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 0.568 sec. to 108.568 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.764703 ( -0.335202 0.374755 )
Norm@50keV : 5.23647E-04 ( -0.000103856 9.96412e-05 )
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#Fit statistic : Chi-Squared = 52.26 using 59 PHA bins.
# Reduced chi-squared = 0.9168 for 57 degrees of freedom
# Null hypothesis probability = 6.533286e-01
Photon flux (15-150 keV) in 108 sec: 6.02747E-02 ( -0.011179 0.0112597 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.70955e-07 ( -1.25545e-07 1.26458e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.568 sec. to 108.568 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -0.757519 ( -0.406674 1.08759 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 5.27466E-04 ( -0.000104003 -0.000527499 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.27 using 59 PHA bins.
# Reduced chi-squared = 0.9333 for 56 degrees of freedom
# Null hypothesis probability = 6.169408e-01
Photon flux (15-150 keV) in 108 sec: 6.08720E-02 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 6.76976e-07 ( -1.32494e-07 1.27057e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 7.568 sec. to 8.568 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.737404 ( -0.529493 0.673377 )
Norm@50keV : 3.75007E-03 ( -0.00122614 0.00109897 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.57 using 59 PHA bins.
# Reduced chi-squared = 1.150 for 57 degrees of freedom
# Null hypothesis probability = 2.040907e-01
Photon flux (15-150 keV) in 1 sec: 0.432321 ( -0.123471 0.124203 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.50236e-08 ( -1.30494e-08 1.32149e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 7.568 sec. to 8.568 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.758317 ( -0.507989 0.994819 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 3.80164E-03 ( -0.00107698 0.00898292 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.59 using 59 PHA bins.
# Reduced chi-squared = 1.171 for 56 degrees of freedom
# Null hypothesis probability = 1.784643e-01
Photon flux (15-150 keV) in 1 sec: 0.438677 ( -0.163896 0.152148 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.51606e-08 ( -1.67821e-08 7.50415e-09 ) ergs/cm2
Time-resolved spectra
