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 0.272 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.34751 ( -0.469008 0.45613 )
Norm@50keV : 9.91768E-03 ( -0.00331672 0.00331611 )
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#Fit statistic : Chi-Squared = 54.45 using 59 PHA bins.
# Reduced chi-squared = 0.9552 for 57 degrees of freedom
# Null hypothesis probability = 5.714234e-01
Photon flux (15-150 keV) in 0.272 sec: 1.19429 ( -0.41445 0.41702 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.63632e-08 ( -9.10651e-09 9.12699e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 0.272 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 1.43445 ( -2.46258 4.96831 )
Epeak [keV] : 76.9637 ( -19.7429 100.188 )
Norm@50keV : 0.144397 ( -0.14442 8.3193 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.66 using 59 PHA bins.
# Reduced chi-squared = 0.9046 for 56 degrees of freedom
# Null hypothesis probability = 6.765763e-01
Photon flux (15-150 keV) in 0.272 sec: 1.17712 ( -0.411969 0.42155 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.86443e-08 ( -9.75142e-09 9.70069e-09 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.229 sec. to 0.771 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.0117755 ( -0.626319 0.882154 )
Norm@50keV : 4.27923E-03 ( -0.00220813 0.00209005 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.87 using 59 PHA bins.
# Reduced chi-squared = 0.8925 for 57 degrees of freedom
# Null hypothesis probability = 7.028594e-01
Photon flux (15-150 keV) in 1 sec: 0.580123 ( -0.185533 0.193171 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.69219e-08 ( -2.12969e-08 2.12959e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.229 sec. to 0.771 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.0263121 ( -1.50731 2.39391 )
Epeak [keV] : 9834.60 ( -9224.23 -9224.23 )
Norm@50keV : 4.33075E-03 ( -0.00128727 0.0508343 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.87 using 59 PHA bins.
# Reduced chi-squared = 0.9084 for 56 degrees of freedom
# Null hypothesis probability = 6.687921e-01
Photon flux (15-150 keV) in 1 sec: 0.577733 ( -0.182624 0.182282 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.70566e-08 ( -2.13585e-08 2.13151e-08 ) ergs/cm2
Time-resolved spectra
