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 -0.440 sec. to 13.884 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.51625 ( -0.0545532 0.0545142 )
Norm@50keV : 1.82115E-02 ( -0.000542311 0.000542269 )
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#Fit statistic : Chi-Squared = 53.44 using 59 PHA bins.
# Reduced chi-squared = 0.9375 for 57 degrees of freedom
# Null hypothesis probability = 6.095474e-01
Photon flux (15-150 keV) in 14.32 sec: 2.28365 ( -0.07457 0.07477 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.46788e-06 ( -7.73566e-08 7.74436e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.440 sec. to 13.884 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.19556 ( -0.214879 0.225838 )
Epeak [keV] : 136.625 ( -35.0038 153.342 )
Norm@50keV : 2.56520E-02 ( -0.005134 0.00679332 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.79 using 59 PHA bins.
# Reduced chi-squared = 0.8355 for 56 degrees of freedom
# Null hypothesis probability = 8.048790e-01
Photon flux (15-150 keV) in 14.32 sec: 2.23520 ( -0.08053 0.08081 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.41965e-06 ( -8.43485e-08 8.39961e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.020 sec. to 1.020 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.00389 ( -0.0520721 0.0525137 )
Norm@50keV : 9.77956E-02 ( -0.00321003 0.00320571 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 82.33 using 59 PHA bins.
# Reduced chi-squared = 1.444 for 57 degrees of freedom
# Null hypothesis probability = 1.573321e-02
Photon flux (15-150 keV) in 1 sec: 0.418499 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.05616e-06 ( -3.58785e-08 3.59339e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.020 sec. to 1.020 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.313757 ( -0.229815 0.242363 )
Epeak [keV] : 143.397 ( -22.6061 41.657 )
Norm@50keV : 0.197149 ( -0.0399291 0.0527351 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.38 using 59 PHA bins.
# Reduced chi-squared = 0.9532 for 56 degrees of freedom
# Null hypothesis probability = 5.746726e-01
Photon flux (15-150 keV) in 1 sec: 2.01556E-04 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03899e-06 ( -3.73538e-08 3.72274e-08 ) ergs/cm2
Time-resolved spectra
