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 -3.640 sec. to 149.552 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.86189 ( -0.183808 0.178105 )
Norm@50keV : 2.82300E-03 ( -0.000314075 0.000309855 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 89.68 using 59 PHA bins.
# Reduced chi-squared = 1.573 for 57 degrees of freedom
# Null hypothesis probability = 3.717259e-03
Photon flux (15-150 keV) in 153.2 sec: 0.398756 ( -0.041512 0.041639 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.97675e-06 ( -4.39313e-07 4.43417e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -3.640 sec. to 149.552 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.09203 ( -0.779836 0.951504 )
Epeak [keV] : 54.4157 ( -13.1487 516.403 )
Norm@50keV : 7.27530E-03 ( -0.00442873 0.0160311 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 86.87 using 59 PHA bins.
# Reduced chi-squared = 1.551 for 56 degrees of freedom
# Null hypothesis probability = 5.125119e-03
Photon flux (15-150 keV) in 153.2 sec: 0.384101 ( -0.04414 0.044185 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.73834e-06 ( -4.9174e-07 5.0325e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 3.896 sec. to 4.896 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.34866 ( -0.35113 0.30055 )
Norm@50keV : 1.56427E-02 ( -0.00430484 0.00424607 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 86.89 using 59 PHA bins.
# Reduced chi-squared = 1.524 for 57 degrees of freedom
# Null hypothesis probability = 6.556256e-03
Photon flux (15-150 keV) in 1 sec: 2.80912 ( -0.63041 0.63177 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.51091e-07 ( -3.61884e-08 3.66936e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 3.896 sec. to 4.896 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 1.76165 ( -1.98404 3.51112 )
Epeak [keV] : 38.9646 ( -6.56452 6.62208 )
Norm@50keV : 3.44635 ( -4.33177 291.534 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.16 using 59 PHA bins.
# Reduced chi-squared = 1.271 for 56 degrees of freedom
# Null hypothesis probability = 8.347744e-02
Photon flux (15-150 keV) in 1 sec: 2.78873 ( -0.63153 0.63498 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
