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 -0.208 sec. to 0.328 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.64518 ( -0.227075 0.220136 )
Norm@50keV : 1.30708E-02 ( -0.00190965 0.00187761 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.18 using 59 PHA bins.
# Reduced chi-squared = 1.144 for 57 degrees of freedom
# Null hypothesis probability = 2.135354e-01
Photon flux (15-150 keV) in 0.536 sec: 1.70409 ( -0.22621 0.22628 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.52012e-08 ( -1.00386e-08 1.01942e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.208 sec. to 0.328 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.09883 ( -0.721405 1.24466 )
Epeak [keV] : 72.8519 ( -25.8901 -72.7758 )
Norm@50keV : 2.65474E-02 ( -0.0150449 0.110482 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.24 using 59 PHA bins.
# Reduced chi-squared = 1.147 for 56 degrees of freedom
# Null hypothesis probability = 2.101635e-01
Photon flux (15-150 keV) in 0.536 sec: 1.67856 ( -0.23207 0.23113 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.17585e-08 ( -1.18269e-08 1.1797e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.438 sec. to 0.562 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.83598 ( -0.248678 0.235974 )
Norm@50keV : 7.90359E-03 ( -0.00134905 0.00131953 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.60 using 59 PHA bins.
# Reduced chi-squared = 1.133 for 57 degrees of freedom
# Null hypothesis probability = 2.283204e-01
Photon flux (15-150 keV) in 1 sec: 1.10472 ( -0.156276 0.15629 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.27009e-08 ( -1.22768e-08 1.25875e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.438 sec. to 0.562 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.370597 ( -1.30859 1.91545 )
Epeak [keV] : 43.5858 ( -8.99171 43.1545 )
Norm@50keV : 6.03227E-02 ( -0.0604063 0.873754 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.86 using 59 PHA bins.
# Reduced chi-squared = 1.087 for 56 degrees of freedom
# Null hypothesis probability = 3.051910e-01
Photon flux (15-150 keV) in 1 sec: 1.06252 ( -0.159315 0.16044 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.22874e-08 ( -1.26579e-08 1.51409e-08 ) ergs/cm2
Time-resolved spectra
