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 52.128 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.2676 ( -0.0736326 0.0739903 )
Norm@50keV : 4.20639E-03 ( -0.000153662 0.000153571 )
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#Fit statistic : Chi-Squared = 68.92 using 59 PHA bins.
# Reduced chi-squared = 1.209 for 57 degrees of freedom
# Null hypothesis probability = 1.338851e-01
Photon flux (15-150 keV) in 52.13 sec: 0.498966 ( -0.019661 0.019767 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.18478e-06 ( -8.68647e-08 8.71134e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 52.128 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26385 ( -0.066187 0.0835907 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 4.22449E-03 ( -0.00015384 0.000153826 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.13 using 59 PHA bins.
# Reduced chi-squared = 1.234 for 56 degrees of freedom
# Null hypothesis probability = 1.118002e-01
Photon flux (15-150 keV) in 52.13 sec: 0.498849 ( -0.019706 0.019728 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.18373e-06 ( -8.67772e-08 8.7068e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.772 sec. to 1.772 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.573923 ( -0.0752766 0.0767681 )
Norm@50keV : 5.27574E-02 ( -0.00231556 0.00229802 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.33 using 59 PHA bins.
# Reduced chi-squared = 1.093 for 57 degrees of freedom
# Null hypothesis probability = 2.923955e-01
Photon flux (15-150 keV) in 1 sec: 0.391461 ( -0.015424 0.166929 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.83282e-07 ( -3.0001e-08 3.008e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.772 sec. to 1.772 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.566558 ( -0.0745437 0.0788096 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 5.32055E-02 ( -0.00233889 0.0117317 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.38 using 59 PHA bins.
# Reduced chi-squared = 1.114 for 56 degrees of freedom
# Null hypothesis probability = 2.599567e-01
Photon flux (15-150 keV) in 1 sec: 6.18366 ( -0.27212 0.26147 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.84353e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
