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 -0.244 sec. to 36.512 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.97205 ( -0.0256071 0.0256499 )
Norm@50keV : 8.88207E-02 ( -0.00119416 0.00119252 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.77 using 59 PHA bins.
# Reduced chi-squared = 0.7854 for 57 degrees of freedom
# Null hypothesis probability = 8.801782e-01
Photon flux (15-150 keV) in 36.76 sec: 13.1557 ( -0.2603 0.2623 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.00764e-05 ( -4.1334e-07 4.12793e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.244 sec. to 36.512 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.90825 ( -0.100381 0.102503 )
Epeak [keV] : 88.3366 ( -24.6494 -88.3366 )
Norm@50keV : 9.42692E-02 ( -0.00443166 0.00919912 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.61 using 59 PHA bins.
# Reduced chi-squared = 0.7787 for 56 degrees of freedom
# Null hypothesis probability = 8.861206e-01
Photon flux (15-150 keV) in 36.76 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 2.99361e-05 ( -4.63731e-07 4.65404e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 12.612 sec. to 13.612 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.87901 ( -0.0310366 0.0310338 )
Norm@50keV : 0.925161 ( -0.0147612 0.0147553 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.73 using 59 PHA bins.
# Reduced chi-squared = 0.7496 for 57 degrees of freedom
# Null hypothesis probability = 9.199135e-01
Photon flux (15-150 keV) in 1 sec: 131.611 ( -2.854 2.872 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.50629e-06 ( -1.35624e-07 1.35625e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 12.612 sec. to 13.612 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.85975 ( -0.0478875 0.119846 )
Epeak [keV] : 430.784 ( )
Norm@50keV : 0.942773 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.65 using 59 PHA bins.
# Reduced chi-squared = 0.7616 for 56 degrees of freedom
# Null hypothesis probability = 9.056243e-01
Photon flux (15-150 keV) in 1 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 8.07477e-06 ( -2.54171e-07 1.45231e-06 ) ergs/cm2
Time-resolved spectra
