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 0.084 sec. to 6.056 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.82046 ( -0.270577 0.254713 )
Norm@50keV : 4.86370E-03 ( -0.000818354 0.000794245 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.14 using 59 PHA bins.
# Reduced chi-squared = 1.038 for 57 degrees of freedom
# Null hypothesis probability = 3.973626e-01
Photon flux (15-150 keV) in 5.972 sec: 0.675633 ( -0.096911 0.096973 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.67276e-07 ( -4.46784e-08 4.55409e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.084 sec. to 6.056 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.55746 ( -0.699755 1.18775 )
Epeak [keV] : 76.5675 ( -76.3549 -76.5674 )
Norm@50keV : 6.77900E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.93 using 59 PHA bins.
# Reduced chi-squared = 1.052 for 56 degrees of freedom
# Null hypothesis probability = 3.687305e-01
Photon flux (15-150 keV) in 5.972 sec: 0.669122 ( -0.10035 0.099786 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.61331e-07 ( -4.96944e-08 4.48939e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.052 sec. to 1.052 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.45682 ( -0.231912 0.23077 )
Norm@50keV : 1.37446E-02 ( -0.00202049 0.00201417 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.89 using 59 PHA bins.
# Reduced chi-squared = 1.121 for 57 degrees of freedom
# Null hypothesis probability = 2.473386e-01
Photon flux (15-150 keV) in 1 sec: 1.69674 ( -0.25191 0.2525 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.3138e-07 ( -2.07533e-08 2.09376e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.052 sec. to 1.052 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.267739 ( -1.06562 1.4537 )
Epeak [keV] : 71.2591 ( -18.0807 164.644 )
Norm@50keV : 5.63819E-02 ( -0.0563855 0.258181 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.19 using 59 PHA bins.
# Reduced chi-squared = 1.075 for 56 degrees of freedom
# Null hypothesis probability = 3.267838e-01
Photon flux (15-150 keV) in 1 sec: 1.63690 ( -0.25958 0.25937 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.21593e-07 ( -2.28992e-08 2.31575e-08 ) ergs/cm2
Time-resolved spectra
