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 -9.912 sec. to 257.160 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.87738 ( -0.126093 0.122615 )
Norm@50keV : 1.41453E-03 ( -0.000115299 0.00011404 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.31 using 59 PHA bins.
# Reduced chi-squared = 1.146 for 57 degrees of freedom
# Null hypothesis probability = 2.102736e-01
Photon flux (15-150 keV) in 267.1 sec: 0.201091 ( -0.014329 0.014338 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.47388e-06 ( -2.8003e-07 2.83062e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -9.912 sec. to 257.160 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.89689 ( -0.529919 0.600785 )
Epeak [keV] : 50.1352 ( -7.29119 12.1333 )
Norm@50keV : 4.89185E-03 ( -0.00235378 0.00549502 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.31 using 59 PHA bins.
# Reduced chi-squared = 0.9698 for 56 degrees of freedom
# Null hypothesis probability = 5.391783e-01
Photon flux (15-150 keV) in 267.1 sec: 0.193435 ( -0.014831 0.014848 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.21206e-06 ( -2.97766e-07 3.07053e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.564 sec. to 2.564 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.91187 ( -0.636509 0.521688 )
Norm@50keV : 9.88488E-03 ( -0.00392955 0.00355764 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.84 using 59 PHA bins.
# Reduced chi-squared = 1.032 for 57 degrees of freedom
# Null hypothesis probability = 4.079551e-01
Photon flux (15-150 keV) in 1 sec: 1.42588 ( -0.42526 0.42525 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.09055e-08 ( -3.29092e-08 3.38156e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.564 sec. to 2.564 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.88843 ( -0.951249 1.73557 )
Epeak [keV] : 212.647 ( )
Norm@50keV : 1.01549E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 58.84 using 59 PHA bins.
# Reduced chi-squared = 1.051 for 56 degrees of freedom
# Null hypothesis probability = 3.717839e-01
Photon flux (15-150 keV) in 1 sec: 1.42220 ( -0.699479 0.42895 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
