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 -29.412 sec. to 55.692 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.62212 ( -0.308146 0.297102 )
Norm@50keV : 7.76377E-04 ( -0.000142727 0.000139601 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 74.42 using 59 PHA bins.
# Reduced chi-squared = 1.306 for 57 degrees of freedom
# Null hypothesis probability = 6.045512e-02
Photon flux (15-150 keV) in 85.1 sec: 0.100467 ( -0.0171172 0.017143 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.16382e-07 ( -1.19675e-07 1.2193e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -29.412 sec. to 55.692 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.42012 ( -0.500188 1.22892 )
Epeak [keV] : 138.857 ( -138.837 -138.837 )
Norm@50keV : 9.90803E-04 ( -0.00099085 0.00320361 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 74.31 using 59 PHA bins.
# Reduced chi-squared = 1.327 for 56 degrees of freedom
# Null hypothesis probability = 5.130064e-02
Photon flux (15-150 keV) in 85.1 sec: 9.96953E-02 ( -0.0175948 0.0175277 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.06903e-07 ( -1.28802e-07 1.28371e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 2.996 sec. to 3.996 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.30029 ( -1.2781 0.85848 )
Norm@50keV : 2.35046E-03 ( -0.00235018 0.00149808 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.91 using 59 PHA bins.
# Reduced chi-squared = 0.7353 for 57 degrees of freedom
# Null hypothesis probability = 9.328582e-01
Photon flux (15-150 keV) in 1 sec: 0.410871 ( -0.15897 0.158878 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.24657e-08 ( -1.13849e-08 1.29822e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 2.996 sec. to 3.996 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.86113 ( -0.019735 5.02802 )
Epeak [keV] : 277.565 ( )
Norm@50keV : 1.18843E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 41.32 using 59 PHA bins.
# Reduced chi-squared = 0.7378 for 56 degrees of freedom
# Null hypothesis probability = 9.288152e-01
Photon flux (15-150 keV) in 1 sec: 0.290645 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
