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 -0.008 sec. to 0.568 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.00943 ( -0.218693 0.224853 )
Norm@50keV : 1.26532E-02 ( -0.0015916 0.00158927 )
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#Fit statistic : Chi-Squared = 47.10 using 59 PHA bins.
# Reduced chi-squared = 0.8264 for 57 degrees of freedom
# Null hypothesis probability = 8.220801e-01
Photon flux (15-150 keV) in 0.576 sec: 1.45750 ( -0.18518 0.18546 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.85583e-08 ( -1.11238e-08 1.12719e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.008 sec. to 0.568 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.391057 ( -0.713982 1.01425 )
Epeak [keV] : 142.866 ( )
Norm@50keV : 2.44151E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.47 using 59 PHA bins.
# Reduced chi-squared = 0.8120 for 56 degrees of freedom
# Null hypothesis probability = 8.415114e-01
Photon flux (15-150 keV) in 0.576 sec: 1.41602 ( -0.19392 0.19355 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.51836e-08 ( -1.22949e-08 1.22348e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.188 sec. to 0.812 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.863632 ( -0.244189 0.256454 )
Norm@50keV : 7.74876E-03 ( -0.0011408 0.00113154 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.38 using 59 PHA bins.
# Reduced chi-squared = 0.7435 for 57 degrees of freedom
# Null hypothesis probability = 9.255783e-01
Photon flux (15-150 keV) in 1 sec: 0.889364 ( -0.129577 0.130106 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.82247e-08 ( -1.35678e-08 1.37025e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.188 sec. to 0.812 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.0977731 ( -0.972499 1.28316 )
Epeak [keV] : 127.855 ( -43.0823 5269.48 )
Norm@50keV : 2.00404E-02 ( -0.0121298 0.0445452 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 39.57 using 59 PHA bins.
# Reduced chi-squared = 0.7065 for 56 degrees of freedom
# Null hypothesis probability = 9.528179e-01
Photon flux (15-150 keV) in 1 sec: 0.851633 ( -0.134807 0.1355 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.38012e-08 ( -1.47438e-08 1.46906e-08 ) ergs/cm2
Time-resolved spectra
