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 22.000 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.09617 ( -0.18478 0.189484 )
Norm@50keV : 2.99444E-03 ( -0.000300007 0.00029954 )
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#Fit statistic : Chi-Squared = 65.14 using 59 PHA bins.
# Reduced chi-squared = 1.143 for 57 degrees of freedom
# Null hypothesis probability = 2.145370e-01
Photon flux (15-150 keV) in 22 sec: 0.347207 ( -0.035713 0.03581 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.89689e-07 ( -7.71938e-08 7.7854e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 22.000 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.09141 ( -0.239491 0.450953 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 3.01046E-03 ( -0.000300195 0.000300344 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.16 using 59 PHA bins.
# Reduced chi-squared = 1.164 for 56 degrees of freedom
# Null hypothesis probability = 1.881960e-01
Photon flux (15-150 keV) in 22 sec: 0.350069 ( -0.038651 0.032837 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.97145e-07 ( -8.53684e-08 6.91797e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.000 sec. to 2.000 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.972026 ( -0.401345 0.438499 )
Norm@50keV : 6.29759E-03 ( -0.00154307 0.00153176 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.07 using 59 PHA bins.
# Reduced chi-squared = 1.089 for 57 degrees of freedom
# Null hypothesis probability = 3.004333e-01
Photon flux (15-150 keV) in 1 sec: 0.724094 ( -0.17849 0.179475 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.87939e-08 ( -1.7835e-08 1.81422e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.000 sec. to 2.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.123693 ( -1.19064 2.60169 )
Epeak [keV] : 117.180 ( -117.137 -117.137 )
Norm@50keV : 1.60997E-02 ( -0.0161104 0.258684 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.37 using 59 PHA bins.
# Reduced chi-squared = 1.096 for 56 degrees of freedom
# Null hypothesis probability = 2.895578e-01
Photon flux (15-150 keV) in 1 sec: 0.701598 ( -0.185161 0.18531 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.44718e-08 ( -2.05803e-08 2.02236e-08 ) ergs/cm2
Time-resolved spectra
