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 -0.040 sec. to 24.136 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.76763 ( -0.127801 0.125577 )
Norm@50keV : 1.07370E-02 ( -0.000803917 0.000798789 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.26 using 59 PHA bins.
# Reduced chi-squared = 0.9870 for 57 degrees of freedom
# Null hypothesis probability = 5.029133e-01
Photon flux (15-150 keV) in 24.18 sec: 1.46146 ( -0.10936 0.10967 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.39374e-06 ( -1.83155e-07 1.84166e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.040 sec. to 24.136 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.38904 ( -0.434116 0.528142 )
Epeak [keV] : 80.8840 ( -23.2744 -80.884 )
Norm@50keV : 1.66689E-02 ( -0.00637165 0.0136086 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 54.41 using 59 PHA bins.
# Reduced chi-squared = 0.9716 for 56 degrees of freedom
# Null hypothesis probability = 5.353678e-01
Photon flux (15-150 keV) in 24.18 sec: 1.43344 ( -0.11482 0.11495 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.33866e-06 ( -1.96869e-07 1.96802e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 12.268 sec. to 13.268 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.0989 ( -0.447067 0.390241 )
Norm@50keV : 1.56193E-02 ( -0.00425371 0.00397937 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 60.94 using 59 PHA bins.
# Reduced chi-squared = 1.069 for 57 degrees of freedom
# Null hypothesis probability = 3.361801e-01
Photon flux (15-150 keV) in 1 sec: 2.45619 ( -0.53271 0.53402 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.45131e-07 ( -3.46189e-08 3.51168e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 12.268 sec. to 13.268 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.99131 ( )
Epeak [keV] : 5.12652 ( )
Norm@50keV : 1.72134E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 61.03 using 59 PHA bins.
# Reduced chi-squared = 1.090 for 56 degrees of freedom
# Null hypothesis probability = 3.001082e-01
Photon flux (15-150 keV) in 1 sec: 2.43566 ( -0.51309 0.52419 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
