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 -0.956 sec. to 7.448 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.78303 ( -0.13936 0.136265 )
Norm@50keV : 6.04657E-03 ( -0.000523054 0.000516326 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.93 using 59 PHA bins.
# Reduced chi-squared = 1.280 for 57 degrees of freedom
# Null hypothesis probability = 7.586639e-02
Photon flux (15-150 keV) in 8.404 sec: 0.827828 ( -0.063323 0.06336 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.68194e-07 ( -4.12945e-08 4.18125e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.956 sec. to 7.448 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.43096 ( -0.485585 0.658973 )
Epeak [keV] : 70.8366 ( -22.1638 -70.8365 )
Norm@50keV : 9.52351E-03 ( -0.00387189 0.0126831 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.82 using 59 PHA bins.
# Reduced chi-squared = 1.282 for 56 degrees of freedom
# Null hypothesis probability = 7.564142e-02
Photon flux (15-150 keV) in 8.404 sec: 0.815628 ( -0.066549 0.066296 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.50554e-07 ( -5.01057e-08 5.011e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.308 sec. to 0.692 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.78161 ( -0.209344 0.200549 )
Norm@50keV : 1.17766E-02 ( -0.00161265 0.0015778 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.47 using 59 PHA bins.
# Reduced chi-squared = 1.096 for 57 degrees of freedom
# Null hypothesis probability = 2.880302e-01
Photon flux (15-150 keV) in 1 sec: 1.61145 ( -0.18495 0.18497 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.08513e-07 ( -1.50478e-08 1.53495e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.308 sec. to 0.692 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.3706 ( -0.796918 1.1621 )
Epeak [keV] : 63.8284 ( -24.1816 -63.8054 )
Norm@50keV : 2.04775E-02 ( -0.00655744 0.0796079 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.90 using 59 PHA bins.
# Reduced chi-squared = 1.105 for 56 degrees of freedom
# Null hypothesis probability = 2.736855e-01
Photon flux (15-150 keV) in 1 sec: 1.58961 ( -0.19281 0.1914 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
