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 -0.848 sec. to 122.732 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.415 ( -0.237065 0.237433 )
Norm@50keV : 5.91471E-04 ( -8.04589e-05 7.96927e-05 )
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#Fit statistic : Chi-Squared = 51.79 using 59 PHA bins.
# Reduced chi-squared = 0.9085 for 57 degrees of freedom
# Null hypothesis probability = 6.704156e-01
Photon flux (15-150 keV) in 123.6 sec: 7.22807E-02 ( -0.0095379 0.0095466 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.04349e-07 ( -1.07509e-07 1.09415e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.848 sec. to 122.732 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.41286 ( -0.898136 0.41609 )
Epeak [keV] : 9999.19 ( -9999.36 -9999.36 )
Norm@50keV : 5.93435E-04 ( -0.00043735 0.00064669 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.79 using 59 PHA bins.
# Reduced chi-squared = 0.9249 for 56 degrees of freedom
# Null hypothesis probability = 6.347482e-01
Photon flux (15-150 keV) in 123.6 sec: 7.25490E-02 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 7.08758e-07 ( -1.25651e-07 1.14998e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.004 sec. to 0.996 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.00093 ( -0.227112 0.235533 )
Norm@50keV : 8.22481E-03 ( -0.00104457 0.00104058 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.95 using 59 PHA bins.
# Reduced chi-squared = 1.087 for 57 degrees of freedom
# Null hypothesis probability = 3.041125e-01
Photon flux (15-150 keV) in 1 sec: 0.946959 ( -0.122155 0.122491 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.89181e-08 ( -1.23549e-08 1.24497e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.004 sec. to 0.996 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.995326 ( -0.293216 0.701456 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 8.27416E-03 ( -0.00103703 0.00904117 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.96 using 59 PHA bins.
# Reduced chi-squared = 1.106 for 56 degrees of freedom
# Null hypothesis probability = 2.720997e-01
Photon flux (15-150 keV) in 1 sec: 0.952261 ( -0.158492 0.147559 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.95241e-08 ( -1.68265e-08 1.57302e-08 ) ergs/cm2
Time-resolved spectra
