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 18.292 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.329 ( -0.190156 0.190456 )
Norm@50keV : 2.88922E-03 ( -0.000307796 0.000307237 )
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#Fit statistic : Chi-Squared = 51.11 using 59 PHA bins.
# Reduced chi-squared = 0.8967 for 57 degrees of freedom
# Null hypothesis probability = 6.944328e-01
Photon flux (15-150 keV) in 18.29 sec: 0.346605 ( -0.037517 0.037601 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.18661e-07 ( -6.19471e-08 6.25236e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 18.292 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23487 ( -0.26697 0.810024 )
Epeak [keV] : 410.609 ( -445.518 -445.518 )
Norm@50keV : 3.20760E-03 ( -0.00127681 0.00444919 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.08 using 59 PHA bins.
# Reduced chi-squared = 0.9121 for 56 degrees of freedom
# Null hypothesis probability = 6.613478e-01
Photon flux (15-150 keV) in 18.29 sec: 0.345183 ( -0.039274 0.037529 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.15482e-07 ( -6.74552e-08 6.48064e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.780 sec. to 2.780 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.06562 ( -0.41931 0.447311 )
Norm@50keV : 5.53000E-03 ( -0.00135728 0.00135027 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.60 using 59 PHA bins.
# Reduced chi-squared = 0.8351 for 57 degrees of freedom
# Null hypothesis probability = 8.079676e-01
Photon flux (15-150 keV) in 1 sec: 0.639476 ( -0.160392 0.1616 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.84736e-08 ( -1.53167e-08 1.55159e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.780 sec. to 2.780 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.637974 ( 0.637804 2.29738 )
Epeak [keV] : 181.888 ( -181.845 -181.845 )
Norm@50keV : 8.60267E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.40 using 59 PHA bins.
# Reduced chi-squared = 0.8464 for 56 degrees of freedom
# Null hypothesis probability = 7.865795e-01
Photon flux (15-150 keV) in 1 sec: 0.628499 ( -0.167147 0.1661 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.73258e-08 ( -1.62855e-08 1.60833e-08 ) ergs/cm2
Time-resolved spectra
