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 -1.744 sec. to 13.200 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.54334 ( -0.141504 0.14059 )
Norm@50keV : 1.18576E-02 ( -0.00096912 0.000966135 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.67 using 59 PHA bins.
# Reduced chi-squared = 0.9241 for 57 degrees of freedom
# Null hypothesis probability = 6.379863e-01
Photon flux (15-150 keV) in 14.94 sec: 1.49827 ( -0.12829 0.12866 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.66956e-06 ( -1.44417e-07 1.45081e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.744 sec. to 13.200 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.34147 ( -0.324936 0.595242 )
Epeak [keV] : 173.179 ( -173.179 -173.179 )
Norm@50keV : 1.48494E-02 ( -0.0148494 0.0134432 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.27 using 59 PHA bins.
# Reduced chi-squared = 0.9335 for 56 degrees of freedom
# Null hypothesis probability = 6.166998e-01
Photon flux (15-150 keV) in 14.94 sec: 1.48443 ( -0.13331 0.13364 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.65287e-06 ( -1.52839e-07 1.51726e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.652 sec. to 0.348 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.53579 ( -0.225057 0.224616 )
Norm@50keV : 2.75375E-02 ( -0.0041068 0.00409865 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.58 using 59 PHA bins.
# Reduced chi-squared = 0.8522 for 57 degrees of freedom
# Null hypothesis probability = 7.787775e-01
Photon flux (15-150 keV) in 1 sec: 3.47207 ( -0.53362 0.53539 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.59806e-07 ( -4.06012e-08 4.08016e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.652 sec. to 0.348 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.157096 ( -1.04166 1.39283 )
Epeak [keV] : 66.4253 ( -14.1655 54.6931 )
Norm@50keV : 0.140041 ( -0.140041 0.572292 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.10 using 59 PHA bins.
# Reduced chi-squared = 0.7697 for 56 degrees of freedom
# Null hypothesis probability = 8.966477e-01
Photon flux (15-150 keV) in 1 sec: 3.37575 ( -0.53913 0.54137 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.45076e-07 ( -4.22424e-08 4.28229e-08 ) ergs/cm2
Time-resolved spectra
