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 -1.424 sec. to 6.736 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.40043 ( -0.103983 0.104163 )
Norm@50keV : 1.57901E-02 ( -0.000952744 0.00095257 )
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#Fit statistic : Chi-Squared = 50.79 using 59 PHA bins.
# Reduced chi-squared = 0.8911 for 57 degrees of freedom
# Null hypothesis probability = 7.057564e-01
Photon flux (15-150 keV) in 8.16 sec: 1.92316 ( -0.12274 0.12301 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.24506e-06 ( -8.04519e-08 8.06845e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.424 sec. to 6.736 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.10461 ( -0.341897 0.439562 )
Epeak [keV] : 163.538 ( -67.6566 -163.538 )
Norm@50keV : 2.18320E-02 ( -0.0065832 0.0130122 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.22 using 59 PHA bins.
# Reduced chi-squared = 0.8789 for 56 degrees of freedom
# Null hypothesis probability = 7.273753e-01
Photon flux (15-150 keV) in 8.16 sec: 1.89858 ( -0.12706 0.12726 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.22693e-06 ( -8.53128e-08 8.47571e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.068 sec. to 1.068 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.14321 ( -0.129078 0.130175 )
Norm@50keV : 4.36651E-02 ( -0.00331107 0.0033054 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.75 using 59 PHA bins.
# Reduced chi-squared = 1.101 for 57 degrees of freedom
# Null hypothesis probability = 2.797050e-01
Photon flux (15-150 keV) in 1 sec: 5.08819 ( -0.40038 0.40112 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.50474e-07 ( -3.65792e-08 3.67291e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.068 sec. to 1.068 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.87885 ( -0.327243 0.551403 )
Epeak [keV] : 248.160 ( -248.16 -248.16 )
Norm@50keV : 5.71722E-02 ( -0.0160036 0.0409074 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.94 using 59 PHA bins.
# Reduced chi-squared = 1.106 for 56 degrees of freedom
# Null hypothesis probability = 2.724556e-01
Photon flux (15-150 keV) in 1 sec: 1.46068 ( -0.700342 0.42559 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.47208e-07 ( -3.75891e-08 3.74551e-08 ) ergs/cm2
Time-resolved spectra
