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 29.344 sec. to 397.088 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.77359 ( -0.0831377 0.0822206 )
Norm@50keV : 1.16445E-03 ( -5.4578e-05 5.42465e-05 )
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#Fit statistic : Chi-Squared = 42.82 using 59 PHA bins.
# Reduced chi-squared = 0.7512 for 57 degrees of freedom
# Null hypothesis probability = 9.183052e-01
Photon flux (15-150 keV) in 367.7 sec: 0.158853 ( -0.007007 0.00702 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.9466e-06 ( -1.90441e-07 1.91909e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 29.344 sec. to 397.088 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.40443 ( -0.31703 0.343303 )
Epeak [keV] : 75.2479 ( -17.1075 142.59 )
Norm@50keV : 1.82028E-03 ( -0.000566532 0.000917091 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 38.80 using 59 PHA bins.
# Reduced chi-squared = 0.6929 for 56 degrees of freedom
# Null hypothesis probability = 9.612124e-01
Photon flux (15-150 keV) in 367.7 sec: 0.155072 ( -0.007677 0.007683 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.79613e-06 ( -2.27241e-07 2.28659e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 73.724 sec. to 74.724 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.63905 ( -0.39631 0.373457 )
Norm@50keV : 4.39141E-03 ( -0.00106469 0.00103003 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 39.79 using 59 PHA bins.
# Reduced chi-squared = 0.6981 for 57 degrees of freedom
# Null hypothesis probability = 9.595813e-01
Photon flux (15-150 keV) in 1 sec: 0.571377 ( -0.122341 0.122393 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.08931e-08 ( -1.03193e-08 1.06606e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 73.724 sec. to 74.724 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.889359 ( -1.31992 2.43571 )
Epeak [keV] : 68.3723 ( -61.5904 -68.3629 )
Norm@50keV : 1.11276E-02 ( -0.0111331 0.198377 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 39.21 using 59 PHA bins.
# Reduced chi-squared = 0.7002 for 56 degrees of freedom
# Null hypothesis probability = 9.568399e-01
Photon flux (15-150 keV) in 1 sec: 0.555073 ( -0.129403 0.127748 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.82807e-08 ( -1.08896e-08 1.20612e-08 ) ergs/cm2
Time-resolved spectra
