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 0.016 sec. to 0.372 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.868494 ( -0.244942 0.25627 )
Norm@50keV : 3.96136E-02 ( -0.00594644 0.00587144 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.23 using 59 PHA bins.
# Reduced chi-squared = 0.9865 for 57 degrees of freedom
# Null hypothesis probability = 5.038664e-01
Photon flux (15-150 keV) in 0.356 sec: 0.171835 0.193786 0.191382 0.188935 0.186678 0.184342 0.114949 7.50212E-02 5.37835E-02 4.27296E-02 3.67811E-02 3.13924E-02 2.65794E-02 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.60258e-07 ( -2.45111e-08 2.45837e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.016 sec. to 0.372 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.486533 ( -0.501304 1.28011 )
Epeak [keV] : 246.351 ( -246.321 -246.321 )
Norm@50keV : 5.70015E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.84 using 59 PHA bins.
# Reduced chi-squared = 0.9971 for 56 degrees of freedom
# Null hypothesis probability = 4.809578e-01
Photon flux (15-150 keV) in 0.356 sec: 4.49549 ( -0.67663 0.68994 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.59269e-07 ( -2.51189e-08 2.49272e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.304 sec. to 0.696 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.904721 ( -0.243922 0.258378 )
Norm@50keV : 1.84231E-02 ( -0.00296828 0.00292739 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.87 using 59 PHA bins.
# Reduced chi-squared = 0.9450 for 57 degrees of freedom
# Null hypothesis probability = 5.934008e-01
Photon flux (15-150 keV) in 1 sec: 2.11464 ( -0.33841 0.34083 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.064e-07 ( -3.21632e-08 3.22437e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.304 sec. to 0.696 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.550265 ( -1.23199 1.75178 )
Epeak [keV] : 107.364 ( -27.9155 221.663 )
Norm@50keV : 7.31570E-02 ( -0.0731571 0.253614 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.64 using 59 PHA bins.
# Reduced chi-squared = 0.8864 for 56 degrees of freedom
# Null hypothesis probability = 7.128785e-01
Photon flux (15-150 keV) in 1 sec: 2.01297 ( -0.34915 0.35259 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.98793e-07 ( -3.43028e-08 3.39464e-08 ) ergs/cm2
Time-resolved spectra
