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 -0.704 sec. to 2.296 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.56336 ( -0.207184 0.194866 )
Norm@50keV : 5.07235E-03 ( -0.000733229 0.000731887 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.09 using 59 PHA bins.
# Reduced chi-squared = 0.8437 for 57 degrees of freedom
# Null hypothesis probability = 7.936561e-01
Photon flux (15-150 keV) in 3 sec: 1.03657 ( -0.085616 0.08566 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.54946e-07 ( -1.55019e-08 1.59966e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from -0.704 sec. to 2.296 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.98914 ( 1.98914 0.949356 )
Epeak [keV] : 0.653123 ( -0.20086 0.383844 )
Norm@50keV : 1.18170E-02 ( -0.00227228 0.00259049 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 48.21 using 59 PHA bins.
# Reduced chi-squared = 0.8609 for 56 degrees of freedom
# Null hypothesis probability = 7.610638e-01
Photon flux (15-150 keV) in 3 sec: 1.00872 ( -0.082315 0.08389 ) 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 0.296 sec. to 1.296 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.57555 ( -0.202037 0.189818 )
Norm@50keV : 9.22000E-03 ( -0.00131387 0.00130995 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 59.09 using 59 PHA bins.
# Reduced chi-squared = 1.037 for 57 degrees of freedom
# Null hypothesis probability = 3.991322e-01
Photon flux (15-150 keV) in 1 sec: 1.89872 ( -0.16001 0.16008 ) ph/cm2/s
Energy fluence (15-150 keV) : 9.42237e-08 ( -9.40141e-09 9.65584e-09 ) ergs/cm2
Cutoff power-law model
Time interval is from 0.296 sec. to 1.296 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.73153 ( -0.262732 1.16724 )
Epeak [keV] : 10.9689 ( )
Norm@50keV : 3.20696E-02 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 56.86 using 59 PHA bins.
# Reduced chi-squared = 1.015 for 56 degrees of freedom
# Null hypothesis probability = 4.426501e-01
Photon flux (15-150 keV) in 1 sec: 1.83877 ( -0.17071 0.16833 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
