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 -0.672 sec. to 15.972 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.27144 ( -0.149756 0.150421 )
Norm@50keV : 6.38708E-03 ( -0.000510119 0.00050991 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.80 using 59 PHA bins.
# Reduced chi-squared = 1.172 for 57 degrees of freedom
# Null hypothesis probability = 1.758210e-01
Photon flux (15-150 keV) in 16.64 sec: 0.758138 ( -0.062639 0.062832 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.05787e-06 ( -9.48131e-08 9.56422e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.672 sec. to 15.972 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.2673 ( -0.150836 0.152385 )
Epeak [keV] : 9998.76 ( -9998.99 -9998.99 )
Norm@50keV : 6.41484E-03 ( -0.00641482 0.00438226 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.80 using 59 PHA bins.
# Reduced chi-squared = 1.193 for 56 degrees of freedom
# Null hypothesis probability = 1.529744e-01
Photon flux (15-150 keV) in 16.64 sec: 0.757974 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.06285e-06 ( -1.17959e-07 8.14293e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 7.228 sec. to 8.228 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.28604 ( -0.230203 0.2303 )
Norm@50keV : 1.60441E-02 ( -0.00227505 0.0022705 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.68 using 59 PHA bins.
# Reduced chi-squared = 0.8716 for 57 degrees of freedom
# Null hypothesis probability = 7.435466e-01
Photon flux (15-150 keV) in 1 sec: 1.90929 ( -0.27144 0.27178 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.59107e-07 ( -2.51424e-08 2.54668e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 7.228 sec. to 8.228 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.0950373 ( -1.07853 1.49459 )
Epeak [keV] : 80.2209 ( -21.6201 237.392 )
Norm@50keV : 6.36741E-02 ( -0.0636741 0.285773 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.06 using 59 PHA bins.
# Reduced chi-squared = 0.8226 for 56 degrees of freedom
# Null hypothesis probability = 8.256105e-01
Photon flux (15-150 keV) in 1 sec: 1.82998 ( -0.28475 0.28286 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.51417e-08 ( -4.8258e-08 8.29491e-09 ) ergs/cm2
Time-resolved spectra
