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 -0.560 sec. to 6.116 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.72868 ( -0.0803243 0.0796071 )
Norm@50keV : 2.21167E-02 ( -0.000960723 0.000956696 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.60 using 59 PHA bins.
# Reduced chi-squared = 1.186 for 57 degrees of freedom
# Null hypothesis probability = 1.589957e-01
Photon flux (15-150 keV) in 6.676 sec: 2.96753 ( -0.13042 0.1309 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.36445e-06 ( -6.16218e-08 6.18375e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.560 sec. to 6.116 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.73009 ( -0.0790603 0.0822274 )
Epeak [keV] : 9999.29 ( -9999.35 -9999.36 )
Norm@50keV : 2.20796E-02 ( -0.00708595 0.00555418 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.62 using 59 PHA bins.
# Reduced chi-squared = 1.208 for 56 degrees of freedom
# Null hypothesis probability = 1.373128e-01
Photon flux (15-150 keV) in 6.676 sec: 2.98675 ( -0.15026 0.1119 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.36423e-06 ( -5.62014e-08 6.18608e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.65449 ( -0.0828892 0.0821027 )
Norm@50keV : 6.53178E-02 ( -0.00323374 0.00322237 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.50 using 59 PHA bins.
# Reduced chi-squared = 0.9562 for 57 degrees of freedom
# Null hypothesis probability = 5.692894e-01
Photon flux (15-150 keV) in 1 sec: 8.54188 ( -0.41887 0.4194 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.07295e-07 ( -3.1696e-08 3.18362e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 1.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.19628 ( -0.322238 0.348536 )
Epeak [keV] : 86.3861 ( -18.8341 82.7001 )
Norm@50keV : 0.112149 ( -0.0346971 0.0557271 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.40 using 59 PHA bins.
# Reduced chi-squared = 0.8643 for 56 degrees of freedom
# Null hypothesis probability = 7.548065e-01
Photon flux (15-150 keV) in 1 sec: 6.84585 ( -0.7608 0.65566 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.88085e-07 ( -3.47986e-08 3.47027e-08 ) ergs/cm2
Time-resolved spectra
