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 -0.208 sec. to 39.584 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23405 ( -0.292271 0.299205 )
Norm@50keV : 1.04899E-03 ( -0.000159148 0.000159139 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.80 using 59 PHA bins.
# Reduced chi-squared = 1.154 for 57 degrees of freedom
# Null hypothesis probability = 1.985151e-01
Photon flux (15-150 keV) in 39.79 sec: 0.123753 ( -0.019491 0.01955 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.1955e-07 ( -7.16021e-08 7.24262e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.208 sec. to 39.584 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.23334 ( -0.29112 0.341364 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.05359E-03 ( -0.000159773 0.00100676 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.81 using 59 PHA bins.
# Reduced chi-squared = 1.175 for 56 degrees of freedom
# Null hypothesis probability = 1.735288e-01
Photon flux (15-150 keV) in 39.79 sec: 0.123733 ( -0.019495 0.019545 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.19307e-07 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.204 sec. to 0.796 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.25186 ( -0.666531 0.700977 )
Norm@50keV : 3.16719E-03 ( -0.00101178 0.00100884 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 36.89 using 59 PHA bins.
# Reduced chi-squared = 0.6473 for 57 degrees of freedom
# Null hypothesis probability = 9.821702e-01
Photon flux (15-150 keV) in 1 sec: 0.374705 ( -0.123336 0.123677 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.16862e-08 ( -1.15067e-08 1.17698e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.204 sec. to 0.796 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.27467 ( -0.646759 0.732358 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 3.15215E-03 ( -0.00101144 0.0103614 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 36.91 using 59 PHA bins.
# Reduced chi-squared = 0.6591 for 56 degrees of freedom
# Null hypothesis probability = 9.771435e-01
Photon flux (15-150 keV) in 1 sec: 0.376972 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.15573e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
