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 0.052 sec. to 0.264 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.515526 ( -0.289243 0.316857 )
Norm@50keV : 4.96249E-02 ( -0.00849594 0.00808563 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.80 using 59 PHA bins.
# Reduced chi-squared = 0.9789 for 57 degrees of freedom
# Null hypothesis probability = 5.202372e-01
Photon flux (15-150 keV) in 0.212 sec: 0.597222 ( -0.279627 0.658038 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.40254e-07 ( -2.15663e-08 2.16605e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.052 sec. to 0.264 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.505138 ( -0.400524 0.731149 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 5.00373E-02 ( -0.00778375 0.0409585 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.83 using 59 PHA bins.
# Reduced chi-squared = 0.9969 for 56 degrees of freedom
# Null hypothesis probability = 4.813895e-01
Photon flux (15-150 keV) in 0.212 sec: 5.86152 ( -0.86043 0.86049 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.340 sec. to 0.660 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.878314 ( -0.299732 0.323531 )
Norm@50keV : 1.58363E-02 ( -0.00274569 0.00267849 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.87 using 59 PHA bins.
# Reduced chi-squared = 1.226 for 57 degrees of freedom
# Null hypothesis probability = 1.176912e-01
Photon flux (15-150 keV) in 1 sec: 1.81748 ( -0.30862 0.31115 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.79263e-07 ( -3.03509e-08 3.05247e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.340 sec. to 0.660 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.871354 ( -0.396917 1.19183 )
Epeak [keV] : 9998.85 ( -9998.85 -9998.85 )
Norm@50keV : 1.59414E-02 ( -0.00257423 0.0326926 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.87 using 59 PHA bins.
# Reduced chi-squared = 1.248 for 56 degrees of freedom
# Null hypothesis probability = 1.006486e-01
Photon flux (15-150 keV) in 1 sec: 1.82001 ( -0.32117 0.30841 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.79461e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
