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 -1.640 sec. to 2.140 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.08769 ( -0.186361 0.19159 )
Norm@50keV : 4.36817E-03 ( -0.000490327 0.00048958 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.58 using 59 PHA bins.
# Reduced chi-squared = 0.9575 for 57 degrees of freedom
# Null hypothesis probability = 5.663925e-01
Photon flux (15-150 keV) in 3.78 sec: 0.506092 ( -0.058046 0.058161 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.73337e-07 ( -2.12328e-08 2.13878e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.640 sec. to 2.140 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.411417 ( -0.734644 0.844682 )
Epeak [keV] : 126.929 ( -45.0065 -126.93 )
Norm@50keV : 9.12362E-03 ( -0.00490333 0.014092 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.20 using 59 PHA bins.
# Reduced chi-squared = 0.9322 for 56 degrees of freedom
# Null hypothesis probability = 6.194244e-01
Photon flux (15-150 keV) in 3.78 sec: 0.493621 ( -0.059861 0.059851 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.66185e-07 ( -2.31832e-08 2.30501e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.032 sec. to 1.032 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.875971 ( -0.280479 0.299884 )
Norm@50keV : 5.22938E-03 ( -0.000980094 0.000970001 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.83 using 59 PHA bins.
# Reduced chi-squared = 0.9970 for 57 degrees of freedom
# Null hypothesis probability = 4.814469e-01
Photon flux (15-150 keV) in 1 sec: 0.600138 ( -0.111262 0.111951 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.9253e-08 ( -1.1127e-08 1.11985e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.032 sec. to 1.032 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.881916 ( -1.37211 2.02545 )
Epeak [keV] : 94.1143 ( -24.7411 121.883 )
Norm@50keV : 3.10010E-02 ( -0.0310054 0.188951 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.62 using 59 PHA bins.
# Reduced chi-squared = 0.9218 for 56 degrees of freedom
# Null hypothesis probability = 6.410954e-01
Photon flux (15-150 keV) in 1 sec: 0.568719 ( -0.112429 0.114119 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.48264e-08 ( -1.21537e-08 1.21019e-08 ) ergs/cm2
Time-resolved spectra
