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 0.168 sec. to 1.584 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.00086 ( -0.270601 0.249749 )
Norm@50keV : 6.33064E-03 ( -0.00125668 0.00123409 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.12 using 59 PHA bins.
# Reduced chi-squared = 1.142 for 57 degrees of freedom
# Null hypothesis probability = 2.150891e-01
Photon flux (15-150 keV) in 1.416 sec: 0.950033 ( -0.146273 0.146287 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.26654e-08 ( -1.53051e-08 1.58045e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.168 sec. to 1.584 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.996732 ( -1.64204 2.23683 )
Epeak [keV] : 38.7865 ( -5.48576 7.07924 )
Norm@50keV : 0.398283 ( -0.411097 8.6162 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.86 using 59 PHA bins.
# Reduced chi-squared = 0.9439 for 56 degrees of freedom
# Null hypothesis probability = 5.944696e-01
Photon flux (15-150 keV) in 1.416 sec: 0.906039 ( -0.143595 0.144501 ) 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 0.200 sec. to 1.200 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.95892 ( -0.288917 0.265312 )
Norm@50keV : 7.25660E-03 ( -0.00150994 0.00147758 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 76.49 using 59 PHA bins.
# Reduced chi-squared = 1.342 for 57 degrees of freedom
# Null hypothesis probability = 4.342697e-02
Photon flux (15-150 keV) in 1 sec: 1.06851 ( -0.176192 0.17619 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.68021e-08 ( -1.31409e-08 1.35524e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.200 sec. to 1.200 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 1.14801 ( -1.78944 2.54084 )
Epeak [keV] : 40.9998 ( -5.97408 7.65019 )
Norm@50keV : 0.468797 ( -0.48875 13.0433 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.63 using 59 PHA bins.
# Reduced chi-squared = 1.172 for 56 degrees of freedom
# Null hypothesis probability = 1.774627e-01
Photon flux (15-150 keV) in 1 sec: 1.00874 ( -0.175932 0.17694 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
