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 -5.304 sec. to 14.456 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.0881 ( -0.112278 0.115059 )
Norm@50keV : 2.44966E-02 ( -0.00172134 0.0017071 )
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#Fit statistic : Chi-Squared = 47.74 using 59 PHA bins.
# Reduced chi-squared = 0.8376 for 57 degrees of freedom
# Null hypothesis probability = 8.038973e-01
Photon flux (15-150 keV) in 19.76 sec: 2.83825 ( -0.21057 0.21187 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.08085e-06 ( -3.34203e-07 3.34505e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -5.304 sec. to 14.456 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.694585 ( -0.431476 0.508788 )
Epeak [keV] : 208.387 ( -83.0502 -208.387 )
Norm@50keV : 3.54624E-02 ( -0.0115361 0.0205984 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.61 using 59 PHA bins.
# Reduced chi-squared = 0.8145 for 56 degrees of freedom
# Null hypothesis probability = 8.379210e-01
Photon flux (15-150 keV) in 19.76 sec: 2.78903 ( -0.2163 0.21835 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.05461e-06 ( -3.39226e-07 3.38473e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 13.580 sec. to 14.580 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.17324 ( -0.360898 0.378768 )
Norm@50keV : 3.54846E-02 ( -0.00767654 0.00758637 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.12 using 59 PHA bins.
# Reduced chi-squared = 0.9143 for 57 degrees of freedom
# Null hypothesis probability = 6.584082e-01
Photon flux (15-150 keV) in 1 sec: 4.15018 ( -0.94664 0.95606 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.62819e-07 ( -7.86806e-08 7.87616e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 13.580 sec. to 14.580 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.11841 ( )
Epeak [keV] : 933.214 ( )
Norm@50keV : 3.75315E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.12 using 59 PHA bins.
# Reduced chi-squared = 0.9306 for 56 degrees of freedom
# Null hypothesis probability = 6.226614e-01
Photon flux (15-150 keV) in 1 sec: 4.14445 ( -0.97751 0.92078 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.62493e-07 ( -8.03495e-08 7.74536e-08 ) ergs/cm2
Time-resolved spectra
