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 0.116 sec. to 0.300 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.713411 ( -0.174889 0.183223 )
Norm@50keV : 4.30052E-02 ( -0.00412786 0.00409354 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.28 using 59 PHA bins.
# Reduced chi-squared = 1.180 for 57 degrees of freedom
# Null hypothesis probability = 1.654564e-01
Photon flux (15-150 keV) in 0.184 sec: 0.263736 ( 0.087171 0.371427 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.60169e-08 ( -1.02859e-08 1.03944e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.116 sec. to 0.300 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.705769 ( -0.177173 0.184449 )
Epeak [keV] : 9999.32 ( -9999.36 -9999.36 )
Norm@50keV : 4.31478E-02 ( -0.00407084 0.0121222 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.37 using 59 PHA bins.
# Reduced chi-squared = 1.203 for 56 degrees of freedom
# Null hypothesis probability = 1.420749e-01
Photon flux (15-150 keV) in 0.184 sec: 4.96430 ( -0.45959 0.46212 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.65089e-08 ( -1.08647e-08 9.82402e-09 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.344 sec. to 0.656 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.712569 ( -0.200663 0.212582 )
Norm@50keV : 1.15558E-02 ( -0.00128457 0.00125679 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.45 using 59 PHA bins.
# Reduced chi-squared = 1.289 for 57 degrees of freedom
# Null hypothesis probability = 7.017479e-02
Photon flux (15-150 keV) in 1 sec: 1.33446 ( -0.13949 0.13999 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.40275e-07 ( -1.56945e-08 1.57772e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.344 sec. to 0.656 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.717036 ( -0.191368 0.226408 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 1.16716E-02 ( -0.00119875 0.00397014 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 73.52 using 59 PHA bins.
# Reduced chi-squared = 1.313 for 56 degrees of freedom
# Null hypothesis probability = 5.815002e-02
Photon flux (15-150 keV) in 1 sec: 1.33405 ( -0.13971 0.13978 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.40653e-07 ( 0 0 ) ergs/cm2
Time-resolved spectra
