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 -1.304 sec. to 2.972 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.71518 ( -0.314738 0.294775 )
Norm@50keV : 4.67777E-03 ( -0.000881097 0.000850935 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 67.35 using 59 bins.
Reduced chi-squared = 1.18158
# Null hypothesis probability of 1.64e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 4.276 sec: 0.624618 ( -0.102047 0.10212 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.85011e-07 ( -3.57598e-08 3.65318e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.304 sec. to 2.972 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.69842 ( -1.9755 1.25961 )
Epeak [keV] : 840.849 ( -826.61 -826.62 )
Norm@50keV : 4.77525E-03 ( -0.000981027 0.0172159 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 67.35 using 59 bins.
Reduced chi-squared = 1.20268
# Null hypothesis probability of 1.42e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 4.276 sec: 0.624207 ( -0.10421 0.102063 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.84756e-07 ( -3.91234e-08 3.6125e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.152 sec. to 0.848 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.56004 ( -0.39674 0.373015 )
Norm@50keV : 7.33184E-03 ( -0.00179196 0.00175792 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 66.04 using 59 bins.
Reduced chi-squared = 1.1586
# Null hypothesis probability of 1.93e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 0.930918 ( -0.213908 0.214232 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.89334e-08 ( -1.78688e-08 1.83316e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.152 sec. to 0.848 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.0123266 ( -1.82364 3.13305 )
Epeak [keV] : 62.8684 ( -14.6765 -62.7733 )
Norm@50keV : 4.62132E-02 ( -0.0469938 1.61633 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 63.92 using 59 bins.
Reduced chi-squared = 1.14143
# Null hypothesis probability of 2.18e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 0.878142 ( -0.226049 0.224458 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.27581e-08 ( -1.80115e-08 1.96595e-08 ) ergs/cm2
Time-resolved spectra
