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 -0.712 sec. to 9.256 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.34833 ( -0.254538 0.25807 )
Norm@50keV : 3.75158E-03 ( -0.000560267 0.000558343 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.47 using 59 PHA bins.
# Reduced chi-squared = 0.9732 for 57 degrees of freedom
# Null hypothesis probability = 5.326170e-01
Photon flux (15-150 keV) in 9.968 sec: 0.451808 ( -0.067793 0.067905 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.65416e-07 ( -6.06699e-08 6.15842e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.712 sec. to 9.256 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.14254 ( -0.98103 1.08837 )
Epeak [keV] : 202.490 ( -202.596 -202.596 )
Norm@50keV : 4.80765E-03 ( -0.00158615 0.0128517 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.32 using 59 PHA bins.
# Reduced chi-squared = 0.9879 for 56 degrees of freedom
# Null hypothesis probability = 5.004860e-01
Photon flux (15-150 keV) in 9.968 sec: 0.448318 ( -0.069597 0.069467 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.58343e-07 ( -7.00271e-08 6.68523e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 2.264 sec. to 3.264 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.37779 ( -0.361166 0.36215 )
Norm@50keV : 8.87545E-03 ( -0.00176857 0.0017582 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.38 using 59 PHA bins.
# Reduced chi-squared = 1.094 for 57 degrees of freedom
# Null hypothesis probability = 2.908985e-01
Photon flux (15-150 keV) in 1 sec: 1.07556 ( -0.216207 0.2171 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.61688e-08 ( -1.90306e-08 1.93743e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.264 sec. to 3.264 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.37443 ( -1.96745 1.27515 )
Epeak [keV] : 9986.50 ( -9984.42 -9984.42 )
Norm@50keV : 8.90890E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.38 using 59 PHA bins.
# Reduced chi-squared = 1.114 for 56 degrees of freedom
# Null hypothesis probability = 2.598930e-01
Photon flux (15-150 keV) in 1 sec: 1.07309 ( -0.224118 0.21877 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.14639e-08 ( -2.42571e-08 1.71891e-08 ) ergs/cm2
Time-resolved spectra
