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 0.336 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.60425 ( -0.231131 0.219852 )
Norm@50keV : 2.30658E-02 ( -0.00348168 0.00343023 )
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#Fit statistic : Chi-Squared = 59.02 using 59 PHA bins.
# Reduced chi-squared = 1.035 for 57 degrees of freedom
# Null hypothesis probability = 4.015232e-01
Photon flux (15-150 keV) in 0.336 sec: 2.96806 ( -0.42008 0.42022 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.2455e-08 ( -1.15996e-08 1.16785e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 0.336 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.14621 ( -0.4328 0.939046 )
Epeak [keV] : 94.8648 ( )
Norm@50keV : 3.96550E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.03 using 59 PHA bins.
# Reduced chi-squared = 1.036 for 56 degrees of freedom
# Null hypothesis probability = 4.003087e-01
Photon flux (15-150 keV) in 0.336 sec: 2.95217 ( -0.4218 0.4216 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.15583e-08 ( -1.20346e-08 1.19634e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.324 sec. to 0.676 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.51297 ( -0.278506 0.269401 )
Norm@50keV : 9.78945E-03 ( -0.00170895 0.00168871 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.33 using 59 PHA bins.
# Reduced chi-squared = 1.006 for 57 degrees of freedom
# Null hypothesis probability = 4.626793e-01
Photon flux (15-150 keV) in 1 sec: 1.22645 ( -0.20446 0.20464 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.26873e-08 ( -1.74869e-08 1.7774e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.324 sec. to 0.676 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.481047 ( -1.1154 1.50935 )
Epeak [keV] : 72.7570 ( -20.8006 -72.757 )
Norm@50keV : 3.30404E-02 ( -0.0330403 0.153311 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.91 using 59 PHA bins.
# Reduced chi-squared = 0.9805 for 56 degrees of freedom
# Null hypothesis probability = 5.163141e-01
Photon flux (15-150 keV) in 1 sec: 1.18719 ( -0.209815 0.20957 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.71184e-08 ( -1.81167e-08 1.87899e-08 ) ergs/cm2
Time-resolved spectra
