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 -6.512 sec. to 131.472 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.51567 ( -0.0811204 0.0808513 )
Norm@50keV : 2.02720E-03 ( -8.60568e-05 8.57587e-05 )
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#Fit statistic : Chi-Squared = 56.77 using 59 PHA bins.
# Reduced chi-squared = 0.9960 for 57 degrees of freedom
# Null hypothesis probability = 4.835136e-01
Photon flux (15-150 keV) in 138 sec: 0.254163 ( -0.01103 0.011061 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.64759e-06 ( -1.23354e-07 1.24005e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -6.512 sec. to 131.472 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.51321 ( -0.109659 0.196499 )
Epeak [keV] : 9999.28 ( -9999.29 -9999.29 )
Norm@50keV : 2.03302E-03 ( -8.41438e-05 0.0005145 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.79 using 59 PHA bins.
# Reduced chi-squared = 1.014 for 56 degrees of freedom
# Null hypothesis probability = 4.453514e-01
Photon flux (15-150 keV) in 138 sec: 0.255898 ( -0.007329 0.009332 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.66667e-06 ( -1.45402e-07 1.02432e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 2.300 sec. to 3.300 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.579819 ( -0.192157 0.204226 )
Norm@50keV : 8.86654E-03 ( -0.00111754 0.00109626 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.35 using 59 PHA bins.
# Reduced chi-squared = 1.076 for 57 degrees of freedom
# Null hypothesis probability = 3.229293e-01
Photon flux (15-150 keV) in 1 sec: 1.03784 ( -0.118919 0.11937 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.14506e-07 ( -1.32409e-08 1.32849e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.300 sec. to 3.300 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: 0.629883 ( -0.956167 1.26104 )
Epeak [keV] : 138.212 ( -39.1405 252.664 )
Norm@50keV : 2.64316E-02 ( -0.0150495 0.0481574 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.43 using 59 PHA bins.
# Reduced chi-squared = 1.008 for 56 degrees of freedom
# Null hypothesis probability = 4.586670e-01
Photon flux (15-150 keV) in 1 sec: 0.998446 ( -0.123435 0.123534 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.10365e-07 ( -1.45044e-08 1.42183e-08 ) ergs/cm2
Time-resolved spectra
