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 0.000 sec. to 3.501 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.19321 ( -0.191866 0.195549 )
Norm@50keV : 1.23366E-02 ( -0.00131663 0.0013163 )
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#Fit statistic : Chi-Squared = 54.43 using 59 PHA bins.
# Reduced chi-squared = 0.9549 for 57 degrees of freedom
# Null hypothesis probability = 5.721633e-01
Photon flux (15-150 keV) in 3.501 sec: 1.44670 ( -0.16 0.16047 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.39078e-07 ( -5.18362e-08 5.21828e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 3.501 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.19442 ( -0.18811 0.202115 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.23729E-02 ( -0.00454002 0.00785404 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.45 using 59 PHA bins.
# Reduced chi-squared = 0.9723 for 56 degrees of freedom
# Null hypothesis probability = 5.338727e-01
Photon flux (15-150 keV) in 3.501 sec: 1.45230 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 4.43591e-07 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.900 sec. to 2.900 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.09869 ( -0.293814 0.305605 )
Norm@50keV : 1.61854E-02 ( -0.00260684 0.00259682 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.58 using 59 PHA bins.
# Reduced chi-squared = 0.7646 for 57 degrees of freedom
# Null hypothesis probability = 9.045551e-01
Photon flux (15-150 keV) in 1 sec: 1.87716 ( -0.31246 0.31356 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.69309e-07 ( -2.95467e-08 2.97583e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.900 sec. to 2.900 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.10245 ( -0.287704 0.397499 )
Epeak [keV] : 9999.35 ( -9999.36 -9999.36 )
Norm@50keV : 1.62380E-02 ( -0.0025943 0.0195102 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.59 using 59 PHA bins.
# Reduced chi-squared = 0.7785 for 56 degrees of freedom
# Null hypothesis probability = 8.864293e-01
Photon flux (15-150 keV) in 1 sec: 1.89041 ( -0.38341 0.35779 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.95458e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
