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 -40.172 sec. to 272.972 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.06689 ( -0.173933 0.165508 )
Norm@50keV : 6.11414E-04 ( -7.08451e-05 6.95453e-05 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.53 using 59 PHA bins.
# Reduced chi-squared = 1.097 for 57 degrees of freedom
# Null hypothesis probability = 2.862826e-01
Photon flux (15-150 keV) in 313.1 sec: 9.46567E-02 ( -0.0081716 0.0081733 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.77371e-06 ( -1.85885e-07 1.90024e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -40.172 sec. to 272.972 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.29476 ( -0.698033 1.00386 )
Epeak [keV] : 36.0597 ( -34.4419 15.91 )
Norm@50keV : 1.76180E-03 ( -0.00109138 0.00534203 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.76 using 59 PHA bins.
# Reduced chi-squared = 1.067 for 56 degrees of freedom
# Null hypothesis probability = 3.406589e-01
Photon flux (15-150 keV) in 313.1 sec: 9.16470E-02 ( -0.0087099 0.008713 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.62276e-06 ( -2.1919e-07 2.39773e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -37.676 sec. to -36.676 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.56949 ( -0.733163 0.558766 )
Norm@50keV : 3.28866E-03 ( -0.00165737 0.00172448 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 64.17 using 59 PHA bins.
# Reduced chi-squared = 1.126 for 57 degrees of freedom
# Null hypothesis probability = 2.397810e-01
Photon flux (15-150 keV) in 1 sec: 0.674594 ( -0.212554 0.213486 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.35151e-08 ( -1.24754e-08 1.37478e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -37.676 sec. to -36.676 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 1.58475 ( -3.35102 7.25837 )
Epeak [keV] : 30.1260 ( -19.7381 8.55405 )
Norm@50keV : 1.48164 ( -1.77319 96687.4 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.47 using 59 PHA bins.
# Reduced chi-squared = 1.062 for 56 degrees of freedom
# Null hypothesis probability = 3.505674e-01
Photon flux (15-150 keV) in 1 sec: 0.656215 ( -0.203292 0.206972 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
