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 -4.996 sec. to 213.636 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.57764 ( -0.018694 0.0187817 )
Norm@50keV : 5.32807E-02 ( -0.000637106 0.000635569 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 27.85 using 59 PHA bins.
# Reduced chi-squared = 0.4886 for 57 degrees of freedom
# Null hypothesis probability = 9.995971e-01
Photon flux (15-150 keV) in 218.6 sec: 6.80046 ( -0.10702 0.10755 ) ph/cm2/s
Energy fluence (15-150 keV) : 0.000109247 ( -1.17585e-06 1.1786e-06 ) ergs/cm2
Cutoff power-law model
Time interval is from -4.996 sec. to 213.636 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.48819 ( -0.0772542 0.0784682 )
Epeak [keV] : 399.813 ( -152.015 1709.22 )
Norm@50keV : 5.73298E-02 ( -0.00316121 0.00372195 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 23.99 using 59 PHA bins.
# Reduced chi-squared = 0.4283 for 56 degrees of freedom
# Null hypothesis probability = 9.999446e-01
Photon flux (15-150 keV) in 218.6 sec: 6.71788 ( -0.12623 0.12724 ) ph/cm2/s
Energy fluence (15-150 keV) : 0.000108903 ( -1.20936e-06 1.21037e-06 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 65.384 sec. to 66.384 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.36072 ( -0.0341517 0.0341962 )
Norm@50keV : 0.321643 ( -0.00590765 0.00590435 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 38.41 using 59 PHA bins.
# Reduced chi-squared = 0.6738 for 57 degrees of freedom
# Null hypothesis probability = 9.721531e-01
Photon flux (15-150 keV) in 1 sec: 1.73042 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.1343e-06 ( -5.8274e-08 5.83404e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 65.384 sec. to 66.384 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23549 ( -0.133637 0.138327 )
Epeak [keV] : 364.469 ( -158.588 -364.485 )
Norm@50keV : 0.363427 ( -0.0395014 0.0510549 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 35.90 using 59 PHA bins.
# Reduced chi-squared = 0.6410 for 56 degrees of freedom
# Null hypothesis probability = 9.832452e-01
Photon flux (15-150 keV) in 1 sec: 38.4639 ( -0.8912 0.8958 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.11652e-06 ( -6.15285e-08 6.13783e-08 ) ergs/cm2
Time-resolved spectra
