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 -0.036 sec. to 0.068 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.69462 ( -0.165705 0.157896 )
Norm@50keV : 7.75132E-02 ( -0.00912239 0.00906176 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 87.31 using 59 PHA bins.
# Reduced chi-squared = 1.532 for 57 degrees of freedom
# Null hypothesis probability = 6.023477e-03
Photon flux (15-150 keV) in 0.104 sec: 10.2756 ( -1.17795 1.1792 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.4685e-08 ( -9.06695e-09 9.08593e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.036 sec. to 0.068 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.110959 ( -0.804279 0.945165 )
Epeak [keV] : 63.7997 ( -8.01271 11.9384 )
Norm@50keV : 0.575363 ( -0.332745 0.989031 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 70.77 using 59 PHA bins.
# Reduced chi-squared = 1.264 for 56 degrees of freedom
# Null hypothesis probability = 8.842928e-02
Photon flux (15-150 keV) in 0.104 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.482 sec. to 0.518 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.73306 ( -0.268223 0.254822 )
Norm@50keV : 1.10761E-02 ( -0.00198423 0.00195628 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.69 using 59 PHA bins.
# Reduced chi-squared = 0.8717 for 57 degrees of freedom
# Null hypothesis probability = 7.432809e-01
Photon flux (15-150 keV) in 1 sec: 1.48846 ( -0.2479 0.24832 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.02334e-07 ( -1.87217e-08 1.89993e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.482 sec. to 0.518 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.0856687 ( -1.18194 1.60714 )
Epeak [keV] : 55.0537 ( -11.4004 27.0858 )
Norm@50keV : 8.18885E-02 ( -0.0818874 0.488712 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.46 using 59 PHA bins.
# Reduced chi-squared = 0.7761 for 56 degrees of freedom
# Null hypothesis probability = 8.892872e-01
Photon flux (15-150 keV) in 1 sec: 1.42485 ( -0.25078 0.25191 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.44735e-08 ( -1.86838e-08 1.96093e-08 ) ergs/cm2
Time-resolved spectra
