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 -4.784 sec. to 3.280 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.48821 ( -0.112855 0.112611 )
Norm@50keV : 2.30904E-02 ( -0.00153737 0.00153632 )
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#Fit statistic : Chi-Squared = 69.79 using 59 PHA bins.
# Reduced chi-squared = 1.224 for 57 degrees of freedom
# Null hypothesis probability = 1.190037e-01
Photon flux (15-150 keV) in 8.064 sec: 2.87362 ( -0.20316 0.20369 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.77007e-06 ( -1.246e-07 1.24977e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -4.784 sec. to 3.280 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.10945 ( -0.417446 0.471439 )
Epeak [keV] : 128.415 ( -45.4376 -128.415 )
Norm@50keV : 3.48431E-02 ( -0.012308 0.02228 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.51 using 59 PHA bins.
# Reduced chi-squared = 1.206 for 56 degrees of freedom
# Null hypothesis probability = 1.394467e-01
Photon flux (15-150 keV) in 8.064 sec: 2.82580 ( -0.2102 0.21063 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.74369e-06 ( -1.29557e-07 1.29274e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.468 sec. to 1.468 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23742 ( -0.230639 0.236577 )
Norm@50keV : 3.45116E-02 ( -0.00464527 0.00463735 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.49 using 59 PHA bins.
# Reduced chi-squared = 0.7630 for 57 degrees of freedom
# Null hypothesis probability = 9.062566e-01
Photon flux (15-150 keV) in 1 sec: 4.07362 ( -0.58054 0.58217 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.46585e-07 ( -4.92541e-08 4.93647e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.468 sec. to 1.468 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.22937 ( -0.231715 0.238654 )
Epeak [keV] : 9998.89 ( -9999.36 -9999.36 )
Norm@50keV : 3.46024E-02 ( -0.0346706 0.029869 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.50 using 59 PHA bins.
# Reduced chi-squared = 0.7768 for 56 degrees of freedom
# Null hypothesis probability = 8.883861e-01
Photon flux (15-150 keV) in 1 sec: 4.08697 ( -0.64118 0.63191 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.48257e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
