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 -0.384 sec. to 5.896 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.2761 ( -0.134947 0.13023 )
Norm@50keV : 6.27231E-03 ( -0.000522278 0.000514689 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 67.71 using 59 PHA bins.
# Reduced chi-squared = 1.188 for 57 degrees of freedom
# Null hypothesis probability = 1.568031e-01
Photon flux (15-150 keV) in 6.28 sec: 1.08187 ( -0.06517 0.06537 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.74886e-07 ( -2.54247e-08 2.5823e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.384 sec. to 5.896 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.98897 ( 1.98897 1.98897 )
Epeak [keV] : 1.60727 ( -0.56101 24.3379 )
Norm@50keV : 9.11556E-03 ( -0.00116876 0.00124246 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 68.02 using 59 PHA bins.
# Reduced chi-squared = 1.215 for 56 degrees of freedom
# Null hypothesis probability = 1.301760e-01
Photon flux (15-150 keV) in 6.28 sec: 1.07971 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 0.276 sec. to 1.276 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.06577 ( -0.150295 0.144621 )
Norm@50keV : 1.48119E-02 ( -0.00139548 0.00137035 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.45 using 59 PHA bins.
# Reduced chi-squared = 1.218 for 57 degrees of freedom
# Null hypothesis probability = 1.246878e-01
Photon flux (15-150 keV) in 1 sec: 2.29188 ( -0.16614 0.16628 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.37224e-07 ( -1.17048e-08 1.19077e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.276 sec. to 1.276 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.85118 ( -0.251885 0.636182 )
Epeak [keV] : 29.0318 ( -24.0065 -29.0322 )
Norm@50keV : 1.96577E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 69.03 using 59 PHA bins.
# Reduced chi-squared = 1.233 for 56 degrees of freedom
# Null hypothesis probability = 1.133859e-01
Photon flux (15-150 keV) in 1 sec: 2.26632 ( -0.17893 0.17664 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
