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 -33.112 sec. to 211.088 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.43457 ( -0.108985 0.108447 )
Norm@50keV : 1.55989E-03 ( -9.3659e-05 9.33196e-05 )
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#Fit statistic : Chi-Squared = 36.82 using 59 PHA bins.
# Reduced chi-squared = 0.6459 for 57 degrees of freedom
# Null hypothesis probability = 9.825965e-01
Photon flux (15-150 keV) in 244.2 sec: 0.191513 ( -0.011302 0.011314 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.65616e-06 ( -2.47643e-07 2.50229e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -33.112 sec. to 211.088 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.17698 ( -0.309532 0.456159 )
Epeak [keV] : 158.823 ( -72.0188 -158.823 )
Norm@50keV : 2.10233E-03 ( -0.000609899 0.00141775 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 35.71 using 59 PHA bins.
# Reduced chi-squared = 0.6377 for 56 degrees of freedom
# Null hypothesis probability = 9.841947e-01
Photon flux (15-150 keV) in 244.2 sec: 0.188580 ( -0.012259 0.012221 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.56324e-06 ( -2.89494e-07 2.89726e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 148.564 sec. to 149.564 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26758 ( -0.203968 0.204819 )
Norm@50keV : 1.35623E-02 ( -0.00156648 0.00155734 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.26 using 59 PHA bins.
# Reduced chi-squared = 0.9344 for 57 degrees of freedom
# Null hypothesis probability = 6.160660e-01
Photon flux (15-150 keV) in 1 sec: 1.60876 ( -0.18182 0.1819 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.35126e-07 ( -1.82084e-08 1.84842e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 148.564 sec. to 149.564 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.26195 ( -0.207032 0.355701 )
Epeak [keV] : 9999.32 ( -9999.36 -9999.36 )
Norm@50keV : 1.36241E-02 ( -0.013623 0.00825932 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.28 using 59 PHA bins.
# Reduced chi-squared = 0.9514 for 56 degrees of freedom
# Null hypothesis probability = 5.784344e-01
Photon flux (15-150 keV) in 1 sec: 1.61747 ( -0.25174 0.23395 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.49593e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
