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 -35.680 sec. to 27.952 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.84527 ( -0.102385 0.100588 )
Norm@50keV : 2.96943E-03 ( -0.000181775 0.000180288 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.68 using 59 PHA bins.
# Reduced chi-squared = 1.030 for 57 degrees of freedom
# Null hypothesis probability = 4.135033e-01
Photon flux (15-150 keV) in 63.63 sec: 0.416609 ( -0.023586 0.023623 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.73769e-06 ( -1.06661e-07 1.07503e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -35.680 sec. to 27.952 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.21814 ( -0.441775 0.497502 )
Epeak [keV] : 57.2582 ( -9.44077 29.9469 )
Norm@50keV : 6.42731E-03 ( -0.00265519 0.00534251 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.57 using 59 PHA bins.
# Reduced chi-squared = 0.9388 for 56 degrees of freedom
# Null hypothesis probability = 6.054401e-01
Photon flux (15-150 keV) in 63.63 sec: 0.402916 ( -0.025463 0.02541 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.6423e-06 ( -1.23912e-07 1.25295e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 7.940 sec. to 8.940 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.65906 ( -0.124378 0.122207 )
Norm@50keV : 2.31435E-02 ( -0.00175725 0.00174509 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.78 using 59 PHA bins.
# Reduced chi-squared = 1.066 for 57 degrees of freedom
# Null hypothesis probability = 3.412683e-01
Photon flux (15-150 keV) in 1 sec: 3.03117 ( -0.2212 0.22144 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.1508e-07 ( -1.72054e-08 1.73381e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 7.940 sec. to 8.940 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.19407 ( -0.469514 0.531042 )
Epeak [keV] : 84.0564 ( -23.3219 905.077 )
Norm@50keV : 4.04227E-02 ( -0.0170438 0.0353323 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.91 using 59 PHA bins.
# Reduced chi-squared = 1.034 for 56 degrees of freedom
# Null hypothesis probability = 4.045862e-01
Photon flux (15-150 keV) in 1 sec: 2.97663 ( -0.22805 0.22804 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.08166e-07 ( -1.88314e-08 1.87839e-08 ) ergs/cm2
Time-resolved spectra
