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 -31.000 sec. to 161.000 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -2.37223 ( -0.257175 0.234206 )
Norm@50keV : 3.58289E-04 ( -6.79785e-05 6.75317e-05 )
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#Fit statistic : Chi-Squared = 45.98 using 59 PHA bins.
# Reduced chi-squared = 0.8066 for 57 degrees of freedom
# Null hypothesis probability = 8.517643e-01
Photon flux (15-150 keV) in 192 sec: 6.52388E-02 ( -0.0075359 0.0075385 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.67085e-07 ( -9.86886e-08 1.02863e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -31.000 sec. to 161.000 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.838958 ( -1.06958 1.55344 )
Epeak [keV] : 26.4772 ( -22.4162 7.14064 )
Norm@50keV : 3.42794E-03 ( -0.00342796 0.0313621 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.38 using 59 PHA bins.
# Reduced chi-squared = 0.7389 for 56 degrees of freedom
# Null hypothesis probability = 9.278647e-01
Photon flux (15-150 keV) in 192 sec: 6.27316E-02 ( -0.007536 0.0076213 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.81931e-07 ( -8.89033e-08 1.08533e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 24.500 sec. to 25.500 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -4.28552 ( 4.26872 4.26872 )
Norm@50keV : 7.01284E-05 ( -7.21972e-05 0.000657201 )
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#Fit statistic : Chi-Squared = 65.80 using 59 PHA bins.
# Reduced chi-squared = 1.154 for 57 degrees of freedom
# Null hypothesis probability = 1.984588e-01
Photon flux (15-150 keV) in 1 sec: 5.62100E-02 ( -0.05621 0.08399 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.95907e-09 ( 1 4.82203e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 24.500 sec. to 25.500 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 9.88335 ( -12.4403 -9.9001 )
Epeak [keV] : 16.6096 ( -6.96989 9.14447 )
Norm@50keV : 9.30265E+07 ( -9.98428e+07 1.50181e+11 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.40 using 59 PHA bins.
# Reduced chi-squared = 1.150 for 56 degrees of freedom
# Null hypothesis probability = 2.063162e-01
Photon flux (15-150 keV) in 1 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.81895e-09 ( 0 0 ) ergs/cm2
Time-resolved spectra
