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 13.956 sec. to 180.892 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.33101 ( -0.192527 0.181645 )
Norm@50keV : 8.06691E-04 ( -0.000104014 0.000102215 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.02 using 59 PHA bins.
# Reduced chi-squared = 1.088 for 57 degrees of freedom
# Null hypothesis probability = 3.018389e-01
Photon flux (15-150 keV) in 166.9 sec: 0.143466 ( -0.011754 0.011758 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.29451e-06 ( -1.30451e-07 1.34073e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 13.956 sec. to 180.892 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.99196 ( 1.99196 1.99196 )
Epeak [keV] : 0.922985 ( -0.361087 1.47496 )
Norm@50keV : 1.28516E-03 ( -0.000240734 0.000269017 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.30 using 59 PHA bins.
# Reduced chi-squared = 1.130 for 56 degrees of freedom
# Null hypothesis probability = 2.344792e-01
Photon flux (15-150 keV) in 166.9 sec: 0.141335 ( -0.011971 0.011087 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.2393e-06 ( -1.30823e-07 1.60921e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 65.640 sec. to 66.640 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.24339 ( -0.82823 1.08134 )
Norm@50keV : 3.03213E-03 ( -0.00110554 0.00110553 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.88 using 59 PHA bins.
# Reduced chi-squared = 0.8926 for 57 degrees of freedom
# Null hypothesis probability = 7.026515e-01
Photon flux (15-150 keV) in 1 sec: 0.358137 ( -0.358137 0.13841 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.04166e-08 ( -1.27175e-08 1.30334e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 65.640 sec. to 66.640 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.08324 ( -1.46294 1.97567 )
Epeak [keV] : 31.1796 ( )
Norm@50keV : 1.17099E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.56 using 59 PHA bins.
# Reduced chi-squared = 0.9029 for 56 degrees of freedom
# Null hypothesis probability = 6.801565e-01
Photon flux (15-150 keV) in 1 sec: 0.358639 ( -0.14005 0.137885 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.02489e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
