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 12.000 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -2.00658 ( -0.0889396 0.0872365 )
Norm@50keV : 1.03394E-02 ( -0.000542745 0.000538547 )
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#Fit statistic : Chi-Squared = 44.60 using 59 PHA bins.
# Reduced chi-squared = 0.7824 for 57 degrees of freedom
# Null hypothesis probability = 8.838785e-01
Photon flux (15-150 keV) in 12 sec: 1.55574 ( -0.07755 0.07778 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.14478e-06 ( -5.74237e-08 5.76833e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 12.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.54316 ( -0.344593 0.373479 )
Epeak [keV] : 46.7198 ( -14.1257 13.8705 )
Norm@50keV : 1.80587E-02 ( -0.00600144 0.0100411 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 39.17 using 59 PHA bins.
# Reduced chi-squared = 0.6994 for 56 degrees of freedom
# Null hypothesis probability = 9.573428e-01
Photon flux (15-150 keV) in 12 sec: 1.51356 ( -0.08305 0.08328 ) 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 2.000 sec. to 3.000 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.70236 ( -0.171496 0.167174 )
Norm@50keV : 1.75359E-02 ( -0.00184296 0.00182669 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 43.76 using 59 PHA bins.
# Reduced chi-squared = 0.7677 for 57 degrees of freedom
# Null hypothesis probability = 9.011565e-01
Photon flux (15-150 keV) in 1 sec: 2.33099 ( -0.23938 0.23981 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.62357e-07 ( -1.76998e-08 1.77954e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.000 sec. to 3.000 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.27586 ( -0.541474 0.704029 )
Epeak [keV] : 85.2615 ( -28.4787 -85.2615 )
Norm@50keV : 2.89180E-02 ( -0.0126487 0.03567 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.38 using 59 PHA bins.
# Reduced chi-squared = 0.7568 for 56 degrees of freedom
# Null hypothesis probability = 9.106095e-01
Photon flux (15-150 keV) in 1 sec: 2.29531 ( -0.2452 0.24533 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.1521e-07 ( -2.38029e-08 2.05213e-08 ) ergs/cm2
Time-resolved spectra
