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 0.532 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.666919 ( -0.16117 0.167705 )
Norm@50keV : 1.88406E-02 ( -0.00182394 0.00179944 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.20 using 59 PHA bins.
# Reduced chi-squared = 1.109 for 57 degrees of freedom
# Null hypothesis probability = 2.667864e-01
Photon flux (15-150 keV) in 0.532 sec: 2.18398 ( -0.19942 0.19969 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.24217e-07 ( -1.20123e-08 1.20752e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 0.532 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.529901 ( -0.420347 0.682908 )
Epeak [keV] : 664.065 ( -664.066 -664.066 )
Norm@50keV : 2.14698E-02 ( -0.00388361 0.018379 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.05 using 59 PHA bins.
# Reduced chi-squared = 1.126 for 56 degrees of freedom
# Null hypothesis probability = 2.410757e-01
Photon flux (15-150 keV) in 0.532 sec: 2.17513 ( -0.20318 0.20323 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.23715e-07 ( -1.24005e-08 1.212e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.234 sec. to 0.766 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.819864 ( -0.195034 0.202684 )
Norm@50keV : 1.03560E-02 ( -0.00117037 0.00116094 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.83 using 59 PHA bins.
# Reduced chi-squared = 1.067 for 57 degrees of freedom
# Null hypothesis probability = 3.396036e-01
Photon flux (15-150 keV) in 1 sec: 1.18949 ( -0.13219 0.13248 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.20033e-07 ( -1.44558e-08 1.45499e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.234 sec. to 0.766 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.67807 ( -0.233489 0.831622 )
Epeak [keV] : 547.082 ( -547.085 -547.085 )
Norm@50keV : 1.19468E-02 ( -0.00249259 0.0145479 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.73 using 59 PHA bins.
# Reduced chi-squared = 1.084 for 56 degrees of freedom
# Null hypothesis probability = 3.094790e-01
Photon flux (15-150 keV) in 1 sec: 1.18333 ( -0.13604 0.13477 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.19226e-07 ( -1.53058e-08 1.48065e-08 ) ergs/cm2
Time-resolved spectra
