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 -10.640 sec. to 17.088 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.1909 ( -0.158906 0.151425 )
Norm@50keV : 9.90969E-03 ( -0.00108751 0.00107329 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.96 using 59 PHA bins.
# Reduced chi-squared = 1.104 for 57 degrees of freedom
# Null hypothesis probability = 2.737814e-01
Photon flux (15-150 keV) in 27.73 sec: 1.63293 ( -0.12972 0.12975 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.58089e-06 ( -2.44316e-07 2.49326e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -10.640 sec. to 17.088 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.394127 ( -0.955561 1.18758 )
Epeak [keV] : 33.4651 ( -6.17062 4.63385 )
Norm@50keV : 0.123525 ( -0.123568 0.554638 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.28 using 59 PHA bins.
# Reduced chi-squared = 0.8979 for 56 degrees of freedom
# Null hypothesis probability = 6.901307e-01
Photon flux (15-150 keV) in 27.73 sec: 1.53113 ( -0.13655 0.13751 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.868 sec. to 1.868 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.02448 ( -0.409815 0.359672 )
Norm@50keV : 2.25215E-02 ( -0.00611301 0.00581383 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.39 using 59 PHA bins.
# Reduced chi-squared = 0.7787 for 57 degrees of freedom
# Null hypothesis probability = 8.884304e-01
Photon flux (15-150 keV) in 1 sec: 3.41709 ( -0.67917 0.67917 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.08022e-07 ( -5.06708e-08 5.25994e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.868 sec. to 1.868 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.82096 ( -0.303179 2.41434 )
Epeak [keV] : 35.6613 ( )
Norm@50keV : 2.97900E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 44.33 using 59 PHA bins.
# Reduced chi-squared = 0.7916 for 56 degrees of freedom
# Null hypothesis probability = 8.699873e-01
Photon flux (15-150 keV) in 1 sec: ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
