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 -21.384 sec. to 62.424 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.26531 ( -0.184784 0.174355 )
Norm@50keV : 2.07414E-03 ( -0.000256724 0.000251502 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.56 using 59 PHA bins.
# Reduced chi-squared = 0.7291 for 57 degrees of freedom
# Null hypothesis probability = 9.380130e-01
Photon flux (15-150 keV) in 83.81 sec: 0.355650 ( -0.030641 0.030655 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.65138e-06 ( -1.68189e-07 1.71663e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -21.384 sec. to 62.424 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.91626 ( -0.0836657 0.818365 )
Epeak [keV] : 9.53149 ( -7.58427 31.2619 )
Norm@50keV : 3.34389E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 40.86 using 59 PHA bins.
# Reduced chi-squared = 0.7296 for 56 degrees of freedom
# Null hypothesis probability = 9.357758e-01
Photon flux (15-150 keV) in 83.81 sec: 0.355296 ( -0.030507 0.016061 ) 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 0.988 sec. to 1.988 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.05842 ( -0.202656 0.190234 )
Norm@50keV : 1.83529E-02 ( -0.00257374 0.00251763 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.84 using 59 PHA bins.
# Reduced chi-squared = 1.190 for 57 degrees of freedom
# Null hypothesis probability = 1.542529e-01
Photon flux (15-150 keV) in 1 sec: 2.82977 ( -0.31871 0.31881 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.6993e-07 ( -2.19544e-08 2.22464e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.988 sec. to 1.988 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.968682 ( -0.894361 1.19233 )
Epeak [keV] : 38.8503 ( -18.4369 13.3863 )
Norm@50keV : 7.98876E-02 ( -0.079896 0.335271 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.52 using 59 PHA bins.
# Reduced chi-squared = 1.134 for 56 degrees of freedom
# Null hypothesis probability = 2.286706e-01
Photon flux (15-150 keV) in 1 sec: 2.75883 ( -0.32484 0.32492 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
