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 0.852 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.795758 ( -0.140615 0.144523 )
Norm@50keV : 3.41811E-02 ( -0.0027168 0.00268913 )
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#Fit statistic : Chi-Squared = 50.99 using 59 PHA bins.
# Reduced chi-squared = 0.8946 for 57 degrees of freedom
# Null hypothesis probability = 6.986248e-01
Photon flux (15-150 keV) in 0.852 sec: 8.17480E-02 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.40964e-07 ( -2.76867e-08 2.78005e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 0.852 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.788235 ( -0.215459 0.332688 )
Epeak [keV] : 9999.12 ( -9999.21 -9999.21 )
Norm@50keV : 3.44242E-02 ( -0.00268666 0.0132685 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.03 using 59 PHA bins.
# Reduced chi-squared = 0.9112 for 56 degrees of freedom
# Null hypothesis probability = 6.630449e-01
Photon flux (15-150 keV) in 0.852 sec: 3.92798 ( -0.30386 0.30414 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.4153e-07 ( -3.48331e-08 3.37016e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.074 sec. to 0.926 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.832446 ( -0.139562 0.14335 )
Norm@50keV : 3.07791E-02 ( -0.00240658 0.00238361 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.93 using 59 PHA bins.
# Reduced chi-squared = 0.9461 for 57 degrees of freedom
# Null hypothesis probability = 5.911627e-01
Photon flux (15-150 keV) in 1 sec: 3.53422 ( -0.27098 0.27205 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.54903e-07 ( -2.84355e-08 2.85481e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.074 sec. to 0.926 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.825204 ( -0.211122 0.30074 )
Epeak [keV] : 9999.28 ( -9999.35 -9999.35 )
Norm@50keV : 3.09909E-02 ( -0.00237706 0.0105885 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.97 using 59 PHA bins.
# Reduced chi-squared = 0.9637 for 56 degrees of freedom
# Null hypothesis probability = 5.521926e-01
Photon flux (15-150 keV) in 1 sec: 3.55181 ( -0.3899 0.35318 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.55656e-07 ( -3.8991e-08 3.74322e-08 ) ergs/cm2
Time-resolved spectra
