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 -5.488 sec. to 130.568 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42713 ( -0.0302075 0.030278 )
Norm@50keV : 1.33772E-02 ( -0.000214991 0.000214654 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 36.02 using 59 PHA bins.
# Reduced chi-squared = 0.6319 for 57 degrees of freedom
# Null hypothesis probability = 9.865024e-01
Photon flux (15-150 keV) in 136.1 sec: 1.63944 ( -0.03137 0.0315 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.74996e-05 ( -2.73852e-07 2.74109e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -5.488 sec. to 130.568 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42261 ( -0.0312984 0.0299575 )
Epeak [keV] : 9997.85 ( -9992.58 -9992.58 )
Norm@50keV : 1.34423E-02 ( -0.0002116 0.00210198 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 36.01 using 59 PHA bins.
# Reduced chi-squared = 0.6430 for 56 degrees of freedom
# Null hypothesis probability = 9.826412e-01
Photon flux (15-150 keV) in 136.1 sec: 1.63496 ( -0.03672 0.01808 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.74682e-05 ( -2.89153e-07 2.85098e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 2.580 sec. to 3.580 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.09646 ( -0.0748746 0.075028 )
Norm@50keV : 8.02229E-02 ( -0.00345279 0.00345226 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.28 using 59 PHA bins.
# Reduced chi-squared = 0.9347 for 57 degrees of freedom
# Null hypothesis probability = 6.155339e-01
Photon flux (15-150 keV) in 1 sec: 9.30215 ( -0.40928 0.40956 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.39789e-07 ( -4.03046e-08 4.04488e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.580 sec. to 3.580 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.70663 ( -0.29027 0.310236 )
Epeak [keV] : 191.833 ( -60.0288 345.224 )
Norm@50keV : 0.119514 ( -0.0299849 0.0428076 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.89 using 59 PHA bins.
# Reduced chi-squared = 0.8551 for 56 degrees of freedom
# Null hypothesis probability = 7.713113e-01
Photon flux (15-150 keV) in 1 sec: 2.30950 ( -0.68565 0.5788 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.54333e-07 ( -3.11757e-08 2.55003e-08 ) ergs/cm2
Time-resolved spectra
