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 0.352 sec. to 170.048 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.20984 ( -0.164698 0.166819 )
Norm@50keV : 1.20715E-03 ( -0.000116202 0.000116202 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.87 using 59 PHA bins.
# Reduced chi-squared = 1.103 for 57 degrees of freedom
# Null hypothesis probability = 2.762008e-01
Photon flux (15-150 keV) in 169.7 sec: 0.141895 ( -0.014071 0.014105 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.07282e-06 ( -2.1979e-07 2.21543e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.352 sec. to 170.048 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.228551 ( -0.728011 0.892295 )
Epeak [keV] : 99.0032 ( -23.5985 116.722 )
Norm@50keV : 3.40927E-03 ( -0.00179738 0.00487008 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.26 using 59 PHA bins.
# Reduced chi-squared = 1.023 for 56 degrees of freedom
# Null hypothesis probability = 4.280169e-01
Photon flux (15-150 keV) in 169.7 sec: 0.135104 ( -0.015091 0.015011 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.95323e-06 ( -2.37134e-07 2.39382e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 31.108 sec. to 32.108 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.74996 ( -0.528982 0.473194 )
Norm@50keV : 6.41770E-03 ( -0.00207966 0.00196657 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.25 using 59 PHA bins.
# Reduced chi-squared = 1.092 for 57 degrees of freedom
# Null hypothesis probability = 2.948783e-01
Photon flux (15-150 keV) in 1 sec: 0.867809 ( -0.23307 0.233131 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.92284e-08 ( -1.89214e-08 1.9763e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 31.108 sec. to 32.108 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.3712 ( -0.89911 2.21798 )
Epeak [keV] : 76.1064 ( -76.1003 -76.1003 )
Norm@50keV : 1.03385E-02 ( -0.0103393 0.168526 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.09 using 59 PHA bins.
# Reduced chi-squared = 1.109 for 56 degrees of freedom
# Null hypothesis probability = 2.681121e-01
Photon flux (15-150 keV) in 1 sec: 0.857348 ( -0.233197 0.237212 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.74315e-08 ( -1.97785e-08 2.05713e-08 ) ergs/cm2
Time-resolved spectra
