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 -31.460 sec. to 566.708 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.36879 ( -0.100446 0.10073 )
Norm@50keV : 1.28883E-03 ( -6.99931e-05 6.9938e-05 )
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#Fit statistic : Chi-Squared = 48.11 using 59 PHA bins.
# Reduced chi-squared = 0.8441 for 57 degrees of freedom
# Null hypothesis probability = 7.929164e-01
Photon flux (15-150 keV) in 598.2 sec: 0.155882 ( -0.00881 0.008837 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.49975e-06 ( -4.50284e-07 4.52797e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -31.460 sec. to 566.708 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.28366 ( -0.134065 0.39524 )
Epeak [keV] : 442.369 ( -443.112 -443.112 )
Norm@50keV : 1.41645E-03 ( -0.000188239 0.000749459 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.96 using 59 PHA bins.
# Reduced chi-squared = 0.8564 for 56 degrees of freedom
# Null hypothesis probability = 7.689805e-01
Photon flux (15-150 keV) in 598.2 sec: 0.155117 ( -0.009402 0.009196 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.44968e-06 ( -5.02058e-07 4.24153e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.900 sec. to 1.900 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.01501 ( -0.232382 0.241091 )
Norm@50keV : 1.56945E-02 ( -0.00222654 0.00221698 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.93 using 59 PHA bins.
# Reduced chi-squared = 0.8760 for 57 degrees of freedom
# Null hypothesis probability = 7.350502e-01
Photon flux (15-150 keV) in 1 sec: 1.80843 ( -0.26107 0.26223 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.68834e-07 ( -2.51925e-08 2.53753e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.900 sec. to 1.900 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.411103 ( -1.18398 1.67863 )
Epeak [keV] : 97.7577 ( -24.2854 173.856 )
Norm@50keV : 6.52071E-02 ( -0.0652133 0.235029 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.51 using 59 PHA bins.
# Reduced chi-squared = 0.8126 for 56 degrees of freedom
# Null hypothesis probability = 8.406271e-01
Photon flux (15-150 keV) in 1 sec: 1.69589 ( -0.28221 0.28059 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.38966e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
