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 -0.016 sec. to 1.108 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.625101 ( -0.0982707 0.100831 )
Norm@50keV : 3.05638E-02 ( -0.00170826 0.00169297 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.44 using 59 PHA bins.
# Reduced chi-squared = 1.148 for 57 degrees of freedom
# Null hypothesis probability = 2.070765e-01
Photon flux (15-150 keV) in 1.124 sec: 9.06882E-02 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 4.34136e-07 ( -2.48223e-08 2.49207e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.016 sec. to 1.108 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.620753 ( -0.0957439 0.105183 )
Epeak [keV] : 9999.34 ( -9999.36 -9999.36 )
Norm@50keV : 3.08103E-02 ( -0.00162199 0.00728106 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.51 using 59 PHA bins.
# Reduced chi-squared = 1.170 for 56 degrees of freedom
# Null hypothesis probability = 1.801315e-01
Photon flux (15-150 keV) in 1.124 sec: 3.55699 ( -0.18622 0.18628 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.36211e-07 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.016 sec. to 0.984 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.603045 ( -0.0995965 0.102267 )
Norm@50keV : 3.31863E-02 ( -0.00187942 0.00186145 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.64 using 59 PHA bins.
# Reduced chi-squared = 1.187 for 57 degrees of freedom
# Null hypothesis probability = 1.581903e-01
Photon flux (15-150 keV) in 1 sec: 0.280324 0.295781 0.256582 0.221264 0.191341 0.166296 0.145553 0.128519 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 4.23809e-07 ( -2.44716e-08 2.45542e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.016 sec. to 0.984 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.594483 ( -0.191862 0.189822 )
Epeak [keV] : 9998.65 ( -9998.67 -9998.67 )
Norm@50keV : 3.34608E-02 ( -0.00175575 0.00717119 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.72 using 59 PHA bins.
# Reduced chi-squared = 1.209 for 56 degrees of freedom
# Null hypothesis probability = 1.355845e-01
Photon flux (15-150 keV) in 1 sec: 3.87200 ( -0.20407 0.20419 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.26265e-07 ( -2.70931e-08 2.19331e-08 ) ergs/cm2
Time-resolved spectra
