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 0.000 sec. to 1.000 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.02119 ( -0.469111 0.415881 )
Norm@50keV : 5.02316E-03 ( -0.00156132 0.00148895 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.95 using 59 PHA bins.
# Reduced chi-squared = 1.069 for 57 degrees of freedom
# Null hypothesis probability = 3.358210e-01
Photon flux (15-150 keV) in 1 sec: 0.760968 ( -0.177134 0.177144 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.63874e-08 ( -1.29502e-08 1.356e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.47694 ( -0.652528 2.99415 )
Epeak [keV] : 37.0419 ( )
Norm@50keV : 1.08332E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.77 using 59 PHA bins.
# Reduced chi-squared = 1.085 for 56 degrees of freedom
# Null hypothesis probability = 3.082888e-01
Photon flux (15-150 keV) in 1 sec: 0.749071 ( -0.18247 0.182948 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.02119 ( -0.469111 0.415881 )
Norm@50keV : 5.02316E-03 ( -0.00156132 0.00148895 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.95 using 59 PHA bins.
# Reduced chi-squared = 1.069 for 57 degrees of freedom
# Null hypothesis probability = 3.358210e-01
Photon flux (15-150 keV) in 1 sec: 0.760968 ( -0.177134 0.177144 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.63874e-08 ( -1.29502e-08 1.356e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.47694 ( -0.653454 2.99415 )
Epeak [keV] : 37.0419 ( )
Norm@50keV : 1.08332E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.77 using 59 PHA bins.
# Reduced chi-squared = 1.085 for 56 degrees of freedom
# Null hypothesis probability = 3.082888e-01
Photon flux (15-150 keV) in 1 sec: 0.749071 ( -0.18247 0.182948 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
