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 -0.364 sec. to 0.796 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.50354 ( -0.289525 0.289473 )
Norm@50keV : 1.29155E-02 ( -0.00205451 0.0020439 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.39 using 59 PHA bins.
# Reduced chi-squared = 1.182 for 57 degrees of freedom
# Null hypothesis probability = 1.633144e-01
Photon flux (15-150 keV) in 1.16 sec: 1.61394 ( -0.26622 0.26733 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.42062e-07 ( -2.4326e-08 2.44473e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.364 sec. to 0.796 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.51789 ( -0.276422 0.307599 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.29286E-02 ( -0.00204851 0.00871411 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.41 using 59 PHA bins.
# Reduced chi-squared = 1.204 for 56 degrees of freedom
# Null hypothesis probability = 1.412953e-01
Photon flux (15-150 keV) in 1.16 sec: 0.847367 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 8.37853e-08 ( -3.80262e-08 2.17646e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.208 sec. to 0.792 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.46916 ( -0.305271 0.306643 )
Norm@50keV : 1.34529E-02 ( -0.00223013 0.00222174 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.84 using 59 PHA bins.
# Reduced chi-squared = 0.9973 for 57 degrees of freedom
# Null hypothesis probability = 4.809236e-01
Photon flux (15-150 keV) in 1 sec: 1.66595 ( -0.28814 0.28949 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.28307e-07 ( -2.30018e-08 2.31154e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.208 sec. to 0.792 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.48447 ( -0.291489 0.510708 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.33871E-02 ( -0.00222605 0.0095512 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.87 using 59 PHA bins.
# Reduced chi-squared = 1.016 for 56 degrees of freedom
# Null hypothesis probability = 4.424366e-01
Photon flux (15-150 keV) in 1 sec: 0.825736 ( -0.439486 0.673284 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.11197e-08 ( -3.57004e-08 2.14673e-08 ) ergs/cm2
Time-resolved spectra
