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 -8.296 sec. to 74.072 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32212 ( -0.220363 0.222576 )
Norm@50keV : 1.35570E-03 ( -0.000161861 0.00016117 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.11 using 59 PHA bins.
# Reduced chi-squared = 1.037 for 57 degrees of freedom
# Null hypothesis probability = 3.982528e-01
Photon flux (15-150 keV) in 82.37 sec: 0.162418 ( -0.01938 0.019421 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.09779e-06 ( -1.49894e-07 1.52096e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -8.296 sec. to 74.072 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32148 ( -0.21919 0.37797 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.36064E-03 ( -0.00136071 0.000847075 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.13 using 59 PHA bins.
# Reduced chi-squared = 1.056 for 56 degrees of freedom
# Null hypothesis probability = 3.619682e-01
Photon flux (15-150 keV) in 82.37 sec: 0.163673 ( -0.027836 0.025287 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.10688e-06 ( -2.09246e-07 1.94006e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.644 sec. to 1.644 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.06926 ( -0.300485 0.311629 )
Norm@50keV : 1.18336E-02 ( -0.00189477 0.00189335 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.88 using 59 PHA bins.
# Reduced chi-squared = 1.016 for 57 degrees of freedom
# Null hypothesis probability = 4.424354e-01
Photon flux (15-150 keV) in 1 sec: 1.36882 ( -0.2225 0.223 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.24977e-07 ( -2.30217e-08 2.33226e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.644 sec. to 1.644 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.07656 ( -0.291321 0.42398 )
Epeak [keV] : 9999.32 ( -9999.35 -9999.35 )
Norm@50keV : 1.18985E-02 ( -0.00190197 0.00190348 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 57.91 using 59 PHA bins.
# Reduced chi-squared = 1.034 for 56 degrees of freedom
# Null hypothesis probability = 4.047921e-01
Photon flux (15-150 keV) in 1 sec: 1.38154 ( -0.2357 0.20986 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.25617e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
