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 5.432 sec. to 130.284 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26787 ( -0.209529 0.217572 )
Norm@50keV : 2.26080E-03 ( -0.000276093 0.000274706 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.72 using 59 PHA bins.
# Reduced chi-squared = 1.135 for 57 degrees of freedom
# Null hypothesis probability = 2.253132e-01
Photon flux (15-150 keV) in 124.9 sec: 0.268191 ( -0.035632 0.035879 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.81321e-06 ( -3.47327e-07 3.4792e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 5.432 sec. to 130.284 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26387 ( -2.56716 0.672569 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 2.27082E-03 ( -0.000276729 0.000271483 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.72 using 59 PHA bins.
# Reduced chi-squared = 1.156 for 56 degrees of freedom
# Null hypothesis probability = 1.984033e-01
Photon flux (15-150 keV) in 124.9 sec: 0.268785 ( -0.037638 0.036631 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.81774e-06 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 11.752 sec. to 12.752 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.852884 ( -0.481055 0.578361 )
Norm@50keV : 1.17459E-02 ( -0.00392367 0.00354011 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.99 using 59 PHA bins.
# Reduced chi-squared = 0.8945 for 57 degrees of freedom
# Null hypothesis probability = 6.989638e-01
Photon flux (15-150 keV) in 1 sec: 1.34825 ( -0.408935 0.42154 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.34317e-07 ( -3.35682e-08 3.35016e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 11.752 sec. to 12.752 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.848092 ( -0.482396 0.673746 )
Epeak [keV] : 9999.32 ( -9999.36 -9999.36 )
Norm@50keV : 1.18366E-02 ( -0.00367771 0.0245333 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.00 using 59 PHA bins.
# Reduced chi-squared = 0.9106 for 56 degrees of freedom
# Null hypothesis probability = 6.643142e-01
Photon flux (15-150 keV) in 1 sec: 1.34912 ( -0.410324 0.42041 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.34215e-07 ( -4.15598e-08 4.17312e-08 ) ergs/cm2
Time-resolved spectra
