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 -22.252 sec. to 389.664 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.33698 ( -0.0477609 0.0479666 )
Norm@50keV : 3.67437E-03 ( -9.41332e-05 9.40437e-05 )
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#Fit statistic : Chi-Squared = 52.22 using 59 PHA bins.
# Reduced chi-squared = 0.9161 for 57 degrees of freedom
# Null hypothesis probability = 6.547072e-01
Photon flux (15-150 keV) in 411.9 sec: 0.441494 ( -0.012624 0.012664 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.48273e-05 ( -3.89795e-07 3.90159e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -22.252 sec. to 389.664 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.16078 ( -0.0953506 0.192315 )
Epeak [keV] : 275.321 ( -112.838 -275.321 )
Norm@50keV : 4.38647E-03 ( -0.000619908 0.000904371 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.56 using 59 PHA bins.
# Reduced chi-squared = 0.8849 for 56 degrees of freedom
# Null hypothesis probability = 7.157514e-01
Photon flux (15-150 keV) in 411.9 sec: 0.435907 ( -0.013802 0.01385 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.46832e-05 ( -4.19232e-07 4.17963e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 98.816 sec. to 99.816 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.12129 ( -0.0675631 0.0677749 )
Norm@50keV : 8.65484E-02 ( -0.00333714 0.00333618 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.60 using 59 PHA bins.
# Reduced chi-squared = 0.9931 for 57 degrees of freedom
# Null hypothesis probability = 4.898917e-01
Photon flux (15-150 keV) in 1 sec: 10.0608 ( -0.40083 0.4012 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.98918e-07 ( -3.78648e-08 3.7975e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 98.816 sec. to 99.816 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.83443 ( -0.259973 0.28013 )
Epeak [keV] : 234.260 ( -87.5664 765.689 )
Norm@50keV : 0.116145 ( -0.0260213 0.0372644 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 53.13 using 59 PHA bins.
# Reduced chi-squared = 0.9488 for 56 degrees of freedom
# Null hypothesis probability = 5.840350e-01
Photon flux (15-150 keV) in 1 sec: 9.93654 ( -0.41578 0.41626 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.88158e-07 ( -3.97007e-08 3.95472e-08 ) ergs/cm2
Time-resolved spectra
