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 -1.928 sec. to 12.408 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.9646 ( -0.190435 0.179694 )
Norm@50keV : 5.35846E-03 ( -0.000675567 0.000661932 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.64 using 59 PHA bins.
# Reduced chi-squared = 0.9059 for 57 degrees of freedom
# Null hypothesis probability = 6.758036e-01
Photon flux (15-150 keV) in 14.34 sec: 0.791020 ( -0.07782 0.077833 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.07619e-07 ( -8.43876e-08 8.62324e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.928 sec. to 12.408 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.968204 ( -0.778717 0.950282 )
Epeak [keV] : 43.8469 ( -11.3306 17.9375 )
Norm@50keV : 1.97697E-02 ( -0.0124904 0.0494408 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.63 using 59 PHA bins.
# Reduced chi-squared = 0.8327 for 56 degrees of freedom
# Null hypothesis probability = 8.095638e-01
Photon flux (15-150 keV) in 14.34 sec: 0.761208 ( -0.080586 0.080798 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.46918e-07 ( -8.92066e-08 9.53819e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.324 sec. to 2.324 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.05878 ( -0.392056 0.347403 )
Norm@50keV : 1.09533E-02 ( -0.00284461 0.00270444 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 76.40 using 59 PHA bins.
# Reduced chi-squared = 1.340 for 57 degrees of freedom
# Null hypothesis probability = 4.413103e-02
Photon flux (15-150 keV) in 1 sec: 1.68915 ( -0.29768 0.29771 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.01419e-07 ( -2.30508e-08 2.41724e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.324 sec. to 2.324 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.12806 ( -0.108793 1.12594 )
Epeak [keV] : 66.5778 ( )
Norm@50keV : 9.85687E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 76.28 using 59 PHA bins.
# Reduced chi-squared = 1.362 for 56 degrees of freedom
# Null hypothesis probability = 3.708749e-02
Photon flux (15-150 keV) in 1 sec: 1.66472 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
