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 -15.200 sec. to 96.800 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.960998 ( -0.0294516 0.0296052 )
Norm@50keV : 1.26088E-02 ( -0.000209253 0.00020834 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 40.95 using 59 PHA bins.
# Reduced chi-squared = 0.7185 for 57 degrees of freedom
# Null hypothesis probability = 9.461659e-01
Photon flux (15-150 keV) in 112 sec: 1.44914 ( -0.02466 0.02475 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.54888e-05 ( -2.3572e-07 2.36089e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -15.200 sec. to 96.800 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.955654 ( -0.0289528 0.0310547 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.26685E-02 ( -0.000198012 0.00119227 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.02 using 59 PHA bins.
# Reduced chi-squared = 0.7326 for 56 degrees of freedom
# Null hypothesis probability = 9.333062e-01
Photon flux (15-150 keV) in 112 sec: 1.44846 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.54921e-05 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 8.300 sec. to 9.300 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.876931 ( -0.0768803 0.0776683 )
Norm@50keV : 5.43900E-02 ( -0.00231502 0.00230877 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.78 using 59 PHA bins.
# Reduced chi-squared = 1.189 for 57 degrees of freedom
# Null hypothesis probability = 1.553271e-01
Photon flux (15-150 keV) in 1 sec: 6.24220 ( -0.26496 0.26515 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.16013e-07 ( -2.92131e-08 2.93142e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 8.300 sec. to 9.300 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.870958 ( -0.0770835 0.0786195 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 5.47553E-02 ( -0.0022932 0.0181055 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.78 using 59 PHA bins.
# Reduced chi-squared = 1.210 for 56 degrees of freedom
# Null hypothesis probability = 1.344020e-01
Photon flux (15-150 keV) in 1 sec: 6.24163 ( -0.27017 0.26434 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.16042e-07 ( -2.84579e-08 2.65125e-08 ) ergs/cm2
Time-resolved spectra
