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 4.000 sec. to 291.000 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.7437 ( -0.149564 0.147091 )
Norm@50keV : 1.21036E-03 ( -0.000115319 0.000114355 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.93 using 59 PHA bins.
# Reduced chi-squared = 1.157 for 57 degrees of freedom
# Null hypothesis probability = 1.954873e-01
Photon flux (15-150 keV) in 287 sec: 0.163290 ( -0.014667 0.014687 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.20702e-06 ( -3.13734e-07 3.17187e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 4.000 sec. to 291.000 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.645486 ( -0.733521 0.945849 )
Epeak [keV] : 53.6203 ( -9.16972 25.0981 )
Norm@50keV : 4.99381E-03 ( -0.00305206 0.0123891 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.70 using 59 PHA bins.
# Reduced chi-squared = 1.048 for 56 degrees of freedom
# Null hypothesis probability = 3.766406e-01
Photon flux (15-150 keV) in 287 sec: 0.156940 ( -0.015311 0.015283 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.89015e-06 ( -3.67934e-07 3.77551e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 18.000 sec. to 19.000 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -3.0385 ( -1.3188 0.941901 )
Norm@50keV : 3.63091E-03 ( -0.00269752 0.00357028 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.99 using 59 PHA bins.
# Reduced chi-squared = 1.105 for 57 degrees of freedom
# Null hypothesis probability = 2.727227e-01
Photon flux (15-150 keV) in 1 sec: 1.02723 ( -0.413175 0.41536 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.44294e-08 ( -2.09304e-08 2.5426e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 18.000 sec. to 19.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 9.27893 ( -11.2817 -9.26101 )
Epeak [keV] : 20.3362 ( -4.41508 6.42137 )
Norm@50keV : 2.64348E+07 ( -2.38326e+07 1.31073e+09 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.65 using 59 PHA bins.
# Reduced chi-squared = 1.101 for 56 degrees of freedom
# Null hypothesis probability = 2.810577e-01
Photon flux (15-150 keV) in 1 sec: 0.947239 ( -0.367833 0.422051 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
