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 0.000 sec. to 15.240 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.27706 ( -0.17998 0.181033 )
Norm@50keV : 3.14450E-03 ( -0.000308222 0.000307586 )
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#Fit statistic : Chi-Squared = 45.48 using 59 PHA bins.
# Reduced chi-squared = 0.7980 for 57 degrees of freedom
# Null hypothesis probability = 8.638064e-01
Photon flux (15-150 keV) in 15.24 sec: 0.373612 ( -0.037297 0.037401 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.76316e-07 ( -5.28823e-08 5.33662e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 15.240 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.27321 ( -0.224647 0.471801 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 3.15803E-03 ( -0.000309612 0.000307438 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 45.49 using 59 PHA bins.
# Reduced chi-squared = 0.8124 for 56 degrees of freedom
# Null hypothesis probability = 8.410031e-01
Photon flux (15-150 keV) in 15.24 sec: 0.375057 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 4.78051e-07 ( -6.03125e-08 5.71841e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 2.976 sec. to 3.976 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.790134 ( -0.386445 0.433769 )
Norm@50keV : 6.01303E-03 ( -0.00143684 0.00136464 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.75 using 59 PHA bins.
# Reduced chi-squared = 1.101 for 57 degrees of freedom
# Null hypothesis probability = 2.798247e-01
Photon flux (15-150 keV) in 1 sec: 0.691338 ( -0.154359 0.155612 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.05684e-08 ( -1.53823e-08 1.54121e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.976 sec. to 3.976 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.79365 ( -0.381536 0.593663 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 6.06691E-03 ( -0.00132484 0.0173236 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.76 using 59 PHA bins.
# Reduced chi-squared = 1.121 for 56 degrees of freedom
# Null hypothesis probability = 2.492625e-01
Photon flux (15-150 keV) in 1 sec: 0.691170 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 7.06529e-08 ( -1.61048e-08 1.59595e-08 ) ergs/cm2
Time-resolved spectra
