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 -44.296 sec. to 133.688 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.48944 ( -0.141752 0.140513 )
Norm@50keV : 1.38660E-03 ( -0.000107983 0.000107372 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.30 using 59 PHA bins.
# Reduced chi-squared = 1.075 for 57 degrees of freedom
# Null hypothesis probability = 3.244203e-01
Photon flux (15-150 keV) in 178 sec: 0.172619 ( -0.013247 0.013271 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.34579e-06 ( -2.02455e-07 2.0462e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -44.296 sec. to 133.688 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.48939 ( -0.139892 0.14357 )
Epeak [keV] : 9999.22 ( -9999.36 -9999.36 )
Norm@50keV : 1.38881E-03 ( -0.00139033 0.000795429 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.31 using 59 PHA bins.
# Reduced chi-squared = 1.095 for 56 degrees of freedom
# Null hypothesis probability = 2.913244e-01
Photon flux (15-150 keV) in 178 sec: 0.173705 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 2.36793e-06 ( -2.30168e-07 1.79307e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 16.804 sec. to 17.804 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.50832 ( -0.442896 0.435065 )
Norm@50keV : 6.66721E-03 ( -0.00165302 0.0015933 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.79 using 59 PHA bins.
# Reduced chi-squared = 1.014 for 57 degrees of freedom
# Null hypothesis probability = 4.460446e-01
Photon flux (15-150 keV) in 1 sec: 0.834226 ( -0.190348 0.190624 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.31713e-08 ( -1.6947e-08 1.74667e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 16.804 sec. to 17.804 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.52007 ( -0.432987 1.00746 )
Epeak [keV] : 9999.34 ( -9999.36 -9999.36 )
Norm@50keV : 6.66440E-03 ( -0.00164834 0.0159544 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.79 using 59 PHA bins.
# Reduced chi-squared = 1.032 for 56 degrees of freedom
# Null hypothesis probability = 4.088281e-01
Photon flux (15-150 keV) in 1 sec: 0.836233 ( -0.194451 0.190297 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.25904e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
