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 -0.004 sec. to 0.332 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.710257 ( -0.127783 0.131777 )
Norm@50keV : 4.76927E-02 ( -0.00367889 0.00364937 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.20 using 59 PHA bins.
# Reduced chi-squared = 0.9509 for 57 degrees of freedom
# Null hypothesis probability = 5.806898e-01
Photon flux (15-150 keV) in 0.336 sec: 5.50843 ( -0.40852 0.40888 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.94724e-07 ( -1.54613e-08 1.55278e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.004 sec. to 0.332 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.399877 ( -0.436714 0.589152 )
Epeak [keV] : 310.465 ( -310.473 -310.473 )
Norm@50keV : 6.47158E-02 ( -0.0194969 0.0482301 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.20 using 59 PHA bins.
# Reduced chi-squared = 0.9500 for 56 degrees of freedom
# Null hypothesis probability = 5.816291e-01
Photon flux (15-150 keV) in 0.336 sec: 5.46140 ( -0.4174 0.41654 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.92601e-07 ( -1.62984e-08 1.60924e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.334 sec. to 0.666 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.768475 ( -0.16731 0.174528 )
Norm@50keV : 1.64925E-02 ( -0.00162752 0.00160429 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.59 using 59 PHA bins.
# Reduced chi-squared = 1.133 for 57 degrees of freedom
# Null hypothesis probability = 2.286291e-01
Photon flux (15-150 keV) in 1 sec: 1.89803 ( -0.18011 0.18077 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.95348e-07 ( -1.89962e-08 1.90941e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.334 sec. to 0.666 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.761229 ( -0.168464 0.176466 )
Epeak [keV] : 9999.31 ( -9999.32 -9999.32 )
Norm@50keV : 1.66112E-02 ( -0.00153656 0.0162812 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.59 using 59 PHA bins.
# Reduced chi-squared = 1.153 for 56 degrees of freedom
# Null hypothesis probability = 2.016350e-01
Photon flux (15-150 keV) in 1 sec: 1.89767 ( -0.1858 0.17986 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.47814e-09 ( 0 0 ) ergs/cm2
Time-resolved spectra
