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
Multiple GTIs in the spectrum
tstart tstop
-47.832000 -14.248800
-13.000000 60.180000
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.64852 ( -0.210702 0.206892 )
Norm@50keV : 9.03853E-04 ( -0.000117039 0.000115271 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.57 using 59 PHA bins.
# Reduced chi-squared = 1.080 for 57 degrees of freedom
# Null hypothesis probability = 3.157672e-01
Photon flux (15-150 keV) in 106.8 sec: 0.117968 ( -0.014025 0.014034 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.98051e-07 ( -1.22873e-07 1.24891e-07 ) ergs/cm2
Cutoff power-law model
Multiple GTIs in the spectrum
tstart tstop
-47.832000 -14.248800
-13.000000 60.180000
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.52044 ( -0.331816 0.879153 )
Epeak [keV] : 165.638 ( -168.314 -168.314 )
Norm@50keV : 1.06695E-03 ( -0.000273562 0.00226694 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.49 using 59 PHA bins.
# Reduced chi-squared = 1.098 for 56 degrees of freedom
# Null hypothesis probability = 2.859024e-01
Photon flux (15-150 keV) in 106.8 sec: 0.117433 ( -0.014384 0.014334 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.85158e-07 ( -1.47625e-07 1.34986e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 49.536 sec. to 50.536 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.10165 ( -0.870091 1.13578 )
Norm@50keV : 3.27518E-03 ( -0.00143824 0.00115349 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.11 using 59 PHA bins.
# Reduced chi-squared = 1.019 for 57 degrees of freedom
# Null hypothesis probability = 4.343542e-01
Photon flux (15-150 keV) in 1 sec: 0.379716 ( -0.379716 0.144199 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.42571e-08 ( -1.37474e-08 1.3735e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 49.536 sec. to 50.536 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -3.4503 ( 3.47771 2.92008 )
Epeak [keV] : 374.548 ( )
Norm@50keV : 3.00009E-04 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.26 using 59 PHA bins.
# Reduced chi-squared = 1.005 for 56 degrees of freedom
# Null hypothesis probability = 4.651030e-01
Photon flux (15-150 keV) in 1 sec: 0.160653 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 3.40942e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
