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 -0.280 sec. to 4.368 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.14808 ( -0.20185 0.206772 )
Norm@50keV : 7.06300E-03 ( -0.000776536 0.000774146 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.19 using 59 PHA bins.
# Reduced chi-squared = 0.9507 for 57 degrees of freedom
# Null hypothesis probability = 5.810726e-01
Photon flux (15-150 keV) in 4.648 sec: 0.823499 ( -0.094167 0.094455 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.38186e-07 ( -4.05086e-08 4.07675e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.280 sec. to 4.368 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.14334 ( -0.254709 0.531892 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 7.09869E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.21 using 59 PHA bins.
# Reduced chi-squared = 0.9680 for 56 degrees of freedom
# Null hypothesis probability = 5.430444e-01
Photon flux (15-150 keV) in 4.648 sec: 0.823353 ( -0.094198 0.094414 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.39505e-07 ( -4.8335e-08 4.58459e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -0.280 sec. to 0.720 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.36914 ( -0.396311 0.396304 )
Norm@50keV : 7.97515E-03 ( -0.00169539 0.00167233 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.32 using 59 PHA bins.
# Reduced chi-squared = 0.8829 for 57 degrees of freedom
# Null hypothesis probability = 7.219014e-01
Photon flux (15-150 keV) in 1 sec: 0.964655 ( -0.201014 0.201555 ) ph/cm2/s
Energy fluence (15-150 keV) : 7.75729e-08 ( -1.86044e-08 1.90233e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.280 sec. to 0.720 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.37622 ( -1.30509 0.912285 )
Epeak [keV] : 9999.34 ( -9999.36 -9999.36 )
Norm@50keV : 7.99273E-03 ( -0.00169588 0.0129964 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 50.33 using 59 PHA bins.
# Reduced chi-squared = 0.8988 for 56 degrees of freedom
# Null hypothesis probability = 6.883984e-01
Photon flux (15-150 keV) in 1 sec: 0.973763 ( -0.213955 0.248737 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.31345e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
