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 -0.328 sec. to 15.608 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42428 ( -0.273583 0.275902 )
Norm@50keV : 2.06708E-03 ( -0.000331202 0.000330223 )
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#Fit statistic : Chi-Squared = 81.15 using 59 PHA bins.
# Reduced chi-squared = 1.424 for 57 degrees of freedom
# Null hypothesis probability = 1.949568e-02
Photon flux (15-150 keV) in 15.94 sec: 0.253159 ( -0.041307 0.041486 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.16882e-07 ( -5.51374e-08 5.59626e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.328 sec. to 15.608 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.30653 ( -1.23578 2.07305 )
Epeak [keV] : 72.8971 ( -21.3844 -72.8796 )
Norm@50keV : 7.77779E-03 ( -0.00778483 0.0776228 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 79.30 using 59 PHA bins.
# Reduced chi-squared = 1.416 for 56 degrees of freedom
# Null hypothesis probability = 2.195390e-02
Photon flux (15-150 keV) in 15.94 sec: 0.239700 ( -0.045824 0.04506 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.85548e-07 ( -6.50325e-08 6.84403e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 2.572 sec. to 3.572 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.17454 ( -0.624447 0.692138 )
Norm@50keV : 4.11713E-03 ( -0.00135768 0.00133151 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.60 using 59 PHA bins.
# Reduced chi-squared = 1.046 for 57 degrees of freedom
# Null hypothesis probability = 3.813640e-01
Photon flux (15-150 keV) in 1 sec: 0.481608 ( -0.164924 0.166878 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.20814e-08 ( -1.45004e-08 1.4694e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.572 sec. to 3.572 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.1738 ( -0.615282 0.710963 )
Epeak [keV] : 61.6752 ( -9999.36 -9999.36 )
Norm@50keV : 1.07698E-03 ( -0.00108627 0.0178457 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.08 using 59 PHA bins.
# Reduced chi-squared = 1.055 for 56 degrees of freedom
# Null hypothesis probability = 3.635445e-01
Photon flux (15-150 keV) in 1 sec: 0.481800 ( -0.165145 0.16661 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.22727e-08 ( -1.66379e-08 1.64519e-08 ) ergs/cm2
Time-resolved spectra
