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 0.028 sec. to 0.284 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.663285 ( -0.305464 0.335935 )
Norm@50keV : 1.34372E-02 ( -0.00247389 0.00238228 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.27 using 59 PHA bins.
# Reduced chi-squared = 0.9170 for 57 degrees of freedom
# Null hypothesis probability = 6.527864e-01
Photon flux (15-150 keV) in 0.256 sec: 1.55815 ( -0.26271 0.26362 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.27021e-08 ( -7.45608e-09 7.49171e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.028 sec. to 0.284 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.655016 ( -0.385522 0.905086 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 1.35430E-02 ( -0.00248354 -0.0135439 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.28 using 59 PHA bins.
# Reduced chi-squared = 0.9337 for 56 degrees of freedom
# Null hypothesis probability = 6.162927e-01
Photon flux (15-150 keV) in 0.256 sec: 1.56577 ( -0.30199 0.28701 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.29921e-08 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.342 sec. to 0.658 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.08893 ( -0.350768 0.369445 )
Norm@50keV : 4.62007E-03 ( -0.00100124 0.00100004 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.42 using 59 PHA bins.
# Reduced chi-squared = 1.288 for 57 degrees of freedom
# Null hypothesis probability = 7.049367e-02
Photon flux (15-150 keV) in 1 sec: 0.535340 ( -0.118138 0.118562 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.84808e-08 ( -1.14196e-08 1.15826e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.342 sec. to 0.658 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.266332 ( -0.997703 1.90702 )
Epeak [keV] : 109.846 ( )
Norm@50keV : 1.16889E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.41 using 59 PHA bins.
# Reduced chi-squared = 1.293 for 56 degrees of freedom
# Null hypothesis probability = 6.911319e-02
Photon flux (15-150 keV) in 1 sec: 0.521224 ( -0.120644 0.120979 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.57267e-08 ( -1.27019e-08 1.26286e-08 ) ergs/cm2
Time-resolved spectra
