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 -0.444 sec. to 95.768 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.62848 ( -0.144571 0.142904 )
Norm@50keV : 1.71904E-03 ( -0.000139227 0.000137782 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.41 using 59 PHA bins.
# Reduced chi-squared = 0.9896 for 57 degrees of freedom
# Null hypothesis probability = 4.973221e-01
Photon flux (15-150 keV) in 96.21 sec: 0.222905 ( -0.017152 0.017191 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.54188e-06 ( -1.33921e-07 1.3534e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.444 sec. to 95.768 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.12844 ( -0.138374 0.153514 )
Epeak [keV] : 50.0426 ( -9999.35 -9999.36 )
Norm@50keV : 9.25714E-04 ( -0.000110235 0.000197258 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.86 using 59 PHA bins.
# Reduced chi-squared = 0.9619 for 56 degrees of freedom
# Null hypothesis probability = 5.561166e-01
Photon flux (15-150 keV) in 96.21 sec: 0.222899 ( -0.017174 0.017173 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.57072e-06 ( -1.63218e-07 1.05995e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 14.392 sec. to 15.392 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.31784 ( -0.409536 0.427064 )
Norm@50keV : 6.40191E-03 ( -0.00143698 0.00143343 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.41 using 59 PHA bins.
# Reduced chi-squared = 1.025 for 57 degrees of freedom
# Null hypothesis probability = 4.233681e-01
Photon flux (15-150 keV) in 1 sec: 0.766341 ( -0.176313 0.176994 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.29985e-08 ( -1.56877e-08 1.59602e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 14.392 sec. to 15.392 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32496 ( -0.402516 0.439052 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 6.42261E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.42 using 59 PHA bins.
# Reduced chi-squared = 1.043 for 56 degrees of freedom
# Null hypothesis probability = 3.866569e-01
Photon flux (15-150 keV) in 1 sec: 0.768335 ( -0.17073 0.176037 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.29492e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
