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 -12.400 sec. to 54.888 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.851553 ( -0.19913 0.210162 )
Norm@50keV : 1.53258E-03 ( -0.000173097 0.000170094 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.78 using 59 PHA bins.
# Reduced chi-squared = 1.119 for 57 degrees of freedom
# Null hypothesis probability = 2.502981e-01
Photon flux (15-150 keV) in 67.29 sec: 0.175922 ( -0.019452 0.019577 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.17992e-06 ( -1.31315e-07 1.31892e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -12.400 sec. to 54.888 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.844738 ( -0.272217 0.519396 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 1.54295E-03 ( -0.000173613 0.000160214 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 63.80 using 59 PHA bins.
# Reduced chi-squared = 1.139 for 56 degrees of freedom
# Null hypothesis probability = 2.212563e-01
Photon flux (15-150 keV) in 67.29 sec: 0.175871 ( -0.019453 0.019534 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.18932e-06 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from -10.404 sec. to -9.404 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.30749 ( -0.564186 0.720879 )
Norm@50keV : 4.60667E-03 ( -0.00184327 0.00162289 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.24 using 59 PHA bins.
# Reduced chi-squared = 0.8113 for 57 degrees of freedom
# Null hypothesis probability = 8.450420e-01
Photon flux (15-150 keV) in 1 sec: 0.567275 ( -0.156022 0.160547 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.85693e-08 ( -1.74423e-08 1.74231e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -10.404 sec. to -9.404 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.293086 ( -0.6814 2.18567 )
Epeak [keV] : 1.00000E+04 ( -10000 -10000 )
Norm@50keV : 4.64380E-03 ( -0.00184693 -0.00464544 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 46.26 using 59 PHA bins.
# Reduced chi-squared = 0.8260 for 56 degrees of freedom
# Null hypothesis probability = 8.201719e-01
Photon flux (15-150 keV) in 1 sec: 0.567351 ( -0.157025 0.160115 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.80754e-08 ( 0 0 ) ergs/cm2
Time-resolved spectra
