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 -0.584 sec. to 6.840 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.89764 ( -0.19992 0.191063 )
Norm@50keV : 2.02625E-02 ( -0.00259979 0.00256623 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.92 using 59 PHA bins.
# Reduced chi-squared = 1.156 for 57 degrees of freedom
# Null hypothesis probability = 1.956754e-01
Photon flux (15-150 keV) in 7.424 sec: 2.90513 ( -0.35417 0.3553 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.38324e-06 ( -1.74764e-07 1.75803e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.584 sec. to 6.840 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.5218 ( -0.981817 1.34272 )
Epeak [keV] : 50.7397 ( -9.18517 18.0786 )
Norm@50keV : 0.107625 ( -0.107631 0.454165 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.69 using 59 PHA bins.
# Reduced chi-squared = 1.066 for 56 degrees of freedom
# Null hypothesis probability = 3.429694e-01
Photon flux (15-150 keV) in 7.424 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.29059e-06 ( -1.89206e-07 1.90558e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.148 sec. to 0.852 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.89867 ( -0.280907 0.257462 )
Norm@50keV : 4.13085E-02 ( -0.00782553 0.00770174 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 78.44 using 59 PHA bins.
# Reduced chi-squared = 1.376 for 57 degrees of freedom
# Null hypothesis probability = 3.136775e-02
Photon flux (15-150 keV) in 1 sec: 5.92506 ( -1.0837 1.08763 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.79848e-07 ( -7.08113e-08 7.10206e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.148 sec. to 0.852 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.562886 ( -1.08261 1.3516 )
Epeak [keV] : 58.7241 ( -8.23741 30.7974 )
Norm@50keV : 0.182200 ( -0.182159 0.580011 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.86 using 59 PHA bins.
# Reduced chi-squared = 1.319 for 56 degrees of freedom
# Null hypothesis probability = 5.516034e-02
Photon flux (15-150 keV) in 1 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.8376e-07 ( -7.14902e-08 7.18151e-08 ) ergs/cm2
Time-resolved spectra
