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 -4.464 sec. to 92.356 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.49674 ( -0.18038 0.177741 )
Norm@50keV : 1.12576E-03 ( -0.000114167 0.000112954 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.36 using 59 PHA bins.
# Reduced chi-squared = 0.9712 for 57 degrees of freedom
# Null hypothesis probability = 5.367886e-01
Photon flux (15-150 keV) in 96.82 sec: 0.140420 ( -0.013522 0.013537 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03468e-06 ( -1.16862e-07 1.18631e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -4.464 sec. to 92.356 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.49427 ( -0.927256 0.625071 )
Epeak [keV] : 9997.37 ( -9997.65 -9997.65 )
Norm@50keV : 1.12914E-03 ( -0.000677655 0.00134556 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.36 using 59 PHA bins.
# Reduced chi-squared = 0.9886 for 56 degrees of freedom
# Null hypothesis probability = 4.989724e-01
Photon flux (15-150 keV) in 96.82 sec: 0.140553 ( -0.014144 0.013481 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03616e-06 ( -1.3385e-07 9.24032e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 53.120 sec. to 54.120 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.775289 ( -0.947265 1.35635 )
Norm@50keV : 2.82082E-03 ( -0.00161925 0.00112687 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.50 using 59 PHA bins.
# Reduced chi-squared = 1.096 for 57 degrees of freedom
# Null hypothesis probability = 2.873511e-01
Photon flux (15-150 keV) in 1 sec: 0.324171 ( -0.324171 0.131341 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.33511e-08 ( -1.36391e-08 1.33944e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 53.120 sec. to 54.120 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -3.82568 ( 3.86004 3.98024 )
Epeak [keV] : 429.423 ( )
Norm@50keV : 1.63118E-04 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.98 using 59 PHA bins.
# Reduced chi-squared = 1.089 for 56 degrees of freedom
# Null hypothesis probability = 3.014301e-01
Photon flux (15-150 keV) in 1 sec: 0.119266 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.31444e-08 ( -1.34728e-08 1.35742e-08 ) ergs/cm2
Time-resolved spectra
