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 6.479 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.45797 ( -0.240963 0.241748 )
Norm@50keV : 9.61085E-03 ( -0.00137126 0.00136929 )
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#Fit statistic : Chi-Squared = 55.28 using 59 PHA bins.
# Reduced chi-squared = 0.9699 for 57 degrees of freedom
# Null hypothesis probability = 5.396809e-01
Photon flux (15-150 keV) in 6.479 sec: 1.18679 ( -0.1787 0.17974 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.9507e-07 ( -8.98644e-08 9.0384e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 6.479 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.791315 ( -0.828675 1.22857 )
Epeak [keV] : 96.6240 ( -34.2025 -96.6244 )
Norm@50keV : 2.00395E-02 ( -0.0113429 0.0541494 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.93 using 59 PHA bins.
# Reduced chi-squared = 0.9631 for 56 degrees of freedom
# Null hypothesis probability = 5.534956e-01
Photon flux (15-150 keV) in 6.479 sec: 1.15230 ( -0.186245 0.18673 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.75477e-07 ( -9.6265e-08 9.55316e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.300 sec. to 1.300 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.60633 ( -0.43931 0.428915 )
Norm@50keV : 1.10960E-02 ( -0.00357739 0.00354772 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.03 using 59 PHA bins.
# Reduced chi-squared = 1.246 for 57 degrees of freedom
# Null hypothesis probability = 1.000946e-01
Photon flux (15-150 keV) in 1 sec: 1.43013 ( -0.450748 0.46236 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03493e-07 ( -3.41568e-08 3.48668e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.300 sec. to 1.300 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 1.84855 ( -2.21592 3.97478 )
Epeak [keV] : 55.8390 ( -11.9835 16.5978 )
Norm@50keV : 0.592651 ( -0.665222 38.6081 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.50 using 59 PHA bins.
# Reduced chi-squared = 1.116 for 56 degrees of freedom
# Null hypothesis probability = 2.563984e-01
Photon flux (15-150 keV) in 1 sec: 1.35004 ( -0.413365 0.4588 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.67721e-08 ( -2.92634e-08 3.36737e-08 ) ergs/cm2
Time-resolved spectra
