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 -29.016 sec. to 36.940 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.72205 ( -0.240581 0.236162 )
Norm@50keV : 2.14004E-03 ( -0.000290052 0.00028677 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.77 using 59 PHA bins.
# Reduced chi-squared = 1.259 for 57 degrees of freedom
# Null hypothesis probability = 9.011103e-02
Photon flux (15-150 keV) in 65.96 sec: 0.286459 ( -0.038827 0.039046 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.305e-06 ( -1.82152e-07 1.84022e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -29.016 sec. to 36.940 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.55058 ( -0.833897 0.980561 )
Epeak [keV] : 129.856 ( -129.854 -129.854 )
Norm@50keV : 2.61513E-03 ( -0.000756533 0.00533001 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.65 using 59 PHA bins.
# Reduced chi-squared = 1.279 for 56 degrees of freedom
# Null hypothesis probability = 7.760368e-02
Photon flux (15-150 keV) in 65.96 sec: 0.283707 ( -0.04118 0.038446 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.28793e-06 ( -2.01076e-07 1.96163e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 32.184 sec. to 33.184 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.94931 ( -0.681477 0.605855 )
Norm@50keV : 6.74221E-03 ( -0.00255052 0.00234089 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.38 using 59 PHA bins.
# Reduced chi-squared = 0.8838 for 57 degrees of freedom
# Null hypothesis probability = 7.199909e-01
Photon flux (15-150 keV) in 1 sec: 0.988544 ( -0.309954 0.312156 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.20555e-08 ( -2.11379e-08 2.19176e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 32.184 sec. to 33.184 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.94072 ( -1.66945 1.88835 )
Epeak [keV] : 350.793 ( )
Norm@50keV : 6.81968E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.38 using 59 PHA bins.
# Reduced chi-squared = 0.8997 for 56 degrees of freedom
# Null hypothesis probability = 6.865754e-01
Photon flux (15-150 keV) in 1 sec: 0.969311 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 6.28507e-08 ( -5.96119e-08 1.83594e-08 ) ergs/cm2
Time-resolved spectra
