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 1.200 sec. to 11.255 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.66413 ( -0.151263 0.148934 )
Norm@50keV : 4.87865E-03 ( -0.000423527 0.000419673 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.55 using 59 PHA bins.
# Reduced chi-squared = 0.9218 for 57 degrees of freedom
# Null hypothesis probability = 6.427192e-01
Photon flux (15-150 keV) in 10.05 sec: 0.640057 ( -0.053628 0.053765 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.55445e-07 ( -4.17063e-08 4.21158e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.200 sec. to 11.255 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.60478 ( -0.68993 0.593501 )
Epeak [keV] : 288.198 ( -320.856 -338.096 )
Norm@50keV : 5.23581E-03 ( -0.00174296 0.00519559 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 52.54 using 59 PHA bins.
# Reduced chi-squared = 0.9383 for 56 degrees of freedom
# Null hypothesis probability = 6.064731e-01
Photon flux (15-150 keV) in 10.05 sec: 0.638263 ( -0.056322 0.054971 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.53259e-07 ( -4.69878e-08 4.37521e-08 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 8.300 sec. to 9.300 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.94844 ( -0.318126 0.296698 )
Norm@50keV : 7.06194E-03 ( -0.00144904 0.00140051 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 70.38 using 59 PHA bins.
# Reduced chi-squared = 1.235 for 57 degrees of freedom
# Null hypothesis probability = 1.096476e-01
Photon flux (15-150 keV) in 1 sec: 1.03502 ( -0.171276 0.17137 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.4998e-08 ( -1.25632e-08 1.29042e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 8.300 sec. to 9.300 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.5486 ( -0.857413 2.13419 )
Epeak [keV] : 46.3103 ( )
Norm@50keV : 1.21297E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 70.14 using 59 PHA bins.
# Reduced chi-squared = 1.253 for 56 degrees of freedom
# Null hypothesis probability = 9.684204e-02
Photon flux (15-150 keV) in 1 sec: 1.02022 ( -0.181298 0.17842 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
