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 -54.332 sec. to 129.360 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.31043 ( -0.0717267 0.0722043 )
Norm@50keV : 3.11592E-03 ( -0.000122922 0.000122868 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.32 using 59 PHA bins.
# Reduced chi-squared = 1.093 for 57 degrees of freedom
# Null hypothesis probability = 2.927247e-01
Photon flux (15-150 keV) in 183.7 sec: 0.372465 ( -0.015885 0.015927 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.64273e-06 ( -2.35448e-07 2.35941e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -54.332 sec. to 129.360 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.22811 ( -0.115652 0.27356 )
Epeak [keV] : 513.193 ( -527.58 -527.58 )
Norm@50keV : 3.39785E-03 ( -0.000371201 0.00108847 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.04 using 59 PHA bins.
# Reduced chi-squared = 1.108 for 56 degrees of freedom
# Null hypothesis probability = 2.695750e-01
Photon flux (15-150 keV) in 183.7 sec: 0.370745 ( -0.016753 0.016779 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.6172e-06 ( -2.49856e-07 2.48629e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 115.412 sec. to 116.412 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.40251 ( -0.15162 0.150916 )
Norm@50keV : 2.39681E-02 ( -0.00207304 0.00206545 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.45 using 59 PHA bins.
# Reduced chi-squared = 1.008 for 57 degrees of freedom
# Null hypothesis probability = 4.582925e-01
Photon flux (15-150 keV) in 1 sec: 2.92059 ( -0.2576 0.2581 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.31505e-07 ( -2.20021e-08 2.2148e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 115.412 sec. to 116.412 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.3989 ( -0.152555 0.54293 )
Epeak [keV] : 9997.11 ( -9998.84 -9998.84 )
Norm@50keV : 2.40601E-02 ( -0.0240551 0.0189607 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.46 using 59 PHA bins.
# Reduced chi-squared = 1.026 for 56 degrees of freedom
# Null hypothesis probability = 4.210435e-01
Photon flux (15-150 keV) in 1 sec: 1.39063 ( -0.3817 0.4108 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.32012e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
