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 -16.968 sec. to 48.032 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.72243 ( -0.176664 0.172441 )
Norm@50keV : 2.12798E-03 ( -0.000234282 0.000231923 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 65.13 using 59 PHA bins.
# Reduced chi-squared = 1.143 for 57 degrees of freedom
# Null hypothesis probability = 2.149247e-01
Photon flux (15-150 keV) in 65 sec: 0.284882 ( -0.030017 0.030068 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.27875e-06 ( -1.45371e-07 1.46513e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -16.968 sec. to 48.032 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.02636 ( -0.70489 0.848624 )
Epeak [keV] : 66.5181 ( -16.5349 846.671 )
Norm@50keV : 4.96086E-03 ( -0.00280917 0.00874956 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 62.29 using 59 PHA bins.
# Reduced chi-squared = 1.112 for 56 degrees of freedom
# Null hypothesis probability = 2.624267e-01
Photon flux (15-150 keV) in 65 sec: 0.277758 ( -0.030995 0.030973 ) ph/cm2/s
Energy fluence (15-150 keV) : 1.21961e-06 ( -1.57398e-07 1.58779e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 1.032 sec. to 2.032 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.31771 ( -0.501334 0.552116 )
Norm@50keV : 6.26546E-03 ( -0.00184553 0.00183832 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.91 using 59 PHA bins.
# Reduced chi-squared = 0.8405 for 57 degrees of freedom
# Null hypothesis probability = 7.991073e-01
Photon flux (15-150 keV) in 1 sec: 0.749987 ( -0.236308 0.238766 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.16581e-08 ( -1.88131e-08 1.89484e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 1.032 sec. to 2.032 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32192 ( -0.49908 0.560655 )
Epeak [keV] : 9999.36 ( -9999.36 -9999.36 )
Norm@50keV : 6.28503E-03 ( -0.00183398 0.0638813 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.91 using 59 PHA bins.
# Reduced chi-squared = 0.8555 for 56 degrees of freedom
# Null hypothesis probability = 7.706874e-01
Photon flux (15-150 keV) in 1 sec: 0.751025 ( -0.238544 0.238207 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.17703e-08 ( -1.98147e-08 1.72757e-08 ) ergs/cm2
Time-resolved spectra
