 )
Norm@50keV : 0.129578 ( -0.130637 12.3317 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.58 using 59 PHA bins.
# Reduced chi-squared = 0.9032 for 56 degrees of freedom
# Null hypothesis probability = 6.794616e-01
Photon flux (15-150 keV) in 7.824 sec: 0.986664 ( -0.291102 0.302286 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.27309e-07 ( -2.01366e-07 2.05363e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 3.500 sec. to 4.500 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.515155 ( -0.90442 0.515155 )
Norm@50keV : 9.88590E-03 ( -0.00720468 0.00661275 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.91 using 59 PHA bins.
# Reduced chi-squared = 1.174 for 57 degrees of freedom
# Null hypothesis probability = 1.734910e-01
Photon flux (15-150 keV) in 1 sec: 1.16798 ( -1.16798 0.72732 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.31817e-07 ( -6.56121e-08 6.56343e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 3.500 sec. to 4.500 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.768697 ( -0.811707 -0.811707 )
Epeak [keV] : 148.455 ( -143.165 -143.165 )
Norm@50keV : 2.80525E-02 ( -0.031109 110.918 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.52 using 59 PHA bins.
# Reduced chi-squared = 1.188 for 56 degrees of freedom
# Null hypothesis probability = 1.585994e-01
Photon flux (15-150 keV) in 1 sec: 1.09589 ( -0.6285 0.74064 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.26579e-07 ( -7.47587e-08 6.86346e-08 ) ergs/cm2
Time-resolved spectra
