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 -1.556 sec. to 133.688 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.32621 ( -0.133534 0.128849 )
Norm@50keV : 1.93607E-03 ( -0.000166594 0.000164962 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.57 using 59 PHA bins.
# Reduced chi-squared = 0.9398 for 57 degrees of freedom
# Null hypothesis probability = 6.046140e-01
Photon flux (15-150 keV) in 135.2 sec: 0.343388 ( -0.020212 0.020237 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.51441e-06 ( -1.71763e-07 1.74937e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.556 sec. to 133.688 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.80709 ( -0.196156 0.710444 )
Epeak [keV] : 13.9350 ( -13.09 14.7885 )
Norm@50keV : 4.00065E-03 ( -0.00126996 0.00687024 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.35 using 59 PHA bins.
# Reduced chi-squared = 0.9169 for 56 degrees of freedom
# Null hypothesis probability = 6.513948e-01
Photon flux (15-150 keV) in 135.2 sec: 0.333312 ( -0.023153 0.022257 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.34767e-06 ( -2.32101e-07 2.2905e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 47.572 sec. to 48.572 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.98192 ( -0.188245 0.179039 )
Norm@50keV : 1.49746E-02 ( -0.00182973 0.00179149 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.53 using 59 PHA bins.
# Reduced chi-squared = 0.8515 for 57 degrees of freedom
# Null hypothesis probability = 7.801760e-01
Photon flux (15-150 keV) in 1 sec: 2.22789 ( -0.20928 0.20931 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.37997e-07 ( -1.57692e-08 1.61588e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 47.572 sec. to 48.572 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32483 ( -0.75187 0.926161 )
Epeak [keV] : 42.5606 ( )
Norm@50keV : 3.58774E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.36 using 59 PHA bins.
# Reduced chi-squared = 0.8279 for 56 degrees of freedom
# Null hypothesis probability = 8.172192e-01
Photon flux (15-150 keV) in 1 sec: 2.22858 ( -0.20902 0.20852 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
