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 -1.864 sec. to 5.384 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.40921 ( -0.360645 0.361643 )
Norm@50keV : 5.21334E-03 ( -0.00103793 0.00103505 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 49.18 using 59 bins.
Reduced chi-squared = 0.862807
# Null hypothesis probability of 7.60e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 7.248 sec: 0.636239 ( -0.131284 0.132025 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.64484e-07 ( -7.89032e-08 7.96439e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.864 sec. to 5.384 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.40635 ( -3.01609 1.40669 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 5.23176E-03 ( -0.00104327 -0.00523179 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 49.18 using 59 bins.
Reduced chi-squared = 0.878214
# Null hypothesis probability of 7.29e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 7.248 sec: 0.639194 ( -0.145695 0.136288 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.65038e-07 ( -7.58054e-08 6.75136e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.364 sec. to 1.364 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.3224 ( -0.461171 0.484881 )
Norm@50keV : 1.08146E-02 ( -0.00282423 0.00282662 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 44.13 using 59 bins.
Reduced chi-squared = 0.774211
# Null hypothesis probability of 8.94e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 1.29570 ( -0.361279 0.36386 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.06309e-07 ( -2.94048e-08 2.95536e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.364 sec. to 1.364 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32582 ( -0.458369 0.493864 )
Epeak [keV] : 9999.35 ( -9999.36 -9999.36 )
Norm@50keV : 1.08375E-02 ( -0.00283563 0.00283616 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 44.14 using 59 bins.
Reduced chi-squared = 0.788214
# Null hypothesis probability of 8.74e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 1.30568 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.06574e-07 ( -3.08524e-08 2.55312e-08 ) ergs/cm2
Time-resolved spectra
