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 -8.864 sec. to 0.880 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.47594 ( -0.0693829 0.0692759 )
Norm@50keV : 1.98277E-02 ( -0.000739104 0.000738696 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 61.17 using 59 bins.
Reduced chi-squared = 1.07316
# Null hypothesis probability of 3.29e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 9.744 sec: 2.45966 ( -0.09793 0.09827 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.84047e-06 ( -7.38294e-08 7.40422e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -8.864 sec. to 0.880 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42588 ( -0.0941255 0.271109 )
Epeak [keV] : 563.601 ( -994.385 -994.385 )
Norm@50keV : 2.09393E-02 ( -0.00129308 0.00666427 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 61.25 using 59 bins.
Reduced chi-squared = 1.09375
# Null hypothesis probability of 2.93e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 9.744 sec: 2.45650 ( -0.10621 0.10101 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.83648e-06 ( -7.94182e-08 7.7146e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -8.520 sec. to -7.520 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.5634 ( -0.127552 0.126402 )
Norm@50keV : 3.23162E-02 ( -0.00240035 0.00238945 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 55.60 using 59 bins.
Reduced chi-squared = 0.975439
# Null hypothesis probability of 5.28e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 4.10720 ( -0.30493 0.30549 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.03697e-07 ( -2.42432e-08 2.43983e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -8.520 sec. to -7.520 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.56117 ( -0.198917 0.444341 )
Epeak [keV] : 9984.86 ( -9955.86 -9955.86 )
Norm@50keV : 3.24023E-02 ( -0.0151158 0.0258679 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 55.60 using 59 bins.
Reduced chi-squared = 0.992857
# Null hypothesis probability of 4.90e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 4.10436 ( -0.3023 0.30752 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.03235e-07 ( -2.59988e-08 2.46866e-08 ) ergs/cm2
Time-resolved spectra
