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 -21.620 sec. to 127.424 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.52493 ( -0.0370114 0.0370307 )
Norm@50keV : 1.94554E-02 ( -0.000368632 0.000368495 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 37.10 using 59 PHA bins.
# Reduced chi-squared = 0.6509 for 57 degrees of freedom
# Null hypothesis probability = 9.809880e-01
Photon flux (15-150 keV) in 149 sec: 2.44551 ( -0.05497 0.0552 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.73953e-05 ( -5.25375e-07 5.25408e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -21.620 sec. to 127.424 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.52348 ( -0.0362971 0.0384429 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.94840E-02 ( -0.000367567 0.00173075 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 37.18 using 59 PHA bins.
# Reduced chi-squared = 0.6639 for 56 degrees of freedom
# Null hypothesis probability = 9.752480e-01
Photon flux (15-150 keV) in 149 sec: 1.69508 ( -0.09988 0.07489 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.74933e-05 ( -6.28367e-07 4.22224e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.132 sec. to 0.868 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42029 ( -0.15749 0.154429 )
Norm@50keV : 7.96116E-02 ( -0.00698165 0.00693836 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.83 using 59 PHA bins.
# Reduced chi-squared = 0.8391 for 57 degrees of freedom
# Null hypothesis probability = 8.013330e-01
Photon flux (15-150 keV) in 1 sec: 9.74097 ( -0.83903 0.84003 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.66231e-07 ( -7.56574e-08 7.62498e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.132 sec. to 0.868 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.41689 ( -0.158928 0.265441 )
Epeak [keV] : 9999.34 ( -9999.36 -9999.36 )
Norm@50keV : 7.98899E-02 ( -0.0798873 0.0284156 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.85 using 59 PHA bins.
# Reduced chi-squared = 0.8545 for 56 degrees of freedom
# Null hypothesis probability = 7.724016e-01
Photon flux (15-150 keV) in 1 sec: 4.71434 ( -1.32537 1.31697 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
