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 -1.748 sec. to 122.072 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.68358 ( -0.0394022 0.0393366 )
Norm@50keV : 1.07732E-02 ( -0.000219114 0.000219107 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 58.18 using 59 bins.
Reduced chi-squared = 1.0207
# Null hypothesis probability of 4.32e-01 with 57 degrees of freedom
Photon flux (15-150 keV) in 123.8 sec: 1.42275 ( -0.03406 0.0342 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.23672e-05 ( -2.56436e-07 2.56641e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -1.748 sec. to 122.072 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.3877 ( -0.164591 0.170709 )
Epeak [keV] : 114.047 ( -22.5842 70.8221 )
Norm@50keV : 1.46684E-02 ( -0.0022633 0.00278643 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 48.57 using 59 bins.
Reduced chi-squared = 0.867321
# Null hypothesis probability of 7.49e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 123.8 sec: 1.38528 ( -0.03908 0.03936 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.21172e-05 ( -2.91629e-07 2.90521e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 88.712 sec. to 89.712 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.90241 ( -0.101738 0.0993167 )
Norm@50keV : 2.74505E-02 ( -0.00189056 0.00187497 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 80.32 using 59 bins.
Reduced chi-squared = 1.40912
# Null hypothesis probability of 2.26e-02 with 57 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 3.94373 ( -0.24399 0.24413 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.52418e-07 ( -1.71353e-08 1.72379e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 88.712 sec. to 89.712 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.619354 ( -0.516689 0.589107 )
Epeak [keV] : 47.1456 ( -4.76258 6.4657 )
Norm@50keV : 0.143501 ( -0.069219 0.163836 )
------------------------------------------------------------
#Fit statistic : Chi-Squared 59.24 using 59 bins.
Reduced chi-squared = 1.05786
# Null hypothesis probability of 3.58e-01 with 56 degrees of freedom
Photon flux (15-150 keV) in 1 sec: 3.81466 ( -0.24913 0.24939 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.32049e-07 ( -1.82676e-08 1.86427e-08 ) ergs/cm2
Time-resolved spectra
