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 0.020 sec. to 106.756 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.31688 ( -0.643359 0.633924 )
Norm@50keV : 3.12851E-04 ( -0.000113804 0.000113475 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.92 using 59 PHA bins.
# Reduced chi-squared = 0.7354 for 57 degrees of freedom
# Null hypothesis probability = 9.328232e-01
Photon flux (15-150 keV) in 106.7 sec: 3.74425E-02 ( -0.0138701 0.0139847 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.28575e-07 ( -1.29125e-07 1.32493e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.020 sec. to 106.756 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.302803 ( -2.13093 8.1274 )
Epeak [keV] : 82.0643 ( -63.8362 -82.0209 )
Norm@50keV : 1.58901E-03 ( -0.00160606 0.719823 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.01 using 59 PHA bins.
# Reduced chi-squared = 0.7323 for 56 degrees of freedom
# Null hypothesis probability = 9.335166e-01
Photon flux (15-150 keV) in 106.7 sec: 3.44888E-02 ( -0.0155142 0.0150745 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.10195e-07 ( -1.26771e-07 1.36575e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.026 sec. to 0.974 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.902895 ( -0.357761 0.385233 )
Norm@50keV : 8.55758E-03 ( -0.00175572 0.00170538 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.57 using 59 PHA bins.
# Reduced chi-squared = 1.098 for 57 degrees of freedom
# Null hypothesis probability = 2.853009e-01
Photon flux (15-150 keV) in 1 sec: 0.982235 ( -0.19792 0.199815 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.59423e-08 ( -1.92168e-08 1.93075e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.026 sec. to 0.974 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.899939 ( -0.358095 0.396643 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 8.61831E-03 ( -0.00163962 0.0323688 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.57 using 59 PHA bins.
# Reduced chi-squared = 1.117 for 56 degrees of freedom
# Null hypothesis probability = 2.545671e-01
Photon flux (15-150 keV) in 1 sec: 0.983113 ( -0.210584 0.197597 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.39053e-09 ( 0 0 ) ergs/cm2
Time-resolved spectra
