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 30.088 sec. to 169.508 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.40361 ( -0.273367 0.272155 )
Norm@50keV : 6.27000E-04 ( -9.89179e-05 9.82929e-05 )
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#Fit statistic : Chi-Squared = 53.15 using 59 PHA bins.
# Reduced chi-squared = 0.9325 for 57 degrees of freedom
# Null hypothesis probability = 6.201383e-01
Photon flux (15-150 keV) in 139.4 sec: 7.64209E-02 ( -0.0119857 0.0120069 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.44039e-07 ( -1.47505e-07 1.4977e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 30.088 sec. to 169.508 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.0505 ( -0.608907 1.34622 )
Epeak [keV] : 135.768 ( -135.768 -135.768 )
Norm@50keV : 9.43764E-04 ( -0.00040822 0.00334225 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.85 using 59 PHA bins.
# Reduced chi-squared = 0.9438 for 56 degrees of freedom
# Null hypothesis probability = 5.948192e-01
Photon flux (15-150 keV) in 139.4 sec: 7.52581E-02 ( -0.0126176 0.0125083 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.21169e-07 ( -1.64718e-07 1.6346e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 61.200 sec. to 62.200 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.901505 ( -0.565347 0.642544 )
Norm@50keV : 3.74406E-03 ( -0.00126444 0.00120499 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.38 using 59 PHA bins.
# Reduced chi-squared = 0.9539 for 57 degrees of freedom
# Null hypothesis probability = 5.741676e-01
Photon flux (15-150 keV) in 1 sec: 0.429737 ( -0.13932 0.141714 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.19981e-08 ( -1.3564e-08 1.37218e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 61.200 sec. to 62.200 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.240051 ( 0.236738 7.08501 )
Epeak [keV] : 167.681 ( -166.998 -166.998 )
Norm@50keV : 6.83444E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.23 using 59 PHA bins.
# Reduced chi-squared = 0.9685 for 56 degrees of freedom
# Null hypothesis probability = 5.420047e-01
Photon flux (15-150 keV) in 1 sec: 0.414433 ( -0.168119 0.152842 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.09836e-08 ( -1.55856e-08 1.43387e-08 ) ergs/cm2
Time-resolved spectra
