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 -0.004 sec. to 0.040 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.750084 ( -0.26986 0.28065 )
Norm@50keV : 7.33989E-02 ( -0.0111179 0.0110269 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.55 using 59 PHA bins.
# Reduced chi-squared = 0.9395 for 57 degrees of freedom
# Null hypothesis probability = 6.052387e-01
Photon flux (15-150 keV) in 0.044 sec: 0.586985 0.397246 0.275941 0.203337 0.161095 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.85587e-08 ( -6.59168e-09 6.64585e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.004 sec. to 0.040 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.742576 ( -0.346102 0.836057 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 7.39459E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.57 using 59 PHA bins.
# Reduced chi-squared = 0.9565 for 56 degrees of freedom
# Null hypothesis probability = 5.675645e-01
Photon flux (15-150 keV) in 0.044 sec: 8.48683 ( -1.50605 1.43989 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.480 sec. to 0.520 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.961571 ( -0.540749 0.592194 )
Norm@50keV : 4.69875E-03 ( -0.00132249 0.00128231 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.75 using 59 PHA bins.
# Reduced chi-squared = 1.154 for 57 degrees of freedom
# Null hypothesis probability = 1.996795e-01
Photon flux (15-150 keV) in 1 sec: 0.540040 ( -0.150381 0.151292 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.15252e-08 ( -1.53759e-08 1.56192e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.480 sec. to 0.520 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.968379 ( -0.532748 0.609977 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 4.73331E-03 ( -0.00128995 0.0165651 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.76 using 59 PHA bins.
# Reduced chi-squared = 1.174 for 56 degrees of freedom
# Null hypothesis probability = 1.747159e-01
Photon flux (15-150 keV) in 1 sec: 0.539994 ( -0.150491 0.151155 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.13606e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
