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 2.120 sec. to 84.744 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.21898 ( -0.158633 0.16236 )
Norm@50keV : 1.93227E-03 ( -0.000181364 0.000180787 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.16 using 59 PHA bins.
# Reduced chi-squared = 0.8449 for 57 degrees of freedom
# Null hypothesis probability = 7.915019e-01
Photon flux (15-150 keV) in 82.62 sec: 0.227434 ( -0.022605 0.022707 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.6113e-06 ( -1.57327e-07 1.581e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.120 sec. to 84.744 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.743235 ( -0.596817 0.738256 )
Epeak [keV] : 147.502 ( -58.4506 -147.503 )
Norm@50keV : 3.19389E-03 ( -0.00135802 0.00353608 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.54 using 59 PHA bins.
# Reduced chi-squared = 0.8311 for 56 degrees of freedom
# Null hypothesis probability = 8.120494e-01
Photon flux (15-150 keV) in 82.62 sec: 0.222820 ( -0.023458 0.023517 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.57516e-06 ( -1.68317e-07 1.66589e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 4.928 sec. to 5.928 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.82008 ( -1.08914 0.895222 )
Norm@50keV : 4.04773E-03 ( -0.00222224 0.00178186 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 83.46 using 59 PHA bins.
# Reduced chi-squared = 1.464 for 57 degrees of freedom
# Null hypothesis probability = 1.272842e-02
Photon flux (15-150 keV) in 1 sec: 0.562293 ( -0.211992 0.211564 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.72092e-08 ( -1.75004e-08 1.84145e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 4.928 sec. to 5.928 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.84136 ( -1.07525 0.918566 )
Epeak [keV] : 9999.36 ( )
Norm@50keV : 4.01861E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 83.47 using 59 PHA bins.
# Reduced chi-squared = 1.490 for 56 degrees of freedom
# Null hypothesis probability = 1.008958e-02
Photon flux (15-150 keV) in 1 sec: 0.450446 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
