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 -235.816 sec. to 132.184 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.4828 ( -0.0903864 0.0904218 )
Norm@50keV : 2.19363E-03 ( -0.000111705 0.000111694 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.70 using 59 PHA bins.
# Reduced chi-squared = 1.047 for 57 degrees of freedom
# Null hypothesis probability = 3.779412e-01
Photon flux (15-150 keV) in 368 sec: 0.272610 ( -0.015089 0.015142 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.68101e-06 ( -4.1145e-07 4.12521e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -235.816 sec. to 132.184 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.18599 ( -0.331217 0.38423 )
Epeak [keV] : 150.080 ( -58.6749 -150.08 )
Norm@50keV : 3.01663E-03 ( -0.000872158 0.00148979 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.69 using 59 PHA bins.
# Reduced chi-squared = 1.030 for 56 degrees of freedom
# Null hypothesis probability = 4.126975e-01
Photon flux (15-150 keV) in 368 sec: 0.268058 ( -0.015975 0.016056 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.56358e-06 ( -4.3902e-07 4.37118e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -36.316 sec. to -35.316 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.900204 ( -0.401352 0.457586 )
Norm@50keV : 1.04834E-02 ( -0.00276643 0.00259711 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.70 using 59 PHA bins.
# Reduced chi-squared = 0.9947 for 57 degrees of freedom
# Null hypothesis probability = 4.863158e-01
Photon flux (15-150 keV) in 1 sec: 1.20325 ( -0.303284 0.30945 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.17655e-07 ( -2.59823e-08 2.59601e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -36.316 sec. to -35.316 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.892986 ( -0.471619 1.68589 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 1.05516E-02 ( -0.00277123 -0.010552 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.70 using 59 PHA bins.
# Reduced chi-squared = 1.013 for 56 degrees of freedom
# Null hypothesis probability = 4.486228e-01
Photon flux (15-150 keV) in 1 sec: 1.20289 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.17706e-07 ( -2.67168e-08 2.52492e-08 ) ergs/cm2
Time-resolved spectra
