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 -0.708 sec. to 102.520 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.53208 ( -0.0340019 0.0340119 )
Norm@50keV : 2.26984E-02 ( -0.000414694 0.000414604 )
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#Fit statistic : Chi-Squared = 56.88 using 59 PHA bins.
# Reduced chi-squared = 0.9980 for 57 degrees of freedom
# Null hypothesis probability = 4.793899e-01
Photon flux (15-150 keV) in 103.2 sec: 2.85889 ( -0.06147 0.06168 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.21131e-05 ( -4.07082e-07 4.0751e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.708 sec. to 102.520 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.24149 ( -0.137861 0.142036 )
Epeak [keV] : 152.785 ( -31.3442 81.407 )
Norm@50keV : 3.02722E-02 ( -0.00377682 0.00444385 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.59 using 59 PHA bins.
# Reduced chi-squared = 0.7785 for 56 degrees of freedom
# Null hypothesis probability = 8.864212e-01
Photon flux (15-150 keV) in 103.2 sec: 2.78885 ( -0.0684 0.06884 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.17891e-05 ( -4.36093e-07 4.35762e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.096 sec. to 0.904 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.30585 ( -0.0455435 0.0455528 )
Norm@50keV : 0.595633 ( -0.0154208 0.0154186 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.27 using 59 PHA bins.
# Reduced chi-squared = 1.005 for 57 degrees of freedom
# Null hypothesis probability = 4.650168e-01
Photon flux (15-150 keV) in 1 sec: 2.79531 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 5.87828e-06 ( -1.60861e-07 1.61067e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.096 sec. to 0.904 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.984222 ( -0.183783 0.191398 )
Epeak [keV] : 183.397 ( -47.1194 156.988 )
Norm@50keV : 0.825770 ( -0.137422 0.171855 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.11 using 59 PHA bins.
# Reduced chi-squared = 0.8591 for 56 degrees of freedom
# Null hypothesis probability = 7.642037e-01
Photon flux (15-150 keV) in 1 sec: 69.9227 ( -2.0775 2.0831 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.80858e-06 ( -1.67659e-07 1.67274e-07 ) ergs/cm2
Time-resolved spectra
