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 19.984 sec.
Spectral model in power-law:
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Parameters : value lower 90% higher 90%
Photon index: -1.80411 ( -0.211636 0.204628 )
Norm@50keV : 4.52042E-03 ( -0.00066312 0.000656076 )
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#Fit statistic : Chi-Squared = 85.90 using 59 PHA bins.
# Reduced chi-squared = 1.507 for 57 degrees of freedom
# Null hypothesis probability = 7.976503e-03
Photon flux (15-150 keV) in 19.98 sec: 0.623962 ( -0.084056 0.084184 ) ph/cm2/s
Energy fluence (15-150 keV) : 8.31372e-07 ( -1.22732e-07 1.24425e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.000 sec. to 19.984 sec.
Spectral model in the cutoff power-law:
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Parameters : value lower 90% higher 90%
Photon index: 0.822467 ( -1.2621 1.67557 )
Epeak [keV] : 47.0933 ( -5.88713 8.19485 )
Norm@50keV : 0.125599 ( -0.132555 0.915709 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.20 using 59 PHA bins.
# Reduced chi-squared = 1.236 for 56 degrees of freedom
# Null hypothesis probability = 1.107820e-01
Photon flux (15-150 keV) in 19.98 sec: 0.582741 ( -0.084875 0.085494 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.18201e-07 ( -1.10884e-07 1.20439e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.660 sec. to 1.660 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.70221 ( -0.289575 0.279337 )
Norm@50keV : 1.16238E-02 ( -0.00214908 0.00211531 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.82 using 59 PHA bins.
# Reduced chi-squared = 0.7862 for 57 degrees of freedom
# Null hypothesis probability = 8.791632e-01
Photon flux (15-150 keV) in 1 sec: 1.54503 ( -0.26861 0.26915 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.07622e-07 ( -2.04775e-08 2.07943e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.660 sec. to 1.660 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.767624 ( -1.04959 1.4888 )
Epeak [keV] : 60.7472 ( -14.4979 -60.7472 )
Norm@50keV : 3.72166E-02 ( -0.0372164 0.210476 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 42.75 using 59 PHA bins.
# Reduced chi-squared = 0.7634 for 56 degrees of freedom
# Null hypothesis probability = 9.036482e-01
Photon flux (15-150 keV) in 1 sec: 1.49998 ( -0.27391 0.27453 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.00425e-07 ( -2.20387e-08 2.2582e-08 ) ergs/cm2
Time-resolved spectra
