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 0.048 sec. to 0.640 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.88569 ( -0.248086 0.260389 )
Norm@50keV : 1.55121E-02 ( -0.00225674 0.0022446 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.49 using 59 PHA bins.
# Reduced chi-squared = 0.8507 for 57 degrees of freedom
# Null hypothesis probability = 7.814769e-01
Photon flux (15-150 keV) in 0.592 sec: 1.78028 ( -0.25807 0.25851 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03648e-07 ( -1.64429e-08 1.66205e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.048 sec. to 0.640 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.519825 ( -0.489487 1.11542 )
Epeak [keV] : 230.197 ( -230.197 -230.197 )
Norm@50keV : 2.26659E-02 ( -0.0090471 0.0440328 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.03 using 59 PHA bins.
# Reduced chi-squared = 0.8577 for 56 degrees of freedom
# Null hypothesis probability = 7.667165e-01
Photon flux (15-150 keV) in 0.592 sec: 1.75557 ( -0.26635 0.2657 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.01511e-07 ( -1.77229e-08 1.74932e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.156 sec. to 0.844 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.794507 ( -0.263769 0.281191 )
Norm@50keV : 9.88203E-03 ( -0.00168132 0.00166625 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.43 using 59 PHA bins.
# Reduced chi-squared = 1.113 for 57 degrees of freedom
# Null hypothesis probability = 2.600729e-01
Photon flux (15-150 keV) in 1 sec: 1.13596 ( -0.189092 0.1897 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.15766e-07 ( -2.03437e-08 2.05479e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.156 sec. to 0.844 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.965177 ( -1.34587 1.94412 )
Epeak [keV] : 95.7994 ( -23.6092 117.239 )
Norm@50keV : 5.90331E-02 ( -0.0590331 0.293154 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.00 using 59 PHA bins.
# Reduced chi-squared = 1.036 for 56 degrees of freedom
# Null hypothesis probability = 4.012907e-01
Photon flux (15-150 keV) in 1 sec: 1.06515 ( -0.196332 0.19759 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.04616e-07 ( -2.20084e-08 2.2661e-08 ) ergs/cm2
Time-resolved spectra
