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 4.984 sec. to 34.476 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.79148 ( -0.351569 0.330495 )
Norm@50keV : 1.18936E-03 ( -0.000279143 0.000271477 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.72 using 59 PHA bins.
# Reduced chi-squared = 1.013 for 57 degrees of freedom
# Null hypothesis probability = 4.485138e-01
Photon flux (15-150 keV) in 29.49 sec: 0.163362 ( -0.031099 0.031099 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.23054e-07 ( -7.51208e-08 7.88058e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 4.984 sec. to 34.476 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.734729 ( -2.34146 4.90323 )
Epeak [keV] : 38.5378 ( -7.89812 2896.5 )
Norm@50keV : 4.63414E-02 ( -0.0518332 50.3283 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.97 using 59 PHA bins.
# Reduced chi-squared = 0.9816 for 56 degrees of freedom
# Null hypothesis probability = 5.138205e-01
Photon flux (15-150 keV) in 29.49 sec: 0.148825 ( -0.031269 0.033653 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.34696e-07 ( -6.02401e-08 1.12981e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 33.570 sec. to 34.570 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.72093 ( -0.972747 0.829941 )
Norm@50keV : 3.06438E-03 ( -0.00164877 0.00147359 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.23 using 59 PHA bins.
# Reduced chi-squared = 0.7233 for 57 degrees of freedom
# Null hypothesis probability = 9.425664e-01
Photon flux (15-150 keV) in 1 sec: 0.410023 ( -0.169818 0.169825 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.83322e-08 ( -1.42085e-08 1.56463e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 33.570 sec. to 34.570 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.54627 ( -1.79814 4.77526 )
Epeak [keV] : 184.658 ( )
Norm@50keV : 1.12756E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.17 using 59 PHA bins.
# Reduced chi-squared = 0.7353 for 56 degrees of freedom
# Null hypothesis probability = 9.310211e-01
Photon flux (15-150 keV) in 1 sec: 0.410849 ( -0.170975 0.168991 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.80537e-08 ( -1.39072e-08 1.56794e-08 ) ergs/cm2
Time-resolved spectra
