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 -9.452 sec. to 151.488 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.22046 ( -0.145502 0.140353 )
Norm@50keV : 1.43908E-03 ( -0.00013652 0.00013494 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 76.97 using 59 PHA bins.
# Reduced chi-squared = 1.350 for 57 degrees of freedom
# Null hypothesis probability = 4.017857e-02
Photon flux (15-150 keV) in 160.9 sec: 0.240861 ( -0.016701 0.016717 ) ph/cm2/s
Energy fluence (15-150 keV) : 2.18396e-06 ( -1.75441e-07 1.78726e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -9.452 sec. to 151.488 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.47753 ( -0.539366 0.738502 )
Epeak [keV] : 26.9649 ( -24.9436 8.77593 )
Norm@50keV : 4.02604E-03 ( -0.00215977 0.00732385 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 72.46 using 59 PHA bins.
# Reduced chi-squared = 1.294 for 56 degrees of freedom
# Null hypothesis probability = 6.857729e-02
Photon flux (15-150 keV) in 160.9 sec: 0.232085 ( -0.017995 0.018045 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.99764e-06 ( -2.09479e-07 2.25447e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 41.948 sec. to 42.948 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.83044 ( -0.662951 0.603265 )
Norm@50keV : 5.15587E-03 ( -0.00193015 0.00176566 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.99 using 59 PHA bins.
# Reduced chi-squared = 0.8419 for 57 degrees of freedom
# Null hypothesis probability = 7.966765e-01
Photon flux (15-150 keV) in 1 sec: 0.719066 ( -0.208281 0.208742 ) ph/cm2/s
Energy fluence (15-150 keV) : 4.74308e-08 ( -1.65108e-08 1.7696e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 41.948 sec. to 42.948 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -2.58324 ( -0.114305 1.89249 )
Epeak [keV] : 196.700 ( )
Norm@50keV : 2.11850E-03 ( )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.30 using 59 PHA bins.
# Reduced chi-squared = 0.8446 for 56 degrees of freedom
# Null hypothesis probability = 7.897061e-01
Photon flux (15-150 keV) in 1 sec: 0.603780 ( ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
