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 0.000 sec. to 7.460 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.8009 ( -0.560347 0.519496 )
Norm@50keV : 1.15642E-02 ( -0.0035987 0.00349883 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.00 using 59 PHA bins.
# Reduced chi-squared = 0.9824 for 57 degrees of freedom
# Null hypothesis probability = 5.127505e-01
Photon flux (15-150 keV) in 7.46 sec: 1.59416 ( -0.49909 0.50656 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.94289e-07 ( -2.44686e-07 2.4721e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 7.460 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.45522 ( -1.08221 2.68991 )
Epeak [keV] : 82.1216 ( )
Norm@50keV : 1.70968E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 55.91 using 59 PHA bins.
# Reduced chi-squared = 0.9983 for 56 degrees of freedom
# Null hypothesis probability = 4.784055e-01
Photon flux (15-150 keV) in 7.46 sec: 1.56601 ( -0.5248 0.5248 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.300 sec. to 1.300 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.34055 ( -0.395932 0.398579 )
Norm@50keV : 4.99247E-02 ( -0.0118401 0.0118225 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.79 using 59 PHA bins.
# Reduced chi-squared = 0.7507 for 57 degrees of freedom
# Null hypothesis probability = 9.187962e-01
Photon flux (15-150 keV) in 1 sec: 6.00296 ( -1.51899 1.539 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.88709e-07 ( -1.19995e-07 1.20365e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.300 sec. to 1.300 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.184414 ( -1.41678 2.85592 )
Epeak [keV] : 92.8469 ( -33.9636 -92.8409 )
Norm@50keV : 0.157427 ( -0.157466 1.85706 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.63 using 59 PHA bins.
# Reduced chi-squared = 0.7434 for 56 degrees of freedom
# Null hypothesis probability = 9.237264e-01
Photon flux (15-150 keV) in 1 sec: 1.35683 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 4.75795e-07 ( -1.24777e-07 1.243e-07 ) ergs/cm2
Time-resolved spectra
