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 -2.028 sec. to 61.696 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.992214 ( -0.159213 0.164542 )
Norm@50keV : 2.35260E-03 ( -0.000208598 0.000206442 )
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#Fit statistic : Chi-Squared = 53.28 using 59 PHA bins.
# Reduced chi-squared = 0.9347 for 57 degrees of freedom
# Null hypothesis probability = 6.153932e-01
Photon flux (15-150 keV) in 63.72 sec: 0.270744 ( -0.024566 0.024681 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.62568e-06 ( -1.43861e-07 1.44451e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -2.028 sec. to 61.696 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.986074 ( -0.224224 0.406973 )
Epeak [keV] : 9999.33 ( -9999.34 -9999.34 )
Norm@50keV : 2.36655E-03 ( -0.000205989 0.00112786 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.31 using 59 PHA bins.
# Reduced chi-squared = 0.9519 for 56 degrees of freedom
# Null hypothesis probability = 5.774262e-01
Photon flux (15-150 keV) in 63.72 sec: 0.270680 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 1.63044e-06 ( -1.86547e-07 1.79922e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.244 sec. to 1.244 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.822632 ( -0.32192 0.347208 )
Norm@50keV : 1.21987E-02 ( -0.00237469 0.00229355 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.51 using 59 PHA bins.
# Reduced chi-squared = 1.097 for 57 degrees of freedom
# Null hypothesis probability = 2.870833e-01
Photon flux (15-150 keV) in 1 sec: 1.40104 ( -0.26113 0.263 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.41228e-07 ( -2.57285e-08 2.57695e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.244 sec. to 1.244 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.814724 ( -0.484086 1.8854 )
Epeak [keV] : 9997.61 ( -9997.73 -9997.73 )
Norm@50keV : 1.22833E-02 ( -0.00221087 0.0467567 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.51 using 59 PHA bins.
# Reduced chi-squared = 1.116 for 56 degrees of freedom
# Null hypothesis probability = 2.562420e-01
Photon flux (15-150 keV) in 1 sec: 1.40225 ( -0.28035 0.26129 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.14101e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
