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 0.912 sec. to 128.524 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.68917 ( -0.130041 0.128198 )
Norm@50keV : 2.20825E-03 ( -0.000168945 0.000167182 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.71 using 59 PHA bins.
# Reduced chi-squared = 0.9949 for 57 degrees of freedom
# Null hypothesis probability = 4.858369e-01
Photon flux (15-150 keV) in 127.6 sec: 0.292191 ( -0.020471 0.020488 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.61156e-06 ( -2.10572e-07 2.13125e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.912 sec. to 128.524 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.59911 ( -0.495087 0.538739 )
Epeak [keV] : 201.156 ( -141.095 -204.539 )
Norm@50keV : 2.47348E-03 ( -0.000489337 0.00233967 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.62 using 59 PHA bins.
# Reduced chi-squared = 1.011 for 56 degrees of freedom
# Null hypothesis probability = 4.517432e-01
Photon flux (15-150 keV) in 127.6 sec: 0.290900 ( -0.021518 0.021422 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.58512e-06 ( -2.57083e-07 2.34106e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 91.968 sec. to 92.968 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.82711 ( -0.206138 0.198028 )
Norm@50keV : 8.25998E-03 ( -0.00108794 0.00106217 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.53 using 59 PHA bins.
# Reduced chi-squared = 1.009 for 57 degrees of freedom
# Null hypothesis probability = 4.553501e-01
Photon flux (15-150 keV) in 1 sec: 1.15046 ( -0.1229 0.1229 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.59924e-08 ( -9.96564e-09 1.01982e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 91.968 sec. to 92.968 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.73243 ( -0.475095 0.809183 )
Epeak [keV] : 119.324 ( )
Norm@50keV : 9.37029E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.48 using 59 PHA bins.
# Reduced chi-squared = 1.026 for 56 degrees of freedom
# Null hypothesis probability = 4.201201e-01
Photon flux (15-150 keV) in 1 sec: 1.14605 ( -0.12707 0.12585 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.50844e-08 ( -1.19669e-08 1.09199e-08 ) ergs/cm2
Time-resolved spectra
