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 -1.356 sec. to 2.380 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.899935 ( -0.170793 0.177779 )
Norm@50keV : 7.58511E-03 ( -0.000754777 0.000749447 )
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#Fit statistic : Chi-Squared = 45.04 using 59 PHA bins.
# Reduced chi-squared = 0.7901 for 57 degrees of freedom
# Null hypothesis probability = 8.742222e-01
Photon flux (15-150 keV) in 3.736 sec: 0.870592 ( -0.086489 0.08674 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.18073e-07 ( -3.29666e-08 3.31451e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.356 sec. to 2.380 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.594798 ( -0.386119 0.758631 )
Epeak [keV] : 263.338 ( -263.34 -263.34 )
Norm@50keV : 1.03824E-02 ( -0.00339088 0.0115012 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.42 using 59 PHA bins.
# Reduced chi-squared = 0.7933 for 56 degrees of freedom
# Null hypothesis probability = 8.677069e-01
Photon flux (15-150 keV) in 3.736 sec: 0.859520 ( -0.089846 0.089876 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.12491e-07 ( -3.60404e-08 3.53473e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.048 sec. to 0.952 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.77045 ( -0.266657 0.288489 )
Norm@50keV : 9.78014E-03 ( -0.00155785 0.00152135 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.71 using 59 PHA bins.
# Reduced chi-squared = 0.7845 for 57 degrees of freedom
# Null hypothesis probability = 8.813884e-01
Photon flux (15-150 keV) in 1 sec: 1.12543 ( -0.171089 0.1722 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.15744e-07 ( -1.80158e-08 1.81281e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.048 sec. to 0.952 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.764559 ( -0.267689 0.346776 )
Epeak [keV] : 9999.19 ( -9999.32 -9999.32 )
Norm@50keV : 9.85439E-03 ( -0.00146476 0.0178813 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.71 using 59 PHA bins.
# Reduced chi-squared = 0.7985 for 56 degrees of freedom
# Null hypothesis probability = 8.607360e-01
Photon flux (15-150 keV) in 1 sec: 1.12552 ( -0.174944 0.17087 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.15776e-07 ( -1.89527e-08 1.69848e-08 ) ergs/cm2
Time-resolved spectra
