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 -6.312 sec. to 74.460 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.37235 ( -0.0908053 0.088877 )
Norm@50keV : 2.37752E-03 ( -0.000127864 0.000126755 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.42 using 59 PHA bins.
# Reduced chi-squared = 1.130 for 57 degrees of freedom
# Null hypothesis probability = 2.329849e-01
Photon flux (15-150 keV) in 80.77 sec: 0.432941 ( -0.018579 0.018659 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.86222e-06 ( -8.00431e-08 8.05472e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -6.312 sec. to 74.460 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.86646 ( -0.146779 0.457726 )
Epeak [keV] : 10.6514 ( -8.71786 14.8006 )
Norm@50keV : 4.64449E-03 ( -0.00113814 0.00384625 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.49 using 59 PHA bins.
# Reduced chi-squared = 1.062 for 56 degrees of freedom
# Null hypothesis probability = 3.499159e-01
Photon flux (15-150 keV) in 80.77 sec: 0.417785 ( -0.021973 0.020462 ) 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 5.444 sec. to 6.444 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.0889 ( -0.160171 0.153965 )
Norm@50keV : 1.11339E-02 ( -0.00116438 0.00114206 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.85 using 59 PHA bins.
# Reduced chi-squared = 0.8921 for 57 degrees of freedom
# Null hypothesis probability = 7.037504e-01
Photon flux (15-150 keV) in 1 sec: 1.74226 ( -0.13904 0.13911 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03357e-07 ( -9.7173e-09 9.87782e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 5.444 sec. to 6.444 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.99371 ( 1.99371 1.99371 )
Epeak [keV] : 2.67278 ( -1.69161 -2.67438 )
Norm@50keV : 1.26772E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.79 using 59 PHA bins.
# Reduced chi-squared = 0.9070 for 56 degrees of freedom
# Null hypothesis probability = 6.717626e-01
Photon flux (15-150 keV) in 1 sec: 1.73991 ( -0.13925 0.1452 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
