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 -36.080 sec. to 302.308 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23993 ( -0.0207847 0.0208776 )
Norm@50keV : 2.13272E-02 ( -0.000271273 0.000270639 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 35.42 using 59 PHA bins.
# Reduced chi-squared = 0.6213 for 57 degrees of freedom
# Null hypothesis probability = 9.889731e-01
Photon flux (15-150 keV) in 338.4 sec: 2.51838 ( -0.03679 0.03691 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.24305e-05 ( -7.99568e-07 7.98076e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -36.080 sec. to 302.308 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.10491 ( -0.0859186 0.0875752 )
Epeak [keV] : 449.104 ( -147.568 644.478 )
Norm@50keV : 2.39150E-02 ( -0.0016394 0.00180231 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 28.25 using 59 PHA bins.
# Reduced chi-squared = 0.5045 for 56 degrees of freedom
# Null hypothesis probability = 9.992751e-01
Photon flux (15-150 keV) in 338.4 sec: 1.46388 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 7.22322e-05 ( -8.07138e-07 8.09456e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 35.096 sec. to 36.096 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.00168 ( -0.0409705 0.0411196 )
Norm@50keV : 0.224092 ( -0.00510883 0.00510409 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.07 using 59 PHA bins.
# Reduced chi-squared = 0.7557 for 57 degrees of freedom
# Null hypothesis probability = 9.138772e-01
Photon flux (15-150 keV) in 1 sec: 1.21964 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 2.42203e-06 ( -5.93767e-08 5.94455e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 35.096 sec. to 36.096 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.793032 ( -0.160094 0.166757 )
Epeak [keV] : 344.914 ( -125.556 831.738 )
Norm@50keV : 0.275150 ( -0.0384653 0.0475488 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 38.13 using 59 PHA bins.
# Reduced chi-squared = 0.6808 for 56 degrees of freedom
# Null hypothesis probability = 9.676332e-01
Photon flux (15-150 keV) in 1 sec: 25.5400 ( -0.6308 0.6316 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.40077e-06 ( -6.21482e-08 6.20348e-08 ) ergs/cm2
Time-resolved spectra
