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 -37.984 sec. to 66.492 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.56615 ( -0.0697265 0.0696076 )
Norm@50keV : 7.08294E-03 ( -0.000277723 0.000277562 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.66 using 59 PHA bins.
# Reduced chi-squared = 0.9064 for 57 degrees of freedom
# Null hypothesis probability = 6.748097e-01
Photon flux (15-150 keV) in 104.5 sec: 0.900935 ( -0.037814 0.037903 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.95322e-06 ( -2.87513e-07 2.88409e-07 ) ergs/cm2
Cutoff power-law model
Time interval is from -37.984 sec. to 66.492 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.3237 ( -0.263509 0.283515 )
Epeak [keV] : 146.524 ( -52.2495 -146.525 )
Norm@50keV : 9.27841E-03 ( -0.00227583 0.00333815 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 49.26 using 59 PHA bins.
# Reduced chi-squared = 0.8796 for 56 degrees of freedom
# Null hypothesis probability = 7.259644e-01
Photon flux (15-150 keV) in 104.5 sec: 0.888769 ( -0.039972 0.040049 ) ph/cm2/s
Energy fluence (15-150 keV) : 6.84867e-06 ( -3.11852e-07 3.1056e-07 ) ergs/cm2
1-s peak spectrum fit
Power-law model
Time interval is from 4.036 sec. to 5.036 sec.
Spectral model in power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -1.32693 ( -0.15999 0.161009 )
Norm@50keV : 3.83072E-02 ( -0.00409444 0.00409423 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 51.59 using 59 PHA bins.
# Reduced chi-squared = 0.9051 for 57 degrees of freedom
# Null hypothesis probability = 6.774949e-01
Photon flux (15-150 keV) in 1 sec: 4.59366 ( -0.51391 0.51483 ) ph/cm2/s
Energy fluence (15-150 keV) : 3.76166e-07 ( -4.22556e-08 4.23095e-08 ) ergs/cm2
Cutoff power-law model
Time interval is from 4.036 sec. to 5.036 sec.
Spectral model in the cutoff power-law:
------------------------------------------------------------
Parameters : value lower 90% higher 90%
Photon index: -0.578381 ( -0.636357 0.760423 )
Epeak [keV] : 105.254 ( -29.6808 238.001 )
Norm@50keV : 8.68738E-02 ( -0.0428435 0.108322 )
------------------------------------------------------------
#Fit statistic : Chi-Squared = 47.44 using 59 PHA bins.
# Reduced chi-squared = 0.8471 for 56 degrees of freedom
# Null hypothesis probability = 7.853494e-01
Photon flux (15-150 keV) in 1 sec: 4.55457 ( -0.51578 0.51671 ) ph/cm2/s
Energy fluence (15-150 keV) : 0 ( 0 0 ) ergs/cm2
Time-resolved spectra
