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 -0.088 sec. to 5.320 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.0516 ( -0.32183 0.346065 )
Norm@50keV : 2.57135E-03 ( -0.000438346 0.000434243 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.49 using 59 PHA bins.
# Reduced chi-squared = 0.9559 for 57 degrees of freedom
# Null hypothesis probability = 5.699589e-01
Photon flux (15-150 keV) in 5.408 sec: 0.297016 ( -0.05209 0.05226 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.47729e-07 ( -2.70489e-08 2.72783e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.088 sec. to 5.320 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.06521 ( -0.306888 0.381496 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 2.58949E-03 ( -0.000434014 0.00191444 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.52 using 59 PHA bins.
# Reduced chi-squared = 0.9736 for 56 degrees of freedom
# Null hypothesis probability = 5.310604e-01
Photon flux (15-150 keV) in 5.408 sec: 0.301659 ( -0.056793 0.04755 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.48111e-07 ( -2.75079e-08 2.67801e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.088 sec. to 0.912 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.803042 ( -0.237819 0.253919 )
Norm@50keV : 8.25025E-03 ( -0.00116714 0.00114651 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.86 using 59 PHA bins.
# Reduced chi-squared = 0.7695 for 57 degrees of freedom
# Null hypothesis probability = 8.991643e-01
Photon flux (15-150 keV) in 1 sec: 0.948107 ( -0.129706 0.130353 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.62986e-08 ( -1.34701e-08 1.35539e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.088 sec. to 0.912 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.505937 ( -0.507626 1.16264 )
Epeak [keV] : 299.331 ( -299.168 -299.168 )
Norm@50keV : 1.10493E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.58 using 59 PHA bins.
# Reduced chi-squared = 0.7782 for 56 degrees of freedom
# Null hypothesis probability = 8.867404e-01
Photon flux (15-150 keV) in 1 sec: 0.936113 ( -0.13572 0.133227 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.48943e-08 ( -1.46914e-08 1.28092e-08 ) ergs/cm2
Time-resolved spectra
