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 -0.272 sec. to 77.276 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.68437 ( -0.0238418 0.0239838 )
Norm@50keV : 3.67948E-02 ( -0.000473709 0.000471994 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 29.80 using 59 PHA bins.
# Reduced chi-squared = 0.5229 for 57 degrees of freedom
# Null hypothesis probability = 9.988905e-01
Photon flux (15-150 keV) in 77.55 sec: 4.86056 ( -0.0861 0.08665 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.6457e-05 ( -3.22078e-07 3.22423e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.272 sec. to 77.276 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.68239 ( -0.0223323 0.0263118 )
Epeak [keV] : 1.00000E+04 ( -9999.99 -10000 )
Norm@50keV : 3.68643E-02 ( -0.000435364 0.000435196 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 29.97 using 59 PHA bins.
# Reduced chi-squared = 0.5352 for 56 degrees of freedom
# Null hypothesis probability = 9.983093e-01
Photon flux (15-150 keV) in 77.55 sec: 4.85932 ( -0.08609 0.08678 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.6454e-05 ( -3.22664e-07 3.22365e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 40.452 sec. to 41.452 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.53419 ( -0.0296656 0.0296983 )
Norm@50keV : 0.322247 ( -0.00516307 0.00516064 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 71.83 using 59 PHA bins.
# Reduced chi-squared = 1.260 for 57 degrees of freedom
# Null hypothesis probability = 8.931898e-02
Photon flux (15-150 keV) in 1 sec: 40.6115 ( -0.7817 0.7845 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.0411e-06 ( -4.8353e-08 4.83417e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 40.452 sec. to 41.452 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.22252 ( -0.121138 0.124313 )
Epeak [keV] : 149.110 ( -25.8091 54.9216 )
Norm@50keV : 0.435706 ( -0.0470757 0.0540707 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.88 using 59 PHA bins.
# Reduced chi-squared = 0.9265 for 56 degrees of freedom
# Null hypothesis probability = 6.313722e-01
Photon flux (15-150 keV) in 1 sec: 39.4721 ( -0.8757 0.8817 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.97788e-06 ( 0 0 ) ergs/cm2
Time-resolved spectra
