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 0.084 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.30587 ( -0.238983 0.234633 )
Norm@50keV : 2.45562E-02 ( -0.00448936 0.00448908 )
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#Fit statistic : Chi-Squared = 59.82 using 59 PHA bins.
# Reduced chi-squared = 1.049 for 57 degrees of freedom
# Null hypothesis probability = 3.738291e-01
Photon flux (15-150 keV) in 0.084 sec: 2.93271 ( -0.55246 0.55376 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.03577e-08 ( -3.87121e-09 3.87483e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 0.084 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.554925 ( -1.10469 1.53749 )
Epeak [keV] : 81.3767 ( -17.7843 37.0229 )
Norm@50keV : 0.168754 ( -0.168754 0.650865 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.43 using 59 PHA bins.
# Reduced chi-squared = 0.9004 for 56 degrees of freedom
# Null hypothesis probability = 6.850107e-01
Photon flux (15-150 keV) in 0.084 sec: 2.99112 ( -0.54711 0.55046 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.16112e-08 ( -4.32618e-09 4.22684e-09 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.456 sec. to 0.544 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.09982 ( -0.540941 0.602846 )
Norm@50keV : 3.17555E-03 ( -0.00106288 0.00105175 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.72 using 59 PHA bins.
# Reduced chi-squared = 0.9425 for 57 degrees of freedom
# Null hypothesis probability = 5.988853e-01
Photon flux (15-150 keV) in 1 sec: 0.368342 ( -0.125843 0.12747 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.32063e-08 ( -1.14643e-08 1.16496e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.456 sec. to 0.544 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.0223411 ( -6.84006 4.57622 )
Epeak [keV] : 95.4720 ( -44.1557 -95.4347 )
Norm@50keV : 1.09417E-02 ( -0.0109526 1.89188 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.10 using 59 PHA bins.
# Reduced chi-squared = 0.9483 for 56 degrees of freedom
# Null hypothesis probability = 5.852108e-01
Photon flux (15-150 keV) in 1 sec: 0.353604 ( -0.129619 0.131479 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.08305e-08 ( -1.29903e-08 1.28161e-08 ) ergs/cm2
Time-resolved spectra
