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 -105.516 sec. to 50.024 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42058 ( -0.0981488 0.0985692 )
Norm@50keV : 2.57467E-03 ( -0.000140589 0.000140526 )
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#Fit statistic : Chi-Squared = 38.44 using 59 PHA bins.
# Reduced chi-squared = 0.6743 for 57 degrees of freedom
# Null hypothesis probability = 9.719174e-01
Photon flux (15-150 keV) in 155.5 sec: 0.315049 ( -0.018211 0.018268 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.8531e-06 ( -2.26999e-07 2.27932e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -105.516 sec. to 50.024 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.35263 ( -0.135764 0.363345 )
Epeak [keV] : 469.163 ( -740.235 -740.235 )
Norm@50keV : 2.77536E-03 ( -0.000252849 0.00126412 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 38.45 using 59 PHA bins.
# Reduced chi-squared = 0.6865 for 56 degrees of freedom
# Null hypothesis probability = 9.646906e-01
Photon flux (15-150 keV) in 155.5 sec: 0.314330 ( -0.018983 0.018274 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.8422e-06 ( -2.42054e-07 2.36015e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 3.548 sec. to 4.548 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.30006 ( -0.176604 0.176997 )
Norm@50keV : 1.96657E-02 ( -0.00209386 0.00209153 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 70.07 using 59 PHA bins.
# Reduced chi-squared = 1.229 for 57 degrees of freedom
# Null hypothesis probability = 1.145962e-01
Photon flux (15-150 keV) in 1 sec: 2.34622 ( -0.25513 0.25557 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.94352e-07 ( -2.27746e-08 2.29381e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 3.548 sec. to 4.548 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.497443 ( -0.727409 0.87405 )
Epeak [keV] : 100.433 ( -27.9815 343.185 )
Norm@50keV : 4.73573E-02 ( -0.0255862 0.0703118 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 66.47 using 59 PHA bins.
# Reduced chi-squared = 1.187 for 56 degrees of freedom
# Null hypothesis probability = 1.597253e-01
Photon flux (15-150 keV) in 1 sec: 2.27362 ( -0.26541 0.26443 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.86294e-07 ( -2.42324e-08 2.43213e-08 ) ergs/cm2
Time-resolved spectra
