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 -0.072 sec. to 8.716 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.11795 ( -0.385241 0.408326 )
Norm@50keV : 1.98798E-03 ( -0.000373191 0.000370257 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.24 using 59 PHA bins.
# Reduced chi-squared = 1.092 for 57 degrees of freedom
# Null hypothesis probability = 2.951490e-01
Photon flux (15-150 keV) in 8.788 sec: 0.231007 ( -0.045264 0.045361 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.81648e-07 ( -3.77217e-08 3.79509e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.072 sec. to 8.716 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.11557 ( -0.357498 0.445559 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 1.99848E-03 ( -0.000370089 -0.00199847 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.27 using 59 PHA bins.
# Reduced chi-squared = 1.112 for 56 degrees of freedom
# Null hypothesis probability = 2.631191e-01
Photon flux (15-150 keV) in 8.788 sec: 0.231079 ( -0.045398 0.045233 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.81355e-07 ( -3.75285e-08 3.80969e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.532 sec. to 2.532 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.5517 ( -0.781783 0.678913 )
Norm@50keV : 3.25643E-03 ( -0.00132059 0.00115707 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.69 using 59 PHA bins.
# Reduced chi-squared = 1.293 for 57 degrees of freedom
# Null hypothesis probability = 6.761998e-02
Photon flux (15-150 keV) in 1 sec: 0.412464 ( -0.136939 0.136811 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.06507e-08 ( -1.25536e-08 1.28203e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.532 sec. to 2.532 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.23821 ( -1.2632 1.82496 )
Epeak [keV] : 87.3210 ( )
Norm@50keV : 1.45389E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.02 using 59 PHA bins.
# Reduced chi-squared = 1.304 for 56 degrees of freedom
# Null hypothesis probability = 6.290808e-02
Photon flux (15-150 keV) in 1 sec: 0.305212 ( -0.305212 0.14707 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.01398e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
