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 -0.500 sec. to 0.644 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.772853 ( -0.321574 0.349206 )
Norm@50keV : 9.82661E-03 ( -0.00188396 0.0018102 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.15 using 59 PHA bins.
# Reduced chi-squared = 0.8974 for 57 degrees of freedom
# Null hypothesis probability = 6.931728e-01
Photon flux (15-150 keV) in 1.144 sec: 1.13064 ( -0.203431 0.20488 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.32906e-07 ( -2.35722e-08 2.36266e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.500 sec. to 0.644 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.773466 ( -0.31731 0.359579 )
Epeak [keV] : 9999.33 ( -9999.36 -9999.36 )
Norm@50keV : 9.90778E-03 ( -0.00174531 0.0177629 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.16 using 59 PHA bins.
# Reduced chi-squared = 0.9135 for 56 degrees of freedom
# Null hypothesis probability = 6.583249e-01
Photon flux (15-150 keV) in 1.144 sec: 1.13282 ( -0.2082 0.20058 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.03294e-08 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.364 sec. to 0.636 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.878173 ( -0.345318 0.372809 )
Norm@50keV : 9.90319E-03 ( -0.00196394 0.00191268 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.95 using 59 PHA bins.
# Reduced chi-squared = 0.8587 for 57 degrees of freedom
# Null hypothesis probability = 7.672239e-01
Photon flux (15-150 keV) in 1 sec: 1.13656 ( -0.220728 0.22183 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.12106e-07 ( -2.22473e-08 2.23468e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.364 sec. to 0.636 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.802397 ( )
Epeak [keV] : 989.203 ( )
Norm@50keV : 1.06322E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.03 using 59 PHA bins.
# Reduced chi-squared = 0.8756 for 56 degrees of freedom
# Null hypothesis probability = 7.336663e-01
Photon flux (15-150 keV) in 1 sec: 1.14439 ( -0.257828 0.2395 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.12336e-07 ( -2.49363e-08 2.45913e-08 ) ergs/cm2
Time-resolved spectra
