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 0.060 sec. to 2.488 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.15548 ( -0.294583 0.303173 )
Norm@50keV : 4.57827E-03 ( -0.000655353 0.000655296 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.54 using 59 PHA bins.
# Reduced chi-squared = 1.255 for 57 degrees of freedom
# Null hypothesis probability = 9.309568e-02
Photon flux (15-150 keV) in 2.428 sec: 0.534259 ( -0.078983 0.079194 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.14264e-07 ( -1.89582e-08 1.91524e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.060 sec. to 2.488 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.15258 ( -0.272275 0.279751 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 4.60080E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.58 using 59 PHA bins.
# Reduced chi-squared = 1.278 for 56 degrees of freedom
# Null hypothesis probability = 7.841989e-02
Photon flux (15-150 keV) in 2.428 sec: 0.212325 ( -0.122966 0.113928 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.14116e-07 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.010 sec. to 0.990 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.13513 ( -0.41311 0.424513 )
Norm@50keV : 5.72711E-03 ( -0.00104506 0.00104505 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.43 using 59 PHA bins.
# Reduced chi-squared = 1.218 for 57 degrees of freedom
# Null hypothesis probability = 1.250103e-01
Photon flux (15-150 keV) in 1 sec: 0.666709 ( -0.125502 0.125571 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.92407e-08 ( -1.30175e-08 1.31312e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.010 sec. to 0.990 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.13622 ( -0.372179 0.479702 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 5.75376E-03 ( -0.00104885 -0.00575377 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.46 using 59 PHA bins.
# Reduced chi-squared = 1.240 for 56 degrees of freedom
# Null hypothesis probability = 1.066716e-01
Photon flux (15-150 keV) in 1 sec: 0.299375 ( -0.299375 0.195412 ) ph/cm2/s
Energy fluence (15-150 keV) : 5.90269e-08 ( -1.28505e-08 1.32867e-08 ) ergs/cm2
Time-resolved spectra
